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In this third edition of " General and Practical Optics" 1 trust that some 
of the faults of previous editions will be found remedied. The subject-matter 
has been revised, condensed, rearranged, and rewritten, to some extent, 
and considerable fresh matter has been introduced. 

Although primarily intended as a textbook for candidates for the examina- 
tion of the Worshipful Company of Spectacle Makers, it is written also as a 
reference book for those engaged in spectacle work, for other students oi 
Optics, and as an introduction to the study of more advanced works. 

In previous editions I acknowledged my indebtedness to Dr. George 

Lindsay Johnson and to Mr. H. Oscar AVood. Here again, and to an increased 

'extent, I repeat my recognition of the invaluable co-operation of Mr. Wood 

in compiling and writing the subject-matter, and in revising and correcting 

the work. 

As stated before, I have endeavoured to cover, in this book and in " Visual 
Optics and Sight-Testing," all that is essential for the sight-testing optician. 



The French inch is divided into 12 lignes or lines, in which the diameter 
of the object-glass of ordinary opera glasses and small telescopes is expressed. 


6 7 8 

(approx.)f "Pi 15 " 

9 10 11 12 

20122 24 26 



I i 





36 38 

is 19 





21 22 

11 19 



24:25 26 

54 56 58 






;-;i i 


32 33 

•2 71 






37 38 39 40 

3 -, 90 


A a . 

.. alpha a 

I i 

. .. iota 



.. rho ...r 

B/3 . 

. beta ..J> 


.. kappa . 



.. sigma s 

ry • 

.. gamma g (hard) 


.. lamda . 



.. tan ...t 

AS . 

. . delta... d 




.. upsilon u or ij 

Ee . 

. . epsilon e (short) 


.. mi 



.. phi ...j>li 

7A ■ 

. . zeta ...: 

.. xi 


x x 

.. chi ...rA(hard) 

H,, . 

.. eta ...e 


.. omicron 

o (short) 


.. psi 

e<9 3 . 

.. theta th 




il CD 

. . omega o (long) 



I. LIGHT ------- 

















XIX. COLOUR ------- 








INDEX - ------ 






S. or 8ph. 

. . Spherical. 


• • • 

. Diopter. 

0. or Oyl. 

. . Cylindrical. 

+ , 

Ox., or Cvx 

Plus, Convex. 


. . Prism. 

~ » 

Gc, or One. 

Minus, Concave. 


. . Axis. 


» • * 

. Degree of deviation. 

J'c. or Peris. 

. . Periscopic. 

± 0} 


. Prism diopter. 

I'cx. or I'cnx. 

. . Periscopic convex. 


. . 

. Prism power. 

Pec. or Pcvc. 

. . Periscopic concave. 


• • • 

. Centrad. 

Dcx. or Dcvx. 

. . Double convex. 


• • • 

. Metran. 

Dec. or Dcvc. 

. . Double concave 



• • • 

. Infinity, a distance in- 

F. or P.F. 

. . Principal focal 


finitely great. 

or focus. 


. Combined with. 

F, and F., 

. . Anterior and 


fi or 

n . . 

. The index of refraction. 

focal distances or 

A o 

■ 8 .. 

. The difference between 


(applied to lines of the 

J\ or u J 
h or v S 

Conjugate focal distances 


or foci. 


• • • . 

. The ratio between the 


. . Object. 

dispersion and refrae 


. . Image. 

tion of a medium. 

Hor. or If. 

. . Horizontal. 


• • ■ 

. The ratio between the re- 

Ver. or V. 

. . Vertical. 

fraction and dispersion 


. . Meridian. 

of a medium. 



. . Metres. 

i in. 

. . Centimetres. 


. . Millimetres. 


. . Microns. 


. . Micromillimetros. 

Ft. or ' . 

.. Foot. 

Iil. or". 

. . Inch. 


. . Line. 


. . Degree. 


. . Minute. 

. . Second. 

*> or 1 /0 

. . Infinity, a number infin- 

itely ureal . 

or l/» 

.. Zero, a number infinitely 



. . Angle. 


. . Is to. 

'. '. • 

. . So is. 

. *. 

.. Therefore. 


. . Because. 


. . Varies as. 


. . Perpendicular to. 


. . Parallel to. 


. . 1 -tight angles to. 


. . (l'i) llai i<> of ciroumfer- 

ence to d-ameter. 

r or i> 
6 <f> 

-r- or I 

X 2 



II '.+ /> 



Any angles. 

Plus, addition. 

Minus, subtraction. 

Either + or - . 

Multiplied by. 

Divided by. 

The diffei'ence between. 

The square root of. 

The cube root of. 

The nth root of. 

x squared. 

x cubed. 

x raised to the power of a 
number equal to n. 

Bond or vinculum, show- 
ing that the numbers 
are to be taken to- 
gether. Is the same as 

Equal to. 

Greater than. 

Less than. 

For ophthalmic abbreviations and symbols, see " Visual Optics and Sight-Testing." 



iii i i 

Page 40, line 13, for A F B read A F B. 

fi k 

„ 41, line \\,for 112 = 13! — read h 2 = hj — 

f 2 fi 



10 5 

43, line 5, for hi x — read h : x — 

5 10 

t cos 1 t cos r 
55, line 22, fori! read t' = 

/A cos 1 /U. cos 1 

,, 65, last line but two, for Maddex read Maddox. 
,, 76, line 10, for Cx. a mi*/ a Cx. 
,, 94, line 5, for F = 20 cm read F = 40 cm. 
,, 144, line 3, for — 1/10 — (— 1/12) read — 1/12 — ( — 1/10). 
„ 184, in the formula for P 2) read 

¥0 = 

/*2 Q 

„ 193, line 19, for wave points read wave fronts. 

„ 229, line 14, for Fig. 239 read Fig. 242. 

,, 231, line 19, for angle read angles. 

„ 241, line 6, for case read cases. 

„ 259, line 6, for Fig. 288 and Fig. 289 read Fig, 278 and 279. 

„ 268, last line, for instances read distances, 

,, 272, line 40, for zero read unity. 

„ 279, line 25, for nickel read Nicol. 

„ 322, in Fig. 337, the rays V and R should be shown crossed in the 
second prism. 

General and Practical Optics. 






Light. — Everything seen is rendered visible by means of a form of radiant 

: ergy termed light. With the exception of certain manifestations such 

: fluorescence, phosphorescence, etc., all light has its source in bodies which 

3 in a condition of incandescence. The source of light itself may not be 

lible, but the reflected light by which objects — the sky, moon, trees, houses, 

';. — are seen, can invariably be traced to the sun, or to some artificial 

j irce of incandescence. 

It was once supposed that light was something which radiated from the eye 

the objects seen, and later it was thought to be due to minute corpuscles 

.ich proceeded from a visible object to the eye at great speed, but it is 

w accepted that light is due to vibrations set up in the luminiferous ether 

• the molecular agitations of an incandescent body. 

> Ether. — This is a medium believed to occupy the whole universe; it fills 
estial space, lies between the particles of the earth's atmosphere and 
ween the molecules and atoms of which solid and liquid bodies are com- 

'••ied, so that everything is saturated with it. A vacuum consists of ether. 

fj tle is known about its nature, its properties being chiefly negative, since 
jannot be appreciated by any of the senses. It has been concluded, 

' : vever, that it possesses density, rigidity and elasticity, properties enabling 

,,;o propagate transverse undulations or waves, generated by vibrations 
incandescent material bodies; these waves travel to an infinite distance 

"hout appreciable loss of energy. Ether is the connecting medium of the 

»verse, and it is due to its presence that material bodies are capable of 
ng on one another at a distance, and by which such forms of radiant energy 
ight, heat, actinism, magnetism, electricity, etc., are made manifest. 

Light Waves and Rays. — Every point L (Fig. 1) of a source of light 

erates an ethereal oscillation in every direction This forms a tiny 

aere, and according to the accepted theory of Huyghen, every point on 



the circumference of this sphere forms a new centre of disturbance which 
generates a fresh sphere, and each of these spheres again forms fresh ones, 
and so on. These spheres lie side by side overlapping each other, and, taken 
collectively, at any distance from the primary centre of disturbance, form 
a wave-front {abode). Each wave-front then forms a series of centres for 

Fig. 1 

the formation of a fresh row of spheres, whose diameter is equal to a wave- 
length. Although it is convenient to consider light as advancing in the 
form of a simple wave-front which forms part of an ever-enlarging sphere, 
yet in reality the process is exceedingly complex. 

The wave motion of the ether takes place in every plane and is always 
transverse, i.e. at right angles to the direction of propagation of the light. 
The ether particles themselves do not travel, but merely oscillate, much in 
the same way as the particles of water bob up and down when ripples arc 
formed on the surface; or as the vibrations travel along a rope when it is 

In every plane each successive wave-front may be considered as the 
crest (W or 2W), and the space between it and the next wave-front as the 
trough of a wave (%W or 1|JP). The length of these waves varies to some 
extent, as does also their frequency, or number of vibrations per second, 
such that V=LT, where V is the speed of the wave travel per second, L is 
the wave-length and T is the frequency. The frequency and the wave- 
length must be within certain limits in order that light, and not some other 
form of radiant energy, may result. 

The incandescence of the sun is, of course, the principal source from 
which light on the earth is derived. Impact, friction, electricity, chemical 
combination, combustion, in fact anything which causes increased molecular 
motion, also may give rise to light. 

Although light is propagated from a luminous point in a series of wave 
fronts, it is more convenient to consider the direction of propagation of any 
particular point on the main wave, which can be shown as a straight line. 
From the luminous point L (Fig. 1) the light radiates in every direction, and 
any line of propagation such as La, Lb, etc., is termed a ray of light. Thus 
" rays " are really the imaginary radii of the wave-fronts, and as such have 
no real existence. For diagrammatic purposes, however, their assumption 
is most useful, since they indicate the directions in which portions of the 
real wave-front are travelling. 


Light, Heat and Actinism. — When the temperature of a body is raised, 
the increased molecular activity causes a generation of ether waves which 
constitutes radiant heat. Their length is too great and their frequency too 
low to cause the sensation of light, and they are termed infra-red. If the 
temperature is raised still more, the activity is proportionally increased, so 
that the waves become shorter and the vibrations more rapid. Thus, when 
the temperature of a body reaches about 500° centigrade, it not only emits 
the relatively long waves of heat, but also the shorter waves of light. The 
longest light waves give rise to the visual sensation of red. On further 
raising the temperature of the body, still shorter waves are also produced 
which cause the sensation of various colours, violet resulting from the shortest 
visible waves. White is a sensation caused by the combined action of all 
waves ranging between red and violet, and is produced when the temperature 
reaches about 1000° G. 

Ether waves which are too short and whose vibrations are too rapid to 
cause the sensation of light are termed ultra-violet : they cause chemical 
action, and are said to be actinic. The difference between these three forms 
of radiant energy exists solely in the length of the waves. 

Density of Media. — The speed with which light travels within a certain 
medium depends on the nature of the latter or, more exactly, on the elasticity 
of the ether within it; thus light travels more slowly in a dense medium, 
i.e. one in which its component particles are crowded together like glass, 
than in a rare one, such as air. 

Velocity of Light. — Light travels in space (free ether) at about 186,000 
miles or 300,000 kilometres per second; in air its speed is practically the same 
although actually slightly less. The velocity is lessened in denser media, 
the decrease being roughly proportional to the density, although this is not 
invariably the case. Thus, in glass, the rate of progression is about one 
third less, and in water one fourth less, than it is in air. 

186,000 miles is a distance equal to about eight times the circumference 
of the earth at the equator, a journey travelled by light in one second. 
From the sun it takes about eight minutes to reach the earth, some 93 million 
miles distant. At this rate light travels six million million miles in a year, 
and the distance of a fixed star, being so enormous, is measured in light 
years, thus expressing the number of years the light from the star takes 
to reach the earth. A light year, termed a Per sac, is thus six billion 

In space — and practically so in air — all light waves travel with the same 
velocity, and therefore it follows that the short waves must have a higher 
frequency than the longer waves. It is only when light passes into material 
bodies, like glass or water, that the velocities of the various waves become 

Measurement of Light-Speed. — Following are four methods by which 
the velocity of light has been measured. 


Rdmer's Method. — One of Jupiter's moons m (Fig. 2) becomes eclipsed 
by the planet J every 48^ hours. At a certain period of the earth's annual 
revolution round the sun it is in opposition to Jupiter. If light were to 
travel instantaneously, the eclipse, and its observation by an observer on 
the earth, would occur simultaneously. The light, however, has to travel 

Fig. 2. 

from Jupiter to the earth before the eclipse can be seen. Let R and r be 
respectively the radii of the orbits of Jupiter and the earth round the sun. 
Then J E (i.e. R — r) is the distance the light has to travel at a velocity V. 
This time, therefore, will be (R— r)/V seconds after the eclipse has taken 
place. After six months the earth and Jupiter will again be in opposition, 
the earth now being at E' on the other side of the sun. The eclipse will 
therefore be observed (R + r)/V seconds after the occurrence, the difference 
between the two observations being equal to 2r=186 million miles. 

Romer observed that, as the earth moved from E to E', the observed 
time steadily exceeded the calculated time. Thus he found that an eclipse 
observed when the earth was at E' occurred 995 seconds later than when it 
was observed at E. Since the diameter of the earth's orbit is 186 million 
miles, V=186,000,000/995=186,000 miles per second (approx.). 

Bradley's Method. — The apparent direction of light from a star, owing 
to the earth's motion, makes an angle with its true direction. As the earth 
pursues its elliptical orbit round the sun it must move in an opposite direc- 
tion to that which it took six months before, so that a telescope directed to 




Fig. 3. 

a star somewhere along a line at right angles to the earth's motion must be 
pointed slightly in front of the mean calculated position at the first period 
of observation, and a similar distance behind at the second observation. 
The angle which the telescope makes between the calculated and the 
observed position is called the aberration of the star. 


Bradley knew the velocity of the earth's motion, he measured the angle 
of aberration, and from these data he proved the velocity of light to be, 


velocity of earth 18 miles 18 

-=180,000 miles per sec. 

tan of angle tan 20" -0001 

Bradley's method may be illustrated as follows; if a shot from a gun 
C (Fig. 3) be fired at a ship, moving at right angles to the direction of the 
shot, the latter will not pass through the ship at right angles to its line 
of travel, but obliquely as if the shot came in the direction of the dotted 
line C. 

Fizeau's Method. — Fizeau's method depends on the interruption of a 
beam of light by the teeth of a revolving wheel. The light from a source S 
(Fig. 4) — rendered convergent by a lens L — falls on a plane unsilvered 
mirror m which is inclined at 45° and situated between the lens and its 
focus F, the latter being at the teeth of the wheel. Another lens U, placed 
at its principal focal length on the other side of the wheel and in a line with 
the mirror, renders the light from F parallel. The beam of light is collected 
by a third lens L", situated at a distance (say four miles), and is brought to 
a focus on a spherical mirror M, from which it is reflected, so as to return 
along the same path, finally forming a real image at F which is viewed by 
the observer at E through an eyepiece. 

Fig. 4. 

Suppose the light escapes through the first gap while the wheel is turning 
slowly, then it will, after travelling eight miles, pass through the same 
opening and a flickering image is seen. If the speed is greater the second 
tooth blocks out the light, but if still greater the light passes through the 
second gap, the wheel having revolved one tooth while the light travelled 
eight miles, and so reappears to an observer at E. The speed of the wheel 
being further increased the light appears and disappears as an additional 
tooth or gap passes by before the light returns. The speed of the toothed 
wheel, the size of the teeth, and the distance between m and M being known, 
Fizeau, and later Cornu, who improved on the apparatus, found the velocity 
of light in air to be about 300,000 km. per second. 


Foucault's Method. — Light (Fig. 5) is passed through a slit S and a 
lens L on to a plane mirror M v whence the light passes to a concave mirror M 2 
placed at a distance equal to its radius. From M 2 the light is again reflected 
back to M x and retracing its path is partly reflected by the glass plate M 3 to 
the eye at T. If M, is then rapidly rotated it will have had time to turn 
through an appreciable angle during the time that the light has travelled 
from M , to M 2 and back again, so that it will not be reflected back to the 

Fig. 5. 

same spot on the mirror M 3 . Thus the image seen by the observer through 
the telescope will not be formed on the cross wires at a, but will be found 
shifted to some point b. If the speed be known at whicb the mirror M 1 
is rotated, and the distance which the light has to travel from M x to M 2 and 
back (which in this case is equal to eight yards) the velocity of light can be 
calculated by the displacement of the image from a to b as seen through the 
telescope T. 

Solar Light is a combination of seven distinct colours — namely, red, 
orange, yellow, green, blue, indigo, and violet. Some authorities omit 
indigo and consider the spectrum to consist of six main colours, and some 
even omit the yellow. The combination of these colours in correct proportion 
produces white light. 

Sunlight is said to consist of about 50 parts red, 30 parts green, and 
20 parts violet in 100, and has about 30 per cent, of luminous rays. Artificial 
light has a higher proportion of heat and red rays, and the proportion of 
luminous rays is much smaller, varying from 20 per cent, for electricity (arc), 
10 per cent, for oils and coal-gas, to 1 per cent, for alcohol. With the excep- 
tion of the electric arc and similar sources, artificial light is very deficient 
in actinic and violet rays. 

Cause of Colour.— Ethereal waves of certain length and frequency always 
produce a mental sensation of a definite colour, in a person of normal colour 
perception. Whether the length of the wave or its frequency, or both, 
give rise to the definite sensation, and whether the retina or the mind 
differentiates between the various waves, are points which are not yet pre- 


cisely settled. As before stated, red is produced by comparatively long waves 
of low frequency, the sensation of violet by short waves of high frequency, 
while the other colours are produced by wave-lengths and frequencies between 
these two. 

The Spectrum. — When sunlight passes through a dense medium, the 
shorter violet waves are more retarded and, if refracted, are bent to a greater 
extent than the longer red waves, so that the component colours become 
separated. The dispersed colours, caused by refraction of white light by a 
prism, can be seen on a screen as a bright-coloured band, called the spectrum, 
which contains the seven principal colours above mentioned. The various 
colours are not sharply separated, but merge so imperceptibly into one 
another that it is almost impossible to locate where one colour ends and 
another commences. The space in the spectrum, formed by a prism, occupied 
by the different colours varies with the refracting medium used for its pro- 
duction. In a solar spectrum, due to refraction by a given prism of flint 
glass, the red is somewhat crowded and the violet drawn out, but if it be 
divided into 100 parts the proportional space occupied approximately by the 
red is 30, by the green 25, and by the violet 45 parts, these three being the 
main colours seen. 

Fraunhbfer's Lines. — When a gas is. rendered incandescent, the spectrum 
of the light emitted by it consists of one or more isolated bright lines, on a 
dark ground, characteristic of the gas in question; this is known as a line 
spectrum. The solar spectrum is continuous ; it is a bright-coloured band 
crossed by dark lines known as the Fraunhofer lines, which are very numerous 
and of varying widths. They show absence of certain wave-lengths. 


Position in Spectrum. 

Metal or Oas producing the 




Red . . 

. . . 

Oxygen (0) 



Red . . 


Water vapour 



Red . . 






Hydrogen (H) 




. . 

Sodium (Na) 



Green . . 

. . 

Iron (Fe) Calcium (Ca) 



Blue -green 


Magnesium (Mg) 



Blue . . 





Dark blue 


Hydrogen Iron 



Violet . . 


Calcium (bright line) . . 


The experiments of Kirchhoff, Bunsen and Fraunhofer have proved that 
the flame of each element radiates characteristic wave-lengths which produce 
the bright lines of its spectrum, and that the vapour of this same element 
at a lower temperature transmits freely all wave lengths except those which 
it would itself give out if it were incandescent, and these waves it absorbs. 
Thus sodium or salt, if burnt in a Bunsen flame, emits monochromatio yellow 
light, and white light from a hotter source would be robbed of precisely the 



same colour, i.e. yellow, on its passage through a sodium flame. The dark 
absorption lines, of the solar spectrum, correspond to the bright lines of 
specific substances, and are the result of the absorption of certain wave- 
lengths from the hot nucleus of the sun by the relatively cooler layers of 
incandescent gases continually being ejected to form its outer envelope. 
Some of the Fraunhofer lines are due to certain unknown substances, while 
some are said to be due to absorption by the terrestrial atmosphere. Absorp- 
tion spectra can be produced experimentally. 

^L6LB C D 




Fig. 6. 

W ave-Lengtlis in fn/x. 

Number of Vibrations in 
Billions per Second. 


100,000,000 (100 mm.) 

Electrical vibrations (Hertzian 
waves). i ■; 

3,000,000 (3 mm.) 

Shortest are about 3 mm. 
Longest 1 metre to several miles. 



Longest heat waves measured by 
Langley by his bolometer. 



■ Infra-red spectrum 

Longest heat waves measured by 
Ruebens and Snow by fluor- 
spar prism and bolometer. 




Longest waves capable of being 

seen by the spectroscope, ac- 

cording to Helmholtz. 









Ordinary visible spoc- 









800 > 




Shortest waves visible according 
to Soret. 



Shortest waves visible according 

- Ultra-violet spectrum 

to Mascart. 



Shortest waves photographed 
through fluor-spar prism alone. 



Shortest wavos photographed by 
means of fluor-spar prism, 
vacuum camera and bromide of 
silver plate without gelatine. 

X and Rontgen Rays (?). 

Note. — In Britain a billion is a million millions. A micromillimetre /t/t = one- 
millionth part of a millimetre or the billionth part of a kilometre. A micron /i = one 
thousandth of a millimetre. In the U.S.A. a billion = 1,000 millions. 


The chief Fraunhofer lines are indicated by letters of the alphabet, and 
as they always correspond to rays of a definite wave-length, they form a 
convenient means of identifying any particular part of the spectrum. Fig. 6 
shows their approximate positions. 

The Visible and Invisible Spectrum. — In general, the spectrum within 
certain limits consists of the long infra-red (heat) waves, the luminous or 
visible portion, and the short ultra-violet (chemical) waves. Besides these, 
there are the long Hertzian (electrical) waves beyond the infra-red, and what 
are supposed to be the X rays beyond the ultra-violet, as shown in the table 
of wave-lengths. 

In addition to light and heat, it is obvious that light waves possess other 
properties, especially the chemical actions which occur in photography, 
bleaching, the generation of carbonic acid, and the formation of chlorophyll 
necessary for vegetable life, although *or the latter, the heat rays may be 
equally active or even more so. 

There is no sharp line of separation between the heat, light and chemical 
parts of the spectrum; the calorific effect of the red dies away gradually 
towards the more luminous portions, and as the latter fade away the actinic 
effect of the blue and violet increases. Only the central part of the spectrum, 
particularly the yellow, can be said to cause light only. 

The existence of the infra-red waves may be shown in various ways. 
Thus a blackened thermometer bulb placed just beyond where the red in the 
spectrum ceases will show a rise of temperature, proving the existence of 
heat rays. Again, by employing a lens made of rocksalt, which readily 
transmits the long heat waves, the latter can be demonstrated when the 
visible spectrum is cut off. 

The existence of the ultra-violet waves can be proved by placing beyond 
the visible violet a screen coated with a substance of a fluorescent nature 
which glows under the influence of the ultra-violet light. A quartz prism, 
which is very transparent to the short vibrations, must be used to produce 
the spectrum. 

Speed and Frequency of Light. — The visible spectrum consists of those 
light waves whose lengths vary approximately between 750 and 400 /x/t, and 
whose vibrations respectively vary between 400 and 750 billions per second. 
The speed of light in air is 300,000 kilometres per second, and if we express 
the length of the waves in billionths of a kilometre, that is, in /a/k, and the 
frequencies in billions per second, then by dividing 300,000 by the wave- 
length in fifj. the number of billions of frequencies per second for any kind of 
light is obtained. The wave-length multiplied by the frequency of any part 
of the spectrum is a constant, i.e. LT=V=300,000. 

In the yellow, which is the most luminous part of the solar spectrum, the 
number of billionths of a kilometre of the wave-length is approximately 
equal to the billions of frequencies per second. The mean refractive index 
of glass, or any other substance, is expressed by that of yellow light (the 
D line). 


Luminous Bodies. — Light is termed incident when it falls on a body. 
A body is luminous when it is, in itself, an original source of light. Every 
visible body, which is not in itself a source of light, is illuminated by the 
light it receives from a luminous source, but it is convenient to consider that 
every visible body is luminous, since light is radiated from every point of it. 
The rays diverging from these points travel without change so long as they 
are in the same medium. 

Transparency, Opacity and Translucency. — A body is transparent when 
light passes freely through it, with a minimum of absorption or reflection, 
such as clear glass. It is opaque when all the rays of light, incident on it, 
are either absorbed or reflected, so that none traverse it. It is translucent 
when it transmits only a portion of the light, as frosted glass and tortoise- 
shell. Much of the light incident on such a body is reflected, scattered or 
absorbed, so that objects cannot be seen clearly through it. 

Reflection. — Reflection is the rebound of light waves from the surface, 
on which they are incident, into the original medium. The reflection is 
regular from a polished surface and irregular from a roughened surface. 
Regularly reflected light causes the image of the original source of light to 
be seen, the reflecting surface being practically invisible, and is treated in 
Chapter III. 

Irregular Reflection.— When light falls on an unpolished surface such as 
white paper it is, owing to the irregular nature of the surface, incident at 
all conceivable angles, at each point of the surface. The incident light is 
broken up so that each point of the surface, giving rise to a fresh series 
of waves, becomes a source of light. No image is therefore formed either 
of the original source, or of any external object, but the diffused light diverg- 
ing in every direction renders the surface visible, no matter from what 
direction it is viewed, and it is either coloured or white according as some 
wave-lengths are, or are not, absorbed. 

Relative Transmission, Absorption and Reflection. — No substance is 
absolutely transparent, the clearest glass or water absorbing some of the 
incident light. It is estimated that below 50 fathoms the sea is dark, at 
least to the human eye, and even glass of sufficient thickness is opaque. 
Again any ordinary opaque object such as stone, metal, etc., may be ground 
or hammered into a sheet so thin asto permit the passage of some light through 
it. Thus gold leaf of sufficient thinness is translucent and transmits greenish 
rays. It follows, therefore, that transparency and opacity are relative, and 
depend not only on the nature of the medium, but also on its thickness. 

A body usually translucent may be rendered transparent by making 
it less capable of reflection. If a drop of Canada balsam be placed on a 
camera focussing-screen, and a cover-glass pressed over it, the screen becomes 
transparent there. The liquid fills the spaces of the rough surface and, 
being of the same index of refraction, converts the whole into a homogeneous 
body. Moistening a piece of paper with oil or water makes it much more 


translucent. The fibres of which the paper is made are optically denser than 
the air, so that, when the latter is replaced by oil or water, the two are more 
nearly alike and less light is scattered. The glass tube of a soda-water 
siphon is visible in the water, but if the water were replaced by oil of the 
same optical density as that of the tube, the latter would be invisible. 

Material, such as tracing paper or frosted glass, which is ordinarily 
translucent, becomes transparent when an object, such as print, is placed 
in contact with it, or has formed on it a real image. 

The rougher the surface, the greater is the proportion of irregularly 
reflected light; the smoother the surface, the greater that of regularly 
reflected light. The proportion of light regularly reflected from a partially 
roughened surface is increased as the angle of incidence of the light becomes 
greater, so that a reflected and fairly distinct image may be obtained with 
very oblique incidence of the light from a body which ordinarily gives no 
definite reflected image, as, for instance, polished wood. 

Total regular reflection never occurs, for even a silvered mirror or highly 
polished surface of metal fails to reflect all the light falling on it, but the 
proportion reflected by metallic surfaces does not vary so much with the 
incidence of the light as it does with glass. Polished silver reflects some 
90 per cent., polished steel some 60 per cent., and mirrors reflect from about 
70 to 85 per cent, of the incident light. Nor is there ever total irregular 
reflection; even fresh snow absorbs some of the light it receives. 

It is probable that the highest amount of diffusive reflection from a perfectly 
diffusive surface, as white blotting-paper, is greatest with normal incidence. 

Some of the incident light is reflected from the polished surface of a trans- 
parent body, and the proportion reflected varies with the nature of the body 
and with the angle of incidence, it being greater as such angle increases. 
The proportion reflected is very small (about 8 per cent.) when the light 
is incident perpendicularly, and it is almost totally reflected if the angle of 
incidence is nearly 90°. 

If with perpendicular incidence practically all the light is transmitted and 
none reflected, and if with an extremely oblique incidence (nearly 90°) prac- 
tically none is transmitted and all reflected, there must be some angle of 
incidence at which half the light is reflected and half transmitted and 
refracted. This occurs when the light is incident at about 70° with the 
normal to the point of incidence. Also the proportion reflected increases as 
the index of refraction of the medium is greater, and vice versa. If glass is 
dusty, the irregularly reflected light is increased and the glass becomes more 
visible. Scratches on a piece of glass roughen the surface and so tend to 
destroy its transparency by irregularly reflecting the light. If the scratches 
be multiplied indefinitely, the glass ceases to be transparent and becomes 

Thus, in the case of every transparent body, some of the incident light 
is always transmitted, some absorbed and some reflected. Of the light 
falling from all sides on to a piece of well-polished transparent glass, about 


75 per cent, is refracted and transmitted, 15 per cent, is regularly reflected 
and gives an image of the source from which the light proceeds, about 5 per 
cent, is irregularly reflected, and so makes the glass itself visible, while the 
remainder is lost, being absorbed and changed into heat, etc. 

Linear Propagation of Light. — The propagation of light is rectilinear, and 
the familiar instance of sunlight, admitted through a hole in the shutter into 
a darkened room, illustrates this fact by the illumination of the dust particles 
in the air along its path. The illuminated dust renders the course of the 
light visible, for light itself is invisible, unless directly received by the eye 
bo as to cause vision. 

Divergent Light. — In nature, light always diverges from luminous points. 

A sphere may be regarded as the common terminal of a multitude of 
straight lines diverging from a point. A wave-front as it advances is an 
arc of a circle of which the luminous point is the centre; the multitude of 
straight lines contained in the arc are rays of light which, diverging from a 
luminous point, form a cone, of which the point itself is the vertex, and 
such a collection of rays is called a pencil of light. From a luminant of 
sensible size an innumerable number of such cones of light diverge, all having 
as their common base the illuminated object itself. 

The divergence of the light is proportional to the angle included between 
the rays, proceeding from the luminous point, which fall on the outermost 
edges of the object; consequently the angle of divergence varies inversely 
with the distance between the source of light and the illuminated body, 
and directly with the size of the body. The latter is usually ignored, because 
it is a fixed quantity for any particular case. 

If the luminous point be very distant the angle of light divergence becomes 
so small that it may be ignored and the rays from that point considered 
parallel to each other; the luminous point is then said to be at infinity. A 
collection of such parallel rays is called a beam of light. 

Parallel Light. — If light from a distant point is regarded as parallel, and 
that from a near point as divergent, there must be some distance at which 
divergence can be assumed to merge into parallelism. In visual optics 
20 feet or 6 metres marks the shortest distance from which light is regarded 
as parallel, and this distance, or any beyond it, is regarded as infinity,, which 
is written thus: <x> . For some branches of optics a much greater distance 
is taken as the divergence limit. Thus in photographic optics it may amount 
to 100 yards or more, while in astronomy the nearest oo point may be taken 
as several miles. 

Convergent Light. — Light is never naturally convergent, but can be 
rendered so by means of a lens or reflector. A collection of convergent rays 
is also called a pencil of light; the apex of the pencil, towards which they 
are convergent, is the focus. Similarly, therefore, if light is converging to 
a focus a great distance off, it may be considered parallel; for visual purposes, 
such distance is 6 M. or more. 



Light Divergence. — If <5 is the angle of divergence, a the aperture of the 
lens, and d the distance of the source, the angular divergence of light is, 
with sufficient exactitude, found from tan 8—a/d. For example, suppose 
the source of light is at 6 M., and the pupil of the eye to be 3-5 mm. in 
diameter, then the angle of divergence will be 2', since 

tan 8z 


= -0006=tan 2'. 


A divergence of 2' is so small that it is negligible, and 6 M. considered 
the same as oo in this connection. At 20 cm., with the same pupil, the 
divergence of the light is 1°. 

As before stated, the size of the receiving body is usually ignored, it 
being taken to be uniform, or as unity, and if circular measure is substituted 
for angles, then the divergence of light is the reciprocal of the distance of 
the source, i.e. 1/d. 

Fig. 7. 

This is shown in Fig. 7, where the light from S has a divergence which 
varies inversely as the receiving surface is at a', a", or a'". 

Later it will be seen that the divergence of light enters into our calcula- 
tions for conjugate foci, and it is then expressed as \/f x or 1/u. 

Object and Image. — The source of the light is, in optics, commonly called 
the object. An image is the reproduction of the object due solely to light; 
it may be real, or only imaginary or virtual. 

Optics, the science treating of light and vision, includes Catoptrics, 
which deals with reflection from polished surfaces, and Dioptrics, which 
deals with refraction by transparent media. 



Shadows. — Since light travels in straight lines, any opaque body in their 
path will arrest their march and cast, on a screen behind it, a negative image 
of itself, called a shadow. When the ground on which the shadow is cast 
is at right angles to the central line connecting the source, the body and the 

Fig. 8. 

ground, the shadow has an outline corresponding to that of the body, because 
then, as in Fig. 8, the periphery of B cuts off the light equally in every direc- 
tion. The shape of the shadow otherwise depends on the inclination of the 
screen to the opaque body and the source of light. 

Fio. 9. 

In general the shadow (Fig. 9) exhibits a dark centre u u' called the 
umbra, from which the light is entirely cut off, and a less black outer portion 
Pu, P'u', called the 'penumbra, which receives a certain amount of illumination. 
The space Pu receives light from S', but none from S", while P'u' receives 
light from S", but none from S'. The area u u' receives light from neither 

S' nor S", 




If the light S is, or approximates to, a point, the shadow is mainly umbra 
and uniformly dark, as u u' in Fig. 8. It becomes larger as the shadow is 
further away. 

If S is of definite size (Fig. 9), but smaller than the intercepting body B, 
both the umbral and penumbral cones are divergent, and become larger as 
the shadow is further from B. 

When S and B are of equal size (Fig. 10), the umbra does not vary in 
size with its distance, but the penumbra increases as it is further away, 
because the penumbral cone diverges. 

When S is largei than B (Fig. 11), the umbra decreases with distance, 
since the umbral cone is convergent, while the penumbra increases, the 

Fig. 11. 

penumbral cone being divergent; beyond a certain point there is no umbra, 
as when the screen is at G C or beyond it at E E' . 

The penumbral cone is always divergent, but the umbral cone may be 
divergent, cylindrical, or convergent according as the source S is smaller 
than, equal to, or larger than the intercepting body B. 

When the hand is held close to a wall, in a well-illuminated room, the 
projected shadow is almost entirely umbra; as the hand is moved away the 
umbra decreases and the penumbra increases until, at a certain distance, 
the whole shadow becomes penumbral. The larger the size of the luminant 
as compared with that of the intercepting body, the smaller is the umbra, 
and the larger and fainter the penumbra, and vice versa. 



Except with a very small source, approximating to a point, the edge of 
a shadow is never cleanly defined, nor are the umbral and penumbral portions 
sharply separated, but merge imperceptibly into each other. Generally 
the brighter the light, the deeper is the shadow cast, for then the contrast 
between the illuminated ground and the part, from which the light is totally 
or partially obstructed, is greater than in a dull light, when shadows are 
barely perceptible. 

Calculations of Umbree and Penumbrse. — The calculations for determining 
the size of the umbra and penumbra are somewhat complicated and vary 
with the conditions under which the shadow is cast, so that every case must 
be worked out on its own merits, and from general principles. But if we 
assume that the size of the luminant is small compared with its distance from 
the intercepting body (and this is so in the great majority of cases), the 
necessary calculations can be much simplified. The angle subtended by the 
luminant at the intercepting body being small, either the edge or centre of 
the luminant (Fig. 12) may be assumed to be in line with either edge of the 
body, so that the edge of the geometrical shadow may be regarded as exactly 
bisecting the penumbral cone on either side. By the geometrical shadow is 
meant an imaginary space on the screen equal in size to the intercepting 

Fig. 12. 

In Fig. 12 let U be the size of the umbra, P that of either penumbral 
cone, T that of the total shadow, S that of the source of light, B that of the 
intercepting body. Let d 2 be the distance of S to B, and d 1 that of B to 
the screen C. Now the angle subtended by S at the edge of B equals the 
angle of the penumbral cone, so that 




so that 

U=B-2 P =B-P 



If P=B there is no umbra, and if P is greater than B, then U is negative. 

As an example, if S be a square window 2 ft. in diameter, the size of P 
and U on a wall 20 ft. distant, cast by a coin 1 in. in diameter held 1 ft . 
from the wall, would be thus — 


:l-26" 17=1 

T=l + l-26=2-26" 





Thus there is no umbra, it being a negative quantity, as on EE', Fig. 11. 
If the coin were 2 in. in diameter, the other conditions being similar, we 
should have 






T=2 + 1-26=3-26" 

Here the umbra is real or positive, as on P P\ Fig. 1 1 . 

When the angle a subtended by the luminant only is known, 

P=d 1 tan a 

Thus if B is 3" diameter, and 100" from a wall, S being the sun sub- 
tending an angle of 30', 

P=100 tan 30 '=100x -0087= -87" £7=3 - -87=2-13* 
T=-87 + 3=3-87". 


Fig. 13. 

Shadows cast on the Ground. — For the length of a shadow cast by a vertical 

narrow body on to a horizontal plane, generally a simple proportion suffices. 

For example, what is the length of the shadow cast by a stick 3 ft. long, 

20 ft. from a lamp post L whose lamp is 10 ft. above the ground ? Then, 

if the length of the shadow be T (Fig. 13), the horizontal distance to the end 

of the shadow is 20 + T, 

20 + T T 

that is, 

10 3 
60 + 3T=10T 
7T=60 and T=8-57 ft. 

Shadows cast by Lenses. — A lens or prism, when placed between a source 
and a screen, casts a shadow like an opaque body. The light transmitted 
by a concave lens is diverged so that a dark area, surrounded by a luminous 
zone, is thrown on the screen. A convex lens condenses on to a small area 
all the light passing through it. This bright area is surrounded by a dart 
one from which all light is excluded. If light be passed through a prism 
the space on the screen immediately behind it is dark, the light deviated 
by the prism falling on another part of the screen, which, being also illu- 
minated directly, exhibits there a bright area. 




Photometry. — The measurement of the luminosity of a light source, or of 
the illumination of a surface, is termed photometry, and the instrument or 
apparatus employed is called a photometer. 

Luminosity is the illuminating power of a light source; it is expressed 
in candle-foiver (C.P.), the latter unit being the luminosity of a standard 
candle, as described later. 

A luminous source, unless it be a point, has a definite area which is seldom 
of equal luminosity throughout. The quantity of light emitted varies at 
different points, but the sum of the light emitted is the total luminosity, 
and it is this which is measured or expressed in C.P. The intrinsic intensity 
of luminosity is the mean quantity of light emitted from a unit of surface, 
and is expressed by the total amount of light emitted divided by the area of 
the luminous source. 

Illumination is the amount of light received by an illuminated surface 
from a luminous source. The intensity of illumination is the amount of light 
which falls on a unit of the illuminated surface, and is expressed in foot- 
candles, the foot-candle (F.C.) being the luminosity of a standard candle at 
the unit distance of 1 foot. The term "foot-candles" expresses the luminosity 
of so many standard candles at 1 foot distance. 

Intensity of Illumination. — To illustrate how the intensity of illumination 
varies with the distance between a source of light and an illuminated area, 
suppose a candle flame to be at the centre of a sphere of one foot radius, 
and let the intensity of the light at the surface be considered unity. The 
area of a sphere is equal to i^x 2 , r being the radius. Now if the radius of 
the spherical envelope be increased from one foot to two feet, i.e. doubled, 
its area will be quadrupled, and therefore the available light is distributed 
over 4 times the area and the amount of light received on each point of 
the sphere is | of what it was when the radius was one foot. If the sphere 
be 5 feet in radius its area will be increased 25 times, and the available light 
on a given area is but ^s that of the first sphere. 

The Law of Inverse Squares. — Since a flat surface virtually forms a portion 
of a sphere having the source of light for its centre, it may also be stated, 
without much error, that the illumination of a flat surface varies inversely 
with the square of its distance from the source of light. 

This is illustrated in Fig. 14, where S is the source of light and A, B and 
C screens subtending equal angles, placed vertically at distances of 1, 2 and 


3 feet respectively. The same amount of light from S is received by all, but 
at B it is spread over 4 times and at C over 9 times the area that it is at A. 
It follows, therefore, that each unit of area of B receives £, and of C 
receives only ^ of the quantity of light received by each similar unit of A, 
practically the same as in the case of a spherical surface. The formula 
which expresses the intensity of illumination I in F.C. received by a surface 
at a given distance d from a souroe of given candle-power C.P. is 


This follows from the law of inverse squares above. 

For example, the illumination received by a surface 5 feet from a 100 C.P. 

lamp is 

T 100 100 t „ „ 

I— = =4 F C 

5 2 25 

Again, at what distance must a 32 C.P. lamp be placed above a table 
to give an illumination of 2 C.P. directly underneath ? 

n 32 
Here 2=^> 

whence d 2 =16 and d=4 feet. 

If at 1 foot a certain intensity of illumination is obtained from a lamp, 
and this be moved to, say, 9 feet, then the intensity becomes 1/9 2 =1/81 of 
the illumination received at one foot, and it will require 81 such lamps to 
obtain an equal intensity as at 1 foot. 

For equal illumination, the luminosity or C.P. of a source is directly pro- 
portional to the square of its distance from the surface. 

It should be noted that I does not depend on the colour or nature of 
the receiving surface, which might reflect much or little of the light it receives. 

A standard of illumination termed a lumen is that of an area of 1 square 
foot illuminated with an intensity of 1 foot-candle. 

Apparent Exceptions. — The law of inverse squares holds good only for 
light received directly on a screen, and not if it passes through a lens system 
so as to form an image, as in a camera or the eye. The light gained by 
bringing the object nearer is exactly neutralized by spreading it over a 
proportionately larger area in the image formed on the screen or retina. 

A luminous or illuminated surface appears equally bright at whatever 
angle it is seen, since, although it receives less light, the area perceived is 
correspondingly diminished. 

Obliquity of Surface or of the Light. — The intensity of illumination depends 
also upon the obliquity of the surface. It varies as the cosine of the angle 
of incidence of the light — that is, the angle that the rays make with the normal 
or perpendicular to the surface. 



In Fig. 15 S is a source, and AB is an illuminated surface tilted through 
the angle b. The angle of incidence is i, which the light from S makes with 
the normal NN', and it is obvious that the angles i and b are equal. 

Suppose parallel light to fall square upon the surface CB (Fig. 16) and 
the latter be then tilted into the position AB through the angle b, so that 
the angle of incidence is i. Then in the latter case only those rays between 

> 1 



D > 




Fig. 16. 

D and B will impinge on the screen, as compared with the full number between 
C and B before the screen is moved. The relative intensity of illumination 
of any point on AB as compared with CB is then 



=cos b. 

But &=t 

So that the full expression for illumination for all conditions is 

T C.P. 

I=-=S- cos % 

d 2 

For example, if a screen be tilted 60° with respect to the incident light, or, 
what is the same thing, the light falls upon it at an angle of incidence of 60°, 
the illumination is exactly one half, because cos 60°= -5. 

Calculations on Illumination. — A 30 C.P. lamp is 5 ft. above a table; then 
on the latter directly underneath 

L- lp —p-14F.C. 


At a point 4 feet away along the table the oblique distance of the lamp is 
d=V4 2 + 5 2 =V41=64 ft. 


CP. .30 5 „__ 

I=-^r- COS %=— X^-r=-6 F.C. 

d 2 41 6-4 

Here the actual value of i is not necessary, as its cosine is obvious. 

In Fig. 17 AC is a floor 20 ft. long, and S is a 100 C.P. lamp 7 ft. above 
A, the point directly underneath. What is the illumination at A, at B 
10 feet from A, and 20 ft. from A % 

At 4 

I=™=2 F.C. 

The oblique distance SB=VSA 2 + AB 2 =V7 2 +10 2 =12 ft. (approx.); and 
since the angle of incidence i^=ASB 

Therefore at B 

and at C 

. AS 7 

C0S l== SB=T2 

T 100 7 . _ _ . 

12 2 X 12 (approx.) 




7 2 + 20 2 V7 2 + 20 2 449 x 21 

•074 F.C. 

In the last example the angle of incidence is i'=ASC. 

In some cases, notably that in Fig. 17, the more obvious angles of obliquity 
of the light are a and b, i.e. those between the light and the illuminated 
surface itself. The same results as in the above examples can be obtained 
provided sin a be substituted for cos i, and sin b for cos i', the angles a and i, 
also b and i', being complementary. 

Photometric Standards. — The usual standard of luminosity in Great 
Britain is that given by a sperm candle | inch in diameter, | of a pound in 
weight, and burning 120 grains per hour. It has a variation of about 20 per 
cent. The luminosity of gas, with an ordinary burner, is from 12 to 16 
British candles (B.C.). 

There are various other photometric units, among them the following: — 

The " Pentane " standard. A mixture of pentane gas and air is burnt 

at the rate of £ cubic foot per hour; the flame is circular, 2 \ inches high 


and I inch in diameter, and there is neither wick nor chimney. Pentane 
is a volatile liquid, like naphtha, prepared from petroleum. The form 
designed by Vernon Harcourt is a 10 candle-power standard, and is largely 
used in this country. It is said to vary less than 1 per cent. 

The German standard is the Hefner- Alteneck lamp, called a " Hefner- 
lamp " (H), having a cylindrical wick 8 mm. in diameter burning amylacetate, 
the flame being 40 mm. high. It is correct to about 2 per cent. 

The French " Carcel " is a lamp of special construction burning 42 grammes 
of colza oil per hour. 

The " Violle " or absolute unit was the standard invented by M. Violle, 
and adopted at the International Congress at Paris in 1884. It consists of 
the light emitted from a square cm. of platinum heated to its melting-point. 
Of all the standards it is the most exact and reliable, but it is expensive and 
difficult to apply. 

The International Congress of 1890 adopted as the standard the " Bougie- 
decimale " or decimal candle, the unit illumination of a surface being that 
produced by one bougie-decimal at one metre. 

The British candle and the bougie-decimal have about the same intensities. 
The " Carcel " equals about 9| candles, and the " Violle " about 20 candles. 
20 bougie-decimals=19-75 B.C.=22-8 Hefner=2-08 Carcel=l Violle. 

Measurement of Light Sources. — Photometry consists of making a com- 
parison of the unknown illuminating power of a source of light with that 
of a known source or standard. Direct comparison would be difficult, but 
the stronger light can be placed at a greater distance, where it produces 
an intensity of illumination equal to that of the standard at some shorter 
distance. The illuminating powers of the two sources are as the squares 
of the distances at which, on a given surface, they respectively produce 
equal intensities of illumination. If the luminosity of the unknown source 
be L and that of tbe standard C, and the distance of L be d 2 and of C be d x 



If a standard candle at 1 ft. and light at 4 ft. give equal intensity of 
illumination at some common point, then the greater luminant is 1 x4 2 = 
16 C.P., because 

1 12 1x16 

c = p or c= n~ =16 ap - 

Four candles 4 ft. from a screen have the same effect as one candle at 
2 ft., for 2 2 /4 2 =4/l6=l/4. 

The Rumford Photometer. — The shadow or Rumford photometer consists 
of a vertical white screen before which is placed a rod. The standard is 
placed (preferably at one foot) in front of the screen and the rod casts a 
shadow. The luminant (Fig. 18) to be measured is placed so far away that 



the shadow cast by the rod from its light is of equal intensity to that of 
the other. The space on the screen, occupied by the candle's shadow, 
is illuminated only by the light from the lamp, while that occupied by the 
lamp's shadow is illuminated only by the standard. It is these intensities 

Fia. 18. 

of illuminations that are actually compared, although apparently it is the 
shadows themselves. Tbe lights should be placed so that the two shadows 
lie near to each other without overlapping. The Iuminant measured is of so 
many candle-power according to the distance at which the shadow pertaining 
to it equals in depth that pertaining to the standard, for then L/d|=C/d2 

The Bunsen Photometer. — The grease spot or Bansen photometer consists 
of a screen of white paper, suitably mounted in a frame, on which there is 
a spot rendered semi-transparent by grease or oil. If the paper be viewed 
on the side remote from a Iuminant the grease spot looks lighter than the 

Fig. 19. 

Fig. 20 

balance of the paper, because more light penetrates (Fig. 19). Viewed from 
the other side, the grease spot looks darker, because less light is reflected 
from it than from the rest of the paper (Fig. 20). Used as a photometer, 
the screen is placed one foot from the standard, the light from which is 
totally reflected by the ungreased part of the screen and transmitted to a 
great extent by the grease spot. The Iuminant to be tested is placed on the 
other side of the screen at such a distance that the amount of light from it, 
transmitted by the grease spot, equals that passing the other way; then the 
paper appears of uniform brightness all over. If there were employed a 
•standard candle at one foot, then the candle-power of the light is equal to 
the square of its distance in feet from the grease spot. Otherwise, as before, 



Instead of moving the lights about these may remain fixed and the screen 
moved about between them in order to obtain a balance. 

The Slab Photometer. — The paraffin slab photometer consists of two thick 
slabs of solid paraffin separated by an opaque layer of tin foil. The two 
lights are placed one on either side, and their intensities are compared by 
viewing the sides of the two slabs simultaneously. This is also known as 
the Joly photometer. 

The Lummer-Brodhun Photometer. — This photometer is largely used in 
scientific laboratories, being accurate to about 1%. Its superiority over 
the Bunsen and some other photometers is due to the fact that, with these, 
the two images to be compared cannot be seen simultaneously. With the 
Lummer-Brodhun instrument one combined image is seen by one eye. 



Fig. 21. 

The instrument (Fig. 21) consists of a rail on which the two luminants 
L v and L 2 can be made to travel at right angles to the opaque screen A B, 
which is whitened on both sides. From A B the light is reflected to the 
two mirrors M y and M 2 and thence through the cube of glass C D made of 
two right-angled prisms cemented together, the hypothenuse of one of which 
is partly cut away. 

The observer looks through a short telescope placed in front of D. The 
light from L x which reaches the telescope passes through the central cemented 
portion of C and D, while that from L 2 is reflected from the peripheral 
portion of D. The two lights therefore enter the eye simultaneously as a 
circle from L y and as a ring from L 2 , as shown in the figure. The lights are 
moved to and fro along the rail until tli3 whole disc appears equally bright. 

The Simmance-Abady " Flicker " Photometer. — This consists essentially 
of a white circular disc or wheel, the edge of which is peculiarly bevelled by 
being " chucked " eccentrically at two positions with the turning tool set 


obliquely at 45°. Thus the periphery of the wheel, when revolved, presents 
a bevel of 45° on the one side, say the right, and no bevel on the left, then 
graduates to a knife edge, and finally to a bevel of 45° on the left and no 
bevel on the right. 

This wheel is so fixed in a box that part only of it projects, and imme- 
diately in front of it, but leaving its projecting portions unobscured, there 
is a sighting tube carrying a Cx. lens for magnifying purposes. The box 
contains a clockwork arrangement by means of which the wheel is made to 
revolve at a rapid speed. The box itself is fixed on a bar 60 inches long, 
scaled in terms of a standard candle, and along which the apparatus can be 
freely moved. 

The two luminants which are to be compared are placed one at each end 
of the bar, and the light from them falls on that part of the revolving disc 
which projects from the box. When the light falls on the bevelled edge at 
45° it is reflected, and, passing through the sighting tube, is seen by the 
observer. When incident on the unbevelled part of the disc, the light does 
not pass through the sighting tube, so that each luminant is alternately light 
and dark to the observer's eye, and both are light at the same time when the 
knife edge is immediately in front of the sighting tube. Then when the 
intensities are equal the light is absolutely steady, while it flickers when 
they are not. If there is flickering the apparatus is moved until this disap- 
pears, and the position is found where L/d|=C/df. The smallest alteration 
of the position of the apparatus towards either light causes flicker. The 
test is made more sensitive, and the point of balanced intensities more exactly 
located, when the speed of revolution of the wheel is lessened. The 
apparatus can be set obliquely for measuring lights at any angle, and one 
of its special advantages is mentioned in the next article. 

Photometry of Coloured Lights. — One of the great difficulties of photo- 
metry is the difference in the nature and colour of various lights; and the 
comparison or measurement of actually coloured or monochromatic lights is 
still more difficult, or rather impossible, by ordinary photometry. 

The eye, although fairly accurate in judging the difference of hue of 
two sources, is very deficient in the comparison of the relative intensities 
of two differently coloured lights. These difficulties seem, however, to be 
obviated by the Simmance-Abady photometer. Here the rapidly alternating 
light from the sources does not afford the eye sufficient time to appreciate 
the difference of colour, but only their difference of intensity, since the flicker 
depends on intensity of illumination on the two sides of the bevelled disc, 
and is independent of the colour of these illuminations. 

Therefore by the flicker photometer coloured lights, and therefore also 
the transmissive qualities of coloured and smoked glasses, can be compared 
and measured. By it also the illuminating power of daylight can be measured, 
as well as that of different sources of artificial light. Coloured lights may, 
however, be compared by occlusion, using for the purpose a series of properly 
graduated smoked glasses. 


Calculations in Photometry. — Having by means of a photometer made 
the intensities of illumination equal, the candle-power of the luminant is 
calculated from the formula 

T _Cd| 

L= dp 

When d x is unity or 1 foot of course no division is necessary, as the square 
of 1 is 1. Thus if the luminant at 5 feet is equal to a standard candle at 
1 foot, the former is of 5 2 =25 C.P. 

If the candle is at 2 feet and the luminant at 8 feet 


2 Z 4 

To compare the intensity of two sources L x and L 2 of different powers, 
if L x be 30 C.P. placed at 20 feet, while L 2 is 200 C.P. at 70 feet, their relative 
intensities are 

30 _ _ 200 

L 2 200 400 5 , 
so that -=_ x w=9 (appro*.). 

The relative distances for equality of illumination of two sources of 9 C.P. 

and 36 C.P. are as y9 : V36= 3 : 6 or as 1 : 2. 

What power lamp at 100 feet would give the same illumination as one 
of 1, COO C.P. at 30 feet? 

L 100 ° t inn 
or L=ll,lll. 

100 2 30 2 

At what distance should an arc lamp of 1,200 C.P. be placed so as to 
give an illumination three times as great as that of an incandescent light 
of 70 C.P. at 15 feet ? 

70 „ 1200 10 1200x225 , no . 
-x3=-^ ord 2 =- n - =1286 
15 2 d 2 70 x 3 

therefore d=Vl286=36 feet (approx.). 

Light Transmission and Absorption. — The transmission and absorption 
of light by smoke glass, frosted glass, etc., can be measured fairly closely 
by means of a simple photometer such as the Bunsen. Take any two sources 
of light, A and B. balance them photometrically in the usual way, and 
measure the distance d x in feet or inches of one of them, say B, from the 
screen. Then interpose the smoke glass to be tested between A and the 
screen, when it will be found necessary to withdraw B in order to secure 
a second balance; let this distance be d 2 . Then the relative intensities of 


illumination of A, with and without the smoke glass, are as df : d|. so 
that the proportion transmitted is 

df or d| '"■ 

Therefore the proportion cut out is 

df • lOO(dj-df) 
^df ° r df /o - 

If the first distance d x is unity there is transmitted by the glass 

1 100 
dl ^ df /o - 

1 lOO(df-l) _. 
And there is cut out 1 — y 2 - or -^ y . 

It will be noticed that only B is moved, A remaining fixed; nor does the 
actual distance of the latter from the screen affect the result. The smoke 
glass should be sufficiently large to cover the light completely, and be close 
to it, although its position between A and screen is immaterial. 

Example: — If B, when at 2 ft., balanced A, and had to be moved to 3 ft. 
when a smoke glass was placed before A, then the light transmitted by the 
glass is 

d 2 2 2 4 

4 5 

And that blocked out is 1 - -=- or 55 %. 

Coloured Glasses. — To measure the absorptive or transmissive power of a 
coloured glass the method described above can be employed, but, for the 
reason given previously, ordinary artificial lights, which are generally white 
or yellowish, cannot be employed alone. To overcome this difficulty the 
following procedure may be followed. Suppose the glass to be measured 
is green. Place over A and B a green glass lighter in tint than the one to 
be measured; this renders the light uniform, though duller, and the necessary 
measurements can then be carried out as for neutral glasses. This subject 
is further discussed in Chapter XIX. 



A normal is a straight line perpendicular to a given point, as P C in 
Fig. 22. The angle of incidence is that which an incident ray makes with 
the normal at the point of incidence. 

Regular Reflection. — When light falls on a smooth surface it is reflected 
in definite directions according to the following laws: — 

(1) The incident and reflected rays are in the same plane as the normal to 
the point of incidence, but on opposite sides of it. 

(2) The angle of reflection is equal to the angle of incidence. 

Fig. 22. 

Oblique Incidence. — In Fig. 22, A B is a reflecting surface at which the 
ray I C is incident at the point C, and reflected in the direction G R. P C is 
the normal to A B at C, and the angle of reflection R C P is equal to the 
angle of incidence I CP. The perpendicular divides equally the angle I C R 
between the incident and reflected rays, and all three lines are in the plane 
of the paper. 

Perpendicular Incidence. — If the ray be incident in a direction P C normal 
to the surface the angle of incidence is zero, and therefore the angle of reflec- 
tion is also zero; the ray is thus reflected back along its original path. 

Images. — An image of a point is formed when the light, diverging from 
it, is caused, by reflection or refraction, to converge to, or to appear to diverge 
from, some other point. An image is said to be real or positive when the 
reflected or refracted rays from the original object-point are made to converge 
and actually meet in the image-point. If the original rays, after reflection or 
refraction, are divergent, they are referred back by the eye to an imaginary 
image-point, and the latter is then said to be virtual or negative. Similarly 



the real or virtual image of an object is made up of the real or virtual 
images of its innumerable points. 

A real image can be received and seen on a screen, or it can be seen in the 
air, where it actually exists. A virtual image cannot be formed on a screen; 
it is only mentally conceived where it appears to be. 

Mirror. — A mirror is an opaque body with a highly polished surface. It 
is usually made of glass backed by a film of mercurial amalgam, or coated 
with an extremely thin layer of silver. It may also be made of polished 

Reflection by Plane Mirror. — If a beam of parallel light falls on a plane 
mirror, all the rays, having similar angles of incidence, are reflected under 
equal angles, and are therefore reflected as parallel light. If a pencil of 
divergent rays be thus incident, after reflection they are equally divergent, 
and appear to come from a point as far behind the mirror as the original 
luminous point is situated in front of it. Accordingly, if an object stands in 
front of a plane mirror the rays, diverging from each point on it, are reflected 
from the surface of the mirror and enter the eye of an observer as so many 
cones of light diverging from so many points behind the mirror, and these 
points, from which the light appears to diverge, constitute the virtual image 
of the original object. The complete image is erect and corresponds exactly 
as regards shape, distance, and size to the object itself, the relative directions 
of the rays from each point on the object being unchanged by reflection. 

If the object is parallel to the surface of the mirror the image is also 
parallel; if the object is oblique to the surface the image forms a similar 
angle with it. 



Fig. 23. 

Construction of Image. — The image can be graphically constructed by 
drawing straight lines from the extremities of the object, perpendicular to the 
mirror or plane of the mirror, and continuing such lines as far behind the 
mirror as the object-points are in front of it. Thus, in Fig. 23, if a line be 
drawn from B to B', another from A to A', and B f and A' be connected, the 
image B' A' is obtained. Rays diverging from A, after reflection, enter the 
eye E, and are projected to a virtual focus at A', from which point they 



appear to diverge. Those from B are projected to B', so that A' B' is the 
virtual image of A B. A* is apparently as far behind M M as A is in front 
of it; so also B and B' are equally distant from M M. 

Lateral Inversion by Reflection. — The image is, however, laterally 
inverted, the right hand of a person becoming the left of his image in the 
mirror, and vke versa. If the eye regards A B (Fig. 23) directly, A is to 
the right of A B, but looking into the mirror A' is seen to the left of A' B' '. 
If the top of a page of printed matter be held obliquely downwards against 
a mirror the letters will be in their true order from left to right, but they will 
be upside down. If held bottom downwards the print is upright but reversed 
right for left. Engravers sometimes use a mirror in front of the letters or 
objects they wish to draw on a wood-block and copy the image as seen in 
the mirror. On taking an impression of the block the letters or objects are 
in their right position. 

Distance of Image. — If a person stands in front of a plane mirror, say at 
2 ft., and looks into it he sees an image of himself at a distance of 4 feet. 
If an object is placed in contact with a glass mirror its image appears behind 
the silvered surface, and only twice the thickness of the glass itself separates 
object and image, although the image appears rather nearer owing to vertical 
displacement by refraction. If the mirror is of polished metal the two are 
in contact. 

As in the case of any transparent dense medium, the apparent thickness 
of a mirror is less than its actual thickness, and the apparent thickness is de- 
creased with increased obliquity of view. 

Fig. 24. 

Fig. 25. 

Position of Image. — Since the angle C M, between the minor H M 
and the object G (Fig. 24) and the angle I C M, between the mirror and 
the image C I, are equal, it follows that the angle C I between the object 
and the image is twice as large as either; therefore if the mirror be placed 
at an angle of 45° with the object, the object and image are at right angles 
to each other, as is shown in Fig. 25. 

Angular Displacement of Image. — If a mirror be turned through any 
angle the image will move through twice that angle. The angles of incidence 
and reflection being equal, the total angular distance between the incident 



and reflected rays is twice the angle of incidence. If the latter be increased 
or decreased, by rotation of the mirror, any reflected light must turn through 
twice the angular displacement of the mirror, and travel at twice the angular 
speed. This fact is allowed for in the construction of the sextant (q.c). 
In the reflecting galvanometer it doubles the delicacy of the readings. 

Size of Mirror. — The smallest plane mirror which will enable a person to 
see his whole image reflected is one which is about half his height. More 
precisely the top of the mirror should be on a level with a point midway 
between the eyes and the top of the head, also it must be half the breadth, 
one eye being closed, but can be rather less if both are open. 

To see in a mirror the whole of a test chart placed over one's head, the 
size of the mirror should be one half that of the chart in both dimensions; 
for other distances of object and observer see page 301. 

Multiple Images. — When there is but one reflecting surface, as in a metal 
mirror, there is but one image, but in a glass mirror having two reflecting 
surfaces, namely, the front surface of the glass A C (Fig. 26) and its silvered 
back surfaced D, there are multiple images of an object. If a candle flame 
be held near to a glass mirror a series of images will be seen by an eye E; 
the first image I v that nearest to the candle, is formed by direct reflection 

r 2 

,'d# d' 

Fig. 26. 


Fig. 27 

from the front surface to the glass along a E; the second image I v which 
is the brightest, is directly reflected from the silvered surface along e E. 
The other images I 3 , 7 4 , etc., equally distant from each other, are formed 
by repeated internal reflection, between the silvered surface and the front of 

the glass, but some of the light escaping by refraction at e, d , after each 

reflection, the images become progressively fainter. 

Ordinarily on looking into a mirror only two images are noticeable, the 
faint one reflected from the front and the bright one from the back surface 
(Fig. 27), 'but the more oblique the line of view and consequently the greater 
the angle of incidence of the light to the mirror, the greater is the separation 



and number of images seen. The total number visible also depends, of 
course, on the luminosity of the flame. 

When the surfaces are truly parallel, and the view is direct, only one image 
is seen, because the multiple images all lie one behind the other in a straight 
line perpendicular to the mirror. 



Fig. 28. 

in v 


Parallel Mirrors. — If two plane mirrors M and M' (Fig. 28) are parallel 
to each other, and an object is placed between them, a series of images 
(the first of which are I and I'), theoretically infinite in number, is produced 
by reflection of the light backwards and forwards between the two mirrors. 
As with the single mirror, the repeatedly reflected light soon becomes feeble 
and the number of images actually visible depends, therefore, on the bright- 
ness of the object. True parallelism of the mirrors is indicated by the 
images forming a straight line. 


Fig. 29. 

Inclined Mirrors. — When two mirrors A M, B M are mutually inclined 
(Fig. 29), the multiple images formed are situated on an imaginary circle 
passing through the object, the radius of which is equal to the distance of 
the object from the junction of the mirrors. The number n of images 
produced, including the object itself, is 



or, the number of images, including the object, being known, the angle can 
be calculated. 



Thus, if the angle is 90° there are four, if 60° there are six, and if 45° 
there are eight images. A single mirror may be regarded as two inclined 
to each other at an angle of 180°; there are then two images, or rather, the 
object itself and its single image in the mirrors. If two mirrors are parallel 
the angle between them is zero, and the number of images is therefore 
360/0= oo, although, as stated, comparatively few are visible to the eye. 

When the number of degrees between the mirrors is an exact even divisor 
of 360, as 45° or 60°, the complete figure is symmetrical from every point of 
view; if the number is an exact odd divisor of 360, such as 120° and 72°, 
the figure is symmetrical or not according to the point of view and position 
of the object. If the number is not an exact divisor of 360, the figure is 
asymmetrical, as some of the images are either incomplete or overlapping. 
Whether the mirrors are precisely at right angles, etc., can therefore be deter- 
mined by the symmetry of the images formed. 

The kaleidoscope (q.v.) is an instrument formed of inclined mirrors. 

Construction of Multiple Images. — To find by construction the images 
formed by inclined mirrors, let M A and M B (Fig. 29) be the mirrors at any 
angle, and the object between them. With M as centre and M O as radius, 
describe a circle; measure off A I t equal to O A, and B I 2 equal to B; 
measure off A 7 3 equal to A I 2 , and similarly B 7 4 equal to B l v Then take 
A I 5 equal to A 7 4 , and so on until two images coincide or overlap. 

Curved Mirrors. 

Spherical Mirrors. — A spherical mirror is a portion of a sphere, the cross 
section of which is an arc of a circle; its centre of curvature is the centre of 
the sphere of which it forms a part. It may be either concave or convex, and 
can be considered as made up of an infinite number of minute plane mirrors, 
each at right angles to one of the radii of the sphere. 



Fig. 30. 

Fig. 31. 

Concave Mirror. — Let AB be a concave mirror (Fig. 30) and C its centre 
of curvature. Then all straight lines drawn from C to any part of AB being 
radii, they are all cf equal length and perpendicular or normal to the surface 
of the mirror, AH rays, therefore, starting from C, on reaching the surface 



of the mirror, will be reflected back along the same paths, and form an image 
at the same point C. 

The exposed surface A B is the aperture, in the centre of which is the 
vertex D. The line passing through G and D is the principal axis : all other 
lines passing through C to the surface are secondary axes. 

If a luminous point (Fig. 31) be infinitely far away, on the principal axis, 
the angle of divergence being very small, the rays are considered parallel to 
each other and to the principal axis. Let A' A, B'B, D'D, etc., be such 
rays, and let G A, C B, and G D be joined; then, since these latter are radii, 
they each form right angles at A, B and D respectively, with the surface of 
the mirror. Therefore A C is a normal to the surface at A, and the ray A' A 
will be reflected to F f making the angle of reflection F AC equal to the angle 
of incidence A' A G. All the other rays, in the same way, are, provided the 
aperture is not too great, reflected to F, which is the common image of a 
single luminous point situated at oo. F is the principal focus of the mirror, 
and the distance D F is the principal focal distance ox focal length, which is 
equal to half the radius D C. 

A Cc. mirror therefore renders parallel light convergent, and since the 
image can be received on a screen, or seen in the air in front of the mirror, 
the focus of a Cc. mirror is real or positive. If light is divergent it is made, 
by a Cc. mirror, convergent, parallel, or less divergent as the case may be. 

The course of a ray can be traced backwards along the same path as that 
by which it arrived; so that if F be the object- point, the rays F E, F A, etc., 
will be reflected parallel to the axis along the lines E E ', A A', etc. Thus, 
image and object are interchangeable. 

Fig. 32. 

Convex Mirror. — Let A B (Fig. 32) be a convex mirror, C the centre of 
curvature, D the vertex, and C D L the principal axis. Then if the object- 
point is at oo on the principal axis the rays proceeding from it to the mirror 
are parallel. Let K I be one of these rays meeting the mirror at I, and let 
C H be a normal to the surface. The ray K I will be reflected at I to I G, 
bo that the angle of reflection H I G is equal to the angle of incidence H I K, 
and the reflected ray 7 G, produced backwards, cuts the axis at F, which is 


the principal focus of the mirror. As with the Cc. mirror the principal focal 
distance is half the radius of curvature. 

A Cx. mirror therefore renders parallel light divergent, and divergent 
light still more divergent. The image thus formed is imaginary, so that the 
focus of a convex mirror is virtual or negative. 

Conjugate Foci. — Conjugate foci may be defined as the relative positions 
of object and image. If the image is real these positions may be reversed, 
and the object placed where the image previously was, and vice versa, the 
distances of the two conjugate points from the mirror remaining the same. 
Conjugate focal distances are the distances of the conjugates from the mirror. 


Fro. 33. 

Conjugate Focal Distances— Cc. Mirror. — If the object-point (Fig. 33) 
be on the principal axis between C and oo, say at/, the image will be at/ 
somewhere between F and C. An object at oo will have its image at F, and 
since the angle of incidence/ K C is smaller than the angle L K C, the angle 
of reflection^ K C, which equals the angle of incidence/ K C, must be smaller 
than the angle F K C, so that/p the image of/ lies nearer to G than F. 

As the object-point approaches C, its real image recedes from the mirror 
towards C; when the object-point is at C the image will also be at C, the ray 
C K being reflected back along its own path. When the object-point arrives 
within C at, say, /j, the real image is beyond C at/ and when it reaches F 
its image is at oo. 

When the object-point, as/ 2 , passes F towards the vertex, the reflected 
ray K I lies outside K L. Then the image is no longer on the same side 
of the mirror as the object, but is found by prolonging K I backwards to/, 
on the other side of the mirror. The image is then not actually formed, 
but is virtual or negative, existing only in the brain of an observer whose 
eye is looking into the mirror. As the object-point travels on towards the 
vertex the image also approaches until the two meet at the mirror. 

Conjugate Focal Distances — Cx. Mirror. — As the object-point /(Fig. 34) 
approaches the mirror from oo the angle of incidence increases; thus /if I 
is greater than L K I, so that the image/ also approaches the mirror from 
F to D. The nearness of the image increases with the nearness of the object, 
until at D object and image coincide. Thus the image is always formed 
behind the mirror either at F, or between it and D, by prolongation backwards 
of the divergent rays, and is always imaginary or virtual. 



Images on Secondary Axes. — In the preceding cases the object is sup- 
posed to be on the principal axis, so that the image is also on the principal 
axis. If the object-point be situated on some secondary axis the image is 
always on that same secondary axis. Also the object hitherto has been 
considered as a point; it can now be supposed to have a definite size. 

Fig. 34. 

Construction of Images — Cc. Mirror. — It is known that — 

(1) A ray parallel to the principal axis passes, after reflection, through 
F the principal focus. 

(2) A ray passing through F is parallel, after reflection, to the principal 

(3) A ray proceeding through C, the centre of curvature, is reflected back 
along its original path. 

A graphical construction of the image of an object placed in front of a 
spherical mirror can be made by tracing any two of such rays from each 
extremity of the object, and their course after reflection. The point where 
these rays meet (produced backwards, if necessary, as in the case of a virtual 
image) is the point where all the rays, which diverge from the object-point, 
also meet, and is therefore the image of that point. 

Fig. 35. 

The graphical construction when the object is beyond C is as follows : 
Let A B (Fig. 35) be the object, C the centre of curvature, and F the 
principal focus. Draw A K parallel to the axis, connect K F, and produce 
it onward ; draw A L through C. These two rays cut each other, after reflec- 
tion, in A', which is therefore the real image of A, situated on the secondary 
axis ACL. If a ray w T ere drawn from A through F to the mirror, its course 
after reflection would be through A', parallel to the axis. 

In the same way, rays drawn from B meet at B', and both B and B' are 



on the secondary axis B C K. By connecting B' and A' the image of A B is 
obtained, and it is real, inverted, and smaller than the object. 

If the object were at B' A' between the centre, of curvature and F, the 
image would be A B, real, inverted, and larger than the object. 

The course of any ray other than those mentioned can be constructed by 
drawing the normal to the point of incidence and making the angle of reflec- 
tion equal to the angle of incidence. 

Graphical construction when the object is between F and the mirror. 




Fig. 36 

Let A B (Fig. 36) be the object. Draw A K parallel to D C,- connect F 
and K, and produce towards A'; draw A, producing it similarly. These 
rays are divergent, and by prolongation backwards meet on the secondary 
axis G A A' in the point A', which is therefore the virtual image-point of A. 
Any ray A D is also reflected as if proceeding from A'. In the same way 
B' can be shown to be the image of B. By connecting B' and A' the image 
B' A' is obtained. It is virtual, erect, and larger than the object. 

Fig. 37. 

Fig. 38. 

The graphical construction of the image of an object at F resolves itself 
into lines parallel to the secondary axes; the image is at infinity (Fig. 37). 

If the object is at C, object and real image coincide, but the image is 
inverted (Fig. 38). 

If the object is at the mirror, no rays can be drawn; object and virtual 
image are in contact with the mirror and coincide. 

Construction of Images — Cx. Mirror. — Draw A K (Fig. 39) and connect 
K with F ; join A C. Where these divergent rays, by prolongation back- 
wards, meet each other at A' is the image of A ; it is on the secondary axis 
A C. Any other ray from A can be shown to be reflected as if proceeding 
from A'. 

By similar construction the position of B', the image-point of B, is deter- 


mined on the secondary axis B C. Connecting A' B' the complete image of 
the object AB is obtained. 

In the case of a convex mirror the image is always virtual, erect, and 
smaller than the object. 

Fig. 39. 

The above is based on: (1) a ray parallel to the axis is reflected as if 
proceeding from F ; (2) a ray directed towards C is reflected as if proceeding 
from C. 

Conjugate Foci of Spherical Mirrors. 

A list of symbols and abbreviations faces page 1. 

If F be the principal focal distance, then 1/F is the reflecting power of 
the mirror; this is termed the focal power; the two are reciprocals of each 
other; thus, if F be 10, then 1/F=1/10. 

Since F=r/2, the power of a mirror can also be written 2/r. 

A Cc. mirror converges incident light, and its power 1/F is positive. 

A Cx. mirror diverges incident light; its power is negative and repre- 
sented by - 1/F. 

Letf x be the distance of the object from which light diverges to the 
mirror; then the divergence of the light is \/f x and this is considered 

If the object is very distant the light divergence is negligible, and there- 
fore equals zero so that the light is reflected to or from F as a result of the 
power 1/F of the mirror. If, however, the light proceeds from a near object 
the divergence is appreciable, and the light is reflected to or from some other 
distance, f % , which distance is determined by the addition of the divergence 
of the light to the converging power of the mirror, i.e. 1/F - 1/f\=^/f v 
where l/f 2 is the reciprocal of the distance/ 2 . 

A Cc. mirror being positive, and the light divergence negative, f 2 is posi- 
tive or negative according as l/fj is respectively a smaller or greater quantity 
than 1/F. With a Cx. mirror f % is always negative because both 1/F and 
\/f x are negative. 

If / be a distance, then \/f is convergence to, and - \/f is divergence 
from, that distance. It is the reflecting power which will cause parallel 
light respectively to converge to, or to diverge from, that distance/. 

Thus the total power of a mirror 1/F is equal to the sum of the powers 
which represent the distances of the object and image. In other words the 
reciprocal of the principal focal distance is equal to the sum of the reciprocals 



of any pair of conjugate foci. Then the formula for conjugate foci for 
spherical mirrors is: — 





11 1 

It can also be written 

F F_ 

A A 

This formula is one of the most important in optics. In enables us to 
find the focal length of a mirror \if x and/ 2 are known; or if F and/ x are 
known we can find/,, (the image). It is universal and holds true for both 
concave and convex mirrors and, as will be seen, for lenses as well. Since 
the two fractions l/fi + l/f 2 added together always produce the same sum, 
it follows that if the one is increased the other is decreased in proportion. 
Thus if a Cc. mirror be of 20 in. radius, or 10 in. focal length, the sum 
l//i + l/f 2 is always 1/10. If a Cx. mirror has F= - 10 in., the sum \/f x + \/f 2 
is always -1/10. When/ 2 is positive the image is real; when negative the 
image is virtual. 

Size of the Image formed by a Mirror. — The relative sizes of image and 
object is termed Magnification (M). Now, object and image subtend the same 
angle at C, the centre of curvature, or at the vertex, so that the size of the 
image bears the same relation to the size of the object, as the distance of 
the image does to the distance of the object from the centre of curvature C, 
or from the mirror. That is 

K = A 

h A 



where h ± is the size of the object, h 2 that of the image, f 2 the distance of the 
image, and/ x that of the object. In the calculation f x and/ 2 must be in 
the same terms, then h 2 will be in the same terms as h x . The formula holds 
good with both Cx. and Cc. mirrors, and whether the image be real or virtual. 

Fig. 40. 

Geometrical Proof for Cc. Mirror. — In Fig. 40 A B is an object whose 
image is B' A'. The aperture of the mirror is taken as small, so that D M 
may be considered a straight line. 

In the similar triangles AC B and B' C A' 




In the similar triangles D F M and B' F A' 


But D M=A B, so that 

B'A' B'F 


Now MF=F, B' F=f 2 -~F, B C=f t -2 F, and B' C=2 F -f r 

F A-2F 

That is 

/ a -F 2F-/ 2 


Fig. 41. 

Proof for Cx. Mirror. — The aperture being small.. D M (Fig. 41), as before, 
may be considered a straight lim. 

In the similar triangles AC B and A' C B' 

A 7 F~BV 

In the similar triangles D F M and A' F' B' 


But D M=A B, so that 

A'B' B'F 


B'F B'C 

Now M F=F, B'F=¥ --/„ B 0=^ + 2 F and B'C=2 F -f z . 

F /; + 2 F 
That is - — .= yi J * 

F-/ 2 2F-/ 2 

whence F/ 2 - F/ 1= -/i/« 

o«" F(/ 2 -/i)=/i/ 2 and -^-7. 


Calculations on Conjugate Foci : Examples — Cc. Mirror. — Let a Cc. mirror 
be of 10 in. F. and let the object be at oo ; then we have 

11 11 11 _ 1 

The image is real and at the principal focal distance, since / 2 =F. 

In these calculations, any considerable distance is regarded as oo, say, 
beyond 6 M. or 20 feet, but although a distance may be taken as oo for the 
calculation of / 2 , its definite distance is needed for calculating h 2 . 

If the object be at F tbe calculation is 

/ 2 F F J2 

F and oo are conjugate distances. 

If the object is at 30" and 2" in height, we get 

1_1 11 
f~ 1Q 30~ 15 

Therefore the image is at 15 in. and real. 

h —I ^-9 X 15 -1" 

2 \7 2 so 

If the object were at 15 in. we find 

11 11 

7a = 10 ~ 15 — 30 

15 in. and 30 in. are conjugate foci with respect to a 10 in. Cc. mirror; 
if the object is at the one distance, the image is at the other. 
If \ is r, then 

If the object be at twice F, that is, at the centre of curvature, say 20 in., 
in front of a 10 in. Cc. mirror, the image is at the same distance, since 

-s=^7. ~ ™=;^ or f 9 =20 ins. 
f 2 10 20 20 J2 

Hf2=fv then /j^/^; object and image are same size. 

When O is within F, a higher number than 1/F being deducted from it, 
the result is negative. Thus if O, 1" high, be 6" in front of a 10" Cc. mirror, 

111 1 1 7 1 15 91- 

The virtual image is 15" behind the mirror and 2-5" high. 


Here - 15 in. is the conjugate of 6 in. in respect to a 10 in. Cc. mirror, and 
6 in. is the conjugate of - 15 in., but not of 15 in. That is to say, if light 
incident on the mirror is convergent to a point 15 in. behind it, it is reflected 
so as to come to a focus 6 in. in front of the mirror, for — 


7 2 = fo + r5=6 

An object 3 yards high is an eighth of a mile fiom a 30" mirror. 
being at oo , the image is at F=30", and 

7 3X3 ° A' U 

* 2= -220- =4mcL 

If f x or f 2 are not known, M can be found from M.= (f 2 -¥)/F and 
M=F/()i-F) respectively. 

The size of image of an inaccessible object can be calculated from the 
angle it subtends at the centre of curvature; for example, the size of the 
image of the moon formed by a Cc. mirror of 16 in. F. 

Fig. 42. 

being at oo (Fig. 42) the light is parallel, and the image I will be at F 
=16 ins. The moon subtends an angle of 32' at C, and therefore 

h 2 =W xtan 32 =16 x -0093=0-1488 in., or about 1/7 inch. 

It will be seen that a real or positive image is obtained with a Cc. mirror 
so long as O is beyond F, and that / becomes virtual or negative when O 
is nearer than F. Also that in all cases l/F=l/f x + l/f 2 . Thus when the 
light diverges from 30" and is converged to 15" we find 1/10=1/30 + 1/15. 
When it diverges from 6" before reflection, and from 15" after reflection, we 
get 1/10=1/6 + (-1/15). 

The nearer is to F, the more distant is Z; as recedes from F, the / 
approaches F, but no positive I can be nearer than F, since no O can be 
more distant than oo. 

The nearer O is to F, the more distant is the negative I. As O recedes 
from F and approaches the mirror, I also approaches the mirror, but I 
is always more distant than O until, when O touches the surface, so also 
does I. 

If light is convergent when incident on a Cc. mirror, the convergence is 
increased after reflection, and in this case the image is nearer to the mirror 
than F. 


Examples — Cx. Mirror. — Let the mirror be of 10 in. F and the at oo. 


1 1 1 1 1 11 

f- : F~f-~U)~n = ~To~~ "To 

The image is virtual or negative and at F. 

If be in front of the mirror at a distance equal to F, / is at half F. 

1 11 1 , 7 , 10 

7 = -i0T0 = -5 and *r a *i*5=-fi*i 

If is 30 in. in front of the Cx. mirror and 2" high 

1 11 1 . n 7 2x7-5 

f t 10 30 7-5 2 30 

The image is virtual, 7| in. behind the mirror and -5" high. 

- 1\ in. is conjugate to 30 in., with respect to a 10 in. Cx. mirror, and 
30 in. is conjugate to -1\ in., but not to 1\ in. If light converged to a 
point 1\ in. behind the surface, the convergence is, by reflection, so much 
reduced that an image is formed 30 in. in front of the mirror. 

If light converges to a point within F the image is real ; if convergent 
to F the light is parallel after reflection, since the convergence of the light 
and divergence of the mirror neutralize each other. If the light is convergent 
to a point beyond F the virtual image is also beyond F. 

The / of an formed by a Cx. mirror is therefore always virtual, and 
cannot be at a greater distance from the mirror than F, the O being then 
at oo. When is nearer than oo the / recedes from F towards the mirror, 
and when touches the surface I does likewise. 

Relationship of Distances from C and from Mirror. 

In the foregoing examples the distances from the mirror have been taken 
for calculating h v but the same ratios would exist were they taken from C. 
Thus 30" and 15" from a 10" Cc. mirror are 30-20=10" and 20-15=5'< 
from C, and 30/15=10/5. 

Similarly with a 10" Cx. mirror, 30" and 7 J in. from it are 30 + 20=50 
and 20 -7£==12| from the centre of curvature, and 30/7-5=50/12-5. 

Unit Magnification. — When object and image are equal in size M=l. 
The plane of unit magnification for real images is at the centre of curvature 
of a Cc. mirror — that is, at 2F. Foi virtual images it is at the mirror itself 
for both Cc. and Cx. The distance from F=F in both cases. 

If M=l J / 2 =/ 15 and 1/F=2//; or 2// 2 — that is, f x or/ 2 =2F. If the 
image is virtual, / 2 is negative, and^ and/ 2 =0. 


Newton's Formula for Conjugate Foci. — If the distance of the object from 
F=A, and that of the image from F=B, then 

AB=F 2 or B=F 2 /A 

Let F=10 and/ x =30, then A=30 - 10=20 

and B=100/20=5, or/ 2 =5 + 10=15 in. 

Let F=10 and/ 1 =6, then A=6 - 10= -4 

and B=100/-4=-25, or / 2 = -25 + 10= -15 in. 

Let F= - 10 and/ 1 =30, then A=30 - ( - 10)=40 

and B=100/40=2-5, or/ 2 =2-5 + ( - 10)= - 7-5 in. 

These examples should be compared with those worked by the ordinary 

Movement of Image. — If a mirror is rotated a real image moves in the 
same, and a virtual image in the opposite direction. If the object is moved, 
its real image moves in the opposite, and its virtual image in the same direc 
tion. If the observer's head be moved a real image apparently moves in 
the opposite, and a virtual image in the same direction. As with a plane 
mirror, the angular movement of any image is twice that of the mirror itself. 
Virtual images are also laterally inverted, but a real image is entirely reversed, 
and therefore not laterally inverted in this sense. 

Recapitulation of Conjugates. 

Cc. Mirror. — at oo, 1 is real, inverted, diminished, at F. 

O between oo and 2F, 1 is real, inverted, diminished, between 2F and F. 

O at 2F, I is real, inverted, equal to 0, at 2F. 

O between 2F and F, I is real, inverted, enlarged, between 2F and oo. 

at F, I is infinitely great, at oo. 

O within F, I is virtual, erect, enlarged, the other side of mirror. 

O at mirror, J is virtual, erect, equal to 0, at mirror. 

Cx. Mirror. — O at oo, / is virtual, erect, diminished, at F. 
O within oo, I is virtual, erect, diminished, within F. 
O at the mirror, / is virtual, erect, equal to O, at mirror. 

Fig. 43. 

Aperture of a Mirror. — In order that a true image of a point may be 
obtained with a spherical mirror, it is essential that the aj)erture should be 
small compared with its radius, subtending an angle of, say, not more than 


20° at G, so that the arc of the aperture may be regarded as a straight 
line. In Fig. 43, E F is the actual, and E C F is the angular aperture of 
the mirror, C D being the principal axis, and G the centre of curvature. 
Join E F. Then if the angle E G D be small (not exceeding 10°) the distance 
D G will also be small, so that C G may, without much error, be taken as 
equal to G E or C D; also E D G=E G G may be taken as a right angle. 


Now tan a= 7r7S , sin a=Tr7,. an ^ cos a ~ ^"Tr 

Since (7 E=C G, sin a=tan a=the arc E D, and cos a=l/l=l. 

Thus all calculations involving mirrors — and, as will be seen later, lenses 
also — are greatly simplified, since the sine and tangent may be considered 
equal, and can be replaced by the arc, and the cosine by unity, whenever 
the angular aperture is small. 

In the proofs for conjugates this approximation is introduced, which is 
permissible, seeing that the portion of the mirror chiefly responsible for the 
production of the image is that immediately surrounding the vertex. Mirrors 
of large aperture do not produce true point images of point objects, and are 
said to suffer from aberration (Chapter XXI.). 



The fact that the velocity of light is lessened in a dense medium is the 
cause of refraction. 

Normal Incidence. — When a beam of light, from air, is incident normally 
on a dense medium such as a plate of glass, the whole of the wave-front is 
retarded simultaneously and equally, and is unchanged in direction during 
its progression through the denser medium. On reaching the second surface, 
each part of the wave-front is again incident at the same time, and is equally 

Fig. 44. 

increased in speed as it passes again into the rarer medium, so that its line 
of progression still remains unchanged. 

Oblique Incidence of Light. — But if the plane wave-front A A' (Fig. 44) 
be incident on the first surface obliquely, one partS' meets the denser medium 
sooner than the rest and is retarded, while the others are still in the rarer 
medium advancing at an undiminished rate of speed. Each wavelet on 
reaching the glass becomes retarded, one by one, until all have passed into 
the denser medium, and in consequence the wave-front is changed in direction. 
When the whole of the wave-front CC is in the denser medium, it travels 
without further deviation, but at a diminished rate of speed. On reaching 
the second surface of the glass the wave-front D D' is again incident sooner 
at one point D' than at others. The wavelet at that point increases its 
speed, while the remainder is still moving less rapidly in the denser medium; 
then other wavelets emerge and increase their speed until, all having passed 



into a rarer medium, the entire wave- front E E' travels more rapidly, that 
is, with its original velocity, and in a direction parallel to its original direction. 
The angular change of direction depends on the distance that the more 
rapidly advancing parts of the wave-front travel before their speed is also 
checked, that is, on the obliquity of the incidence of the light, and on the 
retardation itself, that is, on the optical density of the medium. 

The Laws of Refraction. — When a ray of light is incident (obliquely) on 
the boundary plane of two media of different optical densities: — 

(1) The incident and refracted rays are in the same plane as the normal 
to the point of incidence, but on opposite sides of it. 

(2) A constant ratio exists between the sines of the angles of incidence 
and refraction. 

The ratio in (2) is the mathematical expression of the definition of the 
index of refraction as given in the next article. 

From the second law we can deduce the following : 

A ray passing obliquely from a rarer into a denser medium is refracted 
towards the normal at the boundary plane of the two media. 

A ray passing obliquely from a denser into a rarer medium is refracted 
away from the normal at the boundary plane of the two media. 

A ray suffers no deviation if, at the point of incidence, it is normal to the 
boundary plane of the two media. 

The Index of Refraction. — The index of refraction between two media is 
the ratio of the velocities of the light in these media. The velocity varies in- 
versely with the optical density; thus if the light travels three miles in the 
first medium, while, in the same time, it is travelling two miles in the second, 
then the index is 3/2=1-5; if the direction of the light travel were reversed 
the index would be 2/3. 

Geometrical Proof. — In Fig. 45, let S S be the bounding surface between 
two media, of which the second is the denser, and let the velocities of the 
light in the two media be respectively V x and V 2 . Let DC be a, plane wave- 
front incident on the surface at the angle D C A=i, which, after refraction, 
passes into the second medium at the angle of refraction E A C=r. 

Then A D and C E are distances travelled by the extremities of the wave 
in the same time, D in the rarer and C in the denser medium; A D and C E 
therefore represent the two velocities. 


A D and C E are perpendicular to the wave-front, and the angles ADC 
and A EC are right angles. The hypothenuse A C is common to the triangles 
ADC and A EC, so that A D and C E are the sines of the angles of incidence 
and refraction respectively, thus 

AD Vj sin i 
CE = V 2 = smr 

That is, the index of refraction is the ratio of the velocities of the light in 
the two media, or the ratio of the sines of the angles of incidence and refraction. 

This proof holds good when the incident wave is curved, since the portion 
D C under consideration is so small that it may be considered plane — we 
work from the " ray " FB, which is really the path taken by the wave- front. 
Similarly if the medium S S is curved, the portion A C may also be con- 
sidered plane. 

The angle of incidence of a wave-front is that which it makes with the 
surface, as A C D in Fig. 45, the corresponding angle of refraction being 
C A E. The angle of incidence of a ray is that which it makes with the 
normal as F B N, the angle of refraction being Q B N'. It is immaterial 
as to which is taken since AC D and FBN are equal, as are also E AC 
and QB N'. It is, however, more convenient to treat of the incidence and 
refraction of rays than of wave-fronts. 

Absolute Refractive Index. — It can be taken that the velocity of light 
is a maximum in free ether (i.e. a vacuum) through which light waves, of 
every length, travel with equal speed. Its progression through air is very 
slightly slower, and for all practical purposes no distinction is made. The 
optical density of air is therefore taken as unity or 1, and the density of 
any other medium, such as water or glass, is expressed in terms of this unit, 
and is called the absolute index of refraction, generally denoted by the Greek 
letter ju (mu). Thus if the ju of a certain kind of glass is 1-5, it implies that 
light travels one and a half times as fast in air as in the glass, or the velocity 
in the glass is only 1/1-5=2/3 that in air. fx expresses the optical density 
of a medium, and if ^=1-5, the medium to which it pertains has an optical 
density which is 1*5 times greater than air. To a certain extent the optical 
density varies directly with the specific gravity, but there are some exceptions, 
in transparent media, as for instance with oil and water; oil has the greater 
optical density, but tbe lesser specific gravity than water. 

When reference is made to the ju of a substance it invariably indicates 
the absolute index. Also, unless otherwise stated, fi refers to yellow light; 
the index varies with the colour of the light, but, for the present, we shall 
consider light monochromatic, and the wave-length that of the D line. 

It is usual, when several media are involved in a calculation, to refer to 
their indices as^, /u 2 , fx 3 , etc., but when there are only two media, one of 
which is air, the index of the denser is denoted simply by [i without any 
suffix, that of air being, as before stated, taken as 1, although actually it is 
about 1-000294. 


.u ' 


Relative Refractive Index. — The relative index of refraction, /a , is the 
expression of the refractivity when light passes from one dense medium 
into another, say, from water into glass or vice versa. It is found by dividing 
the absolute index of the medium into which the light passes, by the absolute 
index of the medium from which it proceeds; thus when light passes from 
water i a=l-333 into glass m= 1-545 the relative index is 

u 9 1 -545 

Again, the sines of the angles of incidence and refraction, as light passes 
through two such media, are to each other as the velocities of the light in 
those two media. 

The Law of Sines — commonly known as Snell's Law — is that 

sin i /li 2 
sin r }i x 

where ^ 2 is the optical density of the second medium and/.^ that of the first. 
This is the fundamental formula of refraction. In the case of reflection the 
light returns to the same medium as it comes from, and therefore /u 2 =ju v 
so that sin i=sin r or the angle of reflection is the same as that of incidence. 
The angles i and r are equal in refraction only when light passes obliquely 
through two different media of the same optical density, as crown glass and 
Canada balsam. 

Reciprocal m's. — In the case of any two media A and B the index of 
refraction for light passing from A into B is the reciprocal of the index for 
light passing from B into A. Thus, when light passes from air into. glass, 
the sines of the angles of incidence and refraction are, say, as 3 : 2, and the 
index is 3/2. If it passes from glass into air, the sines of the two angles are 
as 2 : 3 and the index is 2/3. Taking the example above of light passing 
from water to glass with a relative ju of 1-16; if the light passed from the 
glass to the water ^=1-333/1 -545=l/M6=-862. 

The Course of a Ray. — Examples of the application of the law of sines. 
Let a ray be incident from air (mj=1) at 30° with the normal, to glass 
of ^2=1-5, and it is required to find the course of the ray after refraction. 

sin i u 2 sin 30° 1-5 

- — = — , that is — : =— 

sin r ii x sin r 1 

sin30'xl -5 .„««„,, 

therefore sin r= — =— -=-333=sm 19 30 (approx.), 

1-5 1-5 

so that r=19° 30'. 

If light passes at an angle of 30° from glass of / a 1 ==l-5 into air 

sin i Mo . sin 30° 1 

= — , that is 

sinr Mj sin r 1-5 



therefore sin r=sin 30° x l-5=-5 x l-5=-75=sin 48° 30' (approx.), so that 
r=48° 30'. 

It should be noted that in the case of light passing into the denser medium 
it is deviated 10° 30', and when passing into the rare medium it is deviated 
18° 30' for the same angle of incidence — i.e., that of 30°. 

If a ray is incident at 12° to the boundary plane between water ( / a 1 =l , 333) 
and glass (^2=1-545), then 

sin i 1-545 

sinr 1-333 

, and sin r- 


If it passes the other way at the same angle 

sin % 1-333 . -2079x1-545 

; , and sin r= 

sinr 1-545 


r is smaller than i when light passes into a denser medium, and vice versa. 

Further, the angle of incidence i is invariably taken as occurring in the 
first medium jli v and the angle of refraction r in the second medium fj, 2 . 

It is the direction of the light that determines which medium is denoted 
by/^ or ju 2 as the case may be. 

The actual deviation which light undergoes, when passing from one medium 
into another of different density, at a given angle of incidence, depends 
on the ratio between the fi's of the two media, and not on the high value of 
the//, of the second medium. Thus the refraction is greater when light passes 
from air into glass of ^=1-5 than when it passes from water into glass of 
^=1-9. In the former case the density of the second medium relative to the 
first is 1-5, and in the latter it is 1-9/1-33=1-43. 

Fig. 46. 

Graphical Constructions. — The course of a ray can also be graphically 
constructed in the following manner: Let D G be any ray in air incident 
at G on the surface S S (Fig. 46) of a medium whose index is 1-5 or 3/2. 
From D drop the normal D B and divide B G into three equal spaces. Then 



from G mark off G A equal to two such spaces. From A drop a normal 
and from G draw a line G E, equal in length to G D, cutting the perpendicular 
from A in E. Then G E is the direction of the refracted ray. In this con- 
struction B G is equal to and takes the place of D C, which is sin i, and A G 
is equal to and replaces E F, which is sin r. 

In order to trace the course of a ray of light through any refracting body, 
with plane or curved surfaces, the procedure is the same, but in the case 
of a curved surface the tangent to the curve, at the point on which the ray 
is incident, is taken to represent the refracting plane. 

This construction is a graphical representation of the sine law, because 
in the right-angled triangles C I) G and F EG, the hypothenuses I) G and 
G E are equal, and C D and E F. the sines of i and r respectively, are numeri- 
cally in the ratio of 3 and 2. Therefore G E must be the direction of the 
refracted ray. 

The construction is applicable to any pair of media. If they are, say, 
oil of i a 1 =145, and water of /x 2 =l-33, B G would be as 14-5 to A G 13-3. 
When the ratio is complex, as in this case, it is better to mark off, with a 
millimetric rule, the spaces B G and A G, and then drop D B and A E, finally 
filling in D G and G E, which must be of equal length. 

It should be observed, as indicated in Fig. 46, that the length B G, repre- 
senting /li. 2 , is always on the same side of the normal as the incident ray, and 
that the length A G, representing ju v is therefore on the side of the refracted ray. 

(For other Media see Ghap'er XXVII.) 
Air .. .' 1-000 


Canada balsam 
Crown glass 
Flint glass 
Diamond . . 







1-500 to 1-600 

1-530 to 1-800 


The index of glass varies with the materials used in its manufacture, and as a rule the 
higher the ji the softer is the glass. 

Dispersion. — The shorter waves, with rare exceptions, are retarded by 
a medium, more than the longer waves, so that when white light undergoes 
refraction its components are refracted to different extents, and the various 
colours become separated, producing what is known as dispersion or chro- 
matism, which subject is treated later. As before stated the index of a 
medium is its mean/j,, that is, fx^. 

Critical Angle and Total Reflection. — When a ray of light passes from 
a dense into a rare medium, it is bent away from the normal, with which it 
makes a larger angle than before refraction. In Fig. 47, let A B be the 



incident and B C the refracted ray. As the angle of incidence is increased, 
so the corresponding angle of refraction becomes still larger. Hence if the 
ray A'B be incident at an angle sufficiently large, the angle of refraction 
becomes a right angle, and the refracted ray B C will skim along the bound- 
ing surface. The angle of incidence in the denser medium which produces 

Fig. 47. 

this result is termed the critical angle, because the slightest further increase 
of it prevents the ray from passing out of the denser medium. If the incident 
ray be A" B it is reflected as B C", and internal reflection takes place. This 
is termed total to distinguish it from ordinary reflection, which is always 
accompanied by a certain amount of absorption or transmission. 

From the sine formula sin t'/sin r= - a 2 /^ 1 , 

For i we can substitute C, the critical angle. 

Also r=90°, so that sin r=l, and therefore can be omitted. 


sin C= — , or sin C=/.t,. 

The sine of the critical angle is equal to the relative index from the denser 
to the rarer medium. 

If the rarer medium be air, we have: — 

sin C=-, or a sin C=l. 

Thus for glass of ^=1-52 and water 1-33 the critical angle is 61° 18' 

sin C=l-333/l-52=-877=sin 61° 18'. 

For glass of / u=l-5 in air, C=41° 46' since sin C=l/l-5=-666=sin 
41° 16' 

The critical angle when light passes through several media is the same as 
that which obtains directly between the first and the last. 




Index of Refraction. 

Critical Angle. 

Chroniate of lead 






Various precious stones 


25° to 30° 

Flint glass 

■ — ■ 

38° to 40° 

Crown glass 


40° to 43° 






48° 30' 

It will be seen, from the above, that the critical angle varies inversely 
with /u. That of glass in general is about 40°. 

Some Effects of Total Reflection. — On looking upwards through the side 
of an aquarium tank the upper surface glistens like quicksilver, owing to 
the light being reflected downwards. 

If a tank with water has some benzine on the top, the two liquids do 
not mix. As the benzine has the higher index, light from above may be 
totally reflected upwards from the common surface which glistens when 
viewed obliquely. 

A solid bent tube of glass with a strong source of light close to one end 
transmits the light by internal reflection for illumination purposes in micro- 

A crack in a thick plate glass demonstrates total reflection at the film of 
air in the fracture. 

Fig. 48. 

Fig. 49. 

Fig. 50. 

Reflecting Prisms. — If the principal angle of a prism exceeds twice the 
critical angle of the medium of which it is made, total reflection ensues for 
any angle of incidence of the light, because, even for the largeet possible 
angle of incidence — i.e., 90° at the first surface — the internal angle of incidence 
at the second surface is greater than half the principal angle, and is therefore 
greater than the critical angle. Since all glass has a critical angle of less than 
45°, if (Fig. 48), a ray A B enters a right-angled prism normally, it is incident 
at 45° to the surface Y Z, and is then totally reflected in the direction B C. 
It is not refracted at the surfaces D Y and D Z because it is normal to each. 
Thus a right-angled prism serves as a total reflector when the light is incident 
perpendicularly to the one face, the direction of the emergent light being at 
right angles to the original course. 

There is reflection even if the light does not enter at right angles to D Y, 



provided, after refraction, the angle of incidence at Y Z is greater than the 
critical angle. Any dispersion which takes place as the ray enters is reversed 
as it leaves the prism, so that the emergent ray consists of white light similar 
to that which entered. 

If the light falls normally on the hypothenuse side of a right-angled prism 
it causes total reflection twice, at B and C, as in Fig. 49, so that the final 
direction C D of the light is parallel to its original course A B. The forms 
shown in Figs. 48 and 49, with variations, are extensively employed in prism 
binoculars, range finders, etc. With them lateral without vertical inversion, 
or vice versa, can be obtained. 

By means of a right-angled prism, as indicated in Fig. 50, vertical without 
lateral inversion may be obtained. This prism is used in process photo- 
graphy, and in projection work. As shown here and in Fig. 48, if a ray is 
not normal to one of the faces of a right-angled prism, its angle of emergence 
is the same as that of incidence. 

With an equilateral prism ABC (Fig. 51) a ray DE incident normally on 
the surface AB is reflected at the surface AC in the direction EG, and emerges 
normally from the third surface BC. The deviation of the ray is FEG=6Q°, 
that is, the same as the principal angle A. 

Fig. 52. 

Fig. 54. 

Displacement due to Refraction. — In Fig. 52 let C be a luminous point in 
a dense medium from which, after refraction, rays enter an observer's eye 
and are projected back to C, the virtual image of C. Thus a stick ABC 
partly immersed in water and viewed obliquely appears bent towards the 
surface, the bend commencing at the level of the water. The lateral dis- 
placement and the raising of each image-point is proportional to the depth 
of the object-point in the denser medium and the^ of the latter. 


The apparent . position of the object depends also on the oblkjuity of 
view; the nearer the eye to the surface, the greater is the refraction of 
the emergent light, and the greater the apparent raising of the object. If 
the eye be practically at the surface, the object is also apparently raised to 
the surface, but is very distorted. 

Fig. 53 represents the surface of a dense medium and the object. Any 
ray other than A N, normal to the surface, is bent away from the normal, 
and when referred back by the eye appear to come from points /', I", I"', 
these being the images of when the eye is at B', C, and D' respectively. 
The series of images actually form a curve, although in the diagram they are 
projected on to the normal N. 

The position of any particular image-point can be calculated as follows : 

In Fig. 54, let be the object and B any ray making an angle with 
the normal N N'. After refraction it will take the course B B', so that to 
an eye at B' the object is apparently raised to 7. It is required to find the 
apparent depth of the image, i.e. the distance A I in terms of the real depth 
A 0, ju and r, the angle of view with the normal. 

Now the angle A B=OBN =n and A I B=NBB'=r 

L ^ A B , k _ A B A I tan t 

also A 0=- : and A 1= , or -r—^=7 

tan % tan r AG tan r 

Let the real depth A be t and the apparent depth A I be l', and since 
tan ?=sin i/cos i and tan r=sin r/cos r 

sin i cos r 1 cos r , t cos r 

t'=t .X— — =**-X- .or*'- -. 

cos i sin r fi cos * jli cos i 

Thus, knowing /u and r, the angle of view, we can calculate the value of i, 
and after that t' from the known depth t. 

If the eye be on, or near to, the normal A, the angles r and i are very 
small, and cos r and cos i are practically unity. Therefore, without appreciable 
error we can write for the apparent vertical position of an object in a dense 
medium, or the apparent depth of a medium, viewed vertically, 

If the medium be water whose index is 4/3, then the apparent depth is 3/4 
that of the real depth; with glass ^=1-5, £'=2/3 t. 
The apparent vertical displacement d is 

t (u-1) 

(/n - 1)/li is about 1/4 in the case of water, and 1/3 for glass. 

A fish appears nearer the surface than it really is, and when the eye is 
near the surface, it appears distorted, thinner if lengthways, and stuDted if 



with its head towards the surface. Light from its under portions suffers 
relatively more deviation than that from the upper, thus giving the idea 
of vertical compression. Supposing the course of a bullet to be unaltered 
by the water, one would have to aim, with a rifle, well beneath a fish in 
order to hit it. To reach a coin at the bottom of a bath one would have 
to dive towards a point apparently nearer. Again if a coin were hidden 
from view by the rim of a basin, it may come into view if water be poured 
into the basin. 

On the other hand, if the eye were in a dense medium and viewing an 
object in air, the apparent position of would be more distant than it really 
is, such that t'=t{x. 

Refraction by a Parallel Plate.— If a ray A B (Fig. 55) be incident on 
a medium with parallel surfaces such as a plate of glass in air, it is refracted 
towards the normal at the first surface in the direction B C, and after refrac- 
tion at the second surface emerges as C D parallel to its original course A B; 
the angular deviation is zero. 



v /-I 


* '* ' 1 I 

\ v / / 


Fig. 55. 

Fig. 56. 

The ray, however, as a whole, is laterally displaced over the distance 
H D, depending on the angle of incidence i, the ju of the medium, and its 
thickness t. Let d be the displacement and r the angle of refraction in the 

Now H D=EC, the angle EBF=i, CBF=r, and EBC=i-r, while 
FB=t the thickness. 

Then E C=B C sin E B C=B C sin (i - r) 

but B C=B F/cos C B F=*/cos r 

sin (* - r) 


E C=d=t 

cos r 

The value of r is first found from i and /u, and then d is calculated. 

Lateral displacement causes slight distortion of a near object when 
viewed through a plate, but if the thickness is small, the effect is inappreci- 
able. Distortion disappears for any thickness when the light is parallel. 

If the object be viewed through a plate from vertically above, it appears 



to be nearer, but not laterally displaced. The vertical displacement depends 
on the thickness of the plate, and is 



as for an object situated in a dense medium. Thus for glass of index 1*5, the 
object viewed would appear nearer, by about 1/3 the thickness of the plate. 
Fig. 56 shows the course of an oblique pencil AA from which arises the 
apparent vertical displacement of a point L to L' when viewed through a 
plate N. 

Multiple Parallel Media. — If a number of parallel plates of different 
indices be superposed, their combined action is similar to that of a single 
plate of uniform index, provided that the first and last media have the same 
index. The refraction that occurs in this case is such that the angle of 
emergence at the last surface equals the angle of incidence at the first. When 
the first and last media have not the same index the deviation sufiered by 
the light, on emergence, is the same as if the light entered from the first 
medium directly into the last. 

Eye in Dense Media. — There is, of course, no critical angle for light 
passing from a rare into a dense medium, so that to an eye E (Fig. 57) under 
water, a field of 180° is visible when looking upwards from the dense medium. 

Fig. 57. 

Rays A B and D G from objects level with the surface are practically 
parallel to the latter and therefore refracted into the water at the critical 
angle E B N' and E C N' and are referred back in the direction G and F. 
The cone F E G contains a distorted view of all external objects, and its 
angle EB is equal to the sum of the angles E B N' and E C N', that is, to 
twice the critical angle of water — about 96°. Also, as previously stated, 
objects directly above appear more distant by an amount equal to about 1/3 
their real distance above the water, but those cl jser to the surface are dis- 
placed to a rather greater extent. The distortion and indistinctness are 
greatest for objects near the surface, and disappear for those directly above. 

The circular space into which all external objects appear to be crowded 
is, owing to dispersion, bordered by a ring of colour, blue on the in- and red 
on the outside. 



If the two surfaces of a medium are not parallel to each other, all incident 

light must suffer refraction, since no ray can be perpendicular to both surfaces. 

Prism. — An optical prism is a transparent body, usually of glass, having 

two plane refracting surfaces which are inclined to each other and meet in a 

line. For special purpose a prism may be of quartz, rocksalt, fluorspar, etc. 

Defining Terms. — The line of junction AB (Fig. 58) of the two refracting 
surfaces is the edge. F C D E is the base. AB D C and AB E F are the 
two refracting surfaces. The angle between them is the 'principal angle. 
The plane AB K I containing the edge and situated symmetrically with 
respect to the two surfaces is the base-apex plane : generally it bisects the base. 
Any line, as L M, at right angles to the edge and lying in the base-apex plane, 

° =-+-" f 

Fio. 58. 

Fig. 59. 

is a base-apex line. The line G H, parallel to the edge and lying in the base- 
apex plane, midway between the edge and base, is the axis. A principal 
section is any section, as A F C, cutting it from edge to base perpendicularly 
to the axis. The point A, or any point on the edge A B, is the apex. 

In a circular or oval prism the thinnest part L (Fig. 59) is considered the 
apex. M N is the base. The central line L M connecting the thinnest and 
thickest parts is the base-apex line, and is usually marked on the circular 
prisms of the trial case by two small scratches. P, tangent to L and per- 
pendicular to L M, is the imaginary edge. P M N shows a section of such a 
prism along the base-apex line. 

Refraction by a Prism. — All light refracted by a prism is bent towards 
the base. If a ray be incident normally to the first surface, it is undeviated 




until it reaches the second, when it is bent away from the normal. If incident 
other than normally, as it passes from the rarer into the denser medium, it is 
refracted towards the normal at the first surface, and again away from the 
normal as it passes from the denser into the rarer medium, at the second 


Fig. 60. 

Fig. 61. 

If the incident light is parallel (Fig. 60), divergent as from D (Fig. 61) 
or convergent, it is in general the same, respectively, after refraction by the 
prism. Nevertheless, as will be seen later, the degree of divergence or con- 
vergence does not remain quite the same. 

The Principal Angle. — The principal angle at A (Fig. 62), formed by the 
two refracting surfaces, is sometimes known as the refracting angle, or angle 
of inclination. It is indicated in degrees. A prism of 10° is one whose sides 
enclose that angle. 

The Angle of Deviation— An object viewed through a prism appears deviated 
towards the edge. The incident ray D E (Fig. 62) is refracted at E, takes the 


Fig. 62. 

direction E F, and is again refracted at F to pass out in the direction F G as 
if proceeding from J. The angle of deviation d is, in this case, I H G, because 
D E, instead of following the path H I, follows the path H G. An object 
at D, viewed through the prism, appears as if it were situated at J. The 
deviating angle constitutes the important optical property of a prism, and 
expresses its power or refracting effect. 

The apparent deviation of an object is the result of the refraction suffered 
at the two suifaces. It is commonly said to be towards the apex. A ray 
incident at X (Fig. 59), from an object beyond the prism, is refracted towards 


Y and is referred back towards Z, the plane of deviation Z X Y being parallel 
to the base-apex line L M. 

The deviation depends on and varies directly with (1) the angle of the 
prism, (2) the ju of the medium, and (3) the angle of incidence of the ray. 

The last, however, is usually ignored when the power or deviation of a 
prism is considered, and the incidence is taken to be that resulting in minimum 

Minimum Deviation. — For every prism there is one position of the base- 
apex plane in which an incident ray is less deflected than in any other. From 
this position, if the prism be rotated around its axis, either way, the image 
seen through the prism appears still more deviated towards the edge of the 

Minimum deviation obtains ivhen the incident and emergent rays are equi- 
distant from the edge, and, as shown in Fig. 62, the angles of incidence and 
emergence (i and e) are also equal. In this position the ray, as it traverses the 
prism, forms, with the sides, an isosceles triangle, of which it is the base. In 
this case the angle of deviation is formqd in the base-apex plane, which may 
be regarded as the refracting plane of the prism. In other words, minimum 
deviation occurs when the refraction is shared equally between the two 

The Prism Formula. — In the prism B AC (Fig. 63) P is the principal angle, 
d the deviating angle, i the angle of incidence, r the angle of refraction at 
the first surface, s the angle of incidence at the second surface, e the angle of 
emergence, and fi the index. The formula given below connecting these 
factors, when d is minimum, enables us to find the index of refraction of a 
prism when P and d are known, having being measured by the spectrometer 

Fig. 63. 

Geometrical Proof —D E F G is a ray (Fig. 63) traversing the prism B AC 
at minimum deviation. Being symmetrical 

i=e, r=s, and a=&. 

In the quadrilateral E A F H, the angles at E and F are right angles, 
so that P= 180° -x. 

In the triangle E F H the angles r + ,s=180 - x 

therefore P=r + s=2r, or r=P/2. 


The external angle c/=the two internal opposite angles a and b, that is, 

d=a + b=2a, or a=d/2 

so that i=r + a=P/2 + <Z/2=(P + d)/2 

sin i 
and as /M= - — 

sin r 


sm , 

Therefore ft = — — — 

sin ( 


Example. — What is the index of a prism whose angle of minimum devia- 
tion is 28° and principal angle 45° ? We have 

T+d\ . /45° + 28° 

sin -— I • sm 

2 / \ 2 / sin 36° 30' -5948 

. _ . 1.554 

^ ~ /P\ . /45°\ sin 22° 30' -3827 

[ 9 ' 

. fp+d\ 


Sin V 2 / 

. P . P+d 

8in Q 

r bm 2 — n 2 

To Calculate the Angle of Deviation. — If /u and P are known, d can be 
found thus: — 

Since ju 

Let (P + d)/2 be called a. 

Then 2a=Y + d and 2a-Y=d. 

To find the value of d we require two steps, thus : 
(1) Find a from sin a=ju sin P/2; (2) then d=2a - P. 
Expressed as a formula this becomes 

d=2 [sin" 1 (p sin P/2)] - P 

that is, d equals twice that angle whose sine is (jbt sin P/2) less P. 

Example. — What is the angle of deviation of a prism whose principal 
angle is 60° and index 1-62 ? 

Here fJL sin P/2=l-62 sin 30°= 1-62 x -5= -81 

and -81=sin 54° (nearly) 

Therefore d= (2 x 54) - 60=48 c 




To Calculate the Principal Angle. — If (JL and d are known, P can be found 

thus: — 

sin (P/2 + d/2) 


sin P/2 
sin P/2 cos d/2 + cos P/2 sin d/2 


sin P/2 
tan P/2= 

=cos d/2 

sin d/2 
tan P/2 

sin d/2 

Lt - cos (Z/2 

Example. — What angle must be given to a prism of 36° minimum devia- 
tion when li— 1-586 ? 

P sin 18° 

tan -= 




1 -586 - cos 18° 1 -586 - -951 1 -6341 
P/2=26° (nearly), and P=52° 


The Angle of Incidence. — When deviation is a minimum, the angle of 
refraction r at the first surface is equal to half P, so that : — 

sin i=fi sin r=fi sin P/2 

Fig. 64. 

Fig. 65. 

Normal Emergence or Incidence. — When a ray D E F (Fig. 64) enters a 
prism at such an angle that it emerges normally from the second surface, 

i=r + d 

But r + a=90°, alsoP + a=90° .-. r=P 

so that sin i=ju sin r=/u sin P 

If the light is incident normally, as F E, all the refraction takes place at the 
second surface, where r (Fig. 64) is the angle of incidence and r=P; the angle 
of emergence is then i. 

•Angles i and e. — With minimum deviation the angles of incidence i and 
of emergence e are equal. With normal incidence or emergence, the one has 
zero value. As the one increases the other decreases, but for any angle of 

j> + d—i + e 


As the angle of incidence departs from that of minimum deviation, the value 
of d increases, but the increase of d is small compared with the increase of i, 
or the decrease of e, or vice versa. 

To trace the course of a ray through a prism at any angle i, when P and /u 
are known, we have, as in Fig. 65, 

sin r=sin i/f-i and s=P-r 

then sin e=fJi sin s=ju sin (P - r) 

The course of the light might be reversed, e becoming the angle of incidence, 
and i that of emergence. 

General Formula for Given Deviation. — When d is neither minimum, nor 
that resulting when incidence or emergence is normal, the calculation for i 
becomes complicated, but Mr. T. Smith, of the National Physical Labora- 
tory, indicates, in a contribution to the Transactions of the Optical Society, 
a method of finding the angles of incidence and emergence for any value of d 
with a given prism of angle P. On that article the formula below is based. 

Since i+e=I* + d under all conditions, as d varies so i increases and e 
decreases — or vice versa — to the same extent x. Let (P + d)/2 be called a 
and P/2 be called b. 

We have sin (a + x)=[A sin (6 + y) 

and sin (a - x)=[A sin (b - y) 

Expanding these equations, and then taking half their sum and half 
their difference, we get two expressions which, when squared and equated, 
enables y to be eliminated. Further simplification and equation results in 

(sin a + a sin b) (sin a - a sin b) 

sin 2 cc = - - ' 

(sin a + cos a tan b) (sin a - cos a tan b) 

Then i=(P+d)/2 + x and e=(P+d)/2-x 

Thus with P=30° and ^=1-5, we have for minimum deviation c?=15° 42' 
and i=22° 51'; for normal emergence d=!8° 36' and i=48° 36'. There is 
for an increase of i of 25° 45' an increase in d of 2° 54' only. 

For d to be equal to 17° we should have — 

a=(P+<Z)/2=23° 30' and 6=15°; 
whence sin 2 x=-0842 and x=16° 54'; 

so that ;=23° 30' + 16° 54'=40° 24' and e=6° 36'. 

Simpl fiecl Formulae. — By substituting angles for their sines, which can 
be done without serious error when the angles are small, as in ophthalmic 
prisms, the formulae may be greatly simplified as follows. Small angled 
prisms are those not exceeding, say, 15° P. 


1T = P 

whence (?=P(/*-l) 




If the refractive index=l-5, as is practically the case in ophthalmic glass, 
then fi - 1=1/2, and eZ=P/2. 

Thus for a prism of 5° the angle d may be taken as 2° 30'. 

When a prism is thin, any moderate departure from the position of mini- 
mum deviation does not result in any appreciable increase of deviation, so 
that this factor may also be ignored. 

For the angle of incidence, with minimum deviation, 

*=(P+ <2)/2=iUP/2 

and for normal emergence 


Examples. — If the principal angle is 10° and the deviating angle 5-25°, then 

/*=-— + 1=1-525. 

A prism of P=10° and ^=1-54, has an angle of deviation of 

cZ=10x-54=5-4 o =5°24'. 
If a prism of 6-25° d is required, ft being i -56, the prism angle is 

P= 6 ^ 25 =11.166 or 11° 10' 

If P=10° and ^=1-5 the angle of incidence for minimum deviation is 


If P=10° and ^=1-5 the angle of incidence for normal emergence is 

t'=l-5x 10=15° 

Neutralising Prisms. — Two prisms of similar angle d will, when placed in 
opposition, i.e. base to apex, neutralise each other. If they are also of similar 
P and ju they act as a plate, having parallel surfaces, on light passing through 
them. If them's are unequal, so also must be the angles P. 

To calculate the thin prism P 15 made of glass of a certain ju v which will 
neutralise another P 2 , whose ju% is different, we have * 

P 1 ( / a 1 -l)=P 2 (^ 2 -l) 

Thus if a crown glass prism of 15°, whose i w 1 =l-54, has to be neutralised 
by a flint prism whose // 2 = 1-62, then from the above 

15 x -54 
P,,= _ =13° 
2 -62 

If the prisms are thick, P x and P 2 are not then directly proportional to d 
or to (ju - 1), so that d^, the deviation of P r must first be calculated from the 
true formula. The other deviation d 2 must equal d v ajjd. from d 2 the value of 
P 2 for an index of (J. % can be obtained. 



Displacement by a Prism.— In Fig. 66 A is sccu, through the prism, at A'; 
if the object is at B or at 0, its image is seen at B' or C respectively. The 
angular displacement by a given prism depends entirely on the angle of 

Figs. 6G. 

Via. 67. 

deviation and is invariable; but the actual or linear displacement A A', 
BB\ C C, is proportional to the distance of the object, and is represented 
approximately by the tangent of the angle of deviation. 

Construction.— To trace graphically the course of a ray through a prism 
of given P and /* it is necessary to use a double construction like that of 
Fig. 46. At both surfaces the larger space, such as HL, is towards the base, 
and the smaller, as HK, towards the apex, as shown in Fig. 67. 

False Images of a Prism.— On looking through a weak prism at the primary 
image of a bright source, a second and fainter image, due to internal reflec- 
tion, is seen projected parallel to the base-apex line under an angle five or six 
times the deviating angle, so that in strong prisms it lies too far away towards 
the edge to be visible unless specially sought. In " The Clinical Use of 
Prisms " Dr. Maddex suggests its utilisation for the exact adjustment of the 
base-apex line. 

The Measurement and Notation of Prisms are treated in Chaps. X. and XI. 


Curved Surface. — A refracting surface is one which separates two media of 
different densities, so that, when light passes from the one to the other, 
refraction takes place. Only one refraction occurs and in this respect a 
surface differs essentially from a lens, where there are at least two surfaces 
and two refractions of the light. Unless otherwise stated a curved surface 
is deemed to be spherical. 

Since every line drawn from the centre C (Fig. 68) to the circumference 
of a sphere is a radius of curvature, every point on the circumference may be 


Fig. 68. 

regarded as a minute plane at right angles to a radius. Thus C E and C B 
are normal to the surface at E and B respectively, and also when prolonged 
beyond the circumference. 

Any ray AB or P E directed towards C passes into the medium without 
deviation. A ray D E, which is not normal to the surface, is bent towards the 

Fig. 69. 

normal P E C in the direction E F, if the medium is of a higher index of re- 
fraction, or it is bent away from the normal in the direction E G, if of a lower 
index than that of the medium from which the light proceeds. Both media 
are supposed to be of indefinite extent. 

Cx. and Cc. Surfaces. — In Fig. 69 let a mass of glass have a Cx. surface, 
and the outer medium be air. The ray/ x A directed towards A is at normal 



incidence, and passes onward without deviation. The rays f x B and f x D 
form certain angles with the normals to the surface, and each, on passing into 
the denser medium, is bent towards the normal to an amount governed by the 
ratio between the sines of the angles of incidence and refiaction. Thus/ X D 
is bent more than/ x B, and the two meet the line f x f 2 at the point/ 2 . Similarly, 
all rays diverging iiomf x are refracted to/ 2 , which is, therefore, the focus or 
image of the source of light f x , and the points^ and/ 2 are conjugate foci. 
If the object were at/ 2 , the image would be at/ x . 

The focus thus formed by a convex surface of a medium of higher ju is 
positive or real. If the medium is of lower jli, light entering it is rendered 
divergent, and the focus is negative or virtual. If the surface is concave, as 

Fig. 70. 

in Fig. 70, the reverse is the case, and/ 2 is virtual and on the same side of the 
surface as f\. The boundary plane between the two media may be regarded 
either as the convex surface of the one or the concave surface of the other, 
but it is more convenient to express it as convex or concave to the medium 
of lower index, which usually is air. Thus for a dense medium having a con- 
vex surface in contact with air we could calculate the position of f 2 from the 
refractivity and curvature of the dense medium, or from those of the rare 
medium, the result being the same. 

Defining Terms. — The line/ x ^t/ 2 (Fig. 69), is the principal axis. It is 
normal to the surface and passes through the centre of curvature C and the 
principal foci; all other lines passing through C are secondary axes. A C=r 
is the radius of curvature, and C is the centre of curvature. > f x and f 2 are the 
positions occupied by object and image. F x is the anterior principal focus 
formed by the light proceeding from a distant source on the principal axis 
in the denser medium, and F 2 is the posterior principal focus formed by light 
proceeding from a distant source in the rarer medium. The surface itself 
is the refracting plane and the centre of curvature is also the optical centre. 

Formulae connecting J\ and/ 2 . — In Fig. 71, let be an object on the axis 
of a surface, and / its image formed by refraction of the ray D incident at D. 
From C draw the radius C D and let the angle A D=a, A C D=6 and 
A I D—c. The indices of refraction of the first and second medium are ft x 
and [jl 2 . 

Then /j. x sin i=/bi 2 sin r 

But i=a + b and r=b - c 

Therefore fjb x sin (a + 6)= i a 2 sin (b - c) 



If the incident pencil be small and axial, the angles a, b and c are also small, 
so that we can omit sines, and substitute circular measure for the angles 

Fig. 71. 

Let A=f v A I=f 2 and A C=r the radius of curvature.* 

1\ Mi Un a n ju 2 




M--7J or Vl+V±Jh_ 

fl 2 - fl ± 

The Focal Lengths and Powers of a Curved Surface. — The refractive power 
\/F of a curved surface depends on its curvature and the refractive index of 
the medium, so that an increase in either is accompanied by increase of power. 
The focal length F depends on the refractive power, the one being inversely 
proportional to the other, i.e. the greater the power, the shorter is the focal 

Fig. 72. 

In Fig. 72 P is the principal or refracting plane where all refraction 
takes place. C is the optical centre (or nodal point) because all rays passing 
through it are unrefracted. If light is parallel to the principal axis in the 
dense medium, on emergence into the rare medium it is refracted to meet at 
F x situated on the principal axis. P F x is the anterior focal distance, and F x 
the anterior principal focus. If light diverges from F x it is parallel, after 
refraction, in the dense medium. 

* It is so customary to employ r to indicate the angle of refraction, and r also to 
indicate radius, that this symbol is here retained for both. Although the two may appear 
in the same calculation, they never do so in a formula, so that no confusion is likely to arise. 


If light is parallel to the principal axis in the rare medium, after refrac- 
tion it meets at F 2 in the denser medium. P F 2 is the posterior principal 
focal distance and F 2 the posterior principal focus. If light diverges from F., 
it is parallel, after refraction, in the rare medium. 

In the formula given in the preceding article, if/ 2 is at oo so that the light 
in the denser medium may be regarded as parallel, the term f^o/A becomes 
/V oo=0. 

Then th^/HzJh 

A r 

But/j is now the anterior principal focal length, and is written F v 

Therefore £J*2k or F,= ^ - 

I<j r fa-f^i 

lifi is at oo so that the light in the rarer medium is parallel, the term 
[■i J A becomes //j/ oo =0. 

Then jH IH-IH 

A r 

But/ 2 is now the posterior principal focal length and written F 2 . 

Therefore gU^ or F 2 =-^ 

F 2 . r - fa-Pi 

The planes passing through F x and F 2 , perpendicular to the principal axis, 
are respectively the anterior and posterior focal planes. 

It must be particularly noted that ju x always pertains to the medium in 
which the object is situated, and // 2 to the medium towards which the light 
proceeds, but which may or may not be that in which the image is actually 
formed, since this may be either real or virtual. 

If the one medium is air, ju x =l, so that it can be omitted from the formulae; 
the index of the dense medium we can then call /x, and therefore the formulae 
become simplified to 

F x = and F 2 = ^ 

f/, — 1 fz-l 

Examples. — If ^ of the dense medium is'] -5 and the other medium is air, 
for a radius of curvature of 8 in. we have 

^ 1-5x8 nl . 
F 9 = =24 m. 

2 (1-5-1) 
Thus, with glass, having an index of 1-5, F 1 =2r and F 2 =3r. 
If the surface is Cc. to the air, r is negative and its value prefixed in the 
formulae by a -sign; F x and F % become negative, and are situated on the 


same side of the surface as the source of light, i.e. F 2 is in air and F x is in the , 
dense medium. 

Thus let r=-8" and /*=l-5, then 

F x — r=-16in. 

„ 1-5 x( -8) 

F,= v '=-24 in. 


Suppose parallel light passes from water of / a 1 =l-33 into glass of ^2— 1 "5 
and let r=8 in. ; then 

1-5x8 12 nr „ . 

F 2 = = =70-6 in. 

2 1-5-1-33 -17 

If the light passes from glass into water, 

1-33x8 10-64 

F t — = -=62-6 in. 

1 1-5-1-33 -17 

In these calculations the relative^, which equals /Mg/^, can be found, 
and the calculation then made as if the lower /^ were 1. 

Relationship of F x ani F 2 . — The anterior and posterior focal distances 
measured from the refracting surface are proportional to the indices of refraction 
of the two media. Thus in the examples given we have 

F 2 / a 2 _24_l-5 F 2 _70-6_L5 

Y^/Jt^ieTT F 1 _ 62-6 _ r-33 

Also whatever the refractive indices may be, r=F 2 - F v 

In the examples r=S=2i - 16 or 70-6 - 62-6. 

Thus when/u 1 =l, F 2 =F 1 +r=F 1/ w 3 and F X =F 2 - r= YJfJi. 
That F x is shorter than F % follows from the law of sines. If the two ^'s are 
respectively 1 and 1-5, when light passes into the denser medium sin r is 2/3 
sin i, whereas when light passes into the rarer medium sin r is 3/2 sin i; 
hence the angular deviation is greater when the focus is in the air, it being 
then about | i, than when it is in the dense medium, then it is about ^ i. 

In addition to what is stated in the first paragraph of this chapter, a sur- 
face differs from a lens in that, with the former, the first and last media being 
different, F x differs from F 2 , whereas with a lens F X =^F 2 . Also as shown in 
Fig. 71, the optical centre (or nodal point) C does not coincide with the prin- 
cipal point which marks the refracting plane at A, the apex of the surface. 

To find r or //. — The radius or the refractive index can be found by sub- 
stituting known values for the symbols given in the above formulae, and then 
equating. When the denser medium has a concave surface, care must be 
taken that the - sign be given to F and to r in all calculations. 



Position of an Image- Point. — An object-point situated on the principal 
axis has its image on the principal axis. One situated on a secondary axis 
has its image on that same axis and the focus is a secondary focus. One point 
only of an object is situated on the principal axis; every other is situated on a 
different secondary axis, and similarly with the image of the object. 

The image of a luminous point being on a line drawn from that point 
through C, its position on that line can be determined by calculation or con- 
struction. It is on the opposite side of the refracting surface if the rays con- 
verge after refraction; and on the same side if, after refraction, they diverge. 
The greater the convergence or divergence the sooner do the rays meet, or 
appear to meet, and form the image of the object-point from which they 
originally diverged. 

Fig. 73. 

Construction of Image — Cx. Surface. — In Fig. 73 A B is an object situated 
in front of the refracting surface DP H, its image B' A' can be constructed 
in the following way. 

There are three rays emanating from any point of the object, say A, the 
course of which can be easily traced, viz., 

(a) The secondary ray A C passing through G without deviation. 

(b) The ray A D parallel to the principal axis refracted to pass through 
F 2 . 

(c) The ray A G through F^ refracted parallel to the principal axis. 
Where these rays meet at A' is common to all other rays diverging from A 

and is its image. Similar rays from B form an image at B' , and these define 
the position and size of the real inverted image of the object A B. 
It suffices to draw any two only of the three rays specified. 


Fia. 74. 

Let the object be nearer to the surface than F v as A B in Fig. 74. From 
A draw A C which passes through C without deviation; draw A G parallel 
to the axis; this passes through F. z . Since A C K and G F 2 diverge, they can 
meet only by being prolonged back to A'. Similarly, B G and B H are drawn, 
and produced backwards to B' . Thus A'B' is the virtual erect image of A B. 

Course of any Ray— Cx. Surface.— When the object is situated in the 
anterior focal plane the rays, diverging from any point D (Fig. 75) on it are, 



after refraction, parallel to each other and to a secondary axis DC'm the denser 
medium so that the image, in theory, is formed at oo. Similarly if the object 
lies in the posterior focal plane the light is parallel in the rarer medium after 

Fig. 75. 

Any ray S D Q incident on the refracting surface from a point S on the 
principal axis passes through the first focal plane G H at I), and through 
the principal plane at Q, and its course, after refraction at Q, will be parallel 
to D C drawn from D through C; it therefore takes the direction Qf 2 , and/, 
is the image of S. 

Fig. 76. 

If the point S (Fig. 7G) is within F v draw a line S D backwards to D in 
the first focal plane and forwards to Q in the refracting plane. Draw the 
secondary axis D C K; then S Q Q' will be parallel to it after refraction. 
The latter produced back cuts the axis in/ 2 , which is the image of 8. 

The distance a (Fig. 75) between the ray and the principal axis in the 
refracting plane is equal to the sum of b and d, the distances between the ray 
and the axis in, respectively, the first and second focal planes; the point f 2 
can be located by measuring off on the second focal plane d=a - b, and then 
connecting Q through that point to/ 2 . When S is within F 1 , as in Fig. 76, 

Construction of Image — Cc. Surface. — The rays (a) and (b) as given for 
a Cx. serve also for a Cc. surface, but (b) diverges. 

A B is the object (Fig. 77). Draw A G; this, after refraction, diverges as 
if proceeding from F 2 . Draw A C through 0, whose direction is unchanged 



by refraction. Now A C and A G are more divergent in the denser than they 
were originally in the rarer medium, and when projected backwards meet 
at A', which is the virtual image of A. Similar rays from B locate its image at 
B'. Consequently A' B' is the image of the object A B, and is virtual or nega- 
tive, erect and diminished. 

If rays diverge from a distance equal to F x they have their image in a plane 
D E midway between F 2 and the surface. Let S G (Fig. 78) be incident on a 
Cc. surface. Now S G cuts the plane N at a distance F x from the surface in 
H, and if from H we draw the secondary axis // C we determine the point 
where it cuts D E. The ray is refracted as if it came in the direction/, G, 
so that if S is on the principal axis,/!, is its image. 

Fig. 79. 

If the object-point S (Fig. 79) is within N, draw any line II S backwards to 
the plane N and forwards to Q on the surface. Draw H C cutting D E in K ; 
connect K with the surface to meet H S at Q and where K Q cuts the axis 
in/ 2 , is the image of S. 

General Construction for the Course of a Ray. — This is illustrated in Fig. 80. 
Let A B be the incident ray on a surface whose centre is C. Draw D B C 
normal at the point of incidence, and a tangent K H to the surface at B, and 
at right angles to D BO; then H K is the refracting plane, and the procedure 
is exactly as for a plane surface (Fig. 46). 



The Formula for Conjugate Foci. — The object distance being f v the image 
distance/ 2 , and the first medium being air — 



1 1 jU 


1 1 

Wi A 

As will be seen later with lenses, as well as with mirrors, the divergence 
of the light from the object is added to the power of the surface, and the resul- 
tant convergence or divergence gives the position of the image, real or virtual. 

Size of Image. — The sizes of image and object are to each other as their respec- 
tive distances from the centre of curvature, where the axial rays cross each other. 
This is shown in Fig. 81, and whether the image be real or virtual, the object 
and image always subtend the same angle at C. 

Let the distance of the image from the surface be/ 2 and that of the object 
f v and let r be the distance from the surface to the centre of curvature. 

Fig. 81. 

Let the size of the image be h 2 and that of the object h^ and their distances 
from C respectively I C and G; then the magnification, in the case of a 
real image, is 

/, 2 _IC_ /2 -r 

h OC f 1 + r 

From the original formula 

A A% r ' r r 

that is 

so that 




K Aih 

A. r " r At 

A*fh = A - r 

fifa fi + r 

The linear size of / or 0, when the other data are known, is found from 





If f and/, are in the same terms, then h s is in the same terms as h v 
Should the distance of f» or f x not be known, M can be found from 
F i/(fi^*i) or (f 2 -F 2 )/F 2 respectively. 

Unit Magnification. — The object and its real image are the same size when 
they are at ecpaal distances from C, on opposite sides of the surface. They are 


then in the planes of unit magnification. is at 2F X and / is at 2F 2 from the 
surface, or is at 2F l + r, and I is at 2F 2 - r from C. 
Thus, when M=l, then / 2 =M w f\=fi/p 

^-=-x + ^=~ thatis,/;=2F 1 
Fi /i /« /l 


F 2 /"/i /a /s 

that is, /o=2F 



If the image is virtual, w&A a concave or convex surface, M = - 1 can 
occur only when and I are both at the surface and therefore equally distant 
from C. 

Since the axial rays cross at C, the 7 formed at F 2 of a surface equals that 
formed by a lens whose F=F V and that formed at F x equals that formed by 
a lens whose F=F 2 . 

Examples. — Let r =10 mm., i tt 2 =l-5, / tt 1 =l, and/ x be in the air at 100 mm. 
from the surface. \ its height=10 mm.; then 

1-5 1-5-11 4 . , 150 „„„ 

— r = — = — that is, /,= — =37-5 mm. 

f z 10 100 100 j2 4 

. 10x37-5 ftBf 

The image is real, inverted, 2-5 mm. high. 

Let r=8 mm., ^=1-333, fa—l, and the object be in the denser medium at 
3-6 mm. from the surface and 2 mm. in size; then 

1 1-1-333 1-333 1 , 

— = = /,= - 3-05 mm. 

/ a -8 3-6 3-05 J2 

The image is virtual at 3-05 mm. behind the surface, and 

, 2x3-05x1-33 

h 9 = — =2-25 mm. 

2 3-6 

The pupil of the eye, if 2 mm. in diameter, and 3-6 mm. from the cornea, 
appears to be 2-25 mm. in diameter and about 3 mm. behind the cornea. 
Suppose r= - 3", ^=1-5, ^=1 ,/ 1 =20" and 7^=2". Then 

1-5 1-5-11 13 „ •' 90 „.__ 

A=-^T - 20 = ~ 60 therefore/ 2 = - -=*= - 6 rt 

, 2x6i| 6 . 

and /i = =— in. 

2 20x1-5 13 

Another Expression for Conjugate Foci. — Since 


If ^/ 1 =1 and substituting F for ju»F l 

±A* « frJ* and fW* 

Examples. — Suppose the object be 20 inches in front of a Cx. surface where 
F L =6 in. and -F 2 =9 m * 

,20x9 180 

Then / 2 =^^^=^r = 12 " in - 

ya 20-6 14 

If an object is 5" in front of a surface of F 1 =6 in. and F 2 =9 in. 

5x9 45 

Then f<,= = — = - 45 in. The image is negative. 


If /i is situated at F x the denominator is 0, so that/ 2 is at oo ; if/ x is at oo, 

theny 2 corresponds to F 2 . 

Let the one conjugate be 12£ in. behind Cx. a surface whose F z =9 in., 

and 2^=6 in., then 

, 12fx6 77| nn . 
/=■ , ==—^=20 in. 

This example should be compared with the one previously given, where 
the object is in front of the refracting surface, 20" and 12y" being conjugates 
for the given surfaces. 

An object 20 inches from a Cc. surface, whose F x and 2 F are respectively 
— 6 and -9 in. has its virtual image at 

, 20x(-9) -180 

/,= = — — = - ok in. 

J2 20- (-6) 26 ° 

Fig. 82. 

Conjugate Focal Distances — Cx. Surfaces. — If the is at oo represented 
by A (Fig. 82), the light is parallel and, after refraction, meets at F 2 . This 
is the nearest point to the surface at which a real focus can be formed. 

If the light diverges from/ x at a finite distance from the surface, some of 
the converging power of the medium is required to neutralize the divergence 
of the light and there is less residual convergence; the light therefore is con- 
vergent to a greater distance behind the refracting surface than if the light 
had been previously parallel; the I in the denser medium is at some point f 2 
situated between F 2 and oo. 

As the O approaches from oo the I recedes from F 2 , and vice versa, until 
when the is at F 1 the I is at oo. 

If the object is nearer than F x as at O, the image is at I on the same side 


of the surface. As then further approaches the surface so also does /, 
and when touches the surface 1 does so also. 

When is within the dense medium, and the light is parallel, 1 is at F.\ 
as approaches F 2 so I recedes from F x \ thus when is at/j the / is at/ p 
and when is at F 2 the image is at oo. 

When lies nearer to the surface than F 2 the image is virtual and on tho 
same side of the surface as and within the dense medium. Thus in Fig. 83 

Fig. 83. 

if the object is at 0', the image is farther away at 7'; if the is at C then the 
7 also is at C, and if the object is at 0" then the image is nearer the surface 
at 7"; when touches the surface 7 does so also. If light diverges from a 
point beyond C it becomes less divergent by refraction at the surface, and if 
from a point nearer than C it becomes more divergent. 

It should be noticed that when the Ois at the surface of a Cx. dense medium 
the I is the same size, and as the moves away from the surface the 7 in- 
creases in size until, when is at C, I is there also, but with a magnification 
equal to [J, (the dense medium being assumed to be bounded by air). As the 
moves beyond C towards F 2 the image continues to increase in size, until, 
when is at F 2 , I is at oo and infinitely magnified. 

Conjugate Focal Distances — Cc. Surfaces. — When the surface of the 
dense medium is Cc. and the is at oo the 7 is at F 2 . This is the most dis- 
tant point from the surface at which an image can be formed. If the is 
within oo, the original rays being divergent are rendered still more divergent 
after refraction than if they had been originally parallel ; hence the 7 is formed 
nearer to the surface, that is, as approaches the surface so also does 7. 

The virtual 7 is nearer to the surface than the so long as is beyond C; 
when is at C so also is 7, but the latter is diminished ju times; when is 
within C then I is beyond 0, and when touches the surface I does so also 
and M=l. 

When the is in a Cc. dense medium, unit magnification occurs when 
touches the surface; as moves away towards F x the I becomes progres- 
sively smaller until when is at oo, 7 is at F k and proportionately diminished. 

Real Conjugates are always interchangeable. If the is a,tf v its 7 is at 
f 2 , and the positions could be reversed, as can be seen from the various 
examples given. 

Virtual Conjugates. — Virtual conjugate foci, formed by Cx. or Cc. surfaces, 
are not interchangeable as are real conjugates, but if the light were directed 
converging towards/ 2 the image formed would be atf v 


Newton's Formulae for Conjugate Foci and M. — If A and B be respectively 
the distance of from F x and of / from F 2 , then 

I F, B 
AB=F lF2 and It-g-^r 

Dioptral Formulae. — The diopter expresses refracting power and D=\00/F, 
F and r being in cm. The anterior and posterior powers are — 

D = 100 fa- fr) D ^ 100 (/H-/h) 

A rfii p rft 2 

D A : D p as fx 2 : /n v 
For conjugate foci D A =d 1 /j, l + d 2 fi 2 or D p =cZ 1 /a 2 + ^2/^1 


As already defined, a real I is formed by the focus of convergent light, 
and therefore actually exists; a virtual I is formed by divergent light, and 
is imaginary, merely appearing to exist. 

Images are seen in the same way as an ordinary object, from which light 
diverges, and of which a real I is formed on the retina of the eye. To view 
a virtual image, the eye must look through a single lens, whether Cx. or Co., 
but to see a real I, formed in the air or on a screen, the eye must be placed 
a reasonable distance behind the I. The convergent light from the latter 
crosses and diverges as from an ordinary object, and can therefore be viewed 
and magnified by other lenses, as in the telescope and microscope. 

Similarly, a viitual I is seen by looking into a mirror, whether plane, Cx., 
or Cc. ; a real image formed by the convergence of light from a Cc. mirror is 
seen, as in the case of the Cx. lens, in the air or on a screen. 

Position of Object. — It is always taken that an object is in front of a lens 
or mirror, and the image is in front or behind according as it is, respectively, 
on the same side as, or on the opposite side to, the object. 

Optical Signs. — In this work the following convention is followed. Light 
divergence is considered negative, and convergence is considered positive. 

Surfaces, mirrors or lenses that cause, or tend to cause, convergence of 
light, are positive, as also are their focal lengths and powers, and the real 
images and foci produced by them : to all these the + sign is assigned. 

Surfaces, mirrors or lenses that produce, or tend to produce, divergence, 
together with their focal lengths and powers, and virtual images and foci, are 
negative, and given the - sign. 

Thus when a convex spherical surface of glass is in contact with air, 
refraction occurs, and this may be taken as due either to the Cx. glass sur- 
face or to the Cc. air surface; both are + since both cause convergence of 
parallel light. If a double Cc. air lens be in water we can consider the result- 
ing converging effect from the Cc. air surfaces, or the Cx. water surfaces. 
A Cx. surface is not necessarily positive, nor a Cc. negative; when they reflect 
they are the reverse, as they are, also, when refracting if of lower /u than the 
adjacent medium. Usually, however, in optics, a Cx. refracting surface is 
positive and a Cc. negative because it has a higher /.i than the adjacent air, 
but this may not be the cage when light passes successively through various 



Axial and Other Rays. — It is most essential to differentiate between 
the direction of axial rays and that of the rays from the various points on an 
object, with reference to their axes. 

From each point of the object a pencil of rays diverges and each pencil 
has an axis, which is the axial ray of that pencil. Axial rays always converge 
to the optical centre of the lens, and their convergence governs the size of 
the angle subtended by the object and the image at the lens. 

The rays themselves always diverge from the luminous point to the lens, 
and their divergence governs the position or distance of the image, the rays, 
after refraction being more or less divergent or convergent, according to the 
original divergence, and the diverging or converging power of the lens. 
Parallel light is light having a negligible degree of divergence. 

These most important considerations, for students are apt to confuse the 
conditions, should be carefully noted. Thus, in a diagram which shows 
light parallel to the axis, and incident on various parts of the lens surface, 
the rays are presumed to originate, not in various points, but in one single 
point on the axis. These considerations apply not only to all lenses, but to 
surfaces and mirrors as well, and all positions of the object. 

Definition of Lens. — A lens is a transparent body usually made of glass, 
bounded by two surfaces, both of which are curved or the one may be plane. 
It is usually surrounded by air. This definition covers all forms of convex 
and concave sphericals, as well as cylindrical and other special forms of lenses. 

Prismatic Formation. — If a block of glass is formed by two similar prisms 
A C D and BCD base to base, as in Fig. 84, incident rays such as E are bent 
towards the base of the prism AC D, and rays such as F are bent towards 


Fig. 85. 

the base of the prism B C D, so that those refracted by the one prism meet 
those refracted by the other. One ray, viz., G C D H suffers no deviation 
since it coincides with the base of both prisms; L and M are incident nor- 
mally to both surfaces, and are therefore also not deviated. 

If the prisms, as in Fig. 85, be edge to edge all rays incident on them, 
being refracted towards the bases, are deflected from the common edge, 
except the central ray incident at the junction of the two edges. 

What is true of two prisms is also true of any number, and a Cx. or Cc. 
spherical lens may be considered as if formed of an infinite number of prisms 
whose bases or apices respectively have a common centre; every meridian 
may be regarded as if formed of a series of truncated prisms of different 



angles of inclination, increasing gradually towards the periphery, but having 
a common base-apex line. 

Any two point areas as A and B (Fig. 86) opposite each other constitute a 
portion of a prism whose base, in the Cx., and whose apex, in the Cc, is turned 
towards the principal axis of the lens. The areas A and B, near the periphery 
of the lens, are more inclined towards each other than C and D, situated 







e! r 

C M H 




/ \ 

Fig. 86. 

nearer to the axis, and the inclination between the surfaces decreases gradually 
until at G H on the principal axis they are parallel. Since the angle formed 
by A and B is greater than that formed by C and D, a ray passing through 
A B is bent to a greater extent than one passing through C D, while the ray 
which passes along the axis is not deviated at all. 

Each zone of a lens, therefore, whether concave or convex, has a refractive 
power which becomes greater as its distance from the axis is increased, and it 
is due to this fact that rays diverging from a point, and incident on the lens, are 
brought to, or appear to diverge from, a common focus practically as a point. 

1' &' 3' 

Fig. 87. 

Forms of Lenses. — There are (Fig. 87) four forms of thin convex and four 
of concave spherical lenses: 

1. Double Cx. or equi-Cx. having two equally curved Cx. surfaces. 
1'. Double Cc. or equi-Cc. ,, ,, ,, Cc. ,, 

2. Bi-Cx. having two unequally curved Cx. surfaces. 
2'. Bi-Cc. „ „ „ Cc. 

3. Plano-Cx. having one Cx. and one plane surface. 
3'. Plano-Cc. ,, ,, Cc. ,, ,, ,, ,, 

4. Meniscus or periscopic Cx. having one surface Cx. and the other Cc, 

the Cc. being the weaker power. 
4'. Meniscus or periscopic Cc. having one surface Cc. and the other Cx., 

the Cx. being the weaker power. 
Variations of the above, due to increasing the interval between the two 
surfaces, are treated in the chapter on thick lenses. 



Terms of a Lens. — Let Fig. 88 represent a thin Cx. lens; C C are the 
centres of curvature, and the optical centre. The line A OB passing through 
the two centres of curvature, and the optical centre, is the principal axis ; 
it is normal to both surfaces of the lens. The plane L L passing through 

0, perpendicular to A B, is the refracting plane, on which all the refraction 
effected by both surfaces of a thin lens is presumed to be united. Any lines 
as D D, E E directed to 0, are secondary axes ; they are presumed to pass, 
obliquely to the principal axis, through the lens, and without any deviation. 

d _ Z 

Fig. 89. 

Spherical Formation of Lenses.— In each of the diagrams in Fig. 89, which 
shows the formation of lenses by the intersection or non-intersection of 
spheres and planes, the radius of curvature is a line drawn from the centre 
of each sphere to its corresponding surface of the lens. The optical centre 
in each case is 0. 

In the equi-Cx. and bi-Cx. (1 and 2), and the equi-Cc. and bi-Cc. (5 and 6) 
the centres C and C are on opposite sides of the lens. 

In the plano-Cx. (3) and plano-Cc. (7) the centre of curvature of the plane 
surface is taken to be at oo and therefore on either side. 


A Cx. lens consisting of a complete sphere has the centres of its opposite 
surfaces coincident. 

In the periscopic Cx. (4) and periscopic Cc. (8) the centres are on the 
same side. 

The Optical Centre. — In any lens there are innumerable pairs of points 
on the two surfaces as R and S (Fig. 90), such that tangents drawn to the 
surfaces at these points are parallel. A ray T R incident at one of these points 
R emerges from the other S, and its final direction S V is parallel to its initial 

Fig. 90. 

course T R, as though it had passed through a parallel plate. The ray is not 
deviated, but is merely laterally displaced by an amount depending upon the 
radii, thickness and jj, of the lens. There are any number of pairs of points 
similar to R and S, and they are located by drawing from the centres of 
curvature any two mutually parallel radii such as P R and Q S. While in 
the lens the ray takes the direction R S, cutting the principal axis P Q in 0, 
which is a fixed point. is the optical centre, and any line R S passing 
through it is a secondary axis. 

The point N x on the principal axis, towards which a secondary axial 
ray is directed, is the first nodal point, and N 2 , from which it apparently 
emerges, is the second nodal point. From these points the principal and con- 
jugate focal distances are measured, since, as will be shown later in the 
chapter on thick lenses, it is on planes drawn perpendicular to the axis through 
Nj and N 2 that the refraction of the surfaces of the lens is presumed to be 
united. The nodal points are also referred to as principal or equivalent 
points, and the difference between these terms will be explained later. For 
the present lenses will be regarded as thin, the thickness being negligible in 
comparison with the focal length. All lenses employed in visual optics are 
considered to be thin, as distinct from those whose thickness cannot be dis- 
regarded without introducing appreciable error in calculating the power and 
focal length. 

In a thin lens we may assume the interval between the nodal points to be 
so small that they fuse into the optical centre. Similarly the equivalent planes 
passing through the nodal points are also considered to unite into a single 
refracting plane passing through the optical centre, from which all distances 
and foci are measured. The refracting plane is the base-apex plane of the 
component prisms of a symmetrical lens. 


Calculation of O.C. — The position of the optical centre depends on the 

two radii of curvature r x and r 2 and t the thickness of the lens, and is calculated 


tv fv 

0= — — from the one surface and — — from the other. 
7\ + r 2 r ± + r 2 

Thus in a bi-Cx. lens where t = -2 inch, and r x and r 2 are respectively 
6 and 10 inches, 

^•2x6 -2 x 10 

0=- — —=-075 m. from r,, or — =-125 in. from r 9 

6 + 10 v 6 + 10 2 

O lies on the axis proportionately nearer to the surface of greater curvature. 
When both surfaces are Cx. or both Cc, O lies within the lens, but in a peri- 
scopic lens O lies outside it on the side of the surface of greater power. If 
one surface is plane O lies on the vertex of the curved surface. The distance, 
if positive, is measured from each surface inivards towards the other surface, 
but if negative it is measured outwards. 

Let t = *2 in., r x of the Cx. surface be 9 in., and r 2 of the Cc. - 12 in. 
Thenr x + r 2 = 9 - 12 = - 3 and O = 1-8/- 3= - -6 in.; that is, -6" beyond 
the Cx. surface. 

Construction for 0. C. — The method of finding the O. C. by construction is 
described in connection with Fig. 90; and that of any form of lens is shown 
in Fig. 89. From C, in any of the diagrams, draw a radius C D to the surface. 
From C draw a radius C E, to its corresponding surface, parallel to C D. 
Connect the extremities by the line D E, and where it cuts the principal axis 
at 0, is the 0. C. 

In (3) and (7) C being at oo, the only radius from C that can be parallel to 
C E, is the principal axis itself. 

In (4) and (8) D E must be produced to cut the principal axis. 

Characteristics of a Convex or Positive Lens. 

(a) It is thicker at the centre than at the edge. 

(b) It forms a magnified image of an object held within the focus. 

(c) It forms on a screen an inverted real I of, say a distant flame or window. 

(d) It causes the virtual image of an object, viewed through it, to move 
in the contrary diiection as the lens is moved. 

Characteristics of a Concave or Negative Lens. 

(a) It is thinner at the centre than at the edge. 

(b) It diminishes the apparent size of an object seen through it. 

(c) No image can be projected by it on to a screen. 

(d) When moved, an object seen through it appears to move in the same 

Properties of Lenses. — A Cx. lens has positive refracting power and can 
form a real focus and image ; it renders parallel light convergent, and divergent 
light less divergent, parallel or convergent as the case may be. 



A Cc. lens has negative refracting power and can only form a virtual or 
negative focus and image; it renders parallel light divergent, and divergent 
light more divergent. 

The general effect of every spherical (and cylindrical) lens is, as with a 
prism, to bend incident light towards the thickest part. The above apply 
when the lens has a higher /x than the surrounding medium, otherwise the 
reverse occurs. 

When discussing lenses we take them, unless otherwise stated, to be in air. 

The Focus. — A real focus is that point at which rays from a point actually 
meet after refraction. 

A virtual focus is that point from which rays from a point appear to diverge 
after refraction. 

Fig. 91. 

Fig. 92. 

The principal focus F of a Cx. lens is positive and is on the principal axis 
on the opposite side of the lens from the source of light. 

The distance between the 0. C. and F is the principal focal distance of a 
thin convex lens (Fig. 91). 

The anterior focus F t is on the same side as the light source and is that 
point from which light must diverge in order to be parallel after refraction. 

The posterior focus F 2 is on the opposite side to the light source and is 
that point to which originally parallel rays are converged after refraction. 
The parallel rays in the figure are presumed to diverge from a single point 
on the principal axis at oo. 

In a lens F x = F 2 always, provided there is the same medium on both 
sides of it. 

F being the focus of originally parallel rays, it is the nearest point to a Cx. 
lens at which a focus of natural rays can be obtained. 

The principal focus F of a Cc. lens is negative, and is situated on the 
principal axis on the same side of the lens as the source of light. The distance 
between and the focus, Fig. 92, is the principal focal distance, F being the 
point from which, after refraction, parallel rays appear to diverge. It is the 
furthest point from a concave lens at which a focus can be obtained for natural 

A secondary focus is one formed on a secondary axis. 

A conjugate focus denotes one formed of appreciably divergent light, as 
distinct from a principal focus. 

Lens Value. — The value of a lens is expressed by its principal focal length]?, 
by its focal power 1/F; or by its refractive power D. These properties depend 


solely on curvature and /li, since in a thin lens, as stated, the thickness is 
ignored. F and 1/F, being reciprocals, vary inversely with each other, as 
the one is increased the other is proportionately diminished. 

Fig. 93. 

Formulae for F. — Let AB (Fig. 93) be a bi-convex lens of radii r l and r 2 
and index /u 2 , that of the surrounding medium being ja v Then if any ray L M 
parallel to the principal axis be incident at M it will be refracted and tend to 
focus at/ 2 , the posterior focal distance of the first surface. 

Thus / 2 - ^ 

Therefore f 2 is virtually an object with respect to the second surface. 
Since the thickness is disregarded we may take A F as equal to B F. For 
the second surface,// and// being the conjugates, 

But the image distance/ 2 of the first surface is the virtual object distance// 
of the second surface, so that substituting the former for the latter and using 
the negative sign, we get 

U /ViA/^-^i) - r 2 
or t*i_! h-t*i fa-fh 

The final image distance// is the principal focal distance F ; 

$-<*-*) (I + I) or F = r /™ 

i \r l r 2 J (r! + r 2 ) (f*2-f*x) 

These are the general formulae for a thin lens in any medium, but if the 
outer medium is air, which is usually the case, ^=1, and can be omitted. 
Then taking [x as the index of the lens, the above simplify to 

F r \r t r 2 f {r x + r 2 ){ii-\) 


Since \/r 1 and l/r 2 represent the curvatures of the two surfaces, the power 
of a lens is equal to the sum of its curvatures multiplied by the refractivity of the 
medium of which it is made. 

Convex surfaces of a lens are here always taken as positive and concave 
surfaces as negative, and the focus is of the same sign. 

If one surface is positive and the other negative, the focus will be positive 
or negative as the one or other predominates in curvature. 

Examples. — A Cx. lens of ^=1-54, having surfaces of radii of 8 in. and 
5 in. F is positive, thus — 

8x5 40 Kn . 

F=, =• =5-7 in. 

(8 +5) (1-54-1) 7-02 

If the surfaces are concave the negative sign must be prefixed to each; 

and F also is negative. 

-8x(-5) 40 

F= - - = = - 5-7 in. 

(-8-5^ x (1-54-1) -7-02 

In a periscopic Cx. let the two surfaces be respectively - 8 in. and + 4 in. 
and j a=l-6. Here F is positive. 

-8x4 -32 

F= -=— — = + 13-3 in. 

(-8 + 4)x-6 -2-4 

In a periscopic Cc, with surfaces of +8 in. and - 4 in. F is negative. 

8x(-4) -32 

F= - = — -= - 13-3 in. 

(8-4)x-6 2-4 

Simplified Formulae. — If both surfaces have the same radius, i.e. r 1 =r z , as 
in an equi-Cx. or equi-Cc. lens, the formula becomes simplified, for 


(r 1 + r 2 )(^-l) 2/-(^-l) 2(^-1) 

5 5 

Thus if r, and r,=5 andu=l-54, F= — — ^=r7^=4-63 in. 
1 i ' -54x2 1-08 

If ^==1-5 in equi-Cx. or equi-Cc. lenses F=r. 

If one surface is plane, then r x = oo and 1/^=1/ oo=0, so that it may 
be ignored and only the curved surface considered. Then 

F=- ' 


If ^=1-5, in a piano Cx. or Cc. lens F=2 r. 

To find r or /u. — To calculate r x or r 2 when that of the other, as well as fjt 
and F, are known, the values of the known quantities are substituted for the 
symbol in the formula and the equation then worked out, as in the following 
examples : 



If r 2 =8 in. and /t= 1-5 what radius should be given to the other surface 
bo that F=6 in. ? 




8r a 


8r x 




{S + rJx-5 

24+3r 1 =8r 1 

r,= +4-8 in. 

4 + -5^' 

5r 1= 24 

What should be the radius of the Cc. surface of a meniscus when that of 
the Cx. is 5 in., F being 12 in. and /t= 1-6 ? 



{5 + rJ-G' 

or 5r 1 =12x(3 + -6r 1 ) 




= ^16-36 in. 

The same procedure is followed for finding fi. 

If F=24 cm. and the radii are x 6 and - 12 cm., then/t is found from 


6x -12 


(6-12)(m-1) -6^ + 6 

-72= -144^ + 144 and p=l-5 

Distance of F. — In all cases F X =F 2 . Whether the one or other side of an 
equi Cx. or Cc. lens is exposed to the light, F is at the same distance from the 
back surface since is midway between them; but this is not the case with 




FiG. 94. 

Fig. 95. 

other forms of lenses. In Fig. 94 the principal focal distance F of a bi-convex 
lens being measured from 0, the distance of F behind the posterior surface 
depends on which surface faces the light. If A faces the light F lies further 
from B than it does from A when B faces the light. With the periscopic Cx., 
as shown in Fig. 95 (or the periscopic Cc), the difference in the distance of F 
as measured to the right from B or to the left from A is marked; also, but to 
less extent, with the plano-Cx. and plano-Cc, F being measured from the 
curved surface, since is situated thereon. 

Relative Powers. — With similar radii, \h.e power of a lens in air is propor- 
tional, not to//, but to (/j, - 1), the refractivity of the medium. Thus if two 


lenses A and B be ground with the same radii on glasses of different ju's, the 
ratio of their powers is as (f.i A - 1): (// B - 1), their focal lengths being as (/a, b - 1): 
(jt A -I). 

Calculations when /u l is not Air. — Let a double Cx. lens of ^=1-54 and 
8 cm. radius be in water 

8x8x1-33 85-12 

Then F= (8 + 8) (1-54- 1-33) = S^T 25 ' 33 0m ' 

Or the relative index fjL r can be found (rom jli 2 //li v and the formula for thin 
lenses in air employed. Here// r =l-54/l-33=l-158, 


Then F=- — -—=25-33 cm. as above. 

(8 + 8) x -158 

Let a similar lens, but of ,14=1-33, be placed in cedar oil of //=l-54, then 

8x8x1-54 98-66 

F= = , „„ = - 29-33 cm. 

(8 + 8) (1-33-1-54) -3-36 

The lens has a negative power, and a Cc. air lens in water has a positive 
power. Dr. Dudgeon constructed such a lens to enable divers, without 
helmets, to see under water. It consisted of two watch-glasses of deep curva- 
ture cemented into a vulcanite ring. The Cc. surfaces being outward produced 
two Cx. water surfaces in contact with them, and thus gave the required 
refractive power. 

Let a Cc. air lens be of 10 inch radius on both surfaces be in water. 

„ - 10 x -10x1-33 100x1-33 133 

Then F= = = = + 20. 

(-10 -10) (1-1-33) -20x--33 6-66 

A Cx. water lens of the same radius in air has F=15 in. The difference, 
when the conditions are reversed, is. similar to that between the anterior and 
posterior foci of a single surface. If light passes finally into a rare medium 
F is shorter than when it passes finally into a dense medium. 

Dioptral Formulae, r being in cm. 

General formula 

D = 

v?4°) ( 

■ /*1 

Lens in air 


100 (/i 


Equi Cx. or Cc. 

D _200( / a- 


Piano Cx. or Cc. 

D _100(^ 



/100 100\ 
\r 1 + rj 




Course of Light — Cx. Lens. — A beam of rays, shown by the thick lines 
in Fig. 96, incident on a Cx. lens parallel to the principal axis F x F 2 is re- 

A * 

\ C J 


/ n 




Fig. 96. 

fracted to meet at F 2 , the second principal focus, situated on that axis. 
C D drawn through F 2 perpendicular to the axis is the second focal plane. 
If the light diverges from F x (shown by the dotted lines), they are parallel 
after refraction. A B perpendicular to the axis through F ± is the first focal 

If the object-point is situated on a secondary axis E F 2 , the rays from it 
focus at F 2 , on that same axis. 

Construction of I for Cx. Lens. — There are three rays diverging from any 
point whose course, after refraction, it is easy to follow, viz. : 

(a) The secondary axial ray which passes through without deviation. 

(b) The ray parallel to the principal axis, passing through F 2 . 

(c) The ray through F x refracted parallel to the principal axis. 

Two only of these rays are needed, since where they meet all other rays 
diverging from that same point also meet. 

Fig. 97. 

Fig. 98. 

Real I. — Draw from A (Fig. 97) a ray A E parallel to the axis and, when 
refracted, through F 2 . Draw the secondary axial ray A straight through 0. 
These meet at A', the image of A. In the same way B', the image of B, can be 
constructed. B' A' shows the position and size of the real inverted image of 
the object A B. 

Virtual I. — From A (Fig. 98) draw A E parallel to the axis; E F 2 is the 
course after refraction. Draw A passing through the optical centre. 
Since they are divergent after refraction, they can meet only by being pro- 
duced backwards to A', the virtual image of A. Similar rays drawn from B 



locate its image as B', and A' B' is the complete virtual erect image of the 
obj ect A B. 

When the object is in the anterior focal plane, the rays from each point 
are, after refraction, parallel to each other and to a secondary axis, the image 
being, in theory, at infinity. 


Fig. 99. 

The Course of any Ray. — To construct the image of A, a point on the 
principal axis (Fig. 99), draw any line A KB, cutting the first focal plane at K 
and the refracting plane at D. From K draw a line through and from D 
draw DB parallel to K which cuts the principal axis at B, the image of A. 

Fig. 100. 

If the object-points is nearer than F 1 (Fig. 100) horn A draw any line A E, 
and from F x draw F x C parallel to A E which takes the direction C D parallel 
to the principal axis and cuts the second focal plane in D. Connect D and E 
and produce to A' on the principal axis; then A' is the virtual image of A. 









p^ L 



Fig. 1 


Course of Light — Cc. Lens. — If a beam of light parallel to the axis (Fig. 101), 
is incident on a Cc. lens, they apparently diverge, after refraction, from F, 



and A B perpendicular to the axis through F is the focal plane. A point 
on a secondary axis as F' has its image on that same axis. 

Fig. 102. 

Construction of I for Cc. Lens. — The rays (a) and (b) given for the construc- 
tion with a Cx. lens serve also for a Cc, but (b) diverges. From A (Fig. 102) 
trace A 0, the secondary axial ray. Draw A E parallel to the axis and re- 
fracted as if diverging from F. These rays appear to diverge, after refraction, 
from A' the image of A. Similar rays from B locate B', its image. The com- 
plete virtual erect image of A B is A' B' . 

x X 





<""" ? 

X J 

3- JI 

Fig. 103. 

The Course of Any Ray. — To construct the image of a point A on the axis 
(Fig. 103), draw any ray ABC cutting the focal plane in B and the refracting 
plane in C. Erect x y, a plane midway between the focal and refracting 
planes. From B draw B C 0, connect with C", and prolong to A' on the 
principal axis; A' is the image of A. 

General Construction for the Course of a Ray. — The principle is shown in 
Fig. 80, for a surface. For a lens or sphere, the course being determined 
for the first surface, a second construction is needed for the second. 

Numeration of Lenses.— Lenses are numbered by the focal length, com- 
monly termed the inch system and by the dioptric or power system. 

For the focal length system the unit is a lens of one inch focus. Since F 
varies inversely with power 1/F, a lens which brings parallel light to a focus 
at 10 ins. or at 20 ins., has respectively 1/10 or 1/20 the power of the unit; 
while one whose F=l/2 in. has' twice the power; thus focal length and power 


are reciprocals of each other. The abbreviations Cx. and Cc. are commonly 
employed in conjunction with the focal notation of lenses. 

One disadvantage is that the inch, in various countries, differs in value, 
so that a lens of given F in one country may not be the same as one of similar 
number in another. Thus one of 18 French (Paris) inches is about equivalent 
to one of 20 English or American inches. Again, the intervals between the 
lenses, although regular as to their F's, are irregular as to their powers; thus 
there is a far greater difference between the powers of a 5 and a 6 inch, than 
between a 15 and a 16 inch lens. Further, ophthalmic and practical calcula- 
tions involve the use of vulgar fractions. 

For theoretical calculations the F system is superior, and is therefore 
mainly used in textbooks, although it is entirely superseded by the dioptric 
system in practical visual optics. 

The dioptric system is based on the refractive power, and the unit is the 
diopter, which is that power causing parallel light to focus at 1 metre. The 
diopter of refraction is a measure of converging or diverging power, while the 
metre is a unit of linear measurement ; yet it is often convenient to express 
distances in dioptric measure. The symbols + and — are always used 
with this system. 

1/P is commonly termed focal power to distinguish it from the dioptric 
power D. 

The dioptric system is in practice much more simple than the inch, and is 
universal. The unit being weak, the power of most other lenses is a whole 
number, while if fractions are involved they are expressed as decimals. The 
intervals between the lenses are uniform as regards their refracting powers. 

If 1 D has F=l M, a 4 D lens, having four times as much power, has 
F=l/4 M. But since the M can be sub-divided into 100 cm. (or 1000 mm.) 
the F of a 4 D is more conveniently expressed as 100/4=25 cm. A 10 D lens 
has ten times the power; therefore its F=100/10=10 cm., or 1/10 that of 
the unit. A 0-50 D has half the power; consequently its F=100/-5=200 cm., 
or twice that of the standard lens. 

Conversion. — Since the + 1 D lens has F=l M, or 40 inches, it is equal 
to No. 40 of the inch system, and a 40 D lens is the same as a 1 inch lens. 
The M=39-37 English inches, and for all practical purposes may be regarded 
as equivalent to either 40 or 39 inches. Therefore conversion from the one 
system to the other is effected by dividing 40 or 39 by the known number. 

Thus 2-5D=40/2-5=16in., 13 D=39/13=3 in., 

2in.=40/2 =20 D 13 in.=39/13=3 D. 

Some numbers do not divide evenly into 40 or 39, but small remainders 
need not be considered beyond the 1/4, 1/2 and 3/4 in the lower inch numbers, 
and -25, -50, and -75 in the dioptral numbers. For instance, 3-50 D=No. 11"; 
3-25 D=No. 12"; 4-50 D=No. 9", etc. 

To Find F or D. — Dividing 40 or 100 or 1000 by the D number gives F 
in inches, in cm., or in mm. respectively. 


Thus, 5 D lens has F=40/5=8 in., 100/5=20 cm., or 1000/5=200 mm. 
If F is known in cm., mm., or inches, the dioptral number is found by 
dividing respectively into 100 or 1000 or 40. 
Thus, if F=200 mm., D=1000/200=5. 
If F=20 cm., D=100/40=2-5; if F=160 in., D=40/160=-25. 

Obsolete Systems. — Originally lenses were numbered according to the 
radius of curvature. No. 10 meant a DCx. or DCc. of 10" radius. Cc. sphericals 
were formerly numbered by an arbitrary system commencing at 0000 — the 
weakest — and terminating with No. 20 — the strongest. 

Addition of Lenses. — The combined strength 1/F of the two thin lenses 
in contact, whose values are indicated by their focal lengths F x and F 2 re- 
spectively, is obtained by the addition of their focal powers, thus 

1/F=I/F 1 + 1/F 2 

If the two lenses be, say, 24" Cx. and 10" Cx. 

l/F=l/24 + 1/10=34/240=1/7 approx. 

The two are equivalent to a lens of 7" F. 

Here convergence has been added to convergence. If the two lenses are 
Cc, divergence is added to divergence. Thus, if they be 5" and 6" Cc, 

1/F= - 1/5 + ( - 1/8)= - 13/40= - 1/3 approx. 

When the one lens is Cx., and the other Cc, 1/F is positive or negative 
according as F x or F 2 is the shorter. The convergence of the one and the 
divergence of the other neutralise each other more or less, and the residual 
power of the stronger is that of the combination. Thus, with a 15 Cx. and a 
12 -Cc 

1/F=1/I5 + ( - 1/12)=12/180 - 15/180= - 3/180= - 1/60 

A 20 Cc. and a 10 Cx.=l/10 + ( - 1/20)= + 1/20, i.e. a 20 Cx. 
The addition of several lenses is achieved in a similar manner; thus 
10 Cx., 16 Cx., 7 Cx., and 5 Cc. make 1/10 + 1/16 + 1/7-1/5=59/560, 
that is, 9| Cx. approx. 

The combined strength D of two dioptral lenses D x and D 2 in contact is 

D=L\+D 2 

Thus, +2 D and +4 D=+6 D; -5-25 D and -2-50 D=-7-75 D; 
+ 4 D and - 3 D= + 1 D; +3 D and - 3 D=0, they neutralise. 

+ 7 D+4-50 D + l-75 D - 6-50 D=+6-75 D 

Conjugate Foci. — If/ 3 be the distance from the optical centre from which 
light from the object diverges, then \/f x represents that divergence; if f 2 
is the distance of the image then l/f 2 is the ultimate convergence or divergence 
of the light which produces the image. 1/F is positive or negative according 
as it pertains to a converging or diverging lens respectively, while \Jf x is always 



negative. l/f 2 ts found by adding algebraically the divergence of the light \/f 
to the converging or diverging power of the lens, that is, 

1 i /n 


or — =— - 

i 111 

whence -=— +— 

* J\ J2 


The power of the lens is equal to the sum of the reciprocals of any pair of 
conjugate foci, or to the sum of its actions on the light. 

With a Cx. lens f 2 is positive or negative according as the convergence 
of the lens 1/F is greater or less than the divergence of the light l/f v With a 
Cc. lensy* 2 is always negative, since the divergence of the light is added to the 
divergence of the lens. It should be observed that calculations for conjugates 
are the same as the addition of lenses. 

By inverting the formula we get a sometimes useful variation in 

/i/i „ , fJf .... , W 




f & 

and f x — 

/■-I 1 

It can also be written, F//^ + F//" 2 =1 

Geometrical Proof. — In Figs. 104 and 105, A Bis the object and B' A' is the 

image. The triangles A OB and A' OB' are similar, as are also the triangles 
D F and A' F B\ also A B=D 0. 




Fio. 104. 

For the Cx. 

5=/i; B'=f; F=F; B'F=f„ - F. 
A/A=W* - X) or//, - F/f=Ff. 
AA-F(f +/■») ° r 1/^V/x + l/fr 

Fia. 105. 


For the Cc. B=f x ; B'=f 2 ; F=F; B'F=F-f.-,. 

Therefore A/A=F/{F -/■) or Ff, -fJ^Ff,. 

Then fxA=Ftfi-A) or - 1/JML/Ji- l// r 

Conjugate Foci — Examples — Cx. Lens. — The converging power of the lens 
is decreased, neutralised, or exceeded by the divergence of the light from the 
object. The image is real so long as the object is beyond F, and it is virtual 
when the object is within F. Approach of the object causes the light to be 
less convergent after refraction, so that any real conjugate focus is more 
distant than F, which is the nearest point at which a real image can be formed 
from natural rays. 

If F=8" and/ x is at 40", then/ 2 will be at 10", for l/f z =l/8 - 1/40=1/10. 
This is proved by 1/10 + 1/40=1/8. 

If a real image is 16" behind a 7" Cx., the object is at 12|". 

l//l=l/7 - 1/16=9/112. / 1 =112/9=12|. 
When the object is at oo, the image is at F since 

l// 2 =l/F-l/oo =1/F-0=1/F, t.e./ 2 =F 
When the object is at F, the image is at oo since 
1// 2 =1/F-1/F=0, i.e.f 2 = co. 

Therefore F and oo are conjugate focal distances. 

The shortest possible distance between the O and its real I is 4 F. 

When the object is nearer than F, the light is divergent after refraction, 
although less so than before. Whereas the light diverged originally from^ 
it appears after refraction to diverge from f 2 . The virtual or negative con- 
jugate of/ x lies on the same side of the lens. Thus let the object be 6 in. 
from an 8 in. Cx. lens, then 

l// a =l/8- 1/6= -1/24. / 2 =-24". 

If the incident light is convergent, the image is nearer than F. Thus if 
light converges to 24" behind a 8" Cx. lens we have the image at 6". 

l// 2 =l/8 + 1/24=1/6. / 2 =6 inches. 

Conjugate Foci — Examples — Cc. Lens. — The diverging power of the lens 
is increased by the divergence of the light; the image is always virtual. 
When the object is within oo the conjugate focus is nearer to the lens than 
F which is the most distant image-point for natural rays. 

If F=10" and/ 1 isat40", then/ 2 is 8" virtual, for l// 2 =- 1/10 -1/40= - 1/8. 

When the object is at oo the image is at F; when the object is at F the 
image is at F/2. 

If the incident light is convergent, the image is beyond F ; thus, if light is 
convergent towards 15" behind a 6" Cc. lens, then 

1//;= - 1/6 + 1/15 = - 9/90 ; the image is virtual at 10". 

If the light converges to F the light is rendered parallel. If convergent 
to a point nearer than F, a real image is formed. 



The Addition of Conjugates. — 

. If the conjugates are 5" and 10" 
„ 5" and -10" 
„ -5" and 10" 

l/F=l/5 + 1/10=3/10 
l/F=l/5- 1/10=1/10 
1/F=- 1/5 + 1/10= -1/10 

Reciprocity of Conjugates. — Eeal conjugate foci are interchangeable so 
that if is at either of them, I is at the other. Thus when is at 40" in 
front of an 8" Cx. lens, I is at 10", and if I were at 10", would be at 40". 
Virtual conjugates are not interchangeable in this sense. If is at 6" from 
an 8" Cx. lens, I is at 24" virtual. could not be at - 24", which is a negative 
distance, and if it were at 24" actually, I would not be at 6". These conj ugates 
are interchangeable merely in the sense that if light converges towards the 
virtual focus, in this case 24", then I would be at the real distance 6". 

The same occurs with the virtual conjugate of a Cc. lens. If O is at 40" 
and the lens is - 1/10 the I is at 8" virtual; light would need to converge 
towards 8" behind the lens in order that a real image be formed at 40". 

Dioptral Formulae for Conjugates. — A say +5 D lens has F=20 cm., and 
light diverging from 20 cm. is rendered parallel by it, the converging power 
of the lens just neutralising the divergence of the light. Conversely light 
from oo is brought to a focus at 20 cm. 

If the light originates in some point within oo it has then a divergence 
equal to that of a Cc. lens whose F is equal to the distance; the resulting 
image d 2 is the dioptral result of the addition of the divergence of the light d x 
and the power of the lens D. That is, 

D - d 1 =d. z or D=d 1 + d 2 

Fig. 100. 

Or D, the power of a lens, is equal to the sum of the two conjugates 
f\ an( i/^ expressed in diopters as d x and d 2 . 

Fig. 107. 

Let/ X be 100 cm. (Fig. 106). The lens has a converging power of 5 D, and 
the light has a divergence of 1 D. Consequently, after refraction, the light 
has a convergence of 5 - 1 =4 D, the I being at 25 cm. 



In Fig. 107 the + 5 D is shown as if split into two lenses, the + 1 D render- 
ing parallel thelight diverging from 100 cm., while the + 4 D brings the parallel 
rays to a focus at 25 cm. 

Thetwodioptral distances ICO cm. and 25 cm. are + 1 and +4 respectively. 

We may therefore write 1 +4=5 D=the power of the lens. 5 - 1=4 D= 
the dioptral distance of I. 5-4=1 D=the dioptral distance of 0. 


If the lens is Cc. we have D negative, and therefore d 2 is also negative, 
since d 2 is the sum of the divergences D and d x hut, as with a Cx. lens, the sum 
°ffi + fi expressed in diopters as d 1 + d 2 =D (Fig. 108). 

Examples. — Suppose the object be placed 50 cm. in front of a lens having 
its image 12-5 cm. behind it, then to find the power of the lens 

a\=100/50=2; ^=100/12-5=8; D =2 +8=10. 
If an object is 200 cm. in front of a +7 D lens, the image is 

^=100/200 =-5; (? 2 =7 - -5=6-5 ;/ 2 =100/6-5=15 cm. 
An image is 22 cm. behind an 8 D lens, where is the object ? 

o 7 2 =100/22=4-5; d 1 =S- 4-5=3-5 ;/ 1 =100/3-5=28 cm. 

If the object is at oo, then ^=100/ oo =0; the image is at F. 
tZ 2 =D-0=D and 100/D=F. 

If is at F, then ^=100/F=D; the image is oo. 

=0 and 100/0= oo. 

tf 2 =D-D: 

Fig. 109. 

Let the lens be +5 D and be at 14 cm. (Fig. 109) then 

0^=100/14=7 ; f/ 2 =5 - 7= - 2, so that/ 2 =50 cm. virtual. 

The lens has a converging power of 5 D, the light has a divergence of 7 D; 
therefore, after refraction, there is a residual divergence of 2 D. 

d 1 + (Z 2 =D, that is, 7 + ( - 2)= + 5 D. 


If light converges towards 50 cm. behind a + 5 D lens we have 

d 2 =5+2=+7 D, f 2 is at 14 cm. 

Let the lens be - 5 D and/ x at 100 cm.; then 

d 2 = - 5 D - 1 D= - 6 D, and/ 2 =100/ - 6= - 16-66 cm. 

Light diverging from 100 cm. to a - 5 D lens, after refraction is divergent 
as if from 16-66 cm. If convergent towards a point 16-66 cm. behind a - 5 D 
lens it is, after refraction, convergent to 100 cm. 

If the conjugates are 20 and 50 cm. 
,, ,, ,, 20 and -50 cm. 

,, ,, ,, -20 and 50 cm. 


As before stated a calculation on conjugate foci is the same as adding two 
lenses together. This is illustrated in the last examples. 

Whether light diverges from 50 cm., or whether parallel light is rendered 
divergent by an added -2D lens, the converging effect of, say, a + 5 D lens 
is equally reduced, and in both cases/ 2 is at +5 - 2=3 D=33 cm. behind the 

Similarly whether light diverges from 50 cm. (2 D) to a - 5 D lens, or 
whether a - 2 D be added to the - 5 D, and the two combined act on parallel 
light, fo in either case is at - 5 - 2= - 7 D or 14 cm. negative. 

Fig. 110. 

Magnification or Relative Sizes of O and I. — In Fig. 110, the object 
and the image / subtend equal angles at C, the optical centre of the lens, since 
both are contained between the extreme secondary axes A A' and B B' . The 
triangles AC B and A' C B' are similar. 


I B' A' IC 

M=-= = — 


The relative sizes of I and O are proportional to their respective distances 
from the optical centre of the lens. This is true for real and virtual images of 
both Cx. and Cc. lenses. 

The ratio B' A'/ A B is the magnification, and denotes the linear increase 
or decrease in the size of the image with respect to the object. Superficial 
magnification applies to area, and is the linear magnification squared. 


With a Cx. lens, so long as is beyond 2 F the I must be smaller than 0, 
since it is nearer to the lens. When is at 2 F the size of I is the same as 
that of 0, because both are at the same distance. W r hen is within 2 F, I 
is larger, because it is further from the lens than 0. 

To calculate the size of I or of the following formulae are applicable to 
all cases. 

M=-=— , that is, A 2 =— — and %=— — 

"l J l JX J 2 

where f x and/ 2 are the distances of and I respectively from the lens, h x is 
the linear size of 0, and h 2 that of I. h x and/^ must be in similar terms, but 
not necessarily that of/ 2 ; h 2 will then be in the same terms as f 2 , whether 
inches, cm., etc. Or h 2 and/ 2 must be in the same terms; and h^ will be in 
that oif v 

Thus if is at 2 M, and I at 25 cm. and -625 cm. high; then 

, -625X200 B 

lu= — — =5 cm. 

1 25 

is eight times the size of I. If were at 25 cm. and I at 2 M, then I would 
be eight times the size of 0. 

Let 0, 4 yards long, be \ mile distant from a +5 D lens; then the object 
being at o>,/ 2 =20 cm. and 

ft 2 =4x20/440=-18cm. 

The answer here is in cm., showing that, so long as h x and/j are in the 
same terms, and I need not be. 

When the I formed by a Cx. lens is virtual, it is always larger than 0, 
since it is always more distant from the lens. With a Cc. lens the virtual I 
formed is alw r ays smaller than 0, since it is always nearer to the lens. 

Planes of Unit Magnification. — In order that and I be equal in size 
they must be equally distant from the lens, i.e. they must be in the planes 
of unit magnification which, for real images, are the symmetrical planes, which 
cut the axis at twice the principal focal distance; then h x =h 2 . 

If M=l, then/ 1 =/ 2 , and we can write — 

11 12 11 12 

so that /i=2F and / a =2P. 

For a virtual I to be equal in size to 0, that is, M= - 1, it must be in con- 
tact with the lens. This is true for both Cx. and Cc. lenses, so that the planes 
of unit magnification for virtual images is zero. Both planes of unit magnifi- 
cation are from F a distance equal to F. 


Recapitulation of Conjugates — Cx. Lens. 

at oo I real, inverted, diminished, at F. 

between oo and 2 F I real, inverted, diminished, between F and 2 F. 

at 2 F I real, inverted, equal to 0, at 2 F. 

between 2 F and F I real, inverted, enlarged, between 2 F and oo. 

atF I infinitely enlarged, at oo. 

within F I virtual, erect, enlarged, same side as 0. 

at the lens I virtual, erect, equal to 0, at the lens. 

Cc. Lens. 

at oo I virtual, erect, diminished, at F. 

within oo I virtual, erect, diminished, within F. 

at the lens I virtual, erect, equal to 0, at the lens. 

Relationship of Conjugate Distances. — If the distance of the two conjugates 
f± and/ 2 of a Cx. lens be measured respectively from F x and F 2 they arc 
reciprocals of each other in terms of F. If/ X is at a distance n F beyond ¥ v 
then/ 2 is F/n beyond F 2 . Thus, for instance, if the distance of to F x is 2 F, 
then the distance of I to F 2 is F/2. 

Let the distance of to F x be called A, and/ 2 to F 2 be called B; then 
A B=F 2 . 

For M (magnification) =1, both conjugates are at F + F. For M=2 the 
one is at F + 2 F, the other being at F + F/2. For M=3 the one is at F + 3 F, 
the other being at F + F/3, and so on. 

If the object is n F from the lens, the image, with a Cx. lens, is n F/(n - 1 ), 
and with a Cc. the latter is at n F/(n + l). Thus if the distance from a 5" 
Cx. lens is 5 x 4=20", the image is at 5 x 4/3=6-66"; in the case of a 5" Cc. 
if the object is at 5 x 4=20", the image is at 5 x 4/5=4". Then n F x F/w=F 2 . 

The size of the object is to the real and the virtual image, formed by a given 
Cx. lens, the same when is as far beyond F in the first case as it is within F 
in the second case. Thus, suppose situated 14 in. and 6 in. respectively 
in front of a 10 in. Cx. lens, it is in either position 4 in. from F, then the size 
of the image in each case is 2J times that of 0. 

Newton's Formula for Conjugate Foci. — Let the distances A and B be 
as defined in the last article. Now the ordinary formula for conjugate foci is 

111 1 1 , * t, ™ 

- = - + -- = + = then AB=F 2 

F A A F+A + F+B 

This gives an alternative formula for calculating conjugate foci. 

A. F B 

The relative sizes of I and 0=M=-= T =— 

h x A E 

It is essential to remember that positive quantities are measured forwards 
from F x and backwards from F 2 ; also that in Cc. lenses F x is on the remote side 
of the lens, and F 2 on the object side. A is always reckoned from F x and B 


from F 2 . These points make this otherwise valuable formula difficult of 
application. To obtain f x or f 2 the value of F must be added to A or B 

Examples. — Let/ X be 50 cm. in front of a Cx. lens of 10 cm. F. 
A=40; 40 B=10 2 =100; B=2-5; and/ 2 =2-5 + 10=12-5 cm. 
If is 5 cm. high, /t 2 /5=10/40, so that 40 # 2 =50, or # 2 =l-25 cm. 
If an object 5 cm. high be placed 8 cm. in front of a lens of 10 cm. F, 
A=-2; -2 B=10 2 =100; B= - 50, and f 2 = -50 + 10= -40 cm. 
Zf 2 /5=10/2, or #2=25 cm. I is negative at 40 cm. and 25 cm. high. 
If an object 5 cm. high be 50 cm. in front of a Cc. lens of F=10 cm., 
A=60; B=10 2 =100. B=l-66 and/ 2 =l-66 + (-10)= -8-33 cm. 
#2/5=10/60, or h 2 =-833 cm. I is negative at 8-33 cm. and -833 cm. high. 

The Geometrical Proof is the same as shown in Fig. 104. 
But 0B=F + A, 0B'=F+B, F=F, and B' F=B. 
Therefore, (F + A)/{F+B)=F/B ovAB=F 2 . 

Removal of I. — To move the image from f z to some other position f 2 
more distant or nearer, there must be added to the lens another Cc. or Cx. 
respectively whose power is the difference between \/f 2 and l/f 2 . 

Thus, supposing f 2 to be 20 cm. and/ 2 to be 25 cm., the required lens 
4 - 5= -ID. It is Cc. because^' is more distant than/ 2 . 

To place the image at 16 in. behind the lens instead of at/ 2 , which is 
20 in., the added lens must be positive of 1/16 - 1/20 or 80 inches F. 

Position of the Conjugates for given M. — To find/j the position of 
for a given magnification M, the ordinary conjugate formula can be used. 
Since h^ and h 2 are proportional to/j^ andy^ we can express/ 2 in terms of/ r 
Thus, if the I is to be 3 times the size of 0,y,=3/j ; if it is to be 1/3 the size of 
°'/2=/i/ 3 - Then we have 

l/l^l/Zl + l/M/, 

For example, the lens is a 6 in. Cx., a photograph is 2 inches long, and it 
has to be enlarged 4 times. Then 

1/6=1//1 + l/4/i=5/4/i or 4/ 1= 30 and/ 1= 7-5" and/ 2 =30" 

If a reduction is required, M is a fraction. 

If I is virtual with a Cx. or Cc. lens, 1/M/j needs the -sign. 
Similarly f 2 can be found by expressing it in terms of^. 
From the above the following formulae are extracted for finding the position 
of and I when the one has to be magnified a certain number of times. 

a=F(M + l) and b=a/M, 

a is the longer conjugate and b is the shorter. (M + 1) becomes (M - 1) when 
I is virtual, with either a Cx. or a Cc. 

AVhen/j or/ 2 is not known M can be found respectively from 

M=(/ 2 -F)/F and M=F/(/ 1 -F) 


M is positive for a real, but negative for a virtual, image, and is a fraction 
when there is diminution. 

The Position of Lens for given Distance between and I. — The calculation 
necessitates finding two conjugates such that the sum of their reciprocals 
equals the power of the lens. Let d be the distance between and I, and x 
be the one conjugate; then 

1 1 1 

F x d-x. 

or x 2 -dx=-d¥ 

the solution of which involves a quadratic equation. 

With a Cx. lens when d is not less than 4 F, the I is real and may be at 
either conjugate, and there are two positions for the convex lens, between 
and I, which will fulfil the conditions. When d is less than 4 F, the shorter 
conjugate is positive and is the distance of the 0; the greater is negative 
and is that of the virtual I, d then being a negative quantity. 

When the lens is concave, d is positive but F is negative. The greater 
conjugate is positive and is the distance of the 0, while the smaller is negative 
and is that of the virtual I. 

Let F=7 in. and the distance between and I be 36 in. Then 

x t- 36 x=- 252 and x 2 -36x + 324- -252+321=72 

Therefore Va 2 -36x + 324=^/72 or x -18= ±8-5 

sothat x= +8-5 + 18=26-5 or -8-5+18=9-5 

The lens may be either 9-5 in. or 26-5 from 0. 
Let F=5 in. and cZ=16 in.; d is negative. Then 

x 2 + 16x= +80 

and x 2 + 16^ + 64=80 + 64=144 

so that 

x + S= ±12 


x= +12- 

-8= +4 or -12 -8= -20 

The lens is 4 in. from the and 20 in. from the virtual I. 
Let F be 5 in. Cc. and d, as before, 16 in. Then 

x 2_ 16x=8 and x 2 - lQx + 64=80 + 64=144 

a; -8= ±12 and x = +12 +8= +20, or - 12+8= -4. 

The lens is 20 in. from and 4 in. from the virtual I. 

If the strength of the lens is expressed in diopters it is better to convert 
it into focal length for this calculation, but the two distances x and y can 
be calculated by the method in which two numbers, whose sum and multiple 
are known, have to be found, d is in cm. Thus from above 

x+y=d, and x >j=¥d=100d/D } 


The Cylinder. — A cylinder is a body (Fig. Ill) generated by the revolu- 
tion of a rectangle about one of its sides as an axis. Such a body consists of 
two flat circular ends and an intermediate convex surface. 

The cylinder possesses no curvature in any plane parallel to the axis A B. 
At right angles to the axis, in any plane parallel to the direction C D, the 
curvature is spherical, and has its maximum value. In any other direction, 
as E F, the curvature is that of an ellipse. 

Fits. 111. 

Any section of the cylinder at right angles to its axis is a circle whose 
centre lies on the axis of the cylinder; a section in the plane of the axis is a 
parallelogram; one anywhere between these two is an ellipse, as E' F'. 

Fig. 112 represents a Cx. cylindrical lens. It is a segment of a cylinder 
as to the one surface and is plane on the other; it is formed by a cylinder and 
a plane which intersect each other. The Cc. cylindrical lens (Fig. 113) has 
a hollowed surface on one side; it is formed by a cylinder and a plane which do 
not intersect each other. 

The Cx. cyl. lens may be conceived as formed of a series of prisms whose 
bases are directed towards the axis and whose apices are outwards, and the 
Cc. cyl. as formed of prisms whose apices are towards the axis and whose 
bases are outwards; in both cases the power of the prisms increases towards 
the edge of the lens. 




Meridian. — The term meridian in connection with lenses signifies a plane 
passing through the geometrical centre of a lens, as shown in Fig. 114. 

Fig. 113. 

Nomenclature. — A lens with a cyl. curvature only is a piano or simple cyl. 
One having, at right angles to each other, a cyl. curvature on both surfaces 
is a cross-cyl. One having a sph. curvature on the one surface and a cyl. on 
the other is a sphero-cyl. 

The Principal Meridians. — Since in the direction of its axis (Fig. 115) 
a cyl. lens has no curvature, it has in that direction no refractive power; the 
directions of maximum curvature ABC, D E F, G H K, are at right angles 


Fit). 114. 

Fig. 115. 

to the axis. The meridian of no refraction — i.e. the axis — and the meridian 
of power, at right angles to the axis, are the two principal meridians, and these 
alone need be considered when treating of cyl. lenses. 

The other meridians are merely individual elements contributing to the 
total power of the lens, but they have a dioptric value, as will be shown in a 
later chapter. 

The position of a cylindrical is indicated by the direction of its axis. 
Its power is expressed, generally in diopters, by the maximum refractivity, the 
numeration being the same as for spherical lenses. 


The Refraction of a Cylindrical. — A sph. lens has equal curvature and 
therefore similar refractivity in every meridian, so that a point image of a 
point object is obtained. In a cyl. it is only the meridian at right angles to 
the axis that can form a focus, so that all the light from an object-point at oo 
refracted by a cyl. meets in a line at the focal distance of the meridian of 
greatest refraction. This is called the focal line, and it is at right angles to the 
meridian of power and therefore parallel to the axis. Theoretically the cylin- 
drical lens has two focal distances and the image of a point is two lines, but 
since the one focus is at oo, it need not be considered. 

Using for illustration a +5 D cyl. axis vertical, as shown in Fig. 115, the 
meridian of power is horizontal and the focal line is vertical and at 20 cm. 
At any other distance the streak broadens out into a band of light, and a 
section of the emergent light, at any distance from the lens, is rectangular in 
outline. If the lens be rotated the line is rotated with it. 

Since the image of an object consists of the images of its various points, 
and each object-point has its own line image, the complete image consists of 
an infinite number of streaks, parallel to the axis, and narrow as the focal 
length is short, and vice versa. The length of a streak is that of the aperture 
of the lens in the meridian of its axis. 

The refraction of a Cc. cylindrical is similar to that of a Cx. but, of 
course, the focus and the focal line are virtual, and formed in front of the 
lens. The shape of the refracted pencil, however, is not so apparent, because 
the pupil of the eye acts as a very small stop, so that the focal line, on look- 
ing through the lens, is so short as to appear little different from the point 
focus of a concave spherical, unless the cyl. be very strong. 

A square seen through a cyl. with vertical axis appears to be a rectangle 
of natural size in the meridian of the axis, but magnified by a Cx., and dimin- 
ished by a Cc, across the axis. 

If the cyl. is rotated, around its centre, the square takes the form of a 
rhombus, the obliquity of the sides being due to the fact that the light from 
each point diverges from, or tends towards, a line parallel to the axis and there- 
fore appears to come from points in space other than the real ones. The 
series of oblique parallel lines (or ellipses) which constitute the virtual object, 
of which the retinal image is formed, results in vertical and horizontal lines 
appearing oblique. This explains also the dipping of cross lines as a cyl. is 
rotated (vide Neutralisation). The apparent obliquity is lessened if the lens 
is near to the object or very near to the eye. 

Viewing a circular object, say a shilling, through a Cx. cyl. axis Ver., the 
image is an oblate ellipse in form, having its minor axis equal to the diameter 
of the shilling. With a similar Cc. cyl. the image is a prolate ellipse. 

The Refraction of a Sphero -Cylindrical.— When a sph. is combined with 
a cyl., the curvature of the former is ground on the one side of the lens, and 
that of the latter on the other. Since there is no curvature and consequently 
no refractive power along the axis of the cyl., there is, in that meridian, 
only the power of the sph., whereas at right angles to the axis there is the 


united power of the spli. and the cyl. As with the plano-cyl., those are the 
two principal Mers. of the combination, which alone need be considered in 
practice. Further, the lens has two finite focal distances. 

The sign o indicates combined with. 

Let the lens be +4 D Sph. o + 4 D Cyl. Axis Ver. and let the object be a 
point at oo. All the light incident on the lens is so refracted as to pass 
through a vertical line at 12-5 cm. to which it is converged; thence, expand- 
ing horizontally and converging vertically, it meets in a horizontal line at 
25 cm. The vertical meridian acts as a plano-Cx. lens, the horizontal as a 
double Cx. lens, and these principal meridians have true foci. Every ray 
incident on the lens lies in both principal planes and is, therefore, converged 
to a certain extent in the vertical, and to a still greater extent in the hori- 
zontal, the resultant deviation being intermediate as to direction and extent. 
The same rays combine to form both the focal lines. 

The action of the concave sph.-cyl. is similar to that of the convex, except 
that the foci and images are virtual. 

As with the plano-cyl., the images at the two focal planes of an object, of 
definite size, consist of bands of light, whose width and length depend on the 
powers of the lens, and its aperture or diameter. 

A section of the cone of light emergent from the lens is elliptical except 
where the focal lines are formed; also at some position between them, where 
the cone of light has equal diameters in both Mers., producing what is termed 
the circle of least confusion. 

Combined Cylindricals. — If two Cx. cyls. of similar power be placed in 
contact, with their axes corresponding in, say, the vertical meridian, the 
cyl. power is doubled. If the second cyl. be at right angles to the first, they 
are equivalent to a sph. lens of the same power as either cyl. In this case the 
power of the one corresponds to the axis of the other, and in all intermediate 
meridians any deficiency of power in the one is supplied by the other. As 
the second cyl. is rotated from axis vertical to axis horizontal the original 
vertical streak image shrinks until, when the two axes are at right angles, it 
is a point of light, or a complete image as the case may be. When the axes are 
oblique to one another, the effect is that of some sph.-cyl., whose two principal 
powers vary with the angle between the axes. Two unlike cyls. are always 
equivalent to some sph.-cyl. combination no matter what may be the in- 
clination of their axes, except in the case of the axes being parallel, when they 
constitute a plano-cyl. The effect is the same whether the two cyl. powers 
be ground on opposite sides of a piece of plass, or whether two plano-cyls. 
be placed in contact. 

The Interval of Sturm. — The two principal focal distances of a sph.-cyl. 
lens may be indicated by F v the first, and F 2 , the second, and their powers 
by D x and D 2 . The distance between the focal lines is termed the interval of 
Sturm or the focal interval. 

Let a screen beheld close behind a Cx. sph.-cyl., say +4 Sph. o + 4 Cyl. 
axis Ver.; then the light from a small bright source, some distance in front 



of the lens, is cast as a light patch on the screen. If now the latter be gradu- 
ally drawn away from the lens (Fig. 116), at the distance 12-5 cm., which is 
equal to the focal length of the combined sph. and cyl. powers, a Ver. line is 
formed at F x ; as the screen is still slowly receded the line develops gradually 
into a Ver. (prolate) oval at C, an almost perfect circle at B, a Hor. (oblate) 
oval at A, and finally into a Hor. line at F 2 . The screen is then at 25 cm., 
which is F of the sph. As the screen is still further removed from the lens, the 
patch of light takes the form of an ever-enlarging oblate ellipse. 

The lengths of the two focal lines L x and L 2 depend on F x and F 2 , their 
distances from the lens, on d the effective aperture of the lens, and S the 
length of the interval of Sturm, i.e. the distance between F x and F 2 (Fig. 1 16), 
or the dioptric difference D x - D 2 . 

L x =dS/F 2 =dS/D x 
L X F 2 =L 2 F X 

L 2 =dS/F x =dS/D 2 
L X D X =L 2 D 2 



Fig. 11G. 

The circular disc of confusion B divides S into two parts b and a, which 
are proportional to F x and F 2 . 

S=a + b and b/a=L x /L 2 =F x /F 2 =D 2 /D x 

B is distant from L x and L 2 respectively 

7 SF X SZ> , SF SD X 

F x + F 2 D x + D 2 


F x + F 2 D x + D 2 

B is not midway between L x and L 2 , but is always nearer to L x , when 
both powers are positive or both negative. 

Its size is B=bL 2 /S=aL 1 /S 

The distance of B from the lens is E= 

2F X F 2 


^1 + ^2 D x + D 2 
Example with +4 D Sph. o +2 D Cyl. having d=5 cm. 

F 1 =16-66cm. F 2 =25 cm. 

/>,= — — — =1"66 cm. 

#=25 -16-66=8-33 cm. 

r 5x8-33 _ 

L„= =2-5 cm. 

1 16-66 


, 8-33x16-66 •„ 8-33x25 r 

6= =3-33 cm. a— =5 cm. 

25 + 16-66 25 + 16-66 

„ 3-33x2-5 5x1-66 _ 2x16-66x25 

5= = =1 cm. E= — n nn „„ =20 cm. 

8-33 8-33 16-66 + 25 

When the combination is negative the interval of Sturm is also negative ; 
when the combination is mixed, it is partly positive, and partly negative. 

Thus when ^=10", F 2 = - 20", and d=l" we find B behind L x and nega- 
tive. S= - 30, L x = + 1 -5, Z 2 = - 3, b= + 30, a= - 60, B= - 3, E= + 40. 

If the stronger power is negative, B lies in front of L x and is again negative. 
If the + and - powers are numerically equal, B is at oo. 



Standard Angle Notation for the angular location of the principal meridians 
of a cyl. lens (Fig. 117a), is the same for both the right and left eyes. 
The numeration commences on the right hand of the imaginary horizontal 
line drawn through the lens when looked at from the front, that is, the surface 
remote from the eye of the wearer. 

This notation corresponds with the trigonometrical division of the circle 
into 360 degrees. The uppet right quadrant contains the angles between 0° 
and 90°, and the upper left those between 90° and 180°. The notation is 
not carried beyond 180° (the half-circle), since a meridian corresponds to 
a diameter, i.e. to two continuous radii — for instance, 45° is in the same 
meridian as 225°; 10° the same as 190°, etc. The vertical meridian is 90°, 
and the horizontal is 0° or 180°, but is preferably indicated as 180°. 


90 iQ j" i?o 

'm/o'soh m^^ 

Fio. 117a. 

Fig. 117i3. 

Other Notations. — Some trial frames and prescription forms are notated 
differently from that shown in Fig. 117a, and it may occur that the optician 
has to transfer from one notation to another. The most commonly met with 
are the bi-nasal and the bi-temporal methods, in which the zero is placed at, 
respectively, the two nasal and the two temporal extremities of the horizontal 
line of the eye, the numeration running upwards, or conversely running 
downwards. Sometimes zero is placed in the vertical meridian, the numera- 
tion proceeding to the right and left. Indeed, there are many different 
methods of notating the two eyes, but it is hardly necessary to attempt to 
detail them here. Fig. 117b shows a notation reverse to the standard. 
Right eye bi-nasal and left eye bi-temporal correspond to standard. 

To translate to standard a prescription written with the indicated cylin- 



drical axisatl25°accordingtothe notation of Fig. 117b, it must be considered 
how many degrees the required position is from the horizontal or the vertical. 
In this case 125°, in Fig. 117b, is 35° from the vertical on the right and, there- 
fore, corresponds to 55° of Fig. 117a. If the location of the axis is 40° above 
the horizontal on the right, it would be 40° in Fig. 117a and 140° in Fig. 117b. 
The same mode of calculating serves if the cylindrical axis is indicated as 
so many degrees, say, out and down. This last-mentioned method of axis 
indication, unless accompanied by a stroke to show the direction, and, 
sometimes even if so accompanied, does not remove all ambiguity, and may 
lead to error. Some omit the o sign, and write a combination thus: 

+ 4S. 

+ 2-50 C. Axis 70° 

In all methods, however, the direction indicated refers to the front of the 
lens, or the surface away from the wearer's eye. 

Transposition of Sph. Lenses. — A Cx. sph., say, +G D, can be made in 
the form of a piano Cx., in which all the power is on the one side; as an 
equi-Cx., in which the power is equally divided between the two surfaces; as 
a bi-Cx., in which the powers are unequally divided between the two surfaces; 
or as a periscopic-Cx., in which the Cx. power on the one side is more than 
6 D, but the total is reduced to +6 D by the necessary Cc. curvature of the 
other surface. Similarly, a Cc. sph. can be made in various forms. The 
change from one form to another, without altering the refractive power of 
a lens, is called a transposition. The power of the one surface increases ag 
that of the other decreases, so that the number of possible forms for a given 
sph. power is infinite; the position of the optical centre changes with the 
different forms of a lens. 

The trade periscopic has one surface ±1-25 D, to 2 D, and the trade 
meniscus ±6 D. 

Transposition of Cyl. Lenses. — Lenses which contain a cyl. element are 
susceptible of only two or three changes of form, and it is to such a change, 
which does not alter the refractive powers of the two principal meridians, 
that the term " transposition " is generally applied. 

When the two powers have the same sign, they are said to be of like 
nature, or congeneric ; when they are of opposite signs (the one + and the 
other - ) they are of unlike nature, or contrageneric. 

A plano-cyl. possesses no sph. element, but may be regarded as one whose 
sph. is of infinite focal length, and it will be so treated in this chapter. 

A sph.-cyl. has sph. and cyl. elements, and may be a compound cyl, having 
+ or - powers in both principal meridians, or a mixed cyl, having a + power 
in the one and - power in the other. 

A cross-cyl. has two similar or dissimilar cyls. crossed at right angles. 

Powers and Principal Meridians. — The one principal Mer. of a sph.-cyl. 
corresponds to the axis of the cyl., and its power is that of the sph. alone; 



the other is at right angles to the axis of the cyl., and its power is the 
algebraical sum of the sph. and cyl. Thus the powers of — 

+ 3 S. O +2 C. Ax. 70° are +3 at 70° and +5 at 160°. 

+ 3S. o -1C. Ax. 110° are +3 at 110° and +2 at 20°. 

+ 3 S. o - 3 C. Ax. 5° are +3 at 5° and at 95°. 

+ 3 S. o - 5 C. Ax. 120° are + 3 at 120° and - 2 at 30°. 

In the cross-cyl. the two principal powers are those of the cyls. themselves, 
each being in the Mer. corresponding to that of the axis of the other. Thus 
the powers of — 

+ 2C. Ax. 40°O+5C. Ax. 130° are +2 at 130° and +5 at 40°. 
+ 2 C. Ax. 70° o -4 C. Ax. 160° are +2 at 160° and - 4 at 70°. 

Possible Combinations. — A cyl. combination may consist of two different 
powers of similar nature, as +2 and +5, or -3 and - 7, or of two powers 
of dissimilar nature as +2 and -2, or +3 and -4. It can be made in 
three forms, viz., a cross-cyl. and two forms of sph. -cyl. If the one power 






+ 5S 



Fig. 118. 

is it can be made only as a plano-cyl., and in one form of sph.-cyl. If there 
are two similar equal powers the possible forms are only a cross-cyl. and a sph. 

The Various Forms of a Lens with a Cyl. Element. — Where unequal powers 
in the principal Mers. are required, as +3 at 180° and +5 at 90° — 

(a) The + 3 needed at 180° (Fig. 118) can be obtained from + 3 C. Ax. 90°, 
and the +5 at 90° from +5 C. Ax. 180°, the axis of each cyl. being at right 
angles to the direction in which the power is required, as in A. 

(b) The +3 needed at 180° can be obtained from +3 sph., which also 
supplies 3 of the + 5 D needed at 90°, the balance of the latter being obtained 
from +2 C. Ax. 180°, which gives +2 at 90° and at 180°, as in B. 

(c) The +5 needed at 90° can be obtained from +5 sph., but this not 
only supplies the + 3 needed for 180°, but is 2 D too strong. To reduce the 
latter to +3 D a -2 C. Ax. 90° is required, this giving -2 at 180° and 
at 90°, as in C. 

If the two elements of the forms (a) (b) or (c) be placed over one another, 
the total combination is, in each case, +5 at 90° and +3 at 180°. The three 
forms are thus made up by — 

(a) A cyl. of each of the two powers, the axis of each being at right angles 
to the meridian where the power is needed. 


(b) A sph. of the lower power, and a cyl. of the difference between the 
two powers, the axis corresponding to the meridian of least power. If the 
lower power is 0, the sph. is also 0. 

(c) A sph. of the higher power, and a cyl. of the opposite sign and of the 
difference between the two, the axis being in the meridian of greater power. 

Whether the two powers are of like or unlike nature, the number of the 
cyl. is obtained by the algebraical subtraction of the power taken as the sph. 
from that of the other principal power. Thus in the example the powers are 
+ 3 and +5, so that if the sph. is +3, the cyl. is +2; if the sph. is +5 the 
cyl. is - 2. If the two powers are +2 and - 3, then, if the sph. is +2, the 
cyl. is - 5; if the sph. is - 3, the cyl. is +5. 

For - 4 at 60° and - 7 at 150°, the three forms are: 

(a) - 4 C. Ax. 150° O - 7 C. Ax. 60°. 
(b) - 4 S. o - 3 C. Ax. 60°. (c) - 7 S. o +3 C. Ax. 150°. 

For - 1 at 45° and +5 at 135° they are: 

(a) - 1 C. Ax. 135° o +5 C. Ax. 45°. 
(b) - 1 S. o +6 C. Ax. 45°. (c) +5 S. o - 6 C. Ax. 135°. 

For + 3 a.t 120° and at 30° they are: 

(a) S. o +3 C. Ax. 30°. (b) +3 S. o - 3 C. Ax. 120°. 

Rules. — (1) To transpose a sph.-cyl. or plano-cyl. into another form of sph. - 
cyl. or plano-cyl. 

The following apply to all cases, but when the original or the transposed 
form is a plano-cyl., the one power being 0, the sph. may also be 0. 

(a) The new sph. is found by adding algebraically the power of the sph. 

to that of the cyl. 

(b) The new cyl. has the same power as the original cyl., but its sign is 

changed and its axis is at right angles. 

(2) To transpose a sph.-cyl. into a cross-cyl. 

(a) The one cyl. of the new form has the same number and sign as the 

original sph. with its axis at right angles to that of the original cyl. 

(b) The other cyl. has its axis in the same Mer. as that of the original 

cyl. Its sign and number result from the algebraical addition of 
the powers of the original sph. and the original cyl. 

(3) To transpose a cross-cyl. into a sph. cyl. 

(a) The sph. of the new form has the number and sign of the first original 


(b) The new cyl. has its axis corresponding to that of the second original 

cyl. and a sign and number which result from the algebraical sub- 
traction of the first from the second original cyl. 

Since either original cyl. may be taken as the first, there are two forms 
of sph.-cyls. into which a cross-cyl. can be transposed. 


Examples. — The above rules can be better appreciated by studying 
examples at the same time. In the following, which illustrate all possible 
combinations, the first is the original, and those following are the forms into 
which it can be transposed. 

(1) + 4S. o+2C. Ax. 20°= 
+ 6S. o-2C. Ax. 110° 

+ 4 C. Ax. 110° o +G C. Ax. 20° 

(2) - 2-50 S. o - 1-50 C. Ax. 175°= 

- 4-00 S. o + 1-50 C. Ax. 85° 

- 2-50 C. Ax. 85° o - 4-00 C. Ax. 175° 

(3) +3-50 S. o - 2-50 C. Ax. 45°= 
+ 1-00 S. o +2-50 C. Ax. 135° 

+ 1-00 C. Ax. 45° o +3-50 C. Ax. 135° 

(4) +3S. o - 3 C. Ax. 105°= 
+ 3 C. Ax. 15° 

(5) + 2-50S. o-4-50C.Ax. 115°= 
-2-00S. o +4-50 C. Ax. 25° 

+ 2-50 C. Ax. 25° o - 2-00 C. Ax. 115° 

(6) - 1-25 S. o + 1-75 C. Ax. 160°= 
+ 0-50S. o-l-75C.Ax. 70° 

- 1-25 C. Ax. 70° o +0-50 C. Ax. 160° 

(7) +2-75C. Ax. 95°= 

+ 2-75 S. o - 2-75 C. Ax. 5° 

(8) +2 C. Ax. 80° o +3 C. Ax. 170°= 
+ 2S. o+lC.Ax. 170° 

+ 3S. o-lC.Ax. 80° 

(9) - 5-50 C. Ax. 155° o - 2-50 C. Ax. 65°= 

- 2-50 S. o - 3 C. Ax. 155° 
• -5-50S. o+3C.Ax. 65° 

(10) +2-25 C. Ax. 75° o - 2-25 C. Ax. 165°= 
+ 2-25S. o - 4-50 C. Ax. 165° 
-2-25S. o +4-50 C. Ax. 75° 

(11) +3-50C. Ax. 120° o -0-75 C. Ax. 30°= 
+ 3-50 S. o - 4-25 C. Ax. 30° 

-0-75 S. o +4-25 C. Ax. 120° 

(12) - 10-00 C. Ax. 180° o +2 C. Ax. 90°= 
+ 2S. o - 12 C.'Ax. 180° 
-10S.o+12C.Ax. 90 

(13) + 3-50 C. Ax. 90 o + 3-50 C. Ax. 180° 
+ 3-50 S. 

(14) -4S.= 

- 4 C. o - 4 C. with axes at right angles. 



Comparison of Original and Transposed Forms. — The two principal 
powers and Mers. of the original form of a combination can be extracted and 
compared with those of the transposed form, and they must be alike if the 
transposition is correct. Thus, suppose -3 S. o+4 C. Ax. 90°. The two 
principal powers are - 3 at 90° and + 1 at 180°. The power of the - 3 Sph. 
is in both principal meridians, while that of the +4 C. Ax. 90° is only at 
180°; its axis, being at 90°, contributes no refractive power to that meridian. 






Fig. 119. 

The two components separately are represented by A and B of Fig. 119. 
When combined they are represented by C. The two forms into which the 
combination can be transposed are 

{a) + 1 S. o - 4 C. Ax. 180°; (6) + 1 C. Ax. 90° o - 3 C. Ax. 180° 

Proof by Neutralisation. — Since a transposition simply assigns the needed 
powers in a different way, as regards the two surfaces of a lens, and does not 
change the refractive power of the combination, that combination which will 
neutralise the original form will also neutralise the transposed forms. Thus— 

(a) + 1 S. o - 4 C. Ax. 180° transposes into 
(&) -3S.O+4C. Ax. 90° 

(a) is neutralised by - 1 S. o +4 C. Ax. 180°, and these also neutralise (b) as 
can be seen by adding them together thus — 

(-3 S. o+4 C. Ax. 90°) + (-1 S. o+4 C. Ax. 180°) 

The 2 sphs.= -4 S., the 2 cyls.= +4 S.;-4 S. +4 S.=0. 

Best Form. — It is never required in practice to employ crossed cyls. since 
the same effect results from a sph.-cyl., at less cost. The best form to employ 
is usually a +Sph. O -Cyl., or a -Sph. o + CyL, since then a periscopic 
effect is obtained. 

Toric or Toroidal Lenses. — A toric lens is one having two principal powers 
worked in the same surface with, their axes at right, angles to each other, 
as shown in Fig. 120. The curvature of the lens along A B is, say, +3D, 
while along C D it is, say, +5D. It is, therefore, equal to + 3 S. o +2 C. 
and has the same optical effects. The name is derived from the tore or arched 
moulding used at the base of pillars. It has the curvature of a bent tube or 
rod; the side of an egg or the bowl of a spoon resembles a toric surface. 

The curvature of a toroidal surface is spherical in the two principal 


meridians, and elliptical in the intermediate ones, and can be either Cx. or Cc. 
Astigmatism of the cornea is due to its toroidal curvature. 

Since the possible toric forms of any combination are practically infinite, 
it is usual to employ tools of a given base curve. An assortment can then be 

Fig. 120. 

kept of toric lenses having the one surface unworked, on which any spherical 
curve can be ground. The base j)oiver indicates the standard or fixed power of 
the toric surface. It is usually the lower of the two powers, but may be, and 
occasionally is, the higher. In the following it will be taken as if it were 
always the lower toric power. 

Toric tools and lenses are usually made to a base of 6 D, and sometimes 
to 3 D or 9 D, the other power always being stronger by an amount equal to the 
cylindrical effect required in the combination. The number of the toric tool 
or blank is therefore the difference in the principal powers, since the weaker 
power is always 6, 3, or 9, as the case may be; thus a 2 D tool is one having 
a 6 D curve in one direction and 8 D at right angles; or if the series is on a 
3 D base the curvatures would be 3 and 5. 

Therefore if a + 1 S. o+I-5 C. were required in toric form with +6 
base, a 1-5 tool would be used, giving on the Cx. surface powers of +6 and 
+ 7-5. On the other surface -5 D sph. would be necessary in order to 
reduce the principal powers to +1 D and +2-5 D, as required in the com- 

The series of tools being in pairs, the toric surface can be made Cc. if the 
powers of the original lens are not suitable for a Cx. toric. For example, the 
above sph.-cyl. could be made with - 6 D and - 7-5 D powers on the one 
side, the adjusting spherical on the other being +8-5 D. 

Advantages of the Toric Lens. — One utility of the toric form of lens is that 
it permits of the refracting power of a lens to be more equally divided between 
the two surfaces. Thus if + 10 S. c^ + 1 C. be required, instead of 4- 10 S. 
on the one surface and + 1 C. on the other, it can be made with + 4 S. on 
the one and + 6 C. O + 7 C. on the other. Or it can be made with any other 
Cx. sph. power, the virtual cyls. of the toric surface being accordingly stronger 
or weaker, but always having 1 D difference between them. Thus, a strong 
lens as needed in aphakia or high myopia can be made less thick and unsightly 
and more nearly resembling a Dcx. or Dec. Another, and still greater, ad 
vantage of the toric surface is that, with it, a sph.-cyl. can be made periscopic 


to a considerably greater extent than is possible with the ordinary sph-.cyl. 
form. The advantages of highly periscopic lenses are mentioned under 
Menisci, page 248. 

Conversion to Toric Form. — Due regard must be paid to the powers of the 
original lens when selecting the base curve in order to get the best periscopic 
result. If this is not done the result may be little better than what could be 
obtained from the ordinary sph.-cyl., and on the other hand it may be so 
deep as to render the lens clumsy or unsuitable for mounting. Thus - 5 S. 
o - 1 C. Ax. 45° on a - 6 base becomes — 

+ 1S. 

-6 C. Ax. 135° o-7 C. Ax. 45 c 

o , 

This differs but little from the sph.-cyl. form of -6 S. c: +1 C. Ax. 135 
and on a +6 base, the sph. being - 12 D, the lens would be thicker and heavier 
and with doubtful advantages over the ordinary sph.-cyl. The toric is most 
useful, in weak combinations, because then generally only very small peri- 
scopic effects can be obtained from the ordinary forms. A toric surface may 
be expressed as two powers in certain meridians, or as the two virtual cylindri- 
cals, which are contained therein, with their axes at right angles and in certain 
meridians. The latter method is followed in this article. 

Rules for Conversion of a combination into a toric of given base. 

(a) Convert into cross-cyls. 

(b) Find B. Change its sign and this is the sph. 

(c) Add B to each original cyl. for the toric cyls., B is as follows: 

(1) The difference between the lower power and the base, when the 

two powers are of same sign and same as the base. 

(2) The difference between the higher power and the base, when the 

two powers are of same sign but opposite to that of base. 

(3) The difference between the power opposite to that of the base 

and the base, when the two powers are not of the same sign. 

Example of (1) +5 D Sph. O +2 D Cyl. Axis 70° to +6 D base. 

(a) +5 D Cyl. Axis 160° o +7 D Cyl. Axis 70°. 

(6) B= + 6 - 5= + 1 D. The Sph. is - 1 D. 

(c) C x =+5 + l=+6D Axis 160° and C 2 = +7 +1 = +8 D Axis 70°. 

- 1 D Sph. 

that 1S ' +6 D Cyl. Axis 160° O + 3 DCyl. Axis 70° 

Example of (2) +2 D Sph. o +3 D Cyl. Axis 135° to - 6 D base. 

(a) +2 DCyl. Axis 45° o +5 D Cyl. Axis 135°. 
(6) B=-6 -5=-llD. The Sph. is +11 D. 
( c ) d= +2 - 11= - 9 D Axis 45° and C 2 = +5 - 11 = - 6 D Axis 135°. 


+ 11 D Sph. 

that is, 

that is, 

-CD Cyl. Axis 135° o - 9 D Cyl. Axis 45°. 

Example of (3) -ID Sph. o +4 D Cyl. Axis 90° to +3 D base. 

(a) -ID Cyl. Axis 180° o +3 D Cyl. Axis 90°. 
(h) B= + 3-(-l)=+4 D. The Sph. is - 4 D. 
(c) C : = -1+4= +3D Axis 180°. C 2 =+3+4= +7 D Axis 90°. 

- 4 D Sph. 

+ 3 D Cyl. Axis 180° o +7 D Cyl. Axis 90°. 

The Toric, Cyl. and Sph. — If a circle is revolved around a chord not passing 
through its centre a toroid is generated. If the circle is of infinite radius the 
body generated is a cylinder. It is a sphere if the chord becomes a diameter. 
Thus a cyl. lens may be regarded as a toric having one power =0, and a 
sph. lens as one having both powers equal. 




Neutralisation is the process of finding that lens (or lenses) of opposite 
refraction and of known power (from the test case) which stops the movement 
caused by the lens to be analysed. 

1 % 






Fig. 121. 

A Cx. and a Cc. lens (Fig. 121) of the same power, when placed in con- 
tact, have no converging or diverging effect, the convergence of the Cx. being 
counteracted by the divergence of the Cc, and incident parallel light emerges 
parallel. When moved in front of the eye, they cause no movement of the 
image of the object viewed through them, as with a plane glass. 

Fig. 122 

Fig. 123. 

Analysing Card. — Analysis and neutralisation are facilitated by the ust 
of an analysing card, as shown in Fig. 122, although, in its absence, any 
clearly defined straight vertical, or horizontal line, as the framework of a 
window, serves the purpose. The card should be 18 or 20 inches square, with 
two crossed black lines about £ inch in width, running vertically and horizon- 
tally, and for most work should be distant not less than, say, 4 feet. 

Determination of Nature of a Lens. — The first step in the analysis of 
a spectacle lens is to learn whether or not it contains a cyl. element. A lens 




having a sph. power only, on being rotated around its geometrical centre in 
a plane parallel to the card, does not cause any change in the appearance of 
the lines of the analysing chart, because its prismatic elements are alike in all 
meridians. If the lens has a cyl. element the lines become oblique, as shown 
in Fig. 123, where the dotted lines represent the black lines of the chart as seen 
when the lens is rotated. This occurs because the prismatic elements are 
not alike in all meridians, and the subject is treated more fully in Chapter XII. 

Determination of Positive and Negative Power. — If an object be viewed 
through a lens and the latter moved across the line of vision, the virtual image 
seen moves in the opposite direction with a Cx. lens, and in the same direction 
with a Cc. lens. If the lens is displaced, say, downwards, the light from it 
passes through a peripheral portion of greater deviating power than the centre, 
and the object appears deviated in the direction of the apices of the virtual 
prisms of which the lens is formed, that is, towards the edge of a Cx., and to- 
wards the centre of a Cc. lens. The degree of deviation and the rapidity of 
movement of the image are proportional to the strength of the lens, the devia- 
tion being greater, as the part of the lens looked through is near the periphery. 
The apparent motion of the object viewed, as the lens is moved, is due to the 
fact that the lens increases gradually in prismatic or deviating power from centre- 
to periphery. 

D 1 
Fig. 126. 

Let the lens be a sph. or a cyl. whose power is in the horizontal plane. 
When a vertical line is viewed through the centre of the lens the part A B is 
seen continuous with the parts C and D beyond its edges (Fig. 124). Then 
if the lens be moved, say, to the right, A B becomes broken away from C and D 
to the left if the lens is Cx. (Fig. 125), and to the right if it is Cc. (Fig. 126). 
When making this test the lens should be moved slowly in a certain direction, 
and not rapidly from side to side or up and down. The lens should not be 
too close to the eyes, for then the line G and D beyond the edges cannot be 
seen ; the best distance is generally about 10 inches. 

If the object be first viewed through, say, the bottom of the lens, and this 
then moved downwards, the motion of the image is continuously ivith or 
against throughout the journey. 

If, instead of the lens, the head is moved, the image moves with the head 
if the lens is Cx., and in the opposite direction if it is Cc. ; movement of the 
head, say, to the right produces the same effect as movement of the lens 
to the left. 


A piano causes no deviation of the image when it is displaced, nor of the 
lines when it is rotated. 

A prism when displaced causes no further change in the image; its effect on 
being rotated is treated later. 

Magnification. — A square viewed through a sph. appears to be increased 
in size by a Cx. and decreased by a Cc. equally in every direction and (dis- 
regarding distortion) remains a true square. Through a cyl., it is apparently 
magnified across the axis, by a Cx., and diminished by a Cc. ; the size is un- 
altered in the direction of the axis, so that a square appears rectangular. 

Neutralisation of Sphericals. — If a lens has no cyl. element, its nature is next 
determined, and if Cx., a Cc. is selected from the trial case, as near the neces- 
sary power as can be judged, and then the two, held together, are again moved. 
If the movement is against, i.e. still that of a Cx., the power of the neutralising 
Cc. is insufficient, and a stronger one must be tried. If with the first neutralis- 
ing lens the movement of the two combined is with, i.e. that of a Cc, the 
neutralising lens is too strong, and a weaker one must be taken. A few trials 
will enable one to find a lens which, when placed in contact with the unknown 
lens, causes no displacement of the line; then the number of the neutralised 
Cx. is that of the neutralising Cc. To find the power of an unknown Cc. 
lens, a neutralising Cx. must, of course, be used. Practice will soon enable 
one to judge, by the degree or rapidity of movement, the approximate neutral- 
ising power needed, as well as to appreciate such slight movements as occur 
when neutralisation is nearly, but not quite, effected. When neutralising, 
the lenses must be in actual contact, because if separated the Cx. acts with 
increased effect. 

As stated, the best distance for neutralising is some 10", but if the lens 
is a powerful Cx. it must be held nearer the observer's eyes, or nothing can be 
seen through it owing to the strong convergence of the light. The nature 
of such a lens is, however, easily recognised from its form and from the blurred 
view. Again, if held at a distance well beyond its focal length, for instance, 
if a 4 in. Cx. be held 10" from the eye, the apparent movement of the object 
when the lens is moved is the same as with a Cc. lens, because then an inverted 
aerial image of the object is seen, and not the ordinary virtual image. 

The Principal Meridians of a Cylindrical. — If the lens contains a cyl. 
element the cross lines of the analysing card are seen continuous within and 
beyond the edges of the lens, as in Fig. 127, only when the axis of the lens is 
horizontal or vertical. The two principal Mers. then correspond in direction 
to the lines of the chart. Such a position for a cyl. must be found in order 
(a) to learn whether it is a piano- or a sph.-cyl., (b) to determine whether it 
is Cx. or Cc, and (c) to neutralise it. This position being found, the lens is 
first moved vertically and then horizontally. If no movement is observed in 
the one direction it is a plano-cyl. ; if there is movement in both directions 
it is a sph.-cyl., or its equivalent, a cross-cyl. 

Movement against indicates Cx. and movement with indicates Cc. power 



in that meridian. If there is movement in both Mers. they may be both 
against, both with, or the one against and the other with. The movement in 
the one Mer. must differ from that in the other if there is a cyl. element. 

Fig. 127. 

The axis of a plano-cyl. lies in the meridian in which there is no move- 
ment. The axis of the cyl., in a sph.-cyl., which has two positive or two 
negative powers, is in the principal meridian of lesser movement. When 
there are + and - powers the axis of the cyl. is also 'presumed to be in the 
principal meridian of lesser movement. In all cases the axis of the actual cyl. 
might be in the meridian of greater movement, because the same principal 
powers can be obtained in lenses of various forms. (See Transposing.) 

The angular position of the axis' is the same as that of the neutralising cyl. 
This can be determined after a little practice, with a fair degree of accuracy, 
when the lens is held as when in use. With more accuracy its numerical 
position can be determined by holding the lens against the neutralising lenses 
when the latter are in a trial frame, with the long diameter of the neutralised 
lens horizontal. The axis of the trial lens, being marked by a scratch, can 
be read off from the notation of the frame. 

There are several forms of inclinometers or axis-finders — that of Dr. 
Maddox is an excellent one — designed for the location of the axis of an un- 
known cyl. lens. A quick and fairly accurate method of locating the axis 
is by means of the protractor on the " Orthops " rule. 

For accuracy the procedure is as follows: Holding the lens and the neutral- 
ises in position, the axis of the cyl. is marked with a grease pencil on the 
lens by a line coinciding with the axis of the neutralising cyl. ; also the optical 
centre is marked by a dot. The lens is placed on a protractor with the dot 
at the centre, the long diameter of the lens being exactly horizontal; the 
angular position of the axis is then indicated on the protractor. Care must 
be taken that the same meridian is covered by the marked grease line both 
above and beloiv the central horizontal line. When the axis is oblique and the 
lens is not in a frame, consideration must be given as to which of the two faces 
of the lens is supposed to be directed outwards, since the position of the axis 
varies accordingly. The rule is that the Cc. surface of a periscopic or the 
less Cx., or the more Cc, surface of a lens is placed next to the eye. 


Neutralisation of Cylindrical. — For a plano-cyl. the procedure is the same 
as with a sph., except that cyls. are employed. The lens is rotated until the 
principal Mers. are vertical and horizontal, the Mcr. of no power is determined, 
and the other Mer. is then neutralised with a cyl. of opposite nature. The axis 
must be exactly vertical (or horizontal), therefore continuity of the crossed lines 
at the edges of the lens must be looked for, and constantly maintained during the 
process of neutralisation. 

Care also must be taken that the axis of the neutraliser precisely corre- 
sponds to that of the lens. 

In a sph. -cyl. the lesser movement is that due to the sph. alone, while the 
greater movement is caused by the united powers of the sph. and the cyl. 
The lens being held with its axis, say, vertical, that sph. of opposite refraction 
is found which neutralises, in the Ver. meridian, the movement of the Hor. 
line. This being achieved, the lens and the neutralising sph. are held to- 
gether, and the cyl. element is then neutralised with a cyl. axis vertical, of 
opposite refraction, in the same manner as if the lens were a plano-cyl. The 
rapidity and exactitude of the neutralisation depends, as with a plano-cyl., 
on the care exercised in keeping the principal meridians exactly parallel to the 
two lines of the chart, and the axes of the two cyls. exactly corresponding. 

Neutralisation of a sph. -cyl. can also be effected by neutralising each 
principal meridian separately with a sph., or with a cyl. whose axis is placed 
at right angles to the meridian that is being neutralised, the two powers thus 
found being transposed into a sph. -cyl. combination. These methods are, 
however, not so exact, especially for beginners. 

Cross-cyls., torics and oblicpuely crossed cyls. are all merely special forms 
of sph. -cyls., and are therefore analysed and neutralised in a similar manner. 

Expressing Sphero-Cylindricals. — Since any lens having two principal 
meridians can be put up in various forms, the neutralising combinations, while 
correctly indicating the refracting powers of the lens, may not represent the 
exact form in which it is made. It is always correct to express a combination 
as a sph.-cyl. with a sph. of the lower power. 

True Form of a Lens. — This can be learnt by (a) ordinary inspection, 
(b) reflection from the surfaces, (c) the lens measure or spherometer, (d) by a 
straight-edge which, when in contact, easily shows the difference between 
Cx. and Cc. curvature. 

The Scissors Movement. — On rotating a cyl. in a plane parallel to the 
analysing chart the lines on the latter appear to make a scissors-like move- 
ment, and if the rotation be continued, appear to move back again, the 
amount of dipping being dependent on the strength of the cyl. Each line 
appears to bend towards the meridian of greatest positive, or least negative, 
refraction, so that they both rotate towards the axis of a Cc. or away from 
the axis of a Cx. cyl., and since they incline towards each other, they are 
never at right angles except when the principal meridians of the lens corre- 
spond to them in direction. The inclination of the cross lines is due to the 



prismatic formation, the apparent displacement being towards the edges of the 
virtual prisms contained in the lens. 

The scissors movement with both Cx. and Cc. resemble each other, one 
end of the horizontal line moving up, the other down; one end of the vertical 
line moving to the right, the other to the left. For instance, a Cx. cyl. axis 
Ver. and a Cc. cyl. axis Hor., both rotated, say, clock-wise, cause similar 
movements of the cross lines. An attempt to neutralise by " stopping " the 
apparent inclinations might result in selecting for that purpose another cyl. 
of similar power and nature, instead of a cyl. of opposite nature but equal 
power, the two together making a sph. lens. 

Reversion 01 a Cyl. — If a cyl. (Fig. 128), having its axis at, say, 60° when 
the one face is to the front, is turned over so that the other face becomes the 
front, the axis, is then at 120° (Fig. 129). If the one position were 5°, the 
other would be 175°. It is only when the axis is vertical or horizontal that 
no change occurs on reversing the lens. When the one inclination is 45° or at 
135°, turning the lens over brings the axis to a position at right angles to the 
former one. The change in the numerical position of the axis, caused by 
reversing an oblique cyl., is calculated as so many degrees above or below 

the horizontal, or to the right or to the left of the vertical, and assigning 
its position accordingly; or it is done simply by deducting the numerical 
position of the axis from 180°. Thus, suppose the axis is at 60°, this is 30° 
to the right of the vertical; on turning the lens the axis is at 90° + 30°=120°, 
i.e., 30° to the left of the vertical, or more simply by 180° - 60°=120°. 

Prisms — The Base-Apex Plane. — When a prism ora lens having a prismatic 
element, is rotated around its geometrical centre, the base-apex plane and 
the edge of the prism are similarly rotated. If the cross lines of the chart 
ABCD (Fig. 130) be observed, the junction Z of the cross lines being deflected 
towards the edge of the prism, the vertical line moves horizontally and the 
horizontal line moves vertically, but the two always remain at right angles to 
each other. 

In, however, one certain position, there is a continuity of one of the lines 
within and beyond the edges of the glass, as in Fig. 131, where the vertical line 
A B is continuous. The direction of this line indicates that of the base-apex 


plane of the prism, or of the prismatic element of the lens. If the Hor. line 
C D is deflected upwards, as to E F, the apex is then pointing up towards A, 
and the base is doivn towards^. If the deflection of C 1) is downwards towards 


r/ ' 





\ / 

Fig. 131. 


G H the edge of the prism is pointing doivn, and the base is up. If properly 
marked, the indicating scratches of circular trial prisms lie over A B when that 
line appears continuous through the prism. 

Neutralisation of Prisms. — The strength of a prism can be learnt by- 
neutralisation. The base-apex line being located, the displacement of a bar 
of the analyser can be neutralised by trying one prism after another from 
the test case and placing it in opposition to the unknown prism; that is, 
placing the base of the former over the edge of the latter, until that test 
prism is found which causes both chart lines to be seen continuous beyond and 
through the two prisms. The number of the test prism, which neutralises 
the unknown prism, indicates the value of the latter. The deviation of the 
prism is neutralised, although the neutraliser may be numbered according to 
its principal angle. 

If the prism is combined with a sph. (or a sph.-cyl.) this latter must be 
first neutralised. With the lens and neutralisers held together, all having 
their geometrical centres coincident, the prismatic element is located and 
neutralised. It must be remembered that the decentration, with respect to 
each other, of neutralising Cx. and Cc. lenses, introduces prismatic effect not 
actually existing in the lens which is under analysis. Therefore the geometrical 
centres of all the lenses should exactly coincide when any prismatic element is 
suspected, or is being measured. 

If the angular inclination of an oblique prism is needed the base-apex 
line, when located, should be marked with a grease pencil and the angular 
position determined on a protractor, as for the axis of a cyl. 

Points on Neutralising. — Practice is necessary to neutralise rapidly and 
correctly, and it is well to commence with sphs., then proceed to plano-cyls. and 
finally to sph.-cyls. 

Holding several lenses together is difficult, but is rendered easier if the 
adjacent surfaces are Cx. to Cc. 


A lens possessing sph., cyl. and prismatic elements should be neutralised 
in that order. 

The front of the lens, i.e. the Cx. surface of a periscopic, or the more Cx. 
or less Cc. surface of any lens, must face the observer. 

A simple prism may be mistaken for a piano, since neither causes move- 
ment ; rotation is needed to distinguish between them. 

It is necessary to guard against supposing a prismatic element to exist, 
when it may be produced by holding the neutralising lens out of centre with 
the lens which is being tested. 

If the sph. is strong compared with the cyl. it is difficult to appreciate 
the latter until the sph. is partly neutralised. 

Similarly it is difficult to appreciate a weak sph., when combined with a 
strong cyl., until the latter is wholly or partly neutralised. 

When the two powers of a sph. -cyl. are nearly equal it is not always easy 
to determine in which Mer. the movement is the lesser, but this becomes easy 
when the lens is partly neutralised. 

A strong Cx. and a strong Cc. of equal powers (say over 10 D) do not pro- 
perly neutralise owing to the appreciable interval between their optical centres; 
the Cx. effect predominates. This is further considered in Chapter XV. 

When a sph. -cyl. or a toric has to be neutralised by a double, there is con- 
tact at the centre only and neutralisation at the periphery is then not obtained 
owing to separation. Attention must be confined to the centre. 

A great help in neutralising difficult lenses is a diaphragm made of card- 
board, with a quarter inch aperture, held between the two lens. This not 
only reduces the effective aperture of the lens but, also, renders holding them 
together much easier. 

Holding the lens or lenses farther away, or viewing a more remote object, 
facilitates the determination of very weak powers, or whether neutralisation 
is obtained. 

Other methods for measuring the powers of lenses and prisms arc dealt 
with in later chapters. 


Prism Nomenclature. — A prism placed in a spectacle frame with its base 
towards the nose is termed + or base in, one with its base towards the temple 
is - or base out ; it is up if the base is towards the brow, and down if towards 
the cheek. If there is a pair of prisms they are both base in, or both base out, 
or the one is up, and the other down. If they are oblique, the one is, say, out 
and up, the other is then out and down. In all cases they are, with respect to 
each other, in such positions that, if they were placed over each other, they 
would neutralise. 

A prism is horizontal, vertical, or oblique according as the base-apex line is 
Hor., Ver. or oblique respectively. 

Ophthalmic prisms are presumed to be thin, i.e. not exceeding, say, 20° 
principal angle. 

The indicated power of a prism in any notation is that due to its mini- 
mum deviation. 

The symbol A indicates prism power. 

Notation by the Principal Angle. — This actually gives the form only, and 
is somewhat similar to the numeration of lenses according to curvature; 
the true optical effect is not indicated. Two prisms of, say, 3°, the one of fi= 
1-5, and the other // 1-54, are both prisms of 3°, but their optical properties 
are not the same. The unit is a prism of 1° P. (principal angle). 

Notation by the Angle of Deviation indicates the true optical value of the 
prism in angular deviating power. Its value depends on P and//, with both of 
which it varies directly. This system has the drawback that the angle itself 
is inconvenient to measure in practice. The unit is a prism of 1° d. (deviation). 

Relationship of the °P. and the °d— If/t=l-5, l°=-5°d, but the °d increases 
with respect to the ° as the ju is higher. The number of degrees in the 
deviating angle being approximately half that of its principal angle, the °d is 
double the value of the °. Therefore, if two prisms of the same strength be 
numbered respectively in the two systems, its number in °d would be half 
that in °. If, however,// is taken as 1-52, the relative values are slightly 
less than 2 to 1. As here used, the °P is commonly written °. 

Notation by the Prism Diopter. — This notation, introduced by Mr. Charles 
Prentice of New York, is based on the linear deviation, and presents many 
advantages. The unit is the 1A which causes a deviation of 1 cm. (on a 



tangent) at a distance of 1 metre. It is, therefore, a 1% linear deviation, 
and N A/100 =tan d. 

Two prisms, numbered in A, when placed together are, however, equal to 
rather more than the sum of their individual powers. Again, the deviation 
being measured on a flat surface, increase in the linear deviation does not 
result in a corresponding increase of angular deviation. Thus 1A is equal 
to 34' 22|', but a 10 A is of less value in °d than 10 times that amount. These 
differences are, however, so very inconsiderable, especially in the weak prisms 
needed in spectacle work, as to be of no practical importance. 

If ^=1-575, the °=A, for -575°=34' 30", the tangent of which is -01. 
When ,it= 1-52, the refractive index of the glass usually employed, the °=-9A. 
These values can, however, be considered true for small angles only such as 
we find in the optics of spectacle work. 

Relative Values. — The relative values of the three units mentioned, in 
terms of the deviation they cause at the same distance, are 

the °P=-9; the A=l; the °d= 1-745, or say 1-75. 

The above are also the constants employed with each notation, and repre- 
sent percentage of linear deviation. 

Their equivalents are 1° = -52°i=-9A 

1A = .57<y7=M° 

Calculations in Prism Measurement. — The following, while sufficiently 
accurate for all practical purposes, are not exact, for the reasons given, and 
because we take angular and tangential variations to be equal : 

Let A represent the power of the prism, M its distance in metres from 
the object viewed, C the deviation in centimetres, and K a constant for each 
system of prism notation. Then 

C=A M K. 

Thus at 3 metres, the deviation caused by a 4°, a i°d, and a 4A 
respectively is 

4x3x -9 =10-8 cm. 
4x3x1-75=21 cm. 
4x3=12 cm. 

If the deviation caused by a prism at four metres is 5 cm., the prism is 
* =1-4°, or — y ~-~=.7°d, or ?=1-25A. 

4x-9 4x1-75 ' 4 

The distance at which a prism of 5°, one of 5°d, and one of 5A respec- 
tively causes a deviation of 15 cm., is 

6 -i 5 . 9 =3.33M. 5 -^ T6 =1.75M, "-« 


Conversion of Prismatic Values. — For conversion from one system of 
prism notation to another it is only necessary to remember the relative 
values of the units. Thus 

4° =4 x -9=3-6A, or 4 x ■9/l-75=2-06°d 
4A =4/-9=444°, or 4/1 -75 =2-28°d 
4°d=4 x l-75/-9=7-77°, or 4 x 1-75=7*. 

The Centrad is another prism unit, which causes at 1 M. a deviation of 1 cm. 
on the arc of a circle. The deviation is 1% and the difference between the 
arc and the tangent of small angles being negligible, the centrad and A may be 
considered equal. A given prism notated in A would be of fractionally higher 
number than if numbered in centrads. It is, however, much more incon- 
venient to measure on a curved than on a flat surface, and the centrad has 
never come into general use. Ny/100=arc d. Calculations for centrads 
can be taken as the same as for prism diopters. 

The Metran. — Another prism unit, suggested by L. Laurance, is the 
metran, which causes a deviation of 3 cm. when placed in front of the eye at 
one metre from the scale. It has, therefore, about 1-75° (or 1° 45') deviation, 
and is the same as the metre angle for the average interpupillary distance of 
2f in. or 60 mm. The symbol is thus 4 A. 

The Measure of the Principal Angle is termed goniometry. The principal 
angle of a prism can be found roughly by enclosing it between the legs of a 
pair of compasses and finding the angle so obtained on a protractor, or by 
any instrument made for the purpose; also by the goniometer, consisting of a 
pivoted arm, at one end of which there are two legs which rest on the face of 
the prism, the other end indicating the angle on a scale. It can also be deter- 
mined by the pin method described in Chapter XXVIII. The really accurate 
method is that of the spectrometer which is given in Chapter XX. Also, without 
much error for weak ophthalmic prisms, the tangent scale can be, and is, 

The Measure of the Deviating Angle or Prismetry is accurately made 
by the spectrometer method; an approximate pin method is described in 
Chapter XXVIII. The tangent scale and neutralisation methods are the prac- 
tical methods for thin prisms. 

The Measure of the Linear Deviation in A is made by neutralisation or the 
tangent scale. 

The Tangent Scale. — A tangent scale, shown in Fig. 132, serves as the 
most convenient method of measuring ophthalmic prisms. It is a card, say, 
12 inches wide and 30 inches long, scaled so that the intervals between the 
divisions represent the tangents of the angles of deviation, and was originally 
designed by Dr. Maddox. The intervals vary in size with the distance at 
which the card is used. 

The line A C (Fig. 133) is looked at through the prism, which is held 



with its base directed towards A, while the edge points to B. If the line A B 
is displaced upwards or downwards the prism must be rotated in a plane parallel 
to the card until A B is continuous and seen unbroken through the prism. 
The base-apex line is then horizontal, and the deviation is greater than with 
any other position of the prism in a plane parallel to the card. The number, 
towards which the deviated part A points, indicates the prismatic power 


1413 12 111° 9 8 7 6 5 4 3 2 1 


' Y 




Fig. 132. 

Fig. 133. 

of the prism in degrees of deviation, prism diopters or degrees, according to 
which notation the scale is arranged for. The prism must be held sufficiently 
low so that the numbers on the scale may be seen over the top of the prism 
while A is seen through it. 

The deviation caused by the prism varies if its position departs from that of 
minimum deviation ; consequently, when A B is unbroken, the prism must be 
rotated on its axis in order to secure minimum deviation, this being the 
numerical strength of the prism. Thus, in Fig. 133, the prism is presumed to 
be in the position of minimum deviation, and the indicated number is 3, 
but if the edge of the prism were turned either towards or away from the scale, 
the indicated deviation would be greater than 3. 

If the prism is combined with sph. or cyl. powers, these must be neutralised 
before the prismatic power can be measured on a tangent scale, care being 
taken that the geometrical centres of neutralising and neutralised lenses exactly 
coincide ; otherwise a false measure of the prismatic power is obtained. 

A tangent scale arranged for one system could be utilised for others by 
using it at the proper distance. Thus, the intervals on the " Orthops " scale 
(Fig. 132) are 3-5 cm., so that used at 2 M. the numbers indicate degrees of 
deviation, and at 3-5 M. prism diopters. If used at 4 M. it serves for ordinary 
degrees. The construction of tangent scales is dealt with in Chapter XXVI. 

Another Tangent Measurement. — As a modification of the ordinary 
tangent scale, parallel light is passed through a suitable Cx. cyl. and brought to 
a sharp focus as a vertical line at the zero of a tangent scale. The prism is 
then introduced, close to the cyl., with its edge towards the zero and its base- 
apex plane parallel to the horizontal line; the line of light is then deviated 
to some number on the scale, which indicates the value of the prism. This 
method is suggested by Dr. Maddox. 


Oblique Prisms. — A prism so changes the direction of light that an object 
viewed through it appears in a different position from that which it really 
occupies. The deviation is in the base-apex plane and towards the edge of 
the prism. 

If a cross bar be viewed through a prism held with base-apex plane hori- 
zontal, the vertical bar is displaced horizontally to an extent dependent on 
the strength of the prism, and there is no vertical displacement of the hori- 
zontal bar. If, now, the prism be rotated in a plane parallel to the card, 
so that the base-apex line is oblique to both bars, the horizontal deviation 
becomes less, and a vertical deviation is introduced (Fig. 130). If the rotation 
be continued, the horizontal deviation continues to decrease and the vertical 
to increase, until when the base-apex line is vertical all thedeviation is vertical, 
and there is none in the horizontal plane. The maximum effect d of the prism 
is always in the base-apex plane, and when the latter is oblique, its effect can 
be divided into V, a vertical, and H, a horizontal component, which are equal 
when the base-apex line is at 45°. 

Resultant Prism. — The power of a prism varies as cos r, the angle between 
the base-apex plane and a given Mer. (Chapter XXII.). An oblique prism 
has Hor. and Ver. components, so that if Hor. and Ver. prismatic effects are 
needed they can be obtained from a single oblique or resultant prism A> as 
calculated from the following formulae, which are simplified forms of those 
given in Chapter XXII. 

A=VH 2 + V 2 and tanr=V/H 

Where H is the horizontal and V is the vertical component, and r is the 
angular distance of the base-apex plane of the resultant prism from the hori- 

Thus, let a Z°d base-apex line Hor., and 2°d base-apex line Ver. be re- 
then A= V3 2 + 2 2 = Vl3=3-6°cZ=3° 36' 

tan r=V/H=2/3=-666=tan 33° 40', so that r=33° 40' 

The base-apex line is 33° 40' from the Hor., or 56° 20' from the Ver. ; that is, 
approximately, 3-b°d base-apex line at 35°. 

If the original Hor. prism were base in, and the Ver. prism base down, 
A would have its base inwards and downwards; that is, for a right eye, the 
apex would be at 145° (standard notation). If the prism power were divided 
into a pair, then each would be of half the value of A? and that for the left 
eye would be at the same inclination with its base inwards and upwards, that 
is (in standard notation), with the base at 145°. 

Fuller discussions on this and other points in connection with prisms will 
be found in Chapter XXII., and in " Visual Optics and Sight-Testing." 

Construction. — For the construction of the resultant of two prisms at 
right angles, draw a vertical line V (Fig. 134) as many inches (or cm.) long as 



there are units (degrees, etc.) in the Ver. prism, and a horizontal line H as 
many inches (or cm.) long as there are units in the horizontal prism. Theii 

extremities are connected by a third line, P, whose length represents the 
number of units in the resultant prism; the angular distance of P from # or 
V, as measured by a protractor, is that of the base-apex line of the resultant 
prism from the Hor. or Ver. respectively: 

Practical Method. — Holding the Hor. and Ver. prisms together, find on a 
tangent scale the maximum deviation; this is the value of the resultant prism, 
and its direction with respect to the originals is marked with a grease pencil. 
Or the two original prisms can be put into a trial frame and neutralised by a 
single prism from the trial case; the power of the neutraliser is that of the 
resultant prism, and its inclination is indicated. 

Rotary or Variable Prism. — A rotary prism consists of two Ver. prisms of 
equal power conveniently mounted. In the primary position the base of the 
one coincides with the edge of the other, so that the effect is 0. From this 
position they are rotated towards the Hor., so that their bases approach each 
other; thus a gradually increasing Hor. effect is obtained while the Ver. 
remains 0. The maximum effect is obtained when the two bases coincide in 
the Hor. Mer. If the primary position is Hor. a varying Ver. effect is obtained 
while the Hor. remains zero. 

Variable prismatic effect may also be obtained by sliding, one over the 
other, two sph. lenses of equal and opposite power, that is, by their mutual 
decentrations in opposite directions. 



The Optical Centre of a sph. lens is situated on the principal axis, and is 
the point of no prismatic effect. It is, therefore, in the thickest part of a 
convex, and the thinnest part of a concave lens. 

The Geometrical Centre is that point which is equi-distant from the opposite 
edges. It can be located by inspection, or, more exactly, by drawing a line 
connecting the two extremities of the long diameter, and another connecting 
the highest and lowest points; where they cut each other is the geometrical 

^ 1 

o \ 

[ \ 

Fig. 135. 

To locate the 0. C, the lens must be moved about until cross lines seen 
through it are continuous with the parts of the lines seen beyond the edges, 
as in Fig. 135, where G is the geometrical centre of the lens. The optical 
centre coincides with that point of the lens opposite to the intersection 
of the cross lines. It can, if necessary, be marked by a dot with a grease 
pencil or with ink. For strong lenses the test should be made with fine cross 
lines on a small card placed on the table, the lens being held steadily a short 
distance above the card, and in a plane parallel to it. Accuracy is enhanced 
by employing a pinhole, through which the observation is made. The 
analysing card at a reasonable distance is better for weak lenses. 

The same procedure is employed for a sph.-cyl., the principal meridians 
being -parallel to the lines of the card. With a plano-cyl., the central point of the 
axis may be regarded as the 0. C. 

Centered and Decentered Lenses. — A lens is centered when its optical and 
geometrical centres coincide, and is decentered when they do not. When 
an object is viewed through the geometrical centre of a decentered lens the 




effect is precisely the same as if the lens were combined with a prism. Simi- 
larly, if a centered lens is looked through at a point which is not in line with 
the optical and geometrical centres the effect is the same as if a sphero-prism 
were substituted. 

To learn whether a sph. lens is truly centered the analysing card is viewed 
through its geometrical centre. If centered (Fig. 136) the junction of the 
cross lines is seen in line with the exact centre of the lens. If decentered the 

Fig. 136. 

Fig. 137. 

Fig. 138. 

junction does not coincide with the centre of the lens and the Ver. line, as in 
Fig. 137, or the Hor. line as in Fig. 138, is broken at the edges of the lens, or 
both are broken. 

In a sph. lens there is only one point, i.e. the optical centre on the prin- 
cipal axis of the lens where there is no prismatic effect. 

In a plano-cyl. there is a line without prismatic effect along the axis. 

In a sph.-cyl. lens there is a point of no prismatic effect where the axis of 
the cyl. cuts that of the sph., and it is therefore at the geometrical centre 
of a centered lens. 

Fig. 139. 

Fig. 140. 

The Prismatic Action of Sphs. — A sph. lens, at any point other than the 
0. C, acts as a prism, the prismatic power being greater as the part of the lens, 
through which the ray passes, is more distant from the axis. 

Let S S (Fig. 139) be a screen situated in the focal plane of a +1 D lens; 
the distance F is therefore 1 M. The ray A B incident at B situated, say, 
1 cm. from the axis, instead of falling on the screen at B' , as it would if it were 
unrefracted, is refracted to meet the axis at F. It is, therefore, deviated the 
distance B' F=B 0—1 cm. at 1 M. The ray C D incident, say, 2 cm. from the 
axis, is deviated the distance D' F—D 0—2 cm. at I M since it also meets the 



axis at F. The prismatic effect of the lens at B or at D is, therefore, the same 
as that of a prism of 1 A or 2 A since such prisms cause similar deviations. 

In Fig. 140 the lens is +2 D and S S is 1 M from it; a ray AB, parallel 
to the axis, and incident at B, 1 cm. from the axis, meets the latter at F, 
50 cm. from the lens, and the screen at G instead of at B" . The ray is deviated 
a distance B' F=l cm. at 50 cm., and B" (?=2 cm. at 1 M, so that the prismatic 
effect is the same as that of a 2 A acting on a ray unrefracted by the lens. 
If the lens were +4 D, AB would meet the axis at 25 cm. from the lens and 
would be there deviated 1 cm. The +2 D at 2 cm. from the axis has the 
effect of 4 A , while the 4 D at the same point has the effect of 8 A . 

The prismatic power A in prism diopters, of a sph. lens at a point C whose 
distance from the axis is expressed in cm., is 

A=D C. 

The Prismatic Action of Cyls. — In Fig. 141 let the lens be a + cyl., whose 
axis A X is at 45°, B C is a Ver., and D E a Hor. line. On looking through 
the lens the points F G H on the vertical line B C are seen deflected by the 
prismatic action of the cyl. to F'G'W, upwards and to the left, the virtual 
prisms being base down and to the right. The points K L M on the horizontal 
line D E are seen deflected to K'L'M', also upwards and to the left, the virtual 
prisms being base down and to the right. On the other side of the axis the 
virtual prisms are base up and to the left, and the deflections are downwards 
and to the right. Thus a convex cylindrical axis, say, 45°, causes a vertical 
line BC to appear as B'C, and a horizontal line D E to appear as D'E', both 
being deviated away from the axis. 

If another equal + cyl. be placed axis at right angles to the first, the 
horizontal deviation of the vertical line, and the vertical deviation of the 
horizontal, are neutralised, but the vertical effect in the vertical meridian 



and the horizontal effect in the horizontal are doubled, the combination 
being equivalent to a sph. lens in which the prismatic effects are equal in 
every meridian. 

With a concave cyl. the edges of the virtual prisms are towards the axis, 
and if a - cyl. Ax. 45° be looked through (Fig. 142) a vertical line BC appears 

as B' C, and a horizontal line D E appears as D' E', the deviation of these 
lines being towards the axis of the lens, or towards the apices of the virtual 

In Fig. 143 let the lens be a + sph. -cyl., whose axis A X is at 45°. 
Let B be a point situated between the Ver. and the axis. There is, at this 
point, the effect B of a prism base down to the left derived from the sph. 
The cyl. contributes a prismatic effect PB, the base of the virtual prism being 
down to the right. Thus there are two Ver. effects both directed upwards, 

Fig. 143. 

Fig. 144. 

and two Hor., the one directed to the left and the other to the right. These 
latter neutralise each other at some point B, and similarly at every point on 
the line E F. 

Between the axis and the Hor., at some point C, there is the effect C of 
a prism base down and to the left derived from the sph., and from the cyl. 



there is the effect P C of a prism base up and to the left. There are thus two 
Hor. effects both directed to the left, and two Ver., the one up and the other 
down. At some point C the opposing Ver. effects neutralise each other, and 
similarly we have a neutralising effect all along the line G H. 

In a Cc. sph.-cyl. there are similar prismatic effects, but in the opposite 

Let Fig. 144 be a combination of +Cyl. Ax. 45° O -Cyl. Ax. 135°, the 
two being of equal power. C D is the axis of the Cx. cyl., and E F that 
of the Cc. At some point A the Cx. cyl. has an effect X A of a prism base 
down and to the right, the Cc. has an effect YA of one base up and to the 
right. The up and down Ver. effects neutralise each other, but there is a 
combined lateral effect. At the point B the Cx. acts with an effect X B base 
up and to the left, and the Cc. with an effect Y B base up and to the right. 
The right and left Hor. effects neutralising each other, the combined deviation 
being Ver. Thus the point A would be deviated to the left, and B downwards. 
A Ver. line is seen inclined to the left above, and to the right below; a Hor. 
line is inclined downwards on the right, and upwards on the left. 

Locating the Lines of No Prism Effect. — If an oblique sph.-cyl. be moved 
horizontally until the oblique image of a vertical line is seen in contact at 
B (Fig. 145), at the upper edge of the lens, with the line itself seen above 
the lens, and similar contact is then obtained at the lower edge of the lens, 
say at C, the line connecting these two contact points indicates the line of no 

Fig. 146. 

Fig. 147. 

Fig. 148. 



Hor. prismatic effect. Similarly the points can be found where, by moving 
the lens vertically upwards and downwards, a horizontal bar is, at each side, 
in contact with its image; the line connecting them indicates the line of no 
Ver. prismatic effect. 

Prismatic Action by Decentration. — A ray A B (Fig. 146) passing through 
the 0. C. of a Cx. lens L and a prism P, base to the right, is undeviated by 
the lens and is bent towards the right by the prism. If that ray passed 
through the left portion of a Cx. lens (Fig. 147) or the right portion of a Cc. 
(Fig. 148), it is similarly deviated to the right. Therefore, if the action of a 
prism, base in a certain direction, is required it can be obtained by utilising 
the opposite portion of a Cx. and the corresponding portion of a Cc. lens. 

Fig. 149. 

Fig. 150. 

If half only of a lens be utilised (Figs. 149 and 150), the image of a point 
on the axis has its image opposite to one extremity of the lens instead of 
being opposite to the geometrical centre, as with an ordinary centered lens. 

Fig. 151. 

Fig/ 152. 

There is no difference whatever between combining a prism with a sph., 
grinding sph. surfaces on to a prism, or at such an angle to each other that 
a prismatic as well as sph. form results, or by cutting out a lens so that its 
0. C. is displaced from the centre of the lens, that is, by cutting away part 
of the lens as in Fig. 151. In all cases the result is as if two plano-Cx. lenses 
had been cemented to the faces of a prism (Fig. 152). 

Formulae for Decentering. — The prismatic effect obtained by decentration 
is directly proportional to the amount of decentration and to the strength 
of the lens, so that the decentration necessary to obtain a desired prismatic 
effect is directly proportional to the effect required, and inversely proportional 
to the power of the lens. 

Let A represent the prismatic effect needed in A, D the dioptral number 
of the lens, and C the decentration in centimetres, then 


This simple relationship between lenses and prisms was first shown by 
Prentice of New York. 



By introducing the necessary constant K, the formula for prism diopters 
apply also for degrees, whose constant is -9, and to degrees of deviation, the 
constant being 1-75, so that 

' A=D C/K 

The constant -9 for degrees is on the presumption that the prisms used 
have ^=1-52; if ^=1-5, then K=-87 and for ^=1-54, K=-94. 

Direction of Decentration. — To produce the effect of a prism with its 
base in a certain direction, a Cx. lens must be decentered in that same direc- 
tion, and a Cc. in the opposite direction. 

How to Decentre. — Decentering is achieved by so cutting the unedged 
glass disc that the optical centre is nearer than the geometrical centre to one 
part of the edge of the finished lens. The optical centre (Fig. 153) is located 
as previously described, and marked by a dot, the required amount of decen- 
tration is measured off, and the point G, which is to be the geometrical centre 
of the edged lens, is also marked. 

Fig. 153. 

The lens is then cut out so that G is in the centre, as shown in Fig. 153. 

The direction of decentration is indicated by the position ofO, the fixed point 
of a lens, with reference to G. The distance G is marked off contrary to the 
decentration required. If has to be in, the distance measured off, in order to 
mark where G is to be, is out from 0. 

To Measure Decentration. — The geometrical and optical centres are 
marked, and the distance between them is measured by placing the lens on a 
metric rule. 

Examples. — On a + 4-5 D lens, the effect of 2 A base down is required, 
the lens must be decentered 

0=2/4-5=444 cm. down. 

For the effect of -5°^ base in on a + 6 D 

C=-5 x l-75/6=-15 in. 

For the effect of 2°d base in on a -8D lens 

C=2 x 1-75/8=44 cm. out. 
If on a - 5 D lens the effect of 3-5° base down is required, 

C=3-5 x -9/5=-63 cm. up. 


If a + 4 D is decentered out «75 cm., the prismatic effect will then be 

4=.75x4=3 A or •75x4/l-75=l-75°rf, or -75 x4/-9=3-3° 

If the 0. 05 of the lens is -75 cm. from the geometrical centre, and the 
prismatic effect, as measured on a tangent scale, is 3 A , the lens is 

D=3/-75=4 D. 

In using these formula?, fractions of degrees should be expressed as decimals, 
and not as minutes and seconds, and the decentration in cm. and decimals 
thereof. These rules, while sufficiently accurate for practical spectacle work, 
especially as no lens can be decentered to a very great extent, are not exact, 
since the variation of angles has been taken as equivalent to that of their 

Limitations to Decentering. — The smaller the size of the lens required 
and the larger the disc from which it is cut, the greater is the extent of 
decentration possible. If the edged lens were to be about as large as the 
unedged disc in any direction no decentering would be possible. Since the 
usual finished lens is longer in the horizontal than in the vertical diameter, 
a greater vertical than horizontal decentration is possible. Thus a lens 
of No. 1 eye size, when edged, can be decentered about 4 mm. horizontally 
and 7 mm. vertically; for smaller lenses the extents are greater, while for 
larger ones they are smaller. The average size of the uncut disc is 40 to 44 mm. 

Another method of decentering is to place in contact with the lens a prism, 
equal to the effect required, with its base in the opposite direction; mark the 
0. C. on the lens as then found, and this point is the geometrical centre needed. 
By this method one can at once see whether the required effect can be obtained 
by decentering, it being impossible if the marked point be too near the 
periphery, much less if, as may be the case, it is beyond the lens. It is 
specially suitable for oblique decelerations. Thus suppose 1 A base in effect 
is needed on a +4D lens; a 1 A base out is placed with the lens, the 0. C. is 
then displaced outwards, the lens must be shifted -25 cm. inwards to find the 
point of no prism effect, and this indicates the geometrical centre of the 
finished lens. 

Formulae Involving F. — Where F or 1/F is given, it is easier to convert 
into diopters, but the calculations can be made by the following, where both F 
and the decentration are expressed either in inches or cm., K being the 
constant — 


Thus, how much should a 4 in. lens be decentered for 1° ? 

Decentration =1 x 4 x -9/100 =-036 in. 



More Exact Formulae. — More accurate formulas for decentratiou for °d 
are as follows, where F and D have the usual significations, and d is the degree 
of deviation : 

tan d=C/F or C=F tan d ; 


tan d- 

=CD/100 or C=100tand/D. 

These formulas are illustrated in Fig. 139, where D' F equals the tangent 
of the angle of deviation of the ray CDF. 

Resultant Decentrations. — As the value of a prism is at its maximum in the 
base-apex plane, and has a value of A cos r in any other Mer., a lens if decen- 
tered has its maximum prismatic effect in the plane of decentration, and in 
any other Mer. A=DC cos r. An oblique decentration has always Hor. and 
Ver. effects and if a lens has to be decentered for both Ver. and Hor. prismatic 
effects, the two can be obtained by a single oblique decentration. 

Fia. 154. 

Thus in Fig. 154 let be the optical centre. If the geometrical centre is 
moved horizontally from to h and vertically to v, the actual displacement is 
along v. A resultant decentration is calculated by finding the oblique 
prismatic effect required and its angle r, and then decentering accordingly. 

Thus suppose a +5 D lens has to be decentered for a Hor. effect of 2 A , 
and a Ver. effect of 1-5 A ; then 


+ l-5 2 =2-5 A 

and tanr=l-5/2=-75=tan37°(approx.) 

C=2-5/5=-5 cm. 

The two needed prismatic effects are obtained by decentering the lens 
•5 cm. along meridian 37°. 

The Ver. and Hor. decentrations V and H could be found separately and 
a resultant decentration then calculated, but the above method is simpler. 
Thus, in the above example, 

H=2/5=-4cm. and V=l-5/5=-3 cm. 
and A=V-4 2 + -3 2 = V-25 = -5cm. 

tan r=V/H=-3/4=-75=tan 37°. 


The Decentration of Cyls. and Sph.-Cyls. — Those cyls. and sph.-cyls. 
whose principal Mers. are Ver. and Hor. are upright, in contradistinction 
to those which are oblique. 

A lens possessing a cyl. element should not be decentered except in its 
principal meridians, that is to say, upright cyls. ought not to be decentered 
obliquely, nor should oblique cyls. be decentered horizontally or vertically. 
Such decentrations can be made, but the results are difficult to calculate owing 
to the fact that the prismatic elements in a cyl. have their base-apex lines at 
right angles to the axis and therefore, also, it is impossible to obtain a 
Hor. or Ver. effect alone. 

Upright Cyls. — The effect of decentering a cyl. across its axis is the same 
as decentering a sph. in that direction; along the axis there is no effect, since 
there is no refractive power. Thus a cyl. axis Ver. can be decentered hori- 
zontally, but not vertically; a cyl. axis Hor. can only be decentered vertically. 

If +4 C. Ax. 90° requires decentration for the effect of 2 A , base out, 

C=2/4='5 cm. out. 

Upright Sph.-Cyls. — Decentering a sph.-cyl. across the axis of the cyl. 
has the same effect as decentering a sph. whose power is that of the two 
powers combined; while in the direction of the axis it is the same as decen- 
tering the sph. alone. 

If - 3 S. o - 2 C. Ax. 90° is to be decentered for 2 A base in, the power 
in the Hor. Mer. is 3 + 2=5 D; therefore 

C=2/5=-4 cm. out. 

If +2 S. o - 5 C. Ax. 180° needs to be decentered for 2 A base down, the 
power in the Ver. Mer. being -3D, 

C=2/3=-66 cm. up. 

Oblique Cyls. and Decentrations. — For oblique decentrations of upright 
cyls. and sph.-cyls., and the Hor. and Ver. decentrations of oblique cyls. and 
sph.-cyls., and the Hor. and Ver. effects of oblique decentrations see 
Chapter XXII. 



Effect of Altered Position of a Cx. Lens. — The power of a given lens 1/F 
or D is a fixed quantity, but its effect, in relation to a given plane behind it, 
varies with its distance from that plane. 





Fig. 155. 

Fig. 156. 


Thus, in Fig. 155 let a Cx. lens L of 10" focal length be in the plane P, 
so that, if the source of light be distant, F lies 10" behind P. If the lens be 
advanced say, 2", to L' towards the light source, F is similarly advanced to 
F' and lies 8" behind P. Then the effect of the advancement is the same 
as if the 10" had been replaced by an 8" lens in the plane P. Or the effect 
is the same as if 1/8-1/10=1/40 Cx. lens had been added to the 1/10. 
The expression of effectivity for a Cx. lens is 




F V =F-<Z 

where d is the distance between the lens and the plane of reference. 

The increase of effect is due to the fact that the light in the plane of P 
is more convergent when L is in advance of it. 

If J=F then 1/F - fI=l/0= oo ; the converging effect is infinite in a plane 
when the lens is in advance of it a distance equal to its focal length. If d 
exceeds F, then 1/F V becomes negative, the light diverging to the plane after 
coming to a focus in F. 

. The effect of a Cx. lens on P, when the light is parallel, increases, as d 
increases, from 1/F to oo and then becomes negative. 

Effect of Altered Position of a Cc. Lens. — The effect produced by similarly 
moving a Cc. lens is opposite in character. LetP be the plane (Fig. 156), and 
L a 10 in. Cc. lens placed in it. F will then be 10" in front of P if the source 
is distant. If L be moved forward to L' a distance rf=2", for example, then 



F is similarly moved to F', so that the effect in P is the same as if a lens of 
12" F had been substituted for the 10"; or the effect is the same as if a 
- 1/10 - ( - 1/12)= + 1/60 had been added to the - 1/10. The expression 
of effectivity for a Cc. lens is the same as for a Cx., but the focal distance, 
being negative, requires the use of the - sign before the value of F in sub- 

The decrease of effect is due to the fact that the light in the plane of P 
is less divergent when L is in advance of it. The effect of the lens in P 
when the light is parallel decreases, as d increases, from 1/F to 0, the latter 
obtaining when d is infinite. 

For distant objects, therefore, a Cx. lens, on movement away from a 
plane, can never have less + , and a Cc. can never have more - effect than 
its own power. 

Change of Effect.— The altered effect of a lens when moved from one 
position to another in front of a plane, or another lens, is the difference 
between its eflectivity in its original, and in its new, position; thus, a 5 in. 
Cx. lens moved from 1 in. to 2 in. away from a plane, the change is 

1 1111 

5-2 5-1 3 4 12 

or an increase of effect equal to that of an added 1/12 Cx. 

A 5 in. Cc. similarly moved causes a decrease of effect just as if a 1/42 
convex had been added to the concave, as shown by 

-5-2 -5-1 7 \ 6/ 


+ 42 

Cx. Lens and Divergent Light.— Let a 10" Cx. lens be in a plane P and a 
source of light be at some finite distance, say, 40" in front of it. Then /a 
is at (approx.) 13" behind P. If now the lens be advanced a distance d 
towards the source/ 2 tends to be advanced towards P, but since L approaches 
the source, f becomes shorter and in consequence f % becomes longer and 
tends to be further behind P. Of these two counteracting effects the one 
or other predominates obviously according as d is greater or smaller than 
the recession of/ 2 due to the shortening oif v 

IiJ l the anterior conjugate is shortened by an amount d, f 2 the posterior 
conjugate is lengthened less than d if j\ exceeds 2F, and more than d if f x 
is less than 2F. Therefore we have the rule that: — Removal of a Cx. lens 
toivards the source of light causes increased effectivity so long as the' distance 
between the Cx. lens and the object f is not less than 2F. At this distance the 
lens has for the given position of the object with respect toP, the highest possible 
effectivity, which is reduced by any further withdrawal of the lens outwards. 

When the Cx. lens is nearer to the object than F, the light after refraction 
is no longer convergent, but divergent, and when the lens is in contact with 
the object the effectivity of the Cx. lens is zero, because, in this case the diverg- 


enco of the light from the object is infinite in comparison with the power of 
the lens. 

Cc. Lens and Divergent Light. — Let a 10" Cc. lens be in a plane P, and 
the sources be near, say, 40". Then/ 2 is at 8" in front of P. When the lens 
is advanced a distance cl, f 2 tends to be also advanced, but the increased 
divergence of the light, owing to the shortening oif v tends to cause f 2 to 
be also shortened. Of these two opposing effects the former always pre- 
dominates, that is to say, the efEectivity is lessened, and becomes zero when 
the Cc. lens is in contact with the object. Again, in the last case, the diverg- 
ence of light from the object is infinite compared with the power of the lens. 

Summary. — When light is parallel, advance of a Cx. lens always results 
in increased efEectivity, and advance of a Cc. in decreased efEectivity, with 
respect to the original plane. 

If incident light be divergent an increased effect may be obtained by 
increasing the distance between a Cx. lens and a plane behind it, but the 
increase for a given movement is less than if the light were parallel; there 
will be a decreased effect if/ x is less than 2 F. With a Cc. lens the resultant 
effect is always decreased, but the change is smaller as the distance between 
the object and lens is less. 

When a lens, whether Cx. or Cc, is in a given plane its effect there, when 
the light is parallel, is 1/F, and when the light is divergent it is l// 2 . When 
the lens is in contact with uhe object the effect is, as before stated, zero. 

Dioptral Expression for Eff ectivity. — If the power of the lens be expressed 
in diopters, and the source is distant, its effective power D v in a new position 

100 1000 

D ^F^ ° r TTd 

F and d being expressed in cm. or mm. respectively. 

Thus, suppose a + 8 D lens is moved from a given plane to a position 
10 mm. further forward, towards the source of light, then F is 1000/8— 
125 mm. 

D v --1000/(125 - 10) =8-7 

The effect is increased 8-7 - 8=*7D. 
If the lens were - 8 D, similarly moved 

D =1000/ ( - 125 - 10)= - 7-4 

The effect is decreased -6D. 

If a + 10 D lens be moved from 15 to 20 mm. in front of a given plane, 
since F=100 mm., we have 

at 15 mm. D v =1000/(100 - 15)=ll-77 
at 20 mm. D T =1000/(100 - 20)=12-5 

so that the effect is increased by 12-5 - ll-77 = -73 D. 



Similarly, moving the lens back from 20 to 15 mm. decreases the effec- 
tivity to a like extent. 

Effectivity of Two Thin Lenses. — The combined power of two thin lenses, 
placed together, is equal to the sum of their individual powers, thus 

i = i + 1 3+F 2 or F _ Fl F 2 

F F x F, FjF 2 Fj + Fa 

But if they are separated by an interval d the resultant effect is not the 
same as if they were in contact. The distance of F behind the back lens, 
that is, the back surface or effective focal distance F B , is different because the 
effectivity of the front lens has now become l/(F t - d) in the plane of the 
second lens F 2 . Therefore 

1 ' *! or .•-<».-<>*. 

F, F,-rf'F 2 ■ F 1 + F 2 -<( 

where F 2 pertains to the front, F 2 to the back lens, and d is the distance 
between them. 

Fig. 157. 

Effective F of Two Cx. Lenses. — In Fig. 157 let L t and L 2 be two thin 
Cx. lenses of 10" and 7" focal length respectively, separated by 2", then 

(Vj-djJfz (10-2)x7 56 
B F a +F 2 -ri ' 10 + 7-2 "15 15 ' 

The distance of F behind the back lens is shortened. Parallel light in- 
cident on L x is converged towards F v 10 in. behind it, but on its way it 
meets, at 2 in. from L v the 7 in. Cx. lens L 2 , and converges towards a point 
10-2=8 in. behind the latter. The effectivity of L x in the plane of L 2 is 
1/8, or the effect is the same as if an 8 in. lens were in contact with Z/ 2 , and 
the common focus F v is at 3yi in. instead of 4 T y in., where it would be if 
L x were touching L 2 . The separation of Cx. lenses increases the effectivity of 
the combination in the plane of L 2 or any plane behind it. 

The distance of F B differs considerably when the two lenses are of different 
powers, according as the one or the other faces the light. Thus, if the com- 
bination were reversed so that the 7 in. Cx. faced the light, and the 10 in. 
Cx. were 2 in. behind it, F B =3$ in. instead of 3H in. F B is equally distant 
from the second (back) lens only when the lenses are equal and of the same 



When d=F 1 .— If a Cx. lens L^ (Fig. 158) is placed at its principal focal 
distance in front of another Cx. lens L 2 the latter has no effect whatever, 
its power being zero compared -with the infinite effectivity of L v F B ~0 or 

\/F B =cc. 

Fig. 158. 

When d exceeds F x then F B is negative. 

When d=Fj + J?., of two Cx. lenses the system is afocal—i.e. parallel light 
emerges parallel. Such lenses represent the Erecting Eye-piece when the 
two lenses are equal (Fig. 159). They represent the Astronomical Telescope 
when they are unequal. 

When d exceeds F 1 + F 2 the principle of the Microscope obtains. 

When d=Fj - F 2 the Huyghen Eye-piece is represented, and F B —F 2 /2. 

When F t =F 2 and d=F x we have the Kellner Eye-piece. 

When d=2F 1 /3 we have the Ramsden Eye-piece. 

The instruments and eye-pieces above mentioned are treated more fully' 
in Chapter XXVII. 

Fig. 159. 

Effective F of Two Cc. Lenses. — When two Cc. lenses are separated the 
focal length becomes lengthened. Thus let L 1 and L 2 be two thin Cc. lenses 
of, say, 10 in. and 7 in. F respectively. If L x is 2 in. in advance of L 2 


(-10-2)x -7 +84 



- 4 T 8 gr in. 

The distance of F as measured from L 2 is longer, owing to the interval 
between the lenses. Parallel light incident on L^ is rendered divergent as 
if proceeding from 2^=10" in front of L v and therefore 12" in front of L ? . 
The divergence of L x in the plane of L 2 is then 1/12 instead of 1/10, so that 



the combined focus F B is at 4 T V' instead of at 4 T 2 T where it would be if 
the lenses were close together. The separation o/Cc. lenses lessens the effec- 
tivity in the plane of L 2 or in any plane behind it. 

As with Cx. lenses, the distance of F B from the back lens of a combination 
of two unequal Cc. lenses, separated by an interval, varies as the one or the 
other lens faces the light. Thus, if the 7 in. Cc. were 2 in. in front of the 
10 in., jF ==4^£ in. from L 2 . 

— * — \ 

I , 

; I 


> /L 


Fig. 100. 

Fig. 161. 

Effective F of Cx. and Cc. with Cx. in Front. — In Fig. 160 let L x be a 10 in 

Cx. and L 2 a 10 in. Cc. ; in contact with each other tbey neutralise whichever 
lens is to the front. If they be separated (Fig. 161) the increased effect of L x 
in the plane of L 2 \s such that the combination becomes positive, illustrating 
the principle of the Unofocal photographic objective. 
Thus, if rZ=4" 

F = 

x B 

ao-4)x -io 


10-10-4 "-4 

=15 in. 

Parallel light incident on the Cx. is converged to 2^=10" behind it. 
It then meets the Cc. 4" further back, so that F % is 6" behind the latter, and 
the effect of the Cx. in the plane of the Cc. is 1/(10 -4)=l/6; F B is then 
lengthened by the Cc. to 15" as calculated. 


If, however, the combination shown in Fig. 161 be reversed (Fig. 162) 
so that the light is incident first on the Cc. it is rendered divergent as from 
10 + 4=14" from the Cx., and 

1/F B = + 1/10 -1/14-1/35; 

thus F B is at 35", or 20" further from L 2 when the Cc. faces the light than 
when the Cx. does so. The difference in F B on the one and other side of a 
combination is much more pronounced when the lenses are of opposite nature 
than when they are both Cx. or both Cc. Indeed, with the former F n may 


be positive when the light meets the Cc. first and negative when the Cx. is 
in front, as when d exceeds F of the Cx. 

Effective F when the Cx. is the Stronger. — If a Cc. be in contact with a 
stronger Cx. the combined effect is positive whichever lens faces the light. 
With the Cx. to the front separation results in still greater positive effect, 
F B being shorter than when the lenses are in contact. 

If d=F x the Cc. lens has no influence, so that F B =0. If d exceeds F v 
the light refracted by the Cx. is brought to a focus, whence it diverges to 
the Cc, which increases the divergence, so that F B is negative. 

With the weaker Cc. to the front the positive combined effect increases 
with greater separation, but the minimum value of F B is F of the Cx., the 
two being equal when d= o°. Thus, with the Cc. forward, F B must always 
be positive. 

Effective F when the Cc. is the Stronger. — If the Cc. lens has a shorter 
focal length than the Cx., and the two are in contact, there is an excess of 
negative power. If the Cx. be moved outwards it gains in effectivity, but 
the total effect is still negative until, when the separation is equal to the sum 
of their focal lengths, F B is infinite. Further separation will give the two 
lenses a positive effectivity, which is shorter as the separation is increased 
until when d=F of the Cx., F B =0. Still further increased separation results 
in a negative effect. 

Fig. 163. 

Thus, in order that a Cx. and stronger Cc. may neutralise each other, 
and parallel light emerge parallel from the second lens (Fig. 163) d—F x + F 2 , 
the principal focus of the Cx. being behind the Cc. as far as that of the latter 
is in front of it. 

Thus, if F x = + 6 and F 2 = - 4 the separation must be 6 - 4=2 in. Here 
by calculation 

(6-2)x4 16 
F =- — = — =<*> 

whether the one or other lens is to the front, in such a condition the lenses 
are commonly said to be separated by the algebraical sum of their focal 
lengths, so as to include the case of two Cx. lenses, already mentioned, from 
which parallel light emerges also parallel. 

Thus, the Cc. being the stronger, and with the combination either way 
round, there is 

Negative effect when d<^F 1 + F 2 . 


Afocal effect (i.e. neutralisation) when d=F 1 + F 2 . We have here the 
principle of the Galilean Telescope or Opera Glass. 

Positive effect when d>F 1 + F 2 , but less than the focal length of the Cx. 
With +.he latter in front we have here the principle of the Telephoto lens. 

With the Cx. forward and d>F x the effect is negative, but it is positive 
for any separation when the Cc. first receives the light. 

Dioptral Formulae for Effectivity. — The formula for finding the effective 
dioptral lens D B of two separated lenses D x and D 2 is 

D B =D 1+ D a + -^^^bemgincm. 

To find d for a given F B . — This can be obtained from the formula 


or it is better calculated from the original formula. Thus, let parallel light 
fall on a 5" Cx. in combination with a 2" Cc, and the effect required be that 
of a 20 Cx. ; then 

_(5-eZ)x(-2) -!0+2d 
+ 20 = 5-2-T" = 3-d 

60 - 20d= - 10 +2d. 22d=70 and fZ=3 T 2 T " 

If the effect required with the same lenses is that of 20 Cc, then 

- 2oJ 5 " (?)x( " 2) _ ~ l0 + 2 ^ 
5 - 2 - d 3-d 

- 60 + 20d= - 10 + 2d 18d=50 and d=2i>" 

The above examples give the distance between the two component lenses 
of an opera glass when the light emerging from the Cc. is required to have 
respectively a positive and a negative F B =20", or in other words, a converg- 
ence of 2 D in the first case, and a divergence of 2 D in the second. 

It should be noticed that for emergent parallel light d=F l + F 2 , in this 
case 5-2=3", and in order that F B be positive d is more than 3", and for 
F B to be negative d is less than 3". 

The distance d can be deduced from general principles. Thus, using the 
same lenses as in the foregoing example, suppose we need a resultant con- 
vergence of 4 D (to suit the vision of a hypermetrope of 4 D) then the effect 
of the Cx. in the plane of the Cc. must be + 21 D, so that the back focal 
power =+4 D. Then d is the difference between F of the Cx. and F of 


that lens which would, in the plane of the Cc, have the desired effect. In 
this case the two lenses being + 8D and — 20D. 

100 100 
d= — --—=12-5 -4-16=8-34 cm. or 5-40/24=3*" 

8 24 / 3 

For a resultant divergence of 4 D (to suit the vision of a myope of 4 D) 
the Cx. needs an effect of + 16 D in the plane of the Cc, so that 

d=^°° - — =12-5 - 6-25=6-25 cm. or 5 - 40/16=2£* 
8 16 

If a Cx. lens of F=10" and another Cx. of 2" be separated by 12" they 
constitute a telescope. For the emergent light to be parallel d~F t + F. 2 =12" ; 
for the light to be divergent d is less than F 1 + F 2 ; for convergent light d is 
more than F 1 + F . 

With these lenses for F B =+20", rZ=12#"> and for F B = -20, rf=ll T y. 

Effectivity when Light is Divergent. — When the incident light is divergent 
the conditions for neutralisation and certain effectivities with separated lenses 
differ from those obtaining with parallel light; the conjugate focus of the 
front lens of the combination must be found in order to determine its effective 
value in the plane of the second lens. For example, an object is 24 in. in 
front of an 8 in. Cx. lens behind which, at 2 in., a 5 in. Cx. is placed; where 
is the image ? Now, the first conjugate / 2 is at 

7 a 4-al=il and i2 1 - 2 + 5=5. sothat/2 - 3 * in - 

An object is 40 in. in front of a 7 in. Cx., where should a 5 in. Cc. be 
placed so that the light may be rendered parallel ? Now 

l// 2 =l/7 - 1/40=33/280 

the image f is thus 8jf in. behind the Cx., and the Cc. must be placed 
8J| - 5=3^| in. behind the Cx. 

An object is 40 in. in front of a 7 in. Cx. and a 5 in. Cc. For the image 
to be 20 in. behind the back lens/ 2 is 8|§ in. behind the Cx., which must 
have the effect of 1/5 + 1/20=1/4 in the plane of the Cc. Therefore d= 

Ql6 A .!lfi 

Let a +3 D lens be 10 cm. in front of a screen; where must a +6 D be 
placed in front- of the +3 D so that the image of an object 50 cm. from the 
front lens be on the screen ? 

The original divergence is 2 D; after refraction by the front lens there 
is a convergence of 6 - 2=4 D. The convergence needed in the plane of the 
second lens is 10 D, of which the second lens provides 3 D; therefore, 

100 100 
<Z=— - - —=25 - 14=11 cm. 
4 7 

It is important to differentiate clearly between effectivity and equivalence, 
dealt with in the next chapter. 


Equivalence. — Any two or more lenses, whether in contact or separated, 
can be replaced by a single equivalent lens having the same refracting power 
as -the component lenses. Or, to put it in another way, since the size of 
image is proportional to focal length, any number of lenses can always be 
replaced by that single thin lens giving the same magnification. 

If two thin lenses are placed in contact the resultant focal length is the 
same as that of a single lens situated in the same plane, whose power 1/F is 
that of the sum of the two components F 1 and F 2 . The combined power 
and F may be written 

F : 

1 1 

and F= 

F,F 2 

F 1 + F 2 

If the lenses are separated by a distance d, we have seen that the effective 
power and back surface focal distance are 

F b = f7^ + F 2 ' and * B ^F 1 + F 2 -(? 

It now remains to find an expression for the equivalent focal length of 
two thin separated lenses. 

Fig. 1G4. 

Equivalent Lens and Focal Length. — Let L y and L 2 (Fig. 164) be two 
thin Cx. lenses separated by a distance d, and let AB be a ray incident on Zj 
parallel to the principal axis MN. This is deviated by L v and, were it not 
intercepted by L 2 , would focus at N, but it is refracted still more at to 
cross the principal axis in the posterior focus F B0 . 

Now if the incident ray AB be produced, and the final refracted ray CF B2 

prolonged backwards, the two will meet in the point P 9 . Through P 2 drop 




the perpendicular P 2 E 2 . Then if a thin lens of focal length E 2 F b2 be intro- 
duced into the plane P 2 E 2 and the other lenses removed, this single lens would 
give precisely the same result as the combination L X L 2 . For this reason 
the plane P 2 E 2 is called the second equivalent plane and the point E 2 the 
second equivalent point. 

Similarly if parallel light be incident first on L 2 , it will pass through the 
first back focus F Bl and P 1 E 1 is located in the same way &sP 2 E 2 . The plane 
P 1 E 1 is called the first equivalent plane, and E x the first equivalent point, and it 
is here that the equivalent lens must be situated to replace the combination 
for light coming from the side of L 2 . 

Thus it will be seen thatP 1 orP 2 corresponds to the refracting plane of a 
single thin lens, since all refraction appears to take place on either P x orP 2 
depending upon the direction of the light. E l and E 2 likewise correspond 
to the optical centre, because any ray directed towards E x will, after refrac- 
tion, appear to emerge from E 2 in a direction parallel to its initial path. 
This is illustrated in the next diagram. 

Fig. 165. 

In Fig. 165, P x andP 2 are the equivalent planes, E x and E 2 the equivalent 
points, F x and F 2 the principal foci, R F x and Q F 2 the focal planes. Let 
an oblique parallel beam, of which M is the secondary axis, fall on L v The 
ray M E \ directed towards E x is bent towards the axis by L v but is again 
rendered parallel to its original direction by L 2 such that it appears to proceed 
from E 2 towards H. Another ray K G after refraction by L x and L 2 is directed 
towards H in the posterior focal plane, apparently proceeding from a corre- 
sponding point N onP 2 such that the distances of G and N from the axis arc 
equal. Similarly R T is refracted towards H, the point of emergence on 
P 2 being S, such that 8E Z =TE V Thus H is the image of the point from 
which the light originally diverged. Conversely rays diverging fiom H, or 
any other point in the focal plane, will emerge as a parallel beam. 

Since the intrinsic power of a combination is a fixed quantity the equivalent 
focal length is the same on each side, and is the distance E 2 F 2 or E^. The 
equivalent planes P 1 and P 2 are always situated symmetrically with respect 
to the focal planes, and with two ordinarily separated convex lenses P x and 
P 2 are invariably crossed such that E x lies nearer to P 2 than to F v and E 2 



nearei to I\ than to F 2 , that is to say, the 2nd equivalent plane lies nearer 
to the source of light. With combinations other than two Cx. lenses — as also 
with a single thick Cx. lens — however, the equivalent points and planes are 
uncrossed. That which is the first equivalent plane when the light is incident 
on the one lens becomes the second equivalent plane when the lenses are 

The space E X E 2 , over which the light apparently jumps, is called the 
optical interval or equivalent thickness. Were the two lenses brought together 
this interval would vanish, so that E x and E 2 merge to form the optical 
centre of the resultant thin combination, and the united planes P x and P 2 
becomes the refracting plane. 


Fig. 1G6. 

Expression for F E . — In Fig. 166 AB is a ray parallel to the axis and is 
refracted through F B , the back focus. Let the focal lengths of L x and L % be 
F, and F 2 respectively, d the separation, and F E the equivalent focal length. 
Then we have two pairs of similar triangles C F r N and P 2 F B E 2 , also C D N 
and BDM. 


E 2 F B 

P 2 E 2 



E 8 F B = 

M D x N F u 



E 2^B =F E*' 

F 2 (F x - d) 
F x x F 2 (F X - d) F X F 2 

MD=F 1 - NF = 2 

x ' B F x + F 2 


Fe (F 1 + F 2 -d)(F 1 -d) Fj + Fa-tf 

This formula is independent of the direction of the light. The 
equivalent focal power is l/F K =l/F l +l/F 2 -d/F 1 F 2 . 

The distance of the second equivalent point E 2 from L 2 is found by 
subtracting the back from the equivalent focal distance, i.e. F E - F B . Thus 

F 1 F 2 F 2 (F x - d) FJ 

E 2 Fi 

d F X + F 2 -(Z F ± + F 2 -d 

The corresponding distance of E 1 from L x is 

F,F 2 F x (F 2 - d) 



F y +F 2 -d F x + F 2 -d F t + F 2 -d 



The equivalent thickness or optical interval is found from the following 
equations, the first of which also shows whether the equivalent points are 
crossed or not : 

The distance E 1 is measured backwards from the first lens, and E 2 forwards 
from the second lens, that is, in each case towards the other lens. If, however, 
either is a negative quantity, it is measured in the opposite direction or 
away from the other lens. 

The positions of E t and E 2 are unchanged in the combination, no matter 
which lens faces the light; E l is that which theoretically is nearer the source, 
but actually it may not be so. E 2 is that from which the focal length is 
measured, and if the combination is reversed that which was E x then becomes 
E 2 , and vice versa. When the one lens faces the light F E is measured from 
a certain position, and it is measured from another position if the other lens 
faces the light. 

F 1? F 2 , E x and E 2 are the four cardinal points of a combination. 

The Result of Separation. — Separating two Cx. lenses results always in 
reduced power or longer F E — indeed if d is great, F E may become infinite, or 
even negative. With Cc. lenses the reverse occurs, the power being increased, 
or F„ shortened. With a Cx. and a Cc. in combination the result varies 
with the powers of the two components as tabulated later. 

In Chapter XIII. it was shown that separation of two Cx. lenses resulted 
in increased effect or shorter F B , while with two Cc. lenses there is a decreased 
effect or longer F B . 

It is necessary to distinguish between true power and effect. Suppose 
two thin Cx. lenses in contact in a given plane, and the one lens then moved 
outwards. The resultant refractive action is that of a single weaker lens 
placed a certain distance out from that plane, so that, although the com- 
bination is weakened, the distance of F behind the plane is shortened. 

With two Cc. lenses the resultant action, due to separation, is that of a 
single stronger lens placed in advance of the plane occupied by the two 
original lenses. 




Fig. 167. 

Equivalence of Two Cx. Lenses. — Let a 5 in. Cx. lens be 2 in. from a 10 in . 
Cx. lens. Then (Fig. 167) 




5x10 50 . 

ioT5^ri3 -3T * in - 

E 1= 5 x 2/13=l§ in. behind L 3 E 2 =10 x 2/13 = 1^ in. in front of L 2 
or 2 - lyk— Ts m - behind L x 

/10 20\ 4 . 

( = 2 -lis + is)=-r3 m - 

If the 10 in. lens faces the light, the two equivalent points change places, 
F E being the same. Since d—2 in., and E 1 is 10/13 in. behind L v while 
E 2 is ly 5 in. in front of L 2 , the distance t is negative, and the two equiva- 
lent planes are crossed by 4/13 in. 

Special Cases. — The following special cases occur with two separated Cx. 
lenses : 

(1) When d=F 1 - F 2 , then F s =Fy/2, and E 2 is midway between the two 
lenses. This is the case of the Huyghen eye-piece (q.v.). If F 1 =d in., F 2 = 
1 in. and d=2 in. 


F = 

E 3+1-2 

— M 

II in. 

E % is 1 in. in front of the back lens, midway between the two lenses; E 2 , 
being 3 in. behind the front lens, is 1 in. behind the back lens, and outside 
the lens system. Here d> F % but < F v and if the lens of shorter focus faces 
the light F lies in front of the back lens. 

(2) When d=F 1 + F 2 , then F E = oo, this being the case of the telescope 


(3) When d>F x but <i'\ + i , 2 , then ^ E is positive, and E x and E 2 may 
be one or both beyond the lenses and crossed (Fig. 168); d being > F v the 
light, after refraction by L v is divergent to L 2 as if a single lens were placed 
further than its focus from a given plane. 

Fig. 168. 

Let 2^=4 in., F 2 =i in., and rf=6 in. Then 

4x4 16 . 
F= -=-=8 in. 

e 4+4_6 2 

The lenses being equal E, or E,=4 x 6/2=12 in. 

Parallel light incident on L x comes to a focus at 4 in., whence it diverges 



to L 2 , and has its focus, after refraction, at 4 in. in front of L 2 , or 8 in. behind 
E 2 . t= - 18 inches in this case. 

Suppose F x =l in., F 2 =ld> in., and c?=9 in. Then 2^=8 in., E x is 
4|- in. from L v and E 2 is lOf in. from L 2 . The effect is as if an 8 in. lens 
were placed lOf in. in front of the plane of L 2 . Light, refracted by this 
system, is converged to 7 in., and, after the second refraction, diverges as 
if from a point 2| in. in front of L 2 . • 

- • A 

E. X. 


Fig. 169. 

(4) When d>F x + F 2 , then F B is negative, and E 1 and E 2 are also negative 
(Fig. 169). Thus, if two 4 in. lenses are 20 in. apart, we get 

4x4 16 

-= - 1£ m. 

F = - 
E 4-f 

20 -12 

The lenses being similar E x or E 2 =4 x 20/ — 12= — 6§ in. 
Here the equivalent points, being negative, are measured outwards 
instead of inwards, and F B lies behind L 2 , but 1\" in front of E 2 . 

(5) When d=F v then F E =F V and the system illustrates the Kellner 
eye-piece (q.v.) if the lenses are equal. If the lenses are 3" and 1" with 
d=3", we have ^=3", ^=9" and E 2 =3", that is, in the plane of L v 

(6) When d—F 2 , then F^=F 2 , and E x —d, the image being the same as if 
the front lens were not there, but its position is shifted. Thus, with a 
10" and a 1" lens separated by 1" we find F K =V, E 1 =\" and £ 2 = T V which 
is the distance that the image is shifted. This illustrates the case of a lens 
at the anterior focal point of the eye. 

(7) When F X =F 2 , then F B + F li =F 1 or F 2 . This is the case of the 
Ramsden eye-piece. Let F x and F 2 be each of 4 in. focal length, d being 
2| in. Then 


F — ■ 
■ 4 + 4- 


21 b\ 


E l0 rE 2 =4x2f/5£=2" 

F„ is therefore 3 -2=1". 

Equivalence of Two Cc. Lenses. — Example, F ± 
and d=2 in., then 

_ - 8 x ( - 10) 80 

8 in., F 2 = - 10 in.. 



= - 4 in. 

E x = - 8 x 2/ - 20=4 in. E 2 = - 10 x 2/ - 20=1 in. 

*=2-(l+ |in.)=i 



Special Cases.— If d=F t ~ F 2 then F E is half that of the stronger lens, and 
the equivalent point measured from the weaker lens is midway between the 

If F X =F. 2 , then F B + F X =F 1 or l\. 

Fig. 170. 

Equivalence of a Cx, and a Cc. Lens.- -Suppose Fy^-10 cm., F 2 ~ - 15 cm., 
and d=2 cm. Then (Fig. 170) 

10 x ( - 15) - 150 

F„= — — -= — — -21f cm. 

B 10-15-2 -7 

Ej=10 x 2/- 7= - 2^ in front of L t 

E 3 =-15x2/-7=4f cm. in front of L 2 or 4f-2=2f cm. in front of L, 


Fig. 171. 

If the negative lens is in front (Fig. 171), E 2 is 2f cm. behind the Cx., 
or -2r-2=;-4£ cm. behind the Cc. In the first case F E lies 17i cm. 
behind the back lens, and in the second case 24f cm. behind it. The com- 
bination resembles that of a positive meniscus in which the optical centre 
lies outside the Cx. surface. Whether a combination, such as this, will have 
a positive or negative focal length depends, not only on the respective powers 
of the components, but also, and essentially, on the value of d. The weakest 
Cx. can more than neutralise the strongest Cc. if the separation be great 

Special Cases. — When d--F 1 + F 2 . If the two lenses are separated by 
the sum of their focal lengths, the negative being of shorter focus, then 
F E — oo, and the lenses neutralise each other. This is the case of the opera- 
glass. Thus, with 9 in. Cx. and a 4 in. Cc. separated by 5 in. 

« 9-4-5 


If d <F x -l F 2 , the combination is negative; if d > F x + F 2 it is positive. 

When F 1 =F 2 . — If the two lenses have equal focal lengths, F B -F E --F 1 
or F 2 , and the formula for finding F E (which is positive^ becomes simplified, 
to F B =F 2 /rf. In this case E 5 is negative and both equivalent planes lie 
beyond the Cx. lens; E X =F 2 and E 2 — F x ; also l=d. 

To find d for a given F E . — To find the distance d which should separate 
two lenses so that they may have a given F E the original formula can be em- 
ployed, or the following — 


If d results in a negative quantity, it shows that the desired result is 
impossible. If both lenses are similar the formula may be written 

rf-2F-F 2 /F B ; 
and if F x = - F 2 the formula simplifies to rf~F 2 /F B . 

Thus, when F x is 10 in. and F 2 is - 5 in., for F E to be 12" 

d----\0 - 5 - 10 x ( - 5)/12=5 - ( - 4£)=9£ in. 
For F„ to be - 12" we find that 

£=10 - 5 - 10 x ( - 5)/ - 12-5 - 41-1 in. 

Change of F E for Variation in d. — As d increases with two Cx. lenses, 
F E varies directly, and t varies inversely or becomes negative. 

As d increases with two Cc. lenses, F E varies inversely, and t varies directly. 

As d increases with one Cx. and the other Cc, the Cx. being the stronger, 
F E varies inversely and t varies directly. 

As d inci eases with one Cx. and the other Co., the Cc. being the stronger, 
and F B being negative, F E varies directly, and t varies inversely or becomes 

As d increases with one Cx. and the other Cc, the Cc being the stronger, 
and F E being positive, F E varies inversely, and t varies inversely. 

Conjugate Foci. — The ordinary formula? for conjugate foci hold good, 
but the distance oij\ is measured from E r and that of f 2 from E 2 , as with 
thick lenses (q.v.). 

The planes of unit magnification — i.e. the symmetrical planes — are at 
2 F E from E x and E 2 respectively. 

The position of the image can be worked out on general principles, but 
unless the equivalent points are known the magnification cannot be calcu- 
lated. Thus, if an is 10" in front of a 5" Cx. lens, behind which there is 
another Cx. of 10" F, at 2" we could calculate 

1 i 1 1 11 11 

7 2 "^5"Icr"io y; = io^ + io = 4| 

The distance of I behind the back lens is 4|"; or we can find F E — §£, 
Ei=4$ and E a =ff ,. 


Then/, is 10|r from K, and j~ - ~= ^ 

/ 2 =5Hr" from E 2 or 5[ ji - f |==4|* from the back lens. 

Combination of More than Two Lenses.- When more than two lenses 
are separated by intervals, the method of finding F E of the whole system 
is to obtain that of the first pair of lenses, and then combine this combina- 
tion with the third lens, or another pair of lenses, and so on. It must be 
remembered that the distance d between two combinations is that between 
the two theoretically most adjacent equivalent points, that is, between E 2 of the 
first and E, of the second combination; also that the positions of the equiva- 
lent points E t and E 2 of the whole combination are reckoned respectively 
from Ej of the first, and E 2 of the second combination. In fact the calcula- 
tions are similar to those required for two thick lenses (q.v.). 

Dioptral Formulae. — "With dioptral powers, the equivalent power and 
points of two separated lenses are found from the following formula?, where 
D 1 and D 2 are the powers of the two lenses, d is the interval between them 
expressed in cm., D B is the equivalent dioptral lens, Ej and E 2 are respec- 
tively the first and second equivalent points, and I is the distance between 
E x and E 2 : 

D F =D X + D 2 - D^d/lOO 

DJV BfiJ D 2 d 

■ - 1 ~D 1 (D 1 + D a -D 1 D a d/100) = D 1 D, = D»" 

E = D iP 2 <* _D 3 D 2 rf_LV 

2 D 2 (D 1 +D t -i> 1 p t d/lQO) D 2 D E D E 

If d is expressed in terms of a metre, we can write: 

D E =D X +D 2 -L\D 2 d 

If D x is positive and equal in power to D 2 , which is negative, then 

D E =D 2 i/100 

The distance between two dioptral lenses so that they may have a certain 
equivalent dioptral power is found from 

100(D 1+ D 2 -D E ) 
L\D 2 

which, when D 1 and D 2 are equal, simplifies to 


100 (2D- D,) 
D 2 

If the one lens is positive and the other negative and of equal powers, 
the formula becomes 

d^lOQVJD 2 



Hitherto we have considered lenses to be thin, that is, to have no appre- 
ciable thickness in relation to their focal length, so that the refraction caused 
by the two surfaces may be presumed to take place at a single refracting 
plane passing through the optical centre. Further, this plane may be taken 
as coinciding with the surfaces, and therefore all measurements may be taken 
from the lens itself, and secondary axes passing through the optical centre 
assumed to undergo no lateral deviation. With a thick lens, these simpli- 
fications are not permissible. 





A B 



Fig. 172. 

Fig. 173. 

Let Fig. 172 represent a thick bi-Cx. lens of which X and Y are the centres 
of curvature. From X and Y let any two parallel radii, X B and Y A be 
drawn meeting their respective surfaces in B and A; then tangent planes 
drawn through A and B are parallel, so that at these points the lens acts as 
a plate, and there is one ray A' A, incident at A, which, after refraction, emerges 
as .85' parallel to its original course. A' AOBB' is a secondary axial ray and the 
point where it, and all other secondary axial rays, cut the principal axis 
is the optical centre of the lens. The position of on X Y depends upon the 
ratio of the two radii of curvature. 

The point E v towards which A' A is directed, is the first equivalent point, 
while E 2 , from which it apparently emerges, is the second equivalent point. 
E y and E 2 have the same properties as in thin lens combinations, i.e. they 
are the points from which the principal and secondary foci are measured, 





and through which pass the planes where all refraction is presumed to take 
place. In a single thick Cx. lens, however, E x and E 2 are not crossed as they 
are in a thin Cx. lens combination. Fig. 173 shows the equivalent planes 
and optical centre of a bi-concave lens. 

Fig. 174. 

Fig. 175. 

In periscopic Cx. or Cc. lenses (Figs. 174 and 175) both E 1 and E 2 generally 
lie outside the lens on the Cx. side of the PCx., and on the Cc. side of the 
PCc, but in some cases the one point may be outside, and the other still 
within the lens; moreover the optical centre lies beyond both equivalent 
points. A ray directed towards E x appears, after refraction, to proceed 
from E 2 , its course A B within the lens being on a line connecting the optical 
centre 0, the point of incidence A of the ray at the first surface, and the 

Fig. 176. 

Fig. 177. 

point of emergence B at the second surface. The position of is therefore 
virtual and it is determined by producing B A to cut the principal axis. 

In piano Cx. and Cc. lenses (Figs. 176 and 177) the only point on the 
curved surface parallel to any point on the plane surface is at the vertex, 
through which passes the principal axis. Therefore E v the first equivalent 
point, and 0, the optical centre, coincide at the curved surface. All the 
secondary axes proceeding from the various points of a body are directed 
towards E v and after refraction appear to diverge from E 2 , so that they cut 
the principal axis at 0. 



The terms nodal or principal points are sometimes applied to the equivalent 
points ; but it is better to reserve the latter term for points that possess 
the functions of both the former, as they do in lenses where the first and last 
media — usually air — are similar. Nodal and principal points are discussed 
in the chapter on Compound Refracting Systems. 

The Effect of Thickness is shown in the foregoing diagrams, and it may be 
said that a thick lens differs from a thin one in that it has a plate-like power 
of laterally displacing incident light. A thin Cx. lens can be transformed 
into a thick lens by splitting it in the refracting plane and cementing the two 
halves to the opposite sides of a parallel plate. The consequence is similar 
to that which results from the separation of two thin Cx. lenses in that a 
thick Cx. has a weaker equivalent power than a thin one of similar curvature 
and//, while a thick Cc. has a stronger equivalent power than a thin one. 

Fig. 178. 

Fig. 179. 

The Course of Light through Thick Lenses.— Fig. 178 represents a thick 
Cx. lens in front of which is the object A B. Any ray AP parallel to the axis, 
takes the course Q A' after refraction, and passes through F 2 . The secondary 
axial ray A E v directed to E v is refracted so as to proceed from E 2 parallel 
to its original course, and a third ray A R, passing through F v is refracted 
as S A' parallel to the axis. All three rays meet in the image-point A', so 
that B' A' is the complete real image of A B. Any other ray A T directed 
towards the first equivalent plane at T emerges from the second at X, such 
that E x T=E 2 X. 

The construction in the case of thick Cc. is shown in Fig. 179. It needs 
no explanation. 

Direct Formulae for a Single Thick Lens in Air.— To find the back or 
effective focal length, the equivalent focal length, and the positions of the 
equivalent points in terms of the radii, thickness and yt of the lens, let 

F B be the back focal length. 

F E the equivalent focal length. 

Ej and E 2 the first and second equivalent points. 

T the distance between E x and E 2 (the optical interval). 

r x and r 2 the radii of curvature of respectively the first and second surfaces. 

A and B the first and second surfaces at the principal axis. 

/u the index of refraction of the glass. 

t the thickness of the lens on the axis. 



Fig. 180 represents a thick bi-convex lens; let R Q be a ray incident at 
Q and parallel to the principal axis A B; this is deviated towards the axis 
by the first surface, and would, if not intercepted by the second surface, 
cross A B in D, but is brought to a nearer point F B by the further refracting 
power of the second surface. Then, from definition, D is the posterior focus 
of the first surface, F B the principal focal point of the lens as a whole, and B F B 

Fig. 180. 

the back focal distance. Let F B C be produced backward to meet R Q pro- 
longed in P. Now a plane perpendicular to the axis, dropped through P, 
will locate the second equivalent plane, and where it cuts the axis, the second 
equivalent point E 2 . All the refraction of incident light from the direction 
R Q (parallel or otherwise) appears to take place on P E 2 . The distance 
E 2 F B is, therefore, the equivalent focal length, since it is the focal length of 
the single thin lens which, if placed in the plane of E 2 , would have the same 
power as the original thick lens as a whole. 

The distance of F H , the principal focal point of the lens, measured from the 
second surfaced, is determined by the sum of the anterior focal powers 1/F A 
and l/F' A of the two surfaces respectively, that of the first being modified 
by t/fj,, the index and the thickness of the lens, which the light has to traverse, 
before it meets the second surface. 

That is, 

+ . 

F B F A -«//i'F: 
Substituting rj([x - 1) for F A , and r 2 /(ju - 1) for F A we get 



fi- 1 

so that 

F b Ma*" 1 )-'/^ VV- 1 ) *i-*(,u-l)/a) r 2 

F =BF = M>i -*(/*-! )/") 

B {fi-\)(r^r t -t(fJL-l)/fi) 

Similarly for the other surface the back surface power is 


+ . 

VTK-*/? *a 


and the back surface focal length is 

B ip-Vfa + rt-tbi-l)//*) 

In Fig. 180, since the ray R Q is presumed to lie close to the axis, the 
arcs Q A and C B may be taken as straight lines giving two pairs of similar 
triangles G F b B and P F B E 2 , CDBandQ DA. Then it follows that 

E 2 F B PE 2 QA AD 

so that E 2 F B =BF B x 



But E 2 F n is the equivalent focal distance, B F H is the back focal distance, 
A D the posterior focus of the first surface, and B D is this quantity less the 
thickness t. On substituting these values, therefore, in the above equation 
we get as the expression for the equivalent focal length, 

F=FF r a ( r i-*(^-l)/fc) f* r i . ( V r i 

E ^ 2 B (f J i-l)(r 1 + r^-t{^-l)/fjL) p-l'\fjt-l 

V T 

which becomes F E =E 2 F B = 

(ju-1) {r 1 + r ji -t{fji-l)/fi) 

F F is the same whichever surface faces the light, but it is measured from 
the posterior equivalent point. 

The distance of E 2 from the pole B of the second surface, is found by sub- 
tracting the back from the equivalent focal length, which in terms similar 
to those already used is 

2 ~ E B ~/j / {r l + r 2 -t{fj,-l)/fx) 

and the corresponding distance of E x from A is 

E!=F E -F B = 

The distances of the first and second equivalent points are measured 
inwards — that is, respectively from the first towards the second surface, and 
from the second towards the first. If, however, by calculation the value is 
negative, as occurs in some cases, the measurement is outwards from the cor- 
responding surface. 

If we calculate, the quantity Q which enters into the formulae, 

that is Q=»i + r 2 -*(/*- l)//te 

we have F,= , rif ' A=Q % 2 =% 



The equivalent thickness, or optical interval — i.e. the distance between 
the equivalent points, is 

T=f-(E X + E 2 ) 

It should be noted that the formula for F E is the same as for F of a thin 
lens, except that the quantity t(fi - 1)/jli enters into it. 
An approximate formula (accurate when i a=l-5) is 


r x r 2 

(^-l)(r 1 + r 2 -*/3) 

Example of a Bi-Cx. Lens. — If r x and r 2 =10 cm. and 6 cm. respectively, 
^=1-5, f=3 cm., then (Fig. 180) 





•5(10 + 6 -3 x -5/1-5) -5 x (16-1) 7-5 
10x3 30 _ 6x3 


=— =8 cm. 


a.33cm. E 2 = 15x(161) ^ 

1-5 x (16-1) 22-5 

T=3- (1-333 + -8)=-86 cm 

•8 cm. 

F B is anteriorly 8-1-333=6-66 from A, and posteriorly 8 --8=7-2 cm. 
from B. The optical centre is located at 

3 x 6/(10 + 6) = 1-125 cm. from B, and 1-875 cm. from A. 


A thin lens of same radii and a has F= 

60 »B 

- =7-5 cm. 

•5 x (10 + 6) 8 

Thus in a bi-Cx. thick lens the true or equivalent focal length is longer than 
that of the corresponding thin lens, but its back focal length is shorter. In the 
case of the thick lens F=8 cm. from E 2 , but 7-2 cm. from B, while if the lens 
were thin so that Z=0, F is 7-5 cm. from B. If two Cx. lenses be made of 
the same glass and similar curvatures, but the one thicker than the other, 
the thicker lens is actually the weaker, although its effectivity is greater. 

F B 2 






Fig. 181. 

Fig. 182. 

Fig. 183. 

Example of a Bi-Cc. Lens. — In Fig. 181 let r x and r 2 = - 10 cm. and 
6 cm. respectively, /x=l-5 and t=Z cm. 


> -10x(-6) 60 

E -5 x(- 10-6-3 x -5/1-5) -5x(-17) ° m- 

-10x3 ," _ -6x3 

E ' = l-5x(-17r 1,18 Cm< Ea= I-5x(-17) = - 7 Cm - 


Although the true focal length is the same on either side, if the surface 
B faces the light, F lies 7-06 + 1 -18=8-24 cm. from A, while if A faces the light 
F is 7-06+ -7=7-76 cm. from B. ' If the lens were thin F=7-5 cm., so that 
increased thickness causes a Cc. to have a greater equivalent power or a shorter 
equivalent F, but a smaller effeetivity or longer back surface F. 

Example with a Plano-Cx. Lens. — Let r x (Fig. 182) that of the curved 
surface=6 cm.; r 2 of the plano= oo ; ^=1-5; and Z=3 cm. Then since r 2 = 
oo, and this quantity occurs in the upper and lower part of the formula, 
we can omit it from our calculations as well as the other quantities in the 
bracket containing this value. The formula therefore simplifies to that used 
for a thin lens, viz. F E =r 1 /( / a - 1) 

E 1= 6 x 3/1-5 oo =0 E 2 =3/l-5=2 cm. 

F E =6/-5=12 cm. T=3 - 2=1 cm. 

E x is at the curved surface, and E 2 is 2 cm. in front of the plane surface. In 
the above example, when the Cx. surface is exposed to the light, F lies 12-2 
=10 cm. behind the plane, and 13 cm. behind the curved surface. When 
the plane surface is so exposed, F lies 12 cm. behind the curved and 15 cm. 
behind the plane surface. 

Example with a Plano-Cc. Lens. — If r x (Fig. 183) that of the plane surface 
= oo, as before stated, it may be neglected. Let r 2 , that of the Cc.=6 cm., 
^=1-5, and £=3 cm. 

E^ 3/1-5=2 cm. E 2 =6 x 3/1-5 oo =0. 

F E =-6/-5=-12cm. T=3-2=lcm. 

E x is 2 cm. from the plane surface, and E 2 is at the Cc. surface. If the curved 
surface faces the light F is 12+2=14 cm. in front of the plane and 11 cm. 
from the curved surface. When the light is incident on the plane surface, 
F lies 12 cm. from the curved and 9 cm. from the plane surface. 

Example of a Positive Meniscus.— In a periscopic Cx. lens (Fig. 184) let 
r x and r 2 of the Cx. and Cc. surfaces respectively be + 6 cm. and - 10 cm., 
^=1-5 and f=3 cm. 

6x(-10) -60 

F = — ; = =24 cm. 

B -5 (6 -10 -3 x -5/1-5) -5+ (-5) 

E x =6 x 3/1-5 x - 5= - 2-4 cm., E 2 = - 10 x 3/1 -5* - 5=4 cm. 

T=3-(-2-4+4) = l-4cm. 

J 68 


E x being negative must be reckoned outwards from the Cx. surface, so that 
both equivalent points are reckoned the same way, the second being inwards 
from the Cc. E x is 24 cm. and E 2 is 4- 3=1 cm. outside the Cx. surface. 


Fig. 184. 

Fia. 185. 

Fid. 186. 

Fig. 187. 

In some cases, with a periscopic Cx. lens, as when the Cc. surface has very 
little curvature, the one equivalent point lies within the Cx. surface, as in 
Fig. 185. The more nearly equal the two curvatures, the more are E x and 
E 2 displaced beyond the Cx. surface. The distance of F B varies considerably 
as the one or the other surface is exposed to the light. 

Example of a Negative Meniscus. — In a periscopic Cc, as in Fig. 186, let 
r, and r 2 of the Cx. and Cc. surfaces respectively = + 10 cm., and -6 cm., 
^u=l-5 and f=3 cm. 


10 x ( - 6) 


40 cm. 

•5 ( + 10-6- 3 x -5/1-5) -5x(3)" 

E 1= =10 x 3/1-5 x 3=6-66 cm., E 2 = - 6 x 3/1-5 x 3= - 4 cm. 


The distance of both equivalent points are reckoned the same way, E x in- 
wards from the Cx. surface, and E 2 , being negative, outwards from the Cc. 
surface. The first is 6-66-3=3-66 cm. outside the Cc. surface, and the 
second is 4 cm. outside it. 

If the Cc. surface has but little curvature, the one equivalent plane of a 
Cc. meniscus may lie within the Cc. surface (Fig. 187). Also, the difference 
in the distance of F J; is marked as E x or E 2 is taken as the first equivalent 

Special Cases — Afocal Lenses. — In a meniscus when r of the Cx. is longer 
than that of the Cc. surface 

F E = oo if r x + r 2 =t (ju-1)//j,, or t=/u (r x + r 2 )/(/u,- 1) 

F E is positive when r x + r 2 is less than t(/u - l)//j, and negative when r x + r 2 is 
greater than t(/u - l)/u. That is to say, F is positive or negative according as 
t is sufficiently great or small respectively; and that, when t is of certain value, 
the power of the Cx. surface neutralises that of the Cc. This condition 
obtains when Q=0. 

Thus, in order that F= oo when r x = - 1, r 2 = + 3, and/^=l-5. 




This is the principle of the Steinheil cone (Fig. 188), which is practically 
a fixed focus opera-glass. 

If r x = + 10 and 2=3 vrhen/bi=l'5, then r 2 must be - 9 in order that F E = oo. 

Fig.' 188. 

Fig. 189. 

Fig. 190. 

Fig. 191. 

Fig. 189 illustrates the form of the worked globular or coquille of the 
optical trade, where an afocal effect is required; the radius of the Cc. surface 
is shorter than that of the Cx. by an amount equal to approximately a third 
the thickness of the glass. A thick afocal lens can be obtained, also, when 
both radii are positive, if the above-mentioned condition be fulfilled. Thus 
if ^=1-5, r x =2 cm. and r 2 =5 cm., the lens is afocal if t=Z (r 1 +r 2 ), in this 
case 21 cm., for then Q=0. When F= oo, the equivalent points and optical 
centre are also at oo. 

Concentric Lenses. — If r 1 + r i =t (r 2 being negative)— i.e. if r 1 -t=r. 



that the two centres of curvature coincide, the Cc. surface has the shorter 
radius and F is negative. Thus (Fig. 190) let r x =10 cm., r 2 = - 6 cm., 
£=4 cm., and ^=1-5. Then 

10 x ( - 6) - 60 


= - 45 cm. 

•5 (10 - 6 - 4 x -5/1-5) -5(2-666) 
E 1= r 1= 10; E 2 =r 2 = - 6; T=4 - (10 - 6)=0. 

The equivalent points coincide at the common centre of curvature. 
If the glass be thin (Fig. 191), and the centres coincide, there is a slight 
concave power, as is found in the ordinary unworJced globular or coquille. 


Fig. 192. 

Fig. 193. 

Fig. 194. 

Equi-Curved Lenses.— If r,= -r 2 (Fig. 192), F E is positive. Thus, let 
r x = + 10 cm., r 2 = - 10 cm., t—d cm., and / tt=I-5. Then 

10x(-10) -100 nnn 

F = — ; — = =200 cm. 

B -5 (10- 10-3 x -5/1-5) --5 

E x or E 2 =r/(^ - 1), in this case 10/-5=20 cm. 


Other Conditions. — If the radius of the Cx., is shorter than that of the Cc, 
F E is positive. If t is greater than F of the first surface, the light is brought 
to a focus within the dense medium, and, after crossing, diverges to the second 
surface by which it is converged, or diverged according as it is positive or 
negative respectively. 

The Sphere. — In a sphere (Fig. 193), r x =r % and f=the diameter=2r. 
Let ^=1-5, and r=6 cm., so that 2=12 cm. 

6x6 36 

E -5 (6 + 6- 12 x -5/1-5) -5x8 

E 1 or E 2 =6x 12/1-5x8=6 cm. T=12 - (6 + 6)=0. 

Therefore, the equivalent planes of a sphere coincide and pass through the 
centre of curvature C, as in Fig. 193. The formula, in the case of a sphere, 
simplifies to 

F =— ^— - and F B =F E -r 
E 2(^-1) B E 

When^ of a sphere is 1-5, F E =l-5 r, and F B =-5 r. 

Calculations with a sphere are similar to those of any other thick lens, 
when the object is situated outside the sphere. If, however, the object is 
within the sphere, they are similar to those connected with a single surface. 

The Hemisphere.— With the hemisphere (Fig. 194) the Cx. surface to 
the front, F E =r/(^-l), B l =r 1 «/»=0, E 2 =t//Ji; from the Cx. surface 
F B =F E =r/( / a - 1) ; from the plane surface ¥ H =r//n{/j, - 1). 

When/t=l-5, F E =2r ; F B =2r from the Cx., and 1 Jr from the plane surface. 

Other Calculations. — To find /x or one of the radii, when the other data 
are given, involves substituting values for symbols in the formula and 

Thus what radius must be given to a DCx. lens so that F E =5 cm. when 
fi =1-5 and t=-75 cm.? Substituting the known values we have 


r 2 r 2 

r 2 

•5(2r--5x-75/l-5) — -5(2r--25) r 


r 2 _ 5 r== _ . 62 5. 

r 2 - 5r + 6-25= - -625 + 6-25 

r- 2-5= ±2-35 

r=4-85or -15. 

so that 

•15 is an impossible answer, therefore the rermired radius is 4-85 cm. 


Calculations of a Thick Lens in Terms of the Foci of its Surfaces. 

The value of a thick lens in air can also be calculated from the foci of the 
two surfaces. 

Let / and f 2 represent respectively the anterior and posterior focal dis- 
tances of the first surface, and// and // represent respectively the anterior 
and posterior focal distances of the second surface. Let t be the thickness of 
the lens; then 

f _ r i f A 6 h f t I 1 T 2 r t _ r 2 

jU-1 fJb-i /LI -I /U-l 

In Fig. 180 D is the virtual object for the second surface B of radius r 2 , 
and the distance B F B , which is the second back focus F B , is the final image 
distance with respect to D the virtual object. 

Let B D—u and B F B =v. Now the expression connecting the conjugate 
foci of the second surface B is 

1 /LI [I- 1 

v u r 2 

But (fjL-l)/r 2 =l/f' 2 , and u=A D-t=f 2 -t, the latter expression being 
a negative distance since the object is virtual. 


1 1 ju Hfi+ft-t 

whence - = — + -£ — = ' , „ , 

v A h-t fz(fz-t) 
But Hfn=/»J(p-l)*=fi 

Therefore ^F ^ 2 '^ 2 " ° - 

The corresponding back focus from A, by similar reasoning, Is 

F= /i(/i / -0 
A A'+A-t 

Equivalent Focus. — In Fig. 180 P is the second equivalent plane and E 2 
the second equivalent point. As before we may consider C B as being 
sensibly straight. 

rpi nn 

E 2 F B PE 2 QA AD 



„ ,, AD x BF R 
E F — 

*•*** BD 


E 2 F B = 


X E' 

AD=/ 2 , BF B =F B) 

and BD=f 2 -t 


Therefore F E =/ 2 x ^ (/a ~ ° 


It is important to notice that AA'—AA' ^o that F E may be taken as 



when the light is incident first on the surface B. 

Equivalent Points. — The distances of E x and E 2 from the surfaces A and 
B are found by deducting frorn the equivalent focal length the respective 
back foci. Thus 

F=E-E A/1' Aifi-fi ^ ^ 

1 E B A'+A-t A'+A-t A'+A-t 


•pi -ni _ ™ _ ^2/2 A V2 ~h A * 

2 ~ B B A'+A-t A'+A-t A'+A-t 

Example. — Let r 1 —]0 cm., and r 2 =6 cm., ^=1-5, t=3 cm.; then 
, 10 nn ,10x1-5 _ 6x1-5 ,6 

When light is incident first on the surface A 

fj-,' _ 30x12 

E= J7^r«~i8T30 r~ 3 = 8 om - 

and when incident on B 

/,/' 20 x 18 

the equivalent focus, of course, being the same in either case. 

The equivalent points E x and E 2 are distant from A and B respectively 

f,t 20x3 

f't 12x3 

& ——— — =— - =-8 cm. 

fi+fi-t 45 

Thus the back foci from A and B are respectively 8-1-33=6-66 cm., 
and 8 --8=7-2 cm. 

Two Thick Lenses in Combination. — Let A be the first and B the second 
lens of a combination of two thick convex lenses separated by an interval. 
Let r y and r 2 be the radii of curvature of A, and r x ' and r 2 ' those of B. 


Let t± and t 2 be, respectively, the actual thicknesses of A and B. 

Let E x and E 2 be, respectively, the first and second equivalent points 
of A. 

Let E t ' and E% be, respectively, the first and second equivalent points 
of B. 

Let T t and T 2 be, respectively, the equivalent thicknesses of A and B. 

Let F x and F 2 be, respectively, the focal lengths of A and B. 

Let d be their distance apart, this being the distance between their most 
adjacent equivalent points, i.e. the distance between E 2 and E\. 

Let E and E' be, respectively, the first and second equivalent points of 
the combination. 

Let F be the equivalent focal distance of the combination. 

Let T be the equivalent thickness of the combination. 

The equivalent focal distance F of two combined lenses is obtained from 
the formula 

F X F 2 F X F 2 


X + F 2 -d N 

which is the same as for two thin lenses in combination. This illustrates 
the great utility of the equivalent planes in simplifying all thick lens calcula- 
tions, since, provided we measure from the equivalent planes, a combination 
can in every way be treated as a simple system. 

Similarly the distance of E, the first equivalent point of the combination, 
measured from E v the first equivalent point of A, is 

F X (Z _F x d 

The distance of E', the second equivalent point of the combination, 
measured from E 2 , the second equivalent point of B, is 


FJ ¥ 2 d 

F 1 + ¥ 2 -d N 

The distance T=E E', between the equivalent points of the combination, 
is determined by the following 

T=i + T 1 + T 2 -(E + E / ) or T=T X + T 2 - cZ 2 /N. 

As an example let r x =10 cm., r 2 =8 cm., and f x =2 cm. 
r\—9 cm., r' 2 =7 cm., and t 2 =2 cm. 
^=1-5 and cZ=2-5 cm. 

Then, when calculated, we obtain 

F x =9-23 cm., E^-769 cm., E 2 =-615 cm., T x =-616 cm. 
F 2 =8-26 cm., E' 1 =-783 cm., E , 2 =-609 cm., T 2 =-608 cm. 


and for the combination 

9-23 x 8-26 76-2398 


9-23 + 8-26 -2-5 





)-23 + 8-26 -2-5 15 
8-26x2-5 20-65 

=508 cm. 
=1-538 cm. 
=1-377 cm. 


9-23 + 8-26-2-5 15 

T=2-5 + -616 + -608 - (1-538 + 1-377) = -81 cm. 
T=-616 + -608 - 2-5 2 /15-l-224 - 6-25/15=-81 cm. 

The combination is of 5-08 cm. focal length and its equivalent planes are 
81 cm. apart. 

Fig. 195. 

Example with a Convex and a Concave Lens. — Let F 1 = + 12 in.; 

F 2 =-10 in.; d=b in.; T x =-5 in.; T 2 =-2 in.; then combined we obtain 

(Fig. 195) 

„ +12x(-10) -120 

F= -= =+40 in. 

+ 12-10-5 -3 

E=12 x 5/ - 3== - 20 in. E'== - 10 x 5/ - 3=16-66 in. 

T=5 + -5 + -2 - ( - 20 + 16-66)=9-03 in. 

or T=-5 + -2 - 5 2 / - 3=-7 - 25/ - 3=-7 - ( - 8-33) =9-03 in. 

Coincidence of E and E'. — In order that E and E' should coincide, d can 
be found, for two thick lenses, by the following formula. 


V(T X + T 2 ) 2 + 4 (F x + F 2 ) (T x + T 2 ) - (T x + T 2 ) 

Taking as an example a combination where F x =9 in., F 2 =8 in., T x = 
•2 in., and T 2 =-3 in. 

V(-2 + -3) 2 + 4 x (9 + 8) x (-2 + -3) - (-2 + -3) 


V-25 + 34--5 5-8524 --5 
d= =- - = 7: =2-6762 in. 

When the lenses are 2-6762 in. apart T=0. 

To find F E of More than Two Lenses. — When more than two lenses are 
in combination the equivalent cardinal points of two of them are determined, 
and then this combination is again combined with the third lens, or with 
another combination as the case might be. Thus, if there are four lenses, 
A B C D, the equivalent of A and B, also of C and D, are found separately, 
and these two equivalent combinations again merged into a single one, or 
the focal length of such a combination can be found directly by the Gauss 
equation given later. 

Conjugate Foci. — Calculations of conjugate foci with thick lenses are 
the same as with thin lenses provided all measurements are taken from the 
adjacent equivalent planes. 

Let be 20 cm. from the surface A of the lens of F E =8 cm., E 1 =l-33 cm., 
and E 2 =-8 cm. To find the distance of the conjugate image from B, the dis- 
tance /i is 20 cm. from A and therefore 20 + 1-33=21-33 cm. from E v and since 
F is 8 cm. we have l// 2 =l/8 - 1/21 -33, whence/ 2 =12-8 cm. Now/ 2 is mea- 
sured from E 2 , which is -8 cm. from B. Therefore the distance of the image 
from the second surface of the lens is 12-8 - -8=12 cm. The calculation for 
the corresponding thin lens would be l// 2 =l/8- 1/20, whence/ 2 =13-33 cm., 
and since both surfaces are considered coincident with the oj)tical centre, the 
distance of the image, in this case, from the lens is 1-33 cm. more than when 
there is a thickness of 3 cm. Similar calculations can be made for any type 
of thick lens or lens combination. 

Fig. 196. 

Fig. 197. 

Planes of Unit Magnification. — The symmetrical points S x and S 2 (Fig. 196) 
lie on the principal axis at a distance equal to 2F measured from E x anteriorly, 
and from E % posteriorly; they mark the symmetrical planes. An object-point 
A in the one symmetrical plane has its image A' in the other symmetrical 


plane and at an equal distance from the principal axis. Thus, when an object 
A B is situated at the one symmetrical plane, its image B'A' is situated at the 
other, and the two are of equal size; these are the planes of unit magnifica- 
tion for real images. The symmetrical planes are sometimes termed negative 
equivalent planes. 

The planes of unit virtual magnification for thick lenses and lens systems 
lie in the equivalent planes themselves. In other words the equivalent planes 
are virtual images of each other. 

Construction. — The graphical construction of the image has been shown 
at the commencement of this chapter (Figs. 178 and 179). To trace the course 
of a ray through a thick lens, suppose the case of a sphere (Fig. 197). Let 
A B be a ray incident at B ; from C draw the normal C C to B, and the tangent 
P Q to B. ThenP Q may be regarded as the refracting surface, which is divided 
off as shown for an ordinary plane surface. B D is the course of the ray after 
the first refraction, and at D the process is repeated, the emergent ray being 
D F. If the thick lens is other than a sphere, C 1 and C 2 , the two centres 
of curvature will, of course, be at their proper distances from their correspond- 
ing surfaces. 

To trace the course of any ray or to determine the image of any point the 
symmetrical planes S 1 and S 2 and the equivalent planes E x and E 2 can be 
made use of (Fig. 198). 

Let A be such an object-point on the principal axis. Let a ray from A 
strike the first principal plane at 0, and cutting S 1 at B. It will then appear 
to proceed after refraction in the direction C B' , such that E x C=E. 2 C on the 
same side of the axis, and x' B'=xB on opposite sides of the axis. The image 
A' is located where C B' crosses the principal axis. If the object-point, such 
as D, lies nearer the lens than S v the corresponding ray D C must be pro- 
longed backwards to find the distance x y corresponding to B x in the first 
case. After refraction the ray cuts S 2 above the axis. 

Dioptral Formulae — Single Thick Lens from Radii. — Let r x be the radius 
of the first, and r 2 that of the second surface, let D E be the equivalent dioptric 
power, and E x and E 2 the equivalent points. Then 

_ 100 (/u - 1) K + r 2 - 1 (fj, - l^WOOQ {ii - 1) 

E 1= =^ E 2 =^ T^-IEjfEa) 

If the distances are expressed in terms of a metre 

(ju - 1) (rj + r 2 - 1 (jti - l)/fj) Q(ju-l) 


r l r 2 T \ r -2 



Single Thick Lens from Powers. — Let d 1 be the power of the first surface 
found from d=100 (/u - l)/r; d 2 is the power of the second surface; the thick- 
ness t being in cm. 

D » =f ^-io(v 

E 1= 




D Ej u - D E /u 

If t is expressed in terms of a metre 

T> E =d 1 + d 2 -d l d 2 t/jU. 

Combination of Two Thick Lenses.— Let D t and D 2 be the powers of the 
two lenses, T x and T 2 their respective optical thicknesses, and d the distance 
in cm. between the adjacent equivalent planes of the two lenses. 

D=D 1 + D 2 -D 1 D 2 tf/100 

If d is expressed in terms of a metre 

~D=D 1 + ~D 2 -D l D 2 d 

The first equivalent plane E is distant from E x of the first lens 

DjD^ _D 1 D 2 rf_D 2 rZ 

~D 1 (D 1 +D a - ViPzd/100) ~~~ D X D = " ~D~ 

The second equivalent plane E' is distant from E 2 of the second lens 

T>jy 2 d 'D l D 2 d D ]f Z 


D 2 {D 1 + D 2 - D 1 D 2 r//100) D 2 D 
T=(Z + T 1 + T 2 -(E + E') 


Fig. 198. 

F F 

Fig. 199. 

Strong Opposite Lenses. — It is difficult to get absolute neutralisation 
with strong lenses, say over 10 D, there being always some slight positive move- 
ment. This is due to the thickness of the Cx., or rather to the interval 
between the optical centres of the two lenses. As shown in Fig. 199 by the 
dotted lines, the two lenses actually constitute a weak Cx. meniscus, because 
with the same radius of curvature, the total lens is one formed of two inter- 
secting circles, or it is an equicurved lens (q.v.). 




The thickness of a Cc. lens in the centre, no matter how strong it is, can 
be ignored, but this is not the case with a strong Cx. If the focal length of 
the Cx. is equal to that of the Cc, it is clear that F v of the Cc. cannot coincide 
with F z of the Cx. Parallel light incident on B is rendered divergent as if 
proceeding from F v , a point outside F x , and is therefore slightly convergent 
after refraction by A. If parallel light is incident on A, it is converged to 
F x , a point nearer than F v , so that it is still slightly convergent after refrac- 

Fig. 200. 

Fig. 201. 

tion. Thus a strong DCx. and DCc. lens of exactly equal powers do not 
actually neutralise each other. Or it can be explained as follows: 

If the light be incident on the Cx. it is converged, and the convergence is 
increased as it traverses the thickness of the two lenses to an extent that the 
final Cc. surface is unable to neutralise. On the other hand, if the light is 
incident first on the Cc. surface it is diverged, but in passing through the Cx. 
some divergence is lost, with the result that the Cx. surface over-neutralises 
it and produces a slight positive effect. Thus with either lens to the front, 
the result is the same Cx. power, but when the Cx. lens is in advance of the 
Cc. the effectivity of the resultant Cx. power is slightly enhanced; that is, the 
back surface focus is shorter. Again, if a ray of light originally parallel to the 
axis traverses first a Cx. and then a Cc. of equal dioptric power, or vice 
versa, its passage in both cases is, in the Cx., at a part of the lens more distant 
from the axis than that of the Cc. and, therefore, where the prismatic element 
is greater in the former. 

Strong Cx. and Cc. lenses may neutralise each other at the centre and 
not at the periphery or vice versa, with excess of either Cx. or Cc. effect at 
the one or other; or there may be Cc. effect at the centre and Cx. at the 
periphery, or the reverse. In such cases the lenses are not in contact either 
at the centre (Fig. 200) or at the periphery (Fig. 201), and the fault is due to 
the increased effect of a Cx. owing to separation. It is this separation that 
renders the neutralisation of torics and deep menisci so difficult. 

A strong Cc. being thin at its axis, its required radius for a given focal 
length would be calculated by the formula where thickness is ignored, while 
that of a strong Cx. would need to be calculated with its thickness considered. 
The + 20 D from a trial case, being of large diameter, is about -75 cm. thick 
in the centre, and its radius would need to be shorter than that of the - 20 D 
to have equal equivalent power. Giving the same radius to each, the true or 


equivalent power of the Cx. is weaker than that of the Cc. In order that two 
strong opposite lenses should neutralise, the Cc. must be the more powerful, 
the focal length of the Cx. being approximately one third its thickness longer 
than that of the Cc, which, however, is not the case when the radii of curva- 
ture of the two are equal. In short, although a thick Cx. has a longer equi- 
valent focal length than a Cc. of similar radius and /u, it is not sufficiently 
so for the Cx. to be neutralised by the Cc. For a - 20 D whose F= - 5 cm. 
to neutralise a Cx. having a thickness of -75 cm., the Cx. would need have 
F=5-25 cm., or D= + 19, and if ju—1'5 would require a radius of curvature 
of 5-125 cm. In other words the back foci of the lenses must be equal if they 
are to neutralise each other. If, therefore, a Cx. and a Cc. do neutralise, the 
Cc. is stronger, but the difference is quite inappreciable in weak lenses, and 
not of importance in spectacle lenses, even if strong. 

In modern cases of test lenses the concaves are of their indicated strength, 
but the convexes are made to neutralise the concaves of similar numerical 
value. Up to 10 D the difference is negligible, but the nominal + 10 D is 
only 9-8 D approximately, and the nominal + 20 is +18-75 D approx., the 
intermediate numbers being of proportional nominal value. Whether there 
is good reason for this arrangement is somewhat doubtful. 


The Nodal Points. — The term is ap plied to the point or points on the princi- 
pal axis of any system, through which the secondary axes pass. Thus the 
optical centre of a thin lens, and the equivalent points of a thick lens or 
system, bounded on Loth sides by air or media of the same optical density, 
have the properties of nodal points. If, however, the first and last media 
are different, then the equivalent points, although retaining their property 
of locating the principal planes or planes of refraction, no longer act as the 
crossing or nodal points of the secondary axes. Instead, we have a second 
point or pair of points — the nodal points — displaced towards the denser 
medium if the system is positive, and towards the rarer if it is negative. 
This can be illustrated very well by the case of a single refracting surface. 
Here the refracting plane is the surface itself, while the nodal point is at the 
centre of curvature of the surface. 

Principal points and nodal points coincide when the first and the last 
media are of the same refractive index; they are then, in this book, termed 
equivalent points, and the focal length of the system is the same on both sides. 
When the first and last media differ, F x and F 2 also differ, and employing the 
example of the single surface, the difference between them is equal to the 
radius, that is, to the distance between the nodal point and the principal 
point; also the ratio of F x to F 2 is the ratio of the indices of the first and last 
media. Refraction depends on change in the indices of refraction of two 
media. So long as light remains in the same medium there is no change in its 
course, but when it passes into another medium, the alteration of direction 
is the more violent as the change of indices is great. 

Fig. 202. 

The Plano-Cx. Lens. — The formula for a thin plano-Cx. lens, F=r/(// - 1), is 
the same as that for F v the anterior focus of a single surface. If parallel 
light enters at the plane surface of the lens B, all the refraction takes place 




at the other, where light passes from the dense into the rare medium. If the 
light is incident at the curved surface A, it is refracted towards a more 
distant point F 2 , since it passes from the air into a dense medium. But 
at B, the second surface, which the light meets convergently, it is again re- 
fracted such that F 2 becomes F 2 /f.(.=F 1 as measured from the surface B. The 
lens being thin — i.e. t being zero — F is then taken to be the same whether 
the light enters the one surface or the other. 

If the lens is thick, t cannot be ignored. The light on meeting the surface 
B is converging to F 2 -t beyond, that surface, and since F 2 /f,i=F 1 we have 
(F 2 - 0//W=F 1 - If fa which is the back surface F from the plane surface. 
Thus the shortening of F which results from entry of the light into air is 
(F a -*)/w or F x -<//*• 

Passage from One Medium to Another. — If light is tending to a focus F 
in a dense medium, but meets a rare medium before the focus is formed, the 
surface being plane, F is shortened to F' . The shortening is calculated from 
d//ii where d is the distance of F beyond the plane surface. If the final 
medium is denser F is lengthened to dfa Here d is the F 2 - 1 of the last 

Fig. 203. 

Thus in Fig. 203 suppose light is convergent in a medium M, as a small 
tank of water, and bends to focus at F 10" behind A the curved surface, but 
at 6" meets a plane boundary B beyond which is air. 


d=i" and BF'=\/\ -33=3". 

If the outside medium were oil of ^=1-46 instead of air F is lengthened 
to F". 

Then BF"=d x 147/1-33=44" 

In the case of a hemisphere, for example, F of the curved surface =rfi/(fi - 1), 
but the light meets air at a distance=r, so that d=r/u/(ju- l)-r, and this 
divided by jli works down to r/ju([i- 1), which is F B from the plane surface 
of a hemisphere. 

Change of F in Dense Media. — The change in the power and F of a lens 
when transferred from air to some denser medium is very marked. It has been 
shown that F is inversely proportional to (ju- 1), so that when a lens of /u 2 
is immersed in a medium oi fa, we have F: F': : (fa - 1) : (fa - 1), where fa 
is the relative index fa/ fa. The lens has a focal length of F in air, and 



one of F' in the medium (Fig. 203), the same as if it were made of a substanco 
of [i r , and surrounded by air. Thus 


T S 

*y 2 -i) 



Fw. 204. 


> — «j 

For instance, a thin DCx. lens L (Fig. 204) of ( «=l-5 and r—8 in, has in 
air F=8 in. If it be placed into a tank of water where / a r =l-5/l-33=l-13, 


F= 8 ^ 5 =30 in. 

or the dioptral change is from +5 D to +T3 I). Thus a glass lens placed 
into water has its F increased nearly four times, and its power correspondingly 

If, however, the tank were so small that it only just contains the lens, its 
boundaries being T and S beyond which is air, F' is shortened to .F"=30/l-33 
=22-5 in. On the other hand if beyond S there were oil of'//=l-45, F' 
becomes lengthened to F"=30 x 145/1 -33=32-62 in. 

The crystalline lens of the eye in situ has power of about 22 ,D, in air it 
has about 125 D. Here the relative index is about 1-09. The lower the 
relative ju the greater is the change; if a lens is placed into cedar oil all its 
refracting power is lost since the two^'s are practically equal, and / a r =l, so 
that^- 1=0. 

Fig. 205. 

Thin Lens bounded by Different Media.— When a thin lens is bounded, 
say, on one side by air and on the other by some medium denser than air, 
since the lens is thin all the refraction is presumed to take place in the re- 
fracting plane, the position of which is presumed to be unaltered, but the 


focal lengths become lengthened. The distance of the nodal point from 
the principal point is F 2 -F r These are calculated from 

F 1= - W*\ x and F 2 = W * 

Thus let a thin DCx. lens (Fig. 205) of 10 in. radii and ( u=l-5 be bounded 
in front by air and behind by water. Then 

lx 10x10 . . 1-33x10x10 

^1=77; 7^ — r^ -==15 in. and F 2 == -- — — ,,=20 in. 

1 10x-17 + 10x-5 2 10x-17 + 10x-5 

Therefore the distance of the nodal point N through which the secondary 
axes now pass is F 2 -Fj =20-15 =5" behind the refracting plane L L, 
which remains unchanged. 

Cases of Various Media. — When a thin lens of /u z separates two media of 
ju x and /u A — that is, when there are three different media separated by two 
curved surfaces — the following formula can also be employed: 

/^3 /^2 ~t l l , f^3 ~j^2 

F~ r x r 2 

If there are four media 

F r t r 2 r 3 

The power of any number of surfaces separated by negligible distances 
can be found by taking the sum of their anterior focal powers and multiply- 
ing it by the last^a — i.e. by/x, 5 or ^4 as the case may be. If the last medium 
be air, like the first, we have 1/F equal to the sum of the anterior focal 
powers of all the media. 

It should be particularly noted that in the above the numerator of each 
fraction is obtained by deducting the preceding //. from the fi following — 
e.g. fij -fi 2 ' an( ^- th 3 ^ f is positive or negative according as it is respectively Cx. 
or Cc. towards the direction of the light. Also it should be noted that F 
is either F x or F 2 (as calculated in the preceding article). If the light passes 
one way instead of the other, F x and F 2 change places, as do/x x and^, or^ 4 as 
the case may be; also the signs of the radii change. 

We have a case of four media when light passes through a combination 
formed by a bi-f ocal made by the insertion of a deeply curved convex segment 
of high [A into a larger lens of low /u. Such a combination is also formed 
by the contact of a double Cc. lens of, say, ^=1-5 with a double Cx. lens of, 
say, /x=l-6, the two being of equal curvature. The focal power can be found 
by calculating for each lens separately and then adding them together, or 
by calculating for each surface separately, as indicated above. 



Thick Lens bounded by Different Media. — In this case (Fig. 206) the 
thickness of the lens cannot be ignored, and there are now two principal 

Fig. 206. 

and two nodal points in the system such that the distance P 1 N l =P 2 N 2 = i\ 
- F v and F x / F 2 =ju 1 /fi 3 . The cardinal points are calculated from the 
following formulae. 


Wl r 2 

1 i\(fi 2 -/u 3 )+r 2 ({A 2 -fa) - t(/u 2 -fa) {/u 2 -ju 3 )/jh 2 
Let the denominator of the above be called Q, then: 




F 2 = 


j. jvKto-rt from A 

ju 2 <4 

P 2 = 

l^2 r 2 t (l U 2~l U l) 

jU 2 Q 

from B. 

The back surface focal distances can be obtained by deducting P : from F 3 
and P 2 from F 2 . 

As an example, suppose the case of the crystalline lens of the eye with 
the cornea and aqueous removed (Fig. 206). Let ju 1 = l, /u 2 = l-i5, 
(jl 3 = 1-33, r x = 10 mm., r 2 = 6 mm., and t, the thickness of the crystalline, 
= 3-6 mm. 

Working from the given data we find 

Fj = 15-93 and F 2 = 21-24 

P x = -8 from A and P 2 = 2-63 from B. 

The distances of the nodal points from the equivalent points are 

N x = F a - Fj = 21-24 - 15-93 = 5-31 from P t 
N 2 = F 2 - F x = 21-24 - 15-93 = 5-31 from P 2 

or Nj is 6-11 mm. from A, and N 2 is 2-68 mm. from B 

The equivalent thickness or optical interval T = -17 mm., and the same 
interval exists between N x and N 2 . 

Combinations of Two Systems when// j differs f rom// 4 . — Let F 1 and F 2 be the 

anterior and posterior focal distances of the first system, and F/ and F 2 ', 



those of the second system. Ej and E 2 pertain to the first, and E/ and E 2 ' 
to the second system. The distance d between the two systems is that 

% .- 

Fig. 207. 

between E 2 and E/, *.e. between the two most adjacent points. Let Q be 
the distance between F/ and F 2 , that is, 

Q=F 2 +F 1 '-d. 

F A and F p are the anterior and posterior focal lengths of the combined 
system, P x and P 2 are the principal points, and N x and N 2 are the nodal 

P 1= ^ from E a Pa=^ from E' 2 

„ F,F' F 2 F 2 ' 

F — F = 

A Q p Q 

F P - F A =P X - N 1= =P 2 - N 2 , P X F A =N 2 F P , P^N^ 

T=d+T 1 + T 2 -(F 1 + ~P 2 ) 

Such a system as the above is found in the eye (Fig. 207), taking the two 
components independently; or in a lens placed in front of the eye, the latter, 
as a whole, being the second system. 

Calculations concerning the eye are to be found in the chapter on the 
Gauss Equation (q.v.), but they are more fully treated in " Visual Optics 
and Sight Testing." 

Some Recapitulated Points on Compound Systems. — Rays parallel to the 
principal or a secondary axis in the first medium meet on that same axis 
in the last medium, and vice versa. Rays diverging from a point in the 
focal plane of the first medium are parallel in the last, and vice versa. 

A ray directed to the one nodal point, after refraction, appears to come 
from the other, and its direction is parallel to its original course. 

A ray directed to any point on the one principal plane, appears after 
refraction, to proceed from a corresponding point situated on the other. 
These two points are on the same side of the axis and equally distant from it, 
and each is the image of the other. 

The distances P 1 P 2 =N l N 2 : N 1 F x =P i F 2 .N z F 2 =P 1 F 1 

F 2 -F 1 =P 1 N l =P 2 N 2 =th.e imaginary equivalent radius of curvature. 



F^ F 1 =ju x //u 1 —the imaginary combined relative//, where fi x is that of the 
last medium. 

F^F^ ... *j& - F X = J^ -^ = p iN -p iNi 

Hft=l, F 1 { [ i x -l) = P x N 1 : If^^P^^O 
? 5 

Fig. 208. 

Construction of Image. — In Fig. 208 let P X P 2 be the principal planes, 
N X N 2 the nodal points, F X F 2 the principal foci, and AB any object in the 
rarer medium, the system being positive. A ray AP X parallel to the axis 
is refracted at P 2 through F 2 . A secondary axis A N x passes on emergence 
from 2V 2 parallel to its original course. A ray passing through F x is, after 
refraction, parallel to the axis. 

Where these rays meet in A' is the image of A, so that B' A' is the 
complete image of A B. As will be seen the construction, with the exception 
of the displacement of N x and N 2 , is the same as for any ordinary thick lens 
or system in air. Provided the six cardinal points are known, the most 
complicated system can be reduced to the simplicity of a single lens. 

When the first and last media have the same optical density, the equivalent 
and nodal points coincide, so that the relative sizes of image and object are 
as their distances from the equivalent points; when the media are different 
the relative sizes of image and object depend upon their distances from the 
nodal points. The formulae for single thin lenses, and single refracting 
surfaces are applicable for calculating conjugate foci, provided all measure- 
ments are taken from the appropriate equivalent points. 

Negative System bounded by Different Media. — This does not occur in 
practice so that no special discussion is necessary. The calculations would be 
similar to those for a positive system. 


By the aid of the Gauss equation every optical system can be so simplified 
that all problems of conjugate foci, etc., may be worked by the formula? 
applicable to single thin lenses. The calculations in the case of more than 
two surfaces are necessarily long, but they always involve the solution of a 
continued fraction, so that the difficulties are purely arithmetical. 

In using the equation, which serves for any number of surfaces, media 
and thicknesses, the pencils of light are presumed to be axial and small; in 
other words, aberration is neglected. In order to keep the formula? as sym- 
metrical as possible and avoid a mixture of signs, the following conventions 
must be observed, namely, (1) all distances measured to the left of a surface 
are negative, and to the right positive; (2) all thicknesses are considered 
negative, and therefore, on substituting actual values, it is necessary to use 
the minus sign. 

Thick Lens. — The following formula? are deduced from the consideration 
of the lens having positive radii of curvature according to the above con- 
vention, i.e. a periscopic with the concave surface turned towards the right. 
Let ii x be the refractive index of the surrounding medium, ii 2 that of the 
lens, t the axial thickness, r x the radius of the first surface, and r 2 that of 
the second. Let u be the object distance, t\ the image distance formed by 
refraction at the first surface, and v the final image distance after refraction 
at the second. The fundamental equation connecting u and v x is 

22> - 23-' = £jt^r> - f , , , w 

V t £. ~ ', ' l^2/ v i-/^i/ u =(^2-^i)/ r i 

but in order to simplify the formula? (/^ 2 ~f jl i)/ r i * s replaced by F l5 while 
ju 2 /v x and /u x /u are replaced by l/v x and 1/w respectively. These last two are 
termed reduced expressions, i.e. actual distances divided by the li's of the 
media to which they pertain. Similarly in the expression connecting v x and 
v, given later, (^i-/M 2 V r 2 and ^/v are replaced by F 2 and 1/v respectively, 
while t is also employed reduced, being divided by the fi in which it is 
measured. Consequently the values subsequently found are similarly reduced 
and must be multiplied by the /n in which each occurs, in order that their 
true values may be determined. 

The fundamental formula reduced becomes 

l/v x - l/w=F t , or 1/« 1 =F ] + 1/u 



whence v \=^ tt (') 

The expression connecting v t and v is 

which, in reduced terms, becomes 

1/v - l/(v r + 0=F 2 , or l/v=¥ 2 + \/{i\ 4 f) 

whence t»= — . . . . . (2) 

F 2 + i 

i\ + t 

Substituting in (2) the value of i\ in (1) we have 

«=— i— (») 

2 1 


On working out this continued fraction in (3) we get 

MFj + p + t 
u^Fjt+F^FJ+F^ + l * ' - ' v 

which, for the sake of brevity, is usually written 

Cm + D 

V=7 = (5) 

Au + B 
where A=F 1 F 2 « + F, +F 2 ; B=F 2 £ + 1 

0=F 1 « + 1; D=t. 

No. (5) connects v and u when both are finite distances. If u is at oo 
the quantities D and B disappear and u cancels, so that the focal length 
measured from the second surface is 

«=C/A . . . . . .(G) 

The value of v in equation (6) is the back focal distance as measured from 
the pole of the second surface. 

If v is at oo, then A w + B=0, so that the back focal distance measured 
from the pole of the first surface is 

w=-B/A (7) 

Before proceeding further an expression for the total magnification M 
produced by the lens must be found. 

Let tn l be the magnification due to the first surface, and m 2 that due to 
the second; then the total magnification M is m x x m 2 . 



In Fig. 209 let AB be an object in front of the first surface, and B' A' 
its corresponding image. A ray from A meeting the vertex in x will be 

Fig. 209. 

refracted to A' such that i and r are the angles of incidence and refraction 
respectively. Then 

m 1 =A / B'/AB 

But i and r being small, AB/u may be considered equal to sin ?, and 
A' B / /v 1 =s'm r, and sin //sin i=/u 1 //Li. 2 . 

Therefore m 1 =A / B'/A B=/n 1 v 1 //u 2 u 

But u/fi-i and vj^ are reduced quantities and therefore to preserve our 
notation the refractive indices must be omitted, so that 

m 1 =v 1 /u 

Similarly the magnification m 2 of the second surface is 

m 2 =v/(v 1 +t) 

Therefore the total magnification 

M=v 1 /uxv/(v 1 +t) 

But from (1) v 1 /u=l/{¥ 1 u + 1) 

v 1 
And from (1) and (2) -_=—-— - 

F.,U ,+*) + ! 




F X M + 1 

Fju + l 

Fju + l uiF^Fj + Fi+FJ + Fj + l 


uiF^t + F X + F 2 ) + F 2 t + 1 


Am + B 


Now let the magnification be +1, i.e. let virtual image and object be 

equal in size. Then 



whence M =P 1 =(1 - B)/A (9) 

this distance being measured from the first surface. 

On substituting this value of u in (5), the corresponding value of v is 

^ C-BC+AD C-l 
u=P 2 = =— .... (10) 

because it can be shown that AD-BC = -1. This distance is measured 
from the second surface. 

These planes of unit virtual magnification denote the equivalent planes, 
and the points P x and P 2 where they cut the axis are the equivalent points. If 
it were possible to place a small object in the one plane, then its virtual 
image, identical in all respects to the object, would be situated in the other. 

If the magnification be-1, then the corresponding values of u and v 
will locate the symmetrical planes, where object and real image are equal in size. 

To find, therefore, the equivalent focal distances, the values of (9) and 
(10) must be added to those of u and v in (5); thus 

C-l_C(u + (l-B)/A)+D 
V + ~A~ : ""A(tr+(l-B)/A)+B 

which simplifies to A=l/v-l/u (11) 

This expression (11) should be compared with that of a simple thin lens 
for the focal length in terms u and v. Then if w=°o 

«7=1/A (12) 

and if y= oo u=-l/A (13) 

The princpal focal distances given in (12) and (13) are equal when the 
first and last ju's are of equal optical density. The values are reduced, and multiplied by the^ in which each occurs, so that when in air they 
are unchanged. 

As a simple example, let ^=6, r 2 =8, /i 2 =l -5,^=1 (air), and (=1; then 

K + X 

t + - 

W i+ \ 


•9445 u - -666 
which works out to »=- 

Then, if u= oo 

•1423 u + -9584 

C -9445 

v=-= =6-63 

A -1423 


-B -9584 „ „ 
Also u =—=^^-=-<M 

„ 1-B 1--9584 

p C-l = 9445-1 
2 A -1423 

The equivalent focal distance • 


Multiple Surfaces. — The Gauss equation may be applied to an optical 
system having any number of surfaces surrounded by corresponding media 
of different densities and thicknesses. The equation 



"Am + B 

is universal, although the various values become more complicated as the 
number of surfaces is increased, but the problem always takes this form, 
involving the solution of a continued fraction. 

Suppose the case of the eye having three surfaces, F 4 , F 3 and F 5 with 
thicknesses t 2 and t 4 , with the following data r x =8, r 3 =10, r 5 =6, f 2 =3-6, 
* 4 =3-6, ^=1,^2=1-333, ^3=145, ,a 4 =l-333. Then 

„ Uo-iu, 1-333-1 ni „ 
F n rx = — =-0416 

1 H 8 

^^^ 145 -l-333 = 
H 10 

^- ii 3^1;333-l-45_ oi95i 

5 H -6 

The reduced value of 

t,= - 3-6/1-333= -2-7007 
and that of « 4 =- 3-6/145= -24828 

Then we have 

1 1 

F. + l -0195 + 1 

U + l -24828 + 1 


F^ + l -0117 + 1 

U + l -2-7007 + 1 

F,+- -0416 + - 

1 u u 


which becomes, when worked out, 

•7586 m -5-1050 


•0668 u + -8689 

That is, A=-0668, B = -8689, C=-7586, D = - 5-1050. 
The anterior F= -/u 1 /A= - I/-0668= - 15 mm. 
The posterior F=a 4 /A=l-333/-0668=20 mm. 

P 1 = / u 1 (l - B)/A=-1311/-0668=l-96 mm. from r, 
P 2 =/* 4 (C - 1)/A= - -3128/-0668= - 4-81 mm. from r 5 
or 7-2 - 4-81 =2-39 mm. from r v 

The nodal points N x and N 2 , found by subtraction, are, respectively, 
6-96 and 7-39 mm. from r v Neglecting the intervals between P x and P, 
and that between N 4 and N 2 , we have P at 2-2 mm., and N at 7-2 mm. from 
the apex of the cornea. 

When working with the Gauss equation two things must be borne in 
mind; firstly, the convention as to signs upon which the symmetry of the 
formulae depend; and secondly, the use of reduced instead of absolute dis- 
stances in order to simplify the formulae by the inclusion of the refractive 
indices in other terms. Thus v, the final image distance, is always multiplied 
by the index of the last medium to give the absolute values of the second 
principal focus and the second equivalent point. On the other hand u 
which, in the final expression, denotes the anterior focus and first principal 
point is, except in very rare cases, already reduced, the first medium gener- 
ally being air. In fact, the same may be said of v, as a difference in the 
indices of the first and last media occurs only in the case of the eye, and in 
certain instruments as; for instance, the immersion objective of the microscope. 

The calculation of a continued fraction for three surfaces being compli- 
cated, the results obtained may be checked by the following, which is the 
continued fraction worked down. 


«(F 5 N + F X F 3 « 2 + F 4 + F 5 ) + F 5 R + ¥ 3 t 2 + 1 
where N=F 1 F 3 ^ 4 + F^ 2 + F^ 4 + F 3 / 4 + 1 

and R=F 3 « 2 < 4 +« 2 + « 4 


Curvature is a symmetrical departure from straightness of a line or plan- 
eity of a surface. Unless otherwise stated, it is presumed to be spherical or 
circular, but it may be toroidal or of an aspherical nature. Curvature C is 
the reciprocal of the radius; thus C=l/r, and this applies also to figures other 
than circular, and surfaces other than spherical. In the case of circles and 
spheres, the curvature is equal at all points, but this is not so with conic 
curves. The curvature at any point on any refracting or reflecting surface, 
having a symmetrical axis, is determined by dropping from it a normal 
to the axis; the length of this line is then the radius of curvature of that 
particular point. 

Curvature can also be expressed in diopters; the unit ID having a radius 
of 1 M, and for radius expressed in cm., mm., and inches respectively, 

D=100/r, 1,000/r, and 40/r. 

Thus if r=10" then C=l/10, or 40/10=4 D. 

Curvature Method. — Formulae in connection with mirrors, prisms and 
lenses can be deduced from the paths of the waves. The following are ele- 
mentary examples of the application of this method, which is by some writers 
preferred to the " ray " method, since it represents the actual physical change 
in shape and direction undergone by the wave points when refraction or 
reflection takes place. 


d > 

Fig. 210. 

Fig. 211. 

Plane Surface. — A B (Fig. 210) is a plane wave front incident obliquely 
on the surface CD. If ^=1, and/i 2 =l-5, the part of the wave which enters 
at B travels in the same time to F only 2/3 of the distance A E. With B as 

193 13 



centre and B F as radius describe a small arc, a tangent E F from E showing 
the inclination of the wave front in the dense medium. At the second 
surface a similar construction shows the wave front G H after emergence, 
F' H being 1-5 times E' G. 

Course of a Wave through a Prism at Minimum Deviation. — Let 

C B D (Fig. 211) be a prism on which is incident the plane wave A B at 
an angle of incidence i. The portion B of the wave meeting the base of the 
prism is retarded to a greater extent than A, the portion in air, so that when 
the whole wave enters the prism it takes up the position C M, r being the 
angle of refraction. 

Since the deviation is supposed to be minimum, the total refraction is 
symmetrical with respect to the surfaces C B and C D, so that C M bisects 
the principal angle. The wave is then incident on the second surface at the 
angle u, and on emergence it is swung over still more towards the base, so 
that, when completely clear of the prism, it has the position E D making 
the angle of emergence e with the second surface, e being equal to i. 

Fig. 211a. 

Reflection. — In Fig. 211a let SS be a plane surface, and A a point 
from which waves diverge. The latter are reflected back with their 
curvature unaltered, such that they appear to originate from the virtual 
image C. The distances BC and AB are equal. A ray AD incident at 
the point D is reflected in the direction E as if from the image C. FG is the 
normal to the point of incidence, a' is the angle of incidence and 6 the angle 
of reflection. From the symmetry of the figure it is obvious that the angles 
b and a' are equal, proving that the angles of incidence and reflection are 

Wave Front — Curvature. — The unit of the dioptric curvature system 
being one having a radius of 1 metre, the curvature of any wave may be 
denoted and measured by it. Thus if light diverges from A M or 50 cm. the 
wave is said to have a divergence of 2 D; at some other distance, say 2 M, 
the curvature would be -5 D, and so on. Thus if C denote the actual curva- 
ture of a wave, it may be expressed either as the reciprocal of its radius r in 
metres, or simply in diojDters D. Then C—l/r or D. Now from the sphero 



meter formula, for shallow curvatures r=d 2 /2s, where d is the semi-chord, 
and s the sagitta of the corresponding arc of radius r. In other words, pro- 
vided the chord remains constant, the radius is inversely proportional to the 
sag, and vice versa, while the curvature of the arc is directly proportional 
to the sag on the same chord. Thus we may say that 1/r or Ccc s, or s oc 
or 1/r. It will be seen that the " curvature " formulae are identical with the 
" ray " formulae, only that, with the exception of /u, all the symbols employed 
in the one are the reciprocals of those used in the other, and vice versa. 

P P 

Fig." 212. 

Fig. 213. 

Cc. Mirror — Plane Incident Wave.— Let P R (Fig. 212) be any Cc. mirror 
on which is incident the plane waveP Q R. If the aperture be small the points 
P and R of the wave front first meeting the mirror may be considered to be 
reflected back to M and N while the central point Q is travelling to the vertex 
0. When Q has arrived at the contour of the reflected wave is M N; 
it remains to find the curvature of M N. 

Now since P M=0 Q, Q=Q T and we have T 0=2 Q. But, since 
the curvature of an arc may be taken as proportional to the sag for equal 
Yq chords, T Q. represents the curvature F of the reflected wave M N, and 
Q the curvature C of the mirror. Thus T = 2 Q 0, or F = 2 C. In other 
words the curvature of the reflected wave is double that of the mirror, so 
that the focal distance F is half the radius C. 

Cc. Mirror — Divergent Wave. — Let P S R (Fig. 213) be a wave diverging 
from a near object /jj then while the vertex S of the wave is travelling to 
0, the extremities P and R are reflected to P' and R' respectively such that 
T Q=S 0. ThenP' R! is the reflected wave converging towards/ 2 . Q 
is the mirror sag, and since T Q=S we have T 0=2 S O + Q S— 

Let F l be the curvature of the object waveP S R, F 2 that of the image 
wave P' Q R', while G is the curvature of the mirror, and F its focal curva- 
ture or power. Then Q S=F V Q=G, T 0=F 2 , and F=2 C. Therefore 
T 0=2 QO-Q 8, or F z =2 C - F v so that F 1 + F 2 =2 C=F, i.e. the focal 
power of a Cc. mirror is equal to the sum of the object and image curvatures, 
and this is the formula for expressing conjugate foci. It will be noticed 
that C, the mirror curvature, is the mean of the object and image curvatures; 
thusC=(F 1 + F 2 )/2. 



Convex Mirror — Plane Incident Wave.— Let M N (Fig. 214) be a plane 
wave incident on the Cx. mirror P R. is now the first incident point, 
and this is reflected to Q', while M and N are travelling to P and 22, so that 
P Q' R is the reflected wave, which can be shown to have a curvature double 
that of the mirror, as with a Cc. In other words, since QQ'=2 Q, F— 2 C. 

Convex Mirror — Divergent Wave. — When the wave is divergent from a 
near object^ (Fig. 215), the incident wave isP' R', and the reflected wave 
PQ[R such that Q'=0 T + OQ. 

that is, 

QQ'=OQ + OQ'-OQ+ (OQ + OT)=2 0Q + OT 
F 2 =2C+F 1J orF 2 =F+F 1 

In other words the image curvature is equal to the sum of the object and 
mirror curvatures, because both are divergent in effect. Employing the 
usual convention as to signs this expression would be written as for a Cc. 
mirror, i.e. F x + F 2 = 2 C = F, the negative sign being employed when 
substituting the value of F. 

Fig. 216. 

Fig. 217. 

Single Surface — Cx. — Let M N (Fig. 216) be a plane wave incident on the 
single Cx. refracting surface P Q R such that P Q' R is the refracted wave 
convergent towards the posterior principal focus P B . Let C be the curvature 
of the surface, P B that of the refracted light, and// the index of the medium, 
the first being air. Then we have Q S=/t Q Q'. But 

QQ'=C-F B andQS=C 
C=(C-F B )jU or Y B =C(/i-l)fr 



Similarly an expression can be found for the anterior principal focus of 
the same surface M Q N. Here (Fig. 217) the plane wave advances from the 
denser medium to meet the surface as M N, the retarded wave convergent 
towards the anterior focus F A , being P Q R. Then Q' S=a Q Q'. But 

Q'S=F A + C, andOQ'-C 

Therefore F A + 0=^0. 


F A =C( A /,-l) 

For a concave surface the formulae are the same, C being negative. 

Fia. 218. 

Conjugate Foci — Single Cx. Surface. — Let f (Fig. 218) be any near object 
from which diverges the wave M N to the surface P Q R, and let/ 2 be the 
image formed by the image wave P Q' R. Let TQ = F p Q S = C and 
Q' S = F 2 . Then 

T S=/* Q Q'=^ (S Q - S Q') 

and TS=TQ + QQ' + Q'S 

... i a(C-F 2 )-F i + (C-F) + F 2 or // C-,a F 2 =F t + C 

that is F x +u F 2 =C (/u - 1) 

Similar formulae may be deduced for a concave surface, but here C and F 2 
are negative. 

Fig. 219. 

Thin Convex Lens. — With a lens the curvature of each surface is like- 
wise represented by their respective sags, so that in the case of a double Cx. 
(Fig. 219) Q S represents the sum of the sags C t and C 2 . Let M N be a plane 
wave incident on the lens; then, owing to the greater axial thickness, the 


centre of the wave is retarded more than the periphery, the resulting wave 
front taking the formP S R converging to the focus F B . Let T be the united 
sags of the lens surface and wave fronts; then T=C 1 + C 2 + F. But 

T= A tQS= / a(C 1 + C 2 ) 

C 1 + C 2 + F= / a(C 1 + C 2 ) 

whence F=(C 1 + C 2 ) (fi- 1) 

In other words the power F of the lens is the product of the united curva- 
tures and the refractivity of the glass. 

Similar formulae in the case of conjugate foci and for concave lenses can 
be deduced on similar lines; in numerical examples, of course, C x and C 2 
of concave lenses are reckoned negative. 


Colour is the result of waves of definite length and frequency. 

Primary and Secondary Colours. — There are six or seven distinct colours 
in the solar spectrum (vide Chapter I.), but it was shown by Young, and con- 
firmed by Helmholtz, that every shade of colour in nature can be obtained 
from the mixture of red, green and violet in certain proportions, whereas 
these three colours cannot be produced by mixing others. For this reason 
red, green and blue-violet are termed the primary colours, while the other 
spectrum colours are secondaries. Thus red and green, in varying propor- 
tions, produce orange or yellow, while green and violet produce blue or indigo. 

When a solar spectrum is viewed, there are three main divisions — viz., 
green in the centre, with red at the one end and violet at the other. Between 
the centre and the extremities different observers can distinguish, on either 
or both sides, one or more different colours. Some would describe the spec- 
trum as containing three colours only of varying shades. It should be appre- 
ciated, however, that eveiy point in the visible spectrum is due to a different 
wave length. 

A mixture of all the wave-lengths contained in the visible spectrum forms 
white light; but for white light all of them are not essential provided two com- 
plementary colours are contained in the mixture. 

Colour Sensation. — According to Young and Helmholtz, there exist in the 
eye three sets of nerves, each of which conveys to the brain a primary colour 
sensation. Stimulation of all three produces the sensation of white, of none of 
them black, or absence of colour and light. By the stimulation of one or 
more in varying proportions, all colours are mentally appreciated. This 
subject is more fully treated in, " Visual Optics and Sight-Testing." 

Varying Wave-Lengths. — As described in Chapter I, the infra-red, or heat 
waves, and the ultra-violet, or chemical waves, lie just beyond the two ends 
of the visible spectrum. They are of the same nature as light waves, but 
differ from the latter in their effects, and they are, respectively, too long and 
too short to stimulate the retina. Both heat and actinism are, however, 
produced to a small extent by visible waves which, therefore, have different 
properties — namely, that of light on the eye, and of heat or chemical action 
on bodies. The yellow and green are probably the only waves which are light- 
producing only. 




Complementary Colours. — Two spectrum colours which, when combined, 
form white light, are complementary to each other. Hence a complementary 
colour may be defined as that which, when united with another, produces 
white light. The complement of a primary colour is that secondary colour 
which results from the mixture of the other two primaries; the comple- 
ment of a secondary colour is that primary colour which is not contained 
in it. 

Spectrum Colour. Complement. 

Red. Green-Blue. , 

Orange. Blue. 

Yellow. Blue-Violet. 

Green. Pui pie-Red. 

Blue. Orange. 

Indigo. Orange-Yellow. 

Violet. Green- Yellow. 

The purple-red is not in the visible spectrum, it being a combination of 
red and violet. A graphical presentation of this table is shown in Fig. 220. 

Colours of Light.- — Spectrum red and green will, if mixed in certain pro- 
portions, produce yellow or orange. If spectrum red, green and blue- 
violet be mixed in the correct proportions white light is formed. If the wave- 
lengths of orange-red and blue-green be added together the mean will give the 
wave-length of yellow, thus, 656+518=1174, and 1174/2=587. Taking 
the wave-lengths of red, green and blue respectively, the sum divided by 
three will give the wave-length for the brightest part, that is, yellow, which is 
the nearest approach to white light which the spectrum affords; thus 748 + 
527+486=1761, and 1761/3=587. 




Cyan Blue. 







Dark rose 







Dark rose 













, , 











Sea blue 



Deep blue 

Sea blue 



Cyan blue 








The quantity of light of one colour necessary to mix with any other to 
produce white light, or a third colour, does not appear to follow any definite 
law, but the proportions usually remain the same for different observers. 


Certain colours, e.g. purple, which do not appear in the spectrum are those 
formed by a combination of two or more non-adjacent wave-lengths, the 
resultant effect on the eye being, in general, that colour corresponding to the 
mean wave-length of the components. 

The table on p. 200, according to Helmholtz, shows the effects produced 
by the addition of any two spectrum colours. 

Brightness of Colour. — In a prismatic spectrum the red appears fuller 
than the violet because the former is more crowded together, while the latter 
is spread out; this is not the case in a diffraction spectrum, in which the extent 
of colour is about equal on either side of the yellow. The latter is the brightest 
part of the spectrum to the human eye, and in general the intensity rises 
in the prismatic spectrum from zero, at the extreme red, rapidly to the yellow 
and then, dropping off again, but more slowly, to zero at the extreme violet. 

Colours in Pigments. — The primary colours in pigments (dyes, paints or 
colouring matter) are so-called red, yellow and blue; any other colour is 
obtained by mixing two primaries. 

The primaries and their complements are shown in Fig. 220, from which 
it will be seen that the primaries of pigments are the complements of the primaries 
of light. Thus I, 6 and 10 are the primaries of light, and 4, 7 and 12 are 
the primaries of pigments. Although the primaries of pigments are popu- 
larly known as red, yellow and blue, yet the actual tints are not quite those 
usually associated with the terms. 

Fig. 220. 

Mixing Colours.— The fundamental difference in the results obtained by 
mixing spectrum lights and pigment colours lies in the fact that the former 
is an additive, and the latter a subtractive process. The colouration resulting 


from mingled lights is due to the mixture of wave-lengths, while the resultant 
colour of a mixture of pigments is that remaining after each pigment has 
absorbed a certain wave or series of wave-lengths. The tendency of added 
lights is to give increased illumination and to approximate it to white, while 
with pigments the mixture tends towards black. 

Thus, when the primaries of light, i.e. red, green and blue- violet, are 
mingled — projected, say, from three separate lanterns — the white screen 
reflects all three impartially to the retina, where their superposition produces 
the sensation of white. With pigments, however, the final colour is due to 
that remaining after each pigment, in a certain mixture, has absorbed from 
the incident white light its own complement. In this way the primary 
colours of pigments are those capable of absorbing the three primaries of 
white light, i.e. red, green, and blue- violet, whose respective complements are 
green-blue (peacock blue), purple-red, and yellow. These last three are 
therefore the primaries of pigments because, when mixed in the right pro- 
portion they (theoretically) produce black. In practice, however, owing to 
the natural impurities of pigments, and the impossibility of combining the 
correct proportions, the result is a dark grey. For the same reasons, it is 
impossible accurately to match the spectrum colours by means of pigments, 
and this is especially the case towards the violet end; in fact we cannot 
imitate spectrum violet by any known pigment or combination of pigment 

The additive effect can be roughly imitated by painting yellow and blue 
sectors alternately on a disc which, when rapidly rotated, gives the impression 
of white if the proportions of colour are correct. Here the yellow and blue 
alternately impinge so rapidly on the retina that the sensations caused by 
alternate sectors have not time to fade away, and therefore mentally become 
mingled, and give rise to the sensation of white. The experiment must 
be carried out in white light, but even then the effect is generally far from 
pure owing to the inevitable muddiness of the pigments. By increasing the 
number of sectors, and repeating the six spectrum colours in proper propor- 
tion all round the disc, a better white is secured. 

The result of a pigment mixture may be surprisingly different from the 
result of mingling lights of corresponding colours. If blue and yellow lights 
are mingled in the right proportion on a white screen they cause the sensation 
of white. If blue and yellow pigments are combined, the blue absorbs red, 
the yellow absorbs violet, so that green is produced by such a mixture. Rose 
red and blue-green are complementary colours which, added to one another, 
produce white in the case of coloured lights (additive effect), but neutralise 
each other, i.e. produce black in the case of pigments (sub tractive effect). 

Additive effects can also be produced by the mixture of pigment or coloured 
powders, where absorption does not occur, but both pigments or powders 
reflect light. Especially is this so if the two colours are not complementary, 
or tending to be so ; thus red and yellow combined in pigment make orange 
as they do in the case of lights. Or using the illustration above of blue and 


yellow pigments combined making green, a blue pigment reflects violet and 
green, yellow reflects red and green, so that if the two pigments be mixed 
there is reflected a certain quantity of violet and of red, and a double 
quantity of green. The red, the violet, and a portion of the green combine to 
form white light, so that there is a residue of green light, which gives the 
nature of the colour to the mixture of the two pigments. 

Qualities of Colours. — Colours in pigments possess three qualities, viz., 
tone, brightness and purity. Tone or hue is that quality which differentiates 
between the various colours — say, red and orange; it depends on wave- 
length. Brightness, intensity or luminosity is that quality which represents 
the strength of a colour; it depends on the amount of light reflected; one 
which reflects little light is a dark colour, and one which reflects much light 
is a light colour. Fullness, saturation, tint or purity is that quality which 
represents the depth of a colour; the less the admixture of white or black 
the purer is the colour. Red mixed with white forms pink, whereas red 
mixed with black makes a kind of maroon. Yellow or orange becomes straw 
or brown according as it is mixed respectively with white or black. 

Colours of Bodies. — A substance is said to be of certain colour when it 
reflects or transmits rays of certain wave-lengths and absorbs the rest of the 
spectrum. Thus an object which absorbs the violet and green and reflects 
the red waves appears red; if it absorbs red waves and reflects green and 
violet it has a blue colour. A green body absorbs all but the green waves; 
one which is orange in colour reflects red and green and absorbs violet. The 
colour reflected by a body is usually the same as that which it transmits, but 
some bodies transmit the complementary colour to that which they reflect. 

Others, again, reflect and transmit different colours; thus, gold leaf trans- 
mits green. The colour of a body, whether opaque, translucent, or trans- 
parent, varies also to some extent, and sometimes greatly, with its thickness. 

A body which reflects light of all wave-lengths is called white; a body 
which has affinity for all the colours, so that all are absorbed and none re- 
flected, is called black. No body, however, is of a nature so chemically 
pure as to absorb entirely or reflect all the incident light. An absolutely 
black body does not exist in nature; even those coated with lamp-black and 
soot reflect some light, which renders them visible, and allows of theii form 
and solidity being recognised; on the blackest velvet still blacker shadows 
can be cast. Similarly, there is no object which reflects all the light it 
receives; pure, fresh snow, which is the whitest of all bodies, absorbs some 
15 per cent, of the light it receives, and white paper 20 or 30 per cent. Dark 
colours reflect little light, and slight differences between them are hardly 
appreciated in dull illumination; similarly, light colours reflect much light, 
and slight differences are hardly noticed in very bright illumination. The 
proportion of light reflected varies with the nature and colour of the body. 
Approximately a coloured body absorbs 50 to 80 per cent, of the light which 
falls on it. 


A yellow body will be seen longest as light is reduced and it can be seen 
further, although its colour may not be distinguishable. Generally speaking, 
as a characteristic and recognised colour, red is the most persistent of all; 
owing to its long wave-length it can be recognised at a greater distance than 
others, it freely penetrates haze, fog, or smoke glass, while the penetrations 
of other colours follow more or less in the order of the spectrum. For this 
reason red is employed as the danger signal, while blue-green is employed as 
the contrast signal on railways and ships. The sun appears redder at sun- 
rise, and sunset than at midday, also in fog, the blue-violet end of the 
spectrum being absorbed; the colour of light seen through a thick impure 
smoke glass is generally a brilliant red. 

White, grey and black are, in effect, the same, and really represent vary- 
ing degrees of luminosity, the only difference between them being in the total 
amount of light reflected. By all three the treatment of the different wave- 
lengths is the same, i.e. there is no selective property as with coloured bodies. 
The extent of the light absorption varies in the three cases, but the propor- 
tion of the components in the light reflected remains unaltered. 

White, being produced by the mixture of all colours, is the standard in 
brightness and luminosity, but this standard may be displaced, as when 
coloured illumination is used, or coloured glasses looked through. Black 
may be described as absence of colour and of light. 

Coloured Bodies and Lights. — The real colour of a body is that which it 
exhibits in daylight; it often appears of a quite different colour in artificial 
light in which some particular colour, usually red or orange, predominates, 
and therefore the mental standard of white is temporarily shifted towards 
that colour. Thus the exhibited colour of a body is dependent, to a great 
extent, on the nature of the luminant, and this is the more marked because 
the pigmentation of a body, from which its colour results is never pure in 
the sense that it reflects one wave-length only. In order to reflect a certain 
colour, the object must receive that colour in the light. 

The nearer the colour of the luminant approaches to that of the body 
the whiter will it appear; on the other hand should the colour of the luminant 
approach the complement of the body, the latter will appear darker than it 
would if viewed in white light. Should the light be of a colour exactly corre- 
sponding to that which the body absorbs, none will be reflected, and the 
body will consequently appear black. 

Of course a white body seen by coloured light is really coloured although 
it may be interpreted mentally as white. It certainly is so accepted if 
the colouration of the luminant is not excessive; thus by gas light a white 
paper is actually reddish-yellow, but we still call it white. Painting and 
matching colours is always difficult in artificial light; the difference between 
some blues and greens can barely be distinguished by gas light; and still less 
by lamp or candle light. Even if an artificial illumination is practically 
white it is unlikely to radiate all wave-lengths between 750 ju/x and 375 fjfi, 
so that, in it, coloured bodies would not exhibit their true colours, especially 


those whose colour is not in the light. In order to remedy the excess of red- 
orange in artificial lights many absorption screens have been devised, but the 
latest device for the production of artificial daylight is the invention of Mr. G. 
Sheringham which has been scientifically developed by Mr. L. C. Martin and 
Maj or A. Klein. It consists of a reflecting screen, which is coated with selected 
colours in definite proportion to area. All the light from the source is received 
by the screen and diffused therefrom, so that the solar light values of coloured 
bodies are exhibited. 

As illumination becomes progressively feeble all bodies lose theii distinc- 
tive colours, the latter being replaced by shades varying from light grey to 
black, and in a very dull illumination all appear equally grey. 

Coloured Glass. — Pure neutral or smoke glass absorbs part of all the 
component colours of white light; if not exactly neutral some one colour pene- 
trates it more than the others — generally red and sometimes green — and gives 
a distinct tint to a light seen through it. A glass of definite colour, as red 
or green, transmits not only its distinctive colour, but also some of the adjacent 
colours; thus green transmits some yellow and blue. Spectrum blue blocks 
out both the red and violet ends of the spectrum, and transmits blue, green and 
a little yellow. Cobalt-blue transmits blue and red, but blocks out green 
and yellow. Orange, amber, yellow and green-yellow glass absorb the violet 
and ultra-violet light. White crown, and still more, flint glass is absorptive 
for ultra-violet light, while quartz is specially transmissive for it. White 
glass absorbs also some of the infra-red, and nearly 15% of the visible light. 

Coloured Bodies and Glasses. — All colours are profoundly modified or 
changed when viewed throug'i coloured glass, as they are by coloured lights. 

A body viewed through a glass of the same colour appears white, or at 
least indistinguishable from a white obj ect seen through the same glass. Thus 
with red letters on a white ground, seen through red glass, the white back- 
ground appears the same colour as the letters, so that the whole field is of 
uniform tint ; here the colour of the glass is temporarily the mental standard 
of white. On looking at a red object on a green ground, through a piece of 
red glass, one sees a white object on a black ground. Similar phenomena 
result with other colours. 

If a coloured body be viewed through a coloured glass which absorbs 
the rays reflected by the body, the latter appears black. Thus a red body 
appears black through a green glass of the proper shade, the red rays reflected 
by the body not traversing the glass. If the ground be black, the object is 
barely distinguishable from the ground, or may not be at all, as in the 
"Friend" test. 

Superposition of Coloured Glasses. — Two coloured glasses placed together 
form an example of the subtractive process similar to the mixture of pigments. 
The first glass eliminates from incident white light all but its own colour, 
and if the second glass is the same as the first, no further alteration takes place, 
except a reduction in intensity. If the second glass is not of the same colour 



as the first, a certain amount of absorption by subtraction takes place in the 
second, and the more nearly complementary are the two glasses the more 
nearly will the whole of the incident light be cut off. For example, if a blue- 
green and a red, or an orange and blue glass, be placed together, the com- 
bination is opaque. Cobalt-blue and green glass, on being placed together, 
transmit original white light as blue, since blue is transmitted by each, but 
the remaining colours absorbed. Red, green and blue-violet, together 
absorb all visible rays, but light rose-red, yellow, and blue glasses transmit 
grey — i.e. a dull white. 

Transmissiveness of Coloured Glasses. — For the method of measuring this, 
and the photometry of coloured lights, see Chaj)ter II. 

The proportion of incident light transmitted depends on the thickness of 
the glass, and it is not easy to express variations, but approximately the 
transmission varies inversely as the square of the thickness. 

If a standard No. 6 smoke glass transmits 1/5 of the incident light, a 
second No. 6 placed behind transmits 1/5 of that transmitted by the first — 
i.e. 1/5 x 1/5=1/25 of the total light, originally incident on the first glass, is 
transmitted by the two together. 

If one glass absorbs 20% of the incident light, and another absorbs 30%, 
the total absorbed can be calculated from that which is transmitted, that is 
70% of 80% or 

70 80 56 ,,,„,.,,, 

, so that 44% is absorbed. 

ioo x ioo : 


Coloured glasses are numbered from 1 the lightest to, say, 10. No real 
standards are in general use, but those of the Optical Society are given below. 











Percentage of light transmitted . . 80 


50 40 







Standards are difficult to establish owing to the part played by thickness, 
and further on account of the uncertainty attending the product — i.e., melt- 
ing, etc., of coloured glass. 

Since a Cx. or Cc. lens varies in thickness from centre to periphery it 
cannot, if made of coloured glass, be of uniform tint throughout. The sub- 
jects of colour vision, coloured glasses, lenses, etc., are treated in "Visual 
Optics and Sight-Testing." 


Dispersion or Chromatism. — When white light suffers refraction, this is 
always accompanied by dispersion, because the component waves are deviated 
to different extents and become separated. The shorter waves, with rare ex- 
ceptions, are retarded, by the refracting medium, more than the longer waves. 
Reflection is not accompanied by dispersion. A body is said to be chromatic 
if it causes dispersion, and achromatic if it does not. 

Chromatism is due to the nature of the light, although its degree varies 
also with the nature of the refracting body and the kind of material of which 
it is made. There is no chromatism if the light is monochromatic, i.e. of one 
colour only, nor is there always chromatism if the light is polychromatic as 
with a plate or a corrected refracting body. 

Velocity of Light and Colour. — The velocity of light in free ether is the 
same for all colours, and is taken to be so in air, although this is not quite the 
case, blue being retarded slightly m:>re than red in its passage through the 
atmosphere. If Y ± be the velocity in air (about 300,000 km. per second) 
and V 2 that in a dense medium, then V 1 /V 2 =yU. 

V 2 here refers to the mean of the various wave-lengths which combine 
to form white light, and is represented by the yellow or D line of the spectrum. 
But V 2 is greater for red light (line A), and lower for violet (line H), so that 
[i also represents only the optical density of a medium for the D line. Every 
other line of the spectrum has a different ju which, for a given ordinary 
medium, is higher towards the violet, and lower towards the red end of the 
spectrum. Suppose in a medium ^=1-5, ^=1-51, ,a A =l-49. Then V D = 
300,000/1-5=200,000 km., V H =300,000/1-51=<200,000 km., and V A = 
300,000/1-49= >200, 000 km. per sec. 

Dispersive Index. — Each refracting medium has an index of dispersion, 
which represents the differences between the indices of refraction of the lines 
A and H of the spectrum. Thus, water has an index of refraction for the 
line A of 1-3289, and for the line H of 1-3434; and 1-3434 - l-3289=-0145, is 
the index of dispersion of water. 

Partial dispersion is the difference between the /u's of any two given lines 
of the spectrum. 

Mean dispersion is the difference between the indices of refraction of the 
lines C and F, i.e. between orange-red and blue, and is sometimes represented 
by 8; that is S=^ F -fi o . 




The dispersion of various kinds of glass differs with the materials used 
in their manufacture, and is more or less independent of their refracting power; 
the two examples given in the following table are merely representative. 
Some media of high mean lefraction have low dispersion, and vice versa; 
generally, however, high refractivity and high dispersivity accompany each 






ju = 1-3317 

[1*= 1-3378 





p ¥ = 1-3683 








Canada balsam 








. — 


Crown glass if 

fl a = 1-5376 

/x F = 1-5462 



Flint glass if . . 

(jl c = 1-6199 

/x F = 1-6335 





H?= 2-4355 



v or the Ratio of Refraction to Dispersion. — Since refraction and disper 
sion are more or less independent of each other, neither the total nor the mean 
dispersion indicates the optical properties of a medium; for this we must 
take the ratio between the mean refractivity (jj, d — 1) and the mean dispersivity 
{u v -/W )) which ratio is termed the refractive efficiency, denoted by the symbol 
v (nu), and expressed by 

The formula gives a value which, when compared with that of another 
medium, shows which of the two has the greater power for refracting with 
equal dispersion. It also enables us to calculate the components of an achro- 
matic prism or lens, and by its aid glasses can be tabulated in the order of 
their efficiencies, so that selection can be made for the purposes for which 
they are needed. 

A high value of v denotes high refraction and relatively low dispersion, 
while a low v indicates the reverse, i.e. a low refraction and relatively high 

Thus if in a variety of flint glass, ^=1-6, ^ =1-61, and / tt =l«59 the 
efficiency is 

1.6-1 -6 

"~1.61 - 1.59~.02~" ' 

If a certain crown glass has ^=1-525, // p =l -532 andyit =l«523 

" = .009 =6 ° ( a PP rox> ) 

These values of v, i.e. 30 and 60, show that in the flint the dispersion is 


relatively twice as great as in the crown; or, otherwise expressed, the crown 
has double the mean refraction of the flint for the same amount of dispersion. 
If two glasses have the same ju, but different dispersions, the one with the 
lower dispersion has the higher v. If two glasses have the same dispersion 
but different ju's, the one with the higher// has the higher v. 

In general flint refracts more than crown, but disperses still more, so that 
if a given crown and a given flint were compared it would be found that the 
flint has the higher (fi - 1), and still higher (ju^-fij, so that its v is lower 
than that of the crown. 

fj, D of water = 1.3336, and its mean dispersion = -0061, so that v is nearly 
55. With air /j =1.00029, and the mean dispersion is -0000029, so that v= 
100 (approx.). 

8 and A. — As stated above 8 represents ju r -/u , and A represents the 
difference between the v's of two different media, i.e. A=v 1 - v 2 . 

Expression for <■>. — Calculations with respect to chromatism are some- 
times based on w (omega), the dispersive power, which is the reciprocal of \>, 
and therefore 

W = — . 

Achromatism of a Plate. — When light is incident obliquely on a plate 
(parallel plane surfaces), although dispersion occurs at the first surface, 
it is neutralised at the second. 

Fig. 221. 

Let A B (Fig. 221) represent a beam of parallel light incident on, and 
refracted by, a plate. At B dispersion takes place, violet being deviated the 
most and red the least, and were it possible for the eye to receive the beam 
before it leaves the plate, the object would appear deviated and tinged with 
colour as with prism. At the second surface, however, all the dispersed rays 
are rendered parallel to each other, and therefore, by their overlapping on the 
retina, produce the sensation of white. In other words the appearance of the 
object, so far as dispersion is concerned, is the same as though viewed direct. 
In order to cause chromatism or dispersion, a medium must have the power 
of altering the line of travel of the various colours with respect to each other. 

When a prism or lens is achromatised its action is similar to that of a plate, 
while the course of light, as a whole, is changed. 



Chromatism of a Prism. 

Crown and Flint Prisms. — If a prism of crown and one of flint be taken, 
such that their mean deviations are equal, the spectrum produced by the 
flint is considerably the longer owing to the greater dispersive effect. If 
spectra of the same lengths be required, the crown glass prism must be stronger 
than the flint. 


Fig. 222. 

Virtual Spectrum. — A prism refracts violet waves most, and red least 
towards the base, as shown in Fig. 222, where L is the source of light. If the 
light be received by the eye, the rays are projected back to form a virtual 
spectrum, and the violet is nearest the edge and the red nearest the base. 
Thus, a disc of light viewed through a prism, base down, exhibits blue above 
and red below as shown by the dotted lines in Fig. 222. 

If a white body be viewed through a prism, the latter causes a series of 
separate images of the body to be formed, each characterised by a distinctive 
spectrum colour. These recombine in the centre so that a white virtual 
image is seen, but the ultimate displacements of blue at the one end, and of red 
at the other, cause a fringe of blue to appear on that border nearest the 
edge of the prism, and a red-orange fringe on that nearest the base. 

If the body is black or dark, as compared with its background, the red- 
orange fringe is towards the edge, and the blue fringe towards the base of the 
prism, these resulting from the dispersion of the light from the space or body 
surrounding the black. Thus a window bar viewed in daylight, through a 
prism base down, is blue at the bottom and i eddish-yellow on top, but if 
viewed by artificial light at night the colours are reversed. 

Dispersion of a Prism. — A beam of light, incident on a prism, is refracted 
towards the base, and since the retardation is greater -as the wave-length is 
shorter the blue is, as stated above, more deviated towards the base than the 
red, and the components are separated to form the band of colours known 
as the spectrum. 

The extent of the dispersion varies with the medium of which the prism 
is formed, with the angle of the prism, and with the angle of incidence of the 

The Refraction Spectrum. — The source should be the sun or a bright 
artificial luminant and the light should be admitted through a small horizontal 


aperture A (Fig. 223), preferably about 20 mm. long by «5 to 1 mm. wide 
placed parallel to the edge of the prism P. The light, thus admitted, is inci- 
dent on the prism placed in its path in the position of minimum deviation. 

Fig. 223. 

The resultant spectrum is received on a screen, but it is impure because adja- 
cent colours overlap each other. If, however, an achromatic bi-convex lens 
L be placed close to the prism, with the aperture and screen at approximately 
twice its focal distance on either side of it, the various colours are brought to 
a focus at the screen and a series of coloured real images of the slit are seen, 
forming together a pure refraction spectrum V Y R. If the prism be placed 
base up the violet is above and the red below, and vice versa. Although the 
different colours are well defined, the red end of the spectrum is crowded, 
while the blue is spread out. The lens projects a real image of the slit, and 
the prism produces from this single white image, an innumerable series of 
others corresponding to every wave-length. Much better results are, 
however, obtained with the spectroscope used for viewing and com- 
paring spectra, and the spectrometer for measuring the principal, deviating 
and dispersing angles of a prism. Their construction (q.v.) is given in 
Chapter XXVI. 

It is impossible to obtain a theoretically pure spectrum, since the source 
must be of some definite magnitude, and therefore a certain amount of over- 
lapping takes place between adjacent colours. The purity, however, reaches 
a high standard in the spectroscope where, in addition to the finest possible 
slit, the light received by the prism is parallel, so that prismatic distortion is 
eliminated. The spectrum produced by a given source can be studied and, 
if necessary, the spectra from two sources can, by suitable arrangement, be 
formed side by side for comparison. 

Spectrometry. — To measure the deviating angle the collimator C and 
telescope T are brought into line (Fig. 224) so that the image of the slit appears 
in the centre of the field of view, the objective of the telescope forming a real 
image of the slit in the focal plane of the ocular, through which it is viewed, 
and a reading is taken on the circle. The prism is then placed in position, 
and the telescope must be rotated to T' until the image of the slit can again 
be seen. The angular distance through which T is moved is the deviating 
angle of the prism, care being taken that the deviation is a minimum. This 



can be done by slightly rotating the prism backwards and forwards until a 
position is found when the slightest movement in either direction increases 
the deviation. 

Fjg. 224. 

Fig. 225. 

The principal angle of a prism is measured by turning the prism until its 
edge splits into two halves the beam of light issuing from the collimator 
(Fig. 225). The telescope is rotated to T until the image of the slit is seen 
reflected from the one surface, and then turned to T' to receive the image 
from the other surface of the prism. Half the angle through which the 
telescope has been rotated gives the principal angle of the prism. 

When the principal angle and the deviating angles are known, the refrac- 
tive index and the dispersion of the glass, of which the prism is made, can be 
calculated by the formulae given elsewhere. 

For very accurate determination of refractive index and dispersion, 
various incandescent gases are employed, which give line spectra, instead of 
a white source which produces a continuous spectrum. 

The mean deviation is indicated when the yellow of the spectrum lies on 
the cross wire placed in the focus of the ocular. The deviation of a prism, for 
any other colour, is determined by bringing that colour on to the cross wire. 
By this means, the refractive index, or the total, mean or partial dispersion 
of the medium, of which a prism is made, can be learnt; but the position of 
minimum deviation of the prism must, also, be found for each colour. 

The Diffraction Spectrum, which is purer than that of refraction, is men- 
tioned in Chapter XXV. 

Refraction and Dispersion. — As before stated, refraction by a simple 
medium is, so far as known, always accompanied by dispersion or chromatism. 
If a number of prisms of different substances, but of the same angle, be taken, 
those having the higher refractive index usually, but not of necessity, possess 
the longer spectra. A spectrum can, of course, extend beyond what is visible 
in the ordinary way; thus the photographic representation of the spectrum 
of a quartz prism is about three times as long as that of a crown prism. 

Different spectra can be made of the same length by altering the angles or 
the position of the prisms, or the pcsition of the screens. If (Fig. 226) the 



spectra be placed one under the other so that the B lines at the red and the 
H lines at the blue correspond in position, it will be found that the intermediate 
lines do not do so, rendering it difficult to fix the exact position of lines in the 




B C 



£ C 





a c 



Fig 226. 

spectrum. This want of coincidence of all the colours or the irregularity of 
sequence of the principal colours in any two spectra produced by different 
media, is called spectrum irrationality. 

Anomalous Dispersion. — In glass, water and most substances, the order 
of refrangibility is from the red through the orange, yellow, green, blue, 
indigo to violet, which is the most refrangible, but certain substances have 





the property of refracting the normally more refrangible rays less, and the 
less refrangible more (Fig. 227). This is called anomalous dispersion. The 
substances which exhibit this peculiarity usually possess what is termed 
surface colour, i.e. they have a different colour when viewed by reflected light 
from what they have by transmitted light. They reflect a certain colour, and 
the complementary colour is transmitted, and their spectra exhibit an absorp- 
tion band of more or less considerable dimensions, it being the space which 
would have been occupied by the reflected colour had it been transmitted. 
Such substances are termed dichroic. 

Most metals, except gold and copper, as well as many of the aniline pro- 
ducts, possess this abnormal dispersion, the order of the colours being changed. 
Moreover, Kundt found, in the aniline products, the dispersion abnormally 
increased on the red side of the band, but diminished on the violet side; 



so that in the case of fuchsin, for example, the red end, usually so short, is 
actually more extended than the violet end. 

Recomposition of Dispersed Light. — To recoinbine the dispersed colours 
of a prismatic spectrum and again form white light there can be 
employed — 

1. A prism of equal dispersive power placed in the path of the dispersed 
light, but having its base turned in the opposite direction to that of the first 
prism. (Newton's method.) 

2. A series of plane mirrors arranged so that each receives a different 
portion of the spectrum; from each the light is reflected to the same part of 
a screen, where the colours are recombined. 

3. The dispersed light is received on a concave mirror, from which it is 
reflected on to a screen ; then by rapidly oscillating the mirror the impression 
of white light is produced. Or the prism may be oscillated or rotated to pro- 
duce a similar effect without the interposition of the concave mirror. 

Any mechanical arrangement of rotation or oscillation by which the 
colours of the spectrum, whether produced by dispersion or by transmission, 
through coloured glasses, or by reflection from pigments, are caused to 
successively enter the eye with sufficient rapidity, produces the impression 
of white. Fresh colour sensations are caused while others are still existing, 
and the combination of all results in a sensation of white or grey. Colour 
tops, or discs, divided into sectors of different colours, are examples of this 

Angular Dispersion. — The deviating angle of a prism is that for the mean 
ray (D line), and is expressed (in the case of thin prisms) by cZ=P (fi- 1), 
where P is the refracting, and d the deviating angle. Now, since the red 
ray suffers less, and the blue greater refraction than the D line, their angular 
deviations are respectively 

d =V(/n -l), andrf F =P( / a F -l) 

d and d F being the deviating angles, and ( u and^ F being the indices of refrac- 
tion for red and blue light respectively. 

The angular dispersion of the prism expressed in degrees is then 

P(^ F -l)-P(/^-l)=P( A * F - Wc ) 

Fig. 228. 

Fig. 229. 

Fig. 230. 

If two similar prisms, A and B (Fig. 228) are placed in opposition — base to 
edge — their angles, refractive indices, and dispersions being the same, both 


the deviation and dispersion are neutralised, and all the rays emerge parallel 
to their original course. 

In Fig. 229 let the principal angle of a crown prism of ^=1'54 be 11'3°, 
and that of a flint prism of /^=1-61 be 10°. Their deviating angles arc the 
same, namely, 6-1 . 

If in the crown fj, Q = 1-5 34, ^=1-554, the dispersion =1 1 «3 x (1. 554 - 
1.534) =-226°. If in the flint ^=1-586, ^=1-62, the dispcrsion=10 x 
(1-62 - 1-586) =-34°. The resultant angular dispersion is therefore -34 - .226 
=.114°=6 / 50". Thus, while no deviation of the mean yellow ray occurs, 
the red and blue arc separated by an angle of nearly V. 

Achromatic Prism. — If a crown prism of 3°d and ^=1.54, and a flint of 
2°d and/i=l'61 (Fig. 230), having efficiencies of 45 and 30 respectively, be 
placed in opposition, they neutralise each other's dispersion, while there re- 
mains 1° deviation. Such prisms are said to be achromatized, i.e. they con- 
stitute an achromatic prism, which causes deviation without dispersion. 
The principal angle P of the crown is 3/-54=5.55°, and of the rlint 2/«61 = 
3-28°. Here, as will be seen from Fig. 230, every ray is deviated to the same 
extent, and the recombination of light is secured, as with a plate. 

To Calculate an Achromatic Prism. — Let d be the deviating angle of the 
required achromatic prism. Let d v v x and P x be those of the crown, and 
d 2 , v 2 an( i 1*2 those °f the flint components respectively. 

Now d=d 1 + d v and since they have to be in opposition d x may be regarded 
as positive and d 2 as negative. For achromatism to result 

v i/ v >2—di/ ( h or ^i v 2 = ~ ^z v i an( l ^L"2 +^2 , 'l == 
Or the condition for achromatism is 

P (^ F -^ ) of the crown=P ( ( « F -// C ) of the flint. 

To obtain the values of the two components d t and d v the deviating angle 

d of the required achromatic prism must be divided in proportion to the values 

of v x and v 2 > that is 

dv x - , d v . 2 
d x = , and d. z = 

v x - r' 2 " Vft ~ v \ 

It should be noticed that the deviating, not the principal angles enter into 
the formula?. The principal angles of the two components are found from 
Y=d/(/j, v - 1) which, however, holds good only for thin prisms; if strong, 
P t and P 2 must be found by the more complete formulae previously given. 

As an example, an achromatic prism of 5°d is needed, the glasses of the 
component parts being 

Crown . . 

.. ^=1-53 


// F =l-536 

Flint . . 

.. ^=1-63 


/V = 1-644, 


1-53-1 _'53 1-63-1 -63_ 

Vl "1.536 - L527 - ^009"" 8 * " 2_ l-644 - l-624 = -02 =31 * 5 

5x58-9 294-5 , rtW01 , ^ 10-7 
"'=58^3iT5=274 = 10 - 7 ° d ' and P >=^5 = 2 ° 

5x31-5 157-5 5-7 

^3T^5SWrr274=- 5 - 7 d ' aml P ==^= 9 ° 

rf=10-7 o -5-7 o =5 o . 

To find the Achromatising Prism. — The flint prism d 2 of v v which will 
neutralise the dispersion of a given crown of d x and v 1 is calculated from 

v i A2 ~ d>i/d>z or d 2 = d x Vg/vj 
Thus, let the crown be 10-7°d, v 2 =31-5, and v,=58-9, then 

^=10-7x31 -5/58-9 =5-7°d 
and d=d 1 +d 2 =10'7 - 5-7=5° 

P 2 can be found directly from P 2 S 2 — 1*i^j 

That is P x (/li f -fi c ) of the crown=P 2 ( /j f -fij of the flint. 

^ ^ (u„ -//J of crown 
Whence P 2 =P, f F ^°' f . - — 

Thus in the example above 20 x .009=9 x -02. 

Chromatism of a Lens. — The effect of dispersion, when the refracting 
body is a lens, is to bring the more refrangible blue and violet to a focus 
sooner than the less refrangible red and orange. This different focalisation 
of the various colours is termed chromatism, and the confusion of the image 
caused by it, chromatic aberration. The defect is made apparent by a fringe 
of colour on the edge of the real or virtual image projected by the lens. In- 
deed, lenses being similar in nature to prisms, produce similar chromatic 

An ordinary lens cannot be achromatic for a real image; but when it is 
used as a magnifier the virtual image is really composed of a series of images 
formed by every different colour, which series, being contained within the 
same visual angle, combine on the retina to form a single impression. This 
image, however, appears coloured at the edges, owing rather to the chromatic 
effects of spherical aberration, which is greater for blue than for red. If 
spherical aberration is entirely eliminated, the virtual image is colourless. 

If a horizontal white line (Fig. 231) be observed through the marginal 
portion of a convex lens, a blue- violet fringe will be seen on the side towards 
the edge of the lens, and a red-orange on the other, the blue being projected 
back beyond the red. Viewed through the periphery of a concave, the colours 
are reversed. Looking at a black line, the fringes are seen in the opposite 



order to those on a white line, for the reason given in connection with a 
prism. The centre of the image, whether virtual or real, of a white object, 

V Y R 

Fig. 231. 

Fig. 232. 

appears white, because the different colours are superposed, so that only at 
the extremities, where certain colours are not combined with others, is chro- 
matism apparent. 

Longitudinal and Lateral Aberrations of Colour. — In Fig. 232 a parallel 
beam of light from a point source is refracted by a convex lens; the various 
coloured rays meet at different distances behind the lens, the violet focussing 
at V, the yellow at Y, and the red at R. If a screen be held at V, the diffusion 
patch has a reddish-yellow fringe; the red and orange rays, being convergent 
to a more distant point R, impinge on the screen outside the blue and violet. 
If the screen be placed at R, the fringe becomes blue- violet, since these rays, 
having already met at V and crossed, impinge on the screen outside the red 
and orange. The distance V R is the longitudinal aberration, and the diameter 
a b of the disc of confusion in the plane where the extreme violet and red rays 
cross each other, is the lateral aberration ; this plane is very nearly that of 
F X, where the yellow (most luminous) light is brought to a focus. Here 
the circle formed by the red and blue discs being practically of the same size is 
termed the circle of least confusion. 

F of the Various Colours. — The index of refraction of a given medium 
refers to that of the D (sodium) line, which is situated in the yellow or most 
luminous part of the spectrum. With such a medium, if // D =l-54, the index 
of refraction for the red (line A) might be 1-53 (/^==1«53), while for the 
violet (line H) it might be 1-56 (/^ H =l-56). Suppose a thin double convex 
lens of 10 in. radius, then 


r lH 


"? =9.26 in. 

O'l+'i) (ft* -1 ) (10 + 10) x. 54 10-8 

which is the mean focal length for yellow light. 

Instead of ^=1-54 we must employ ^==1-53, and ^ =1«56 to find the 
focal lengths F A and F n for red and violet light respectively; thus 

F =943 in. and F =8-93 in. 

** H 


The difference in the focal lengths of a lens for red and blue light may 
be illustrated with a cobalt-blue glass (chromatic disc), which transmits red 
and blue light, but absorbs the central part of the spectrum, or by focussing 
with a convex lens light which is rendered monochromatic by being passed 
through respectively standard red and spectrum blue glass. The difference 
in the focal distances with these two coloured lights is sufficiently well marked 
to be appreciated. 

A positive and a negative lens of different dispersions which neutralise 
for white or yellow may not neutralise for red or blue light. 

Expression for Chromatic Aberration. — Let r x and r 2 represent the two 
radii, and F„ the focal length of a thin lens for the D line. Then, if F. and 
F H represent the focal lengths, and /u, A and /j. the indices for extreme red 
and violet respectively, the chromatic focal difference may be expressed by 

A H (ri+r t )(/* A -l)"'(r 1 +r 1 )( ftl -I) fa+rj (fi A "-l) (/* H -1) 

If instead of (^ H -l) [fZ A ~l) there be substituted (^ D -l) 2 > as may be 
done without sensible error, then the longitudinal chromatic aberration is 

F -F ^ ^(/^-^ -a) Jp f^-^ ^p, 
A H (h+r,) (^ D -l) 2 (^-1) ~v~ ° W 

The formula) for the refractive efficiency v, and for the dispersive power w, 
being the same as with a prism, 


As an example let F D =10 in., / tt A =l-60;// D =l-61 and^ H =l«625, then 

10 x (1-625 -1-60) -025 t . 

The lateral chromatic aberration of a lens=diameter of lens/2i/. 
Similar calculations can be used for a thick lens. 

Achromatic Lens. — Chromatism can be remedied by making the lens a 
combination of two different kinds of glass, so chosen that, while the disper- 
sion of the positive component is neutralised by that of the negative, there 
still remains some positive converging power, so that a real image may be 
formed. Such a combination is termed an achromatic lens, and usually con- 
sists of a flint concave and a crown convex. If a negative achromatic lens 
is required, as occurs sometimes in practice — for instance, in the telephoto 
le ns — then the concave is of crown and the convex of flint. 

Spectrum Lines Combined.^ — By an achromatic lens two selected lines of 
the spectrum, usually the C and F (orange-red and blue) are brought to a 
focus at the same distance; by uniting these with a third component a third 
line could also be focussed at the same distance, but for all practical pur- 


poses if the C and F lines, which lie near the more central and luminous part 
of the spectrum, are combined, the combination is one in which chromatism 
does not cause any appreciable blurring of the image, at least for visual 
purposes, in which critical definition is not essential. In photographic lenses 
the lines D and G, or D and H are usually selected in order to unite the violet, 
which is the most chemically active part of the visible spectrum, with the 
visual focus. For astro-photographic purposes, in which vision is of little 
consequence, the lines F and H (or beyond) are brought together. 

Formulae for an Achromatic Combination. — To calculate an achromatic 
combination for two lenses in contact, let F and G be the two lines of the 
spectrum which have to be brought to a common focus. F is the focal length 
of the required combination. F x and v x pertain to the crown component, and 
F 2 and v 2 to the flint; F 2 is negative, and 1/F=1/F X + 1/F 2 . 

In order that chromatism be eliminated 

1 1 _ 1 1 or Fu-F 1h _F 2a -F 2h 

Fi fl F u F 2n F 2A F u F lH F 2a F 2h 

But F u - F 1h = Fj/Vp and F 2a - F„ H = F„/i/ 2 , so without serious error, 
Fi A F ]H =F^ and F 2a F 2h =F 2 *. 

The last equation can then be written 

F, F 2 11 


vJS? v 2 F 2 2 Vl F ± v 2 F 2 

That is, Vl F 1 =- v ^F 2 and ¥ 1 v 1 + F 2 v 2 =0 

The two components l/F t and 1/F 2 are obtained by dividing 1/F pro- 
portionally to the two efficiencies v x and v z ; that is, 

F x F i'i - f 2 F (iq - v 2 ) F 2 F v 2 — vi F( l / 2 -j' 1 ) 


Fi=F^- 2 and F^F*^ 1 . 

l'l »' 2 

Example: a positive achromatic lens of 6| in. Fis required; the indices of 
refraction for the various lines are: — 

For the crown // =1-527, /* D =l-53, // F =l-536. 

For the flint ^=1-630, ^=1-635, ^=1-648. 

1-530-1 -530 B , 1-635-1 1-635 

^ = 1^3T^527 = -009 =58 ' 89 and ^ = 1.648^lT630 = ^lT =35 - 28 

Vl ~v 2 =58-89—35-28= ±23-61 

23-61 . -23-61 

Then F 1 =6-5 x ~^= +2-61 in. and F 2 =6-5 x - - - _ = - 4-358 in. 

= ! or F=6iin. 

F 2-61 4-358 6-5 



To find the Achromatising Cc. — The F of a Cc. of v 2 which, with a given 
Cx. of v\i will make the combination achromatic, is found from 

F 2 l 'i M v _ F l l 'l 

■=-' or F, 


Fj v 2 i 2 

Taking the same figures as in the previous example, if the Cx. has F= 
2-61 in., then 

F 2 =2-61 x 58-89/35-28=4-358. 

Dioptral Formulae. — Let D represent the power of the combination, D x 
and D, the powers respectively of the Cx. and Cc, v x and v 2 the respective 
efficiencies of the crown and flint lenses, v 2 being negative. 

In order to achromatise each other the relationship must be 

D x i' 2 =-D 2 vi or D 1 v 2 +~Do\> 1 =Q, and D=D 1 +D 2 . 
To obtain D 1 and D 2 , we must divide D proportionally to Vl and ,< 2 , that is, 

D x = — ±- and D 2 -- 

v x - v 2 v 2 - v x 

Taking the same glasses as in the previous example, where t> x =58-89, 
r 2 =35.28, and F=6|", or D=6 

D x =6 x 58-89/23-61 =14-97, and D 2 =6 x 35-28/ -23-61 = - 8-97 


These dioptral formulae are similar to those for achromatic prisms, and 
may be preferred to those involving F. 

To find the Achromatising Cc- — Since the powers of the two component 
lenses are proportional to their efficiencies, if „ 2 =60, and v 2 =50, a + 6 D 
and a - 5 D will together make an achromatic + ID. 

If D, the power of the convex, is known, and it is needed to calculate the 
concave required to make it achromatic, the formulae are 

L\ V-, ^ ^ Vo 

X =J or D 2 =D X - 2 
D 2 v 2 v t 

As in the foregoing example, if the crown is + 14-97, the flint is 

D 2 =14-97 x 35-28/58-88=8-97 

Example. — Given an equi-cx. lens, of crown glass, of radius 10 in., there 
is needed to calculate the radius of curvature of a flint Co. so that the two 
combined make an achromatic combination. 

u -1 -5175 

For the crown u =1-5175; u w -^ =-0087, and ^=£-5 = =59. 

D F ° ^-f^a '° 087 

a -I -571 
For the flint ^=1-571; // r -// c =-01327, and , a =^_=_ ^=43. 


Now =.5175 x (— + — )=r-s^ for the Cx. 

F x \J0 10/ 9-662 

1 1 43 43 1 . xl _. 

and .= = x = = for the Cc. 

F 2 9-662 59 570-058 13-257 

1 1 1 3-595 1 „„*„„. 

then -,= _ = ■== or F=35-63 ins. 

F 9-662 13-257 128-089 35-63 

Now, the radii of curvature of the two adjacent surfaces must be equal, 
that is, 10 in. Therefore r, the second radius of the Cc, is found from 

- lOr 

-13-257=; — — so that r=- 31-15 in. 


Example. — A plano-Cx. achromatic combination is required of F=20 in. 
Let the glasses be 

^t c =l-535, ^=1-54, //, p =l-555 for the crown, 

^=1-59, ^ D =l-60, A/ F =l-63 for the flint. 

Then v 1 =-54/-02=27, and „ 2 =-60/.04=15 

12 -12 

F.=20x— =8-88 Cx. and F 2 =20x =16 Cc. 

1 27 2 15 

, - - , ^ -16x8-88 

lhe combination has F= — — 5-^= +20 in. 

- 16 + 8-88 

If the one surface of the Cc. is piano, the other is 

r= - 16 x (1-6-1)= -9-6 in. 

The Cx. must have one surface of radius 9-6 in., and the other — 

r x 9-6 9-6 r 

8-88= = or r=9-6" (approx.). 

-54x(r + 9-6) -54 r + 5-184 v n ' 

The positive lens is a double Cx. ; it is combined with a plano-Cc. 

Illustrating the Dioptral Formulae. — With data as above, since 20 in.= 
2 D w.e have 

D 1= 2x 27/12=4-5 and D 2 =2 x - 15/12= -2-5 

The Cc. having one surface piano, the other surface has 

100 x (1-6-1) 

r= 1— -= - 24 Cm. 


The one surface of the Cx. has r=24 Cm., and since 

100(M-l)(r + r') 100x-54x(24+r) 

D= - we have 4-5= — — — 

r r 24r 


Whence r=24 Cm. As before, there is a DCx. lens of r=24 Cm. and a 
plano-Cc. of r=-24 Cm. 

Chromatic Difficulties. — A combination may bring different coloured rays 
to the same focus, but the images may not be of the same size. 

A combination achromatic for an axial pencil of light may not be so for 
oblique pencils. 

A combination achromatised for light proceeding from a given plane may 
not be so for light proceeding from other planes. 

Irrationality of Dispersion. — If with an achromatic lens, the C and F (or 

D and H) lines coincide, other lines do not. This is called irrationality oj 
dispersion, and the dispersion which thus remains in an achromatic lens is 
residual or secondary, but as stated, it suffices, for practical purposes, to unite 
two certain lines of the spectrum according to the use to which the lens is 
put. With modern glasses, and by careful selection, it is possible to unite 
practically three spectrum lines with two glasses, but a real common focus 
for all colours is impossible at present. 

Apochromatic Lens. — A combination which actually unites three lines of 
the spectrum is termed apochromatic ; for such a lens at least three different 
sorts of glasses must be employed, the residual spectrum still left being so 
small as to be negligible. For such a combination 

F = F + F + F aud F i"i+ F 2i' 2 +F 3 v 3 =0. 

Lens Combinations. — A combination of lenses, having one achromatised 
component, is not perfectly achromatic; in order that it may be so the achro- 
matised component must be suitably overcorrected. When lenses are 
separated the conditions for achromatising are different. 

Two lenses of the same material may be achromatic, for virtual images, 
as is the case with Huyghen's eye-piece. Those rays which pass through 
the thin part of the field lens pass through a thicker part of the eye lens; 
the violet, being relatively nearer to the axis than the red, is less refracted, 
and all the components of white light emerge under the same visual angle. 
Thus, two Cx. lenses of equal v separated by a distance equal to (F x +F 2 )/2 
form an achromatic combination for virtual images. 


Prismatic Aberrations of Form. 

Small Light Pencils.— A pencil of light parallel before refraction is parallel 
after refraction by a prism; if divergent or convergent, it is taken to be 
similarly divergent or convergent after refraction, provided the pencil of 
light is small, and the axial ray suffers minimum deviation. Also the prism 
itself must be of comparatively small angle. 

Large Light Pencils. — In Fig. 233, which is purposely exaggerated for the 
sake of clearness, let a wide pencil of light diverge from a point L, of which 
L E is the central ray, presumed to suffer minimum deviation, and L D, L F, 
are extreme rays incident on the surface of the prism in the base-apex plane. 

These rays suffer unequal deviation towards M, and N respectively, and if 
L E is at minimum deviation, the others cannot be so and are deviated 
relatively more than L E, which is travelling in the direction O'O. Both, when 
produced backwards, cut O'O nearer than 0', but L F, being more deviated 
cuts it in N', while L D cuts it in M'. 

The incidence of rays L Q and LP in a, plane parallel to the axis, is also 
greater than that of L E, but the difference is much les3 than in the base- 
apex plane; the refracted rays T X and R Y, when produced backwards, 
meet in 0', which is nearer to the prism than the original source L. 

Thus rays in the pencil emanating from a point do not have a point- 
image, there being two focal lines, the one nearer the prism being parallel 
to the axis, and the other parallel to the base-apex plane of the prism. A 
circle of least confusion, which lies between 0' and N', may be regarded as the 
image. These defects blur the image and cause it to appear nearer than it 



actually is, and if the prism is in such a position that L F or L D suffers 
minimum deviation, the whole of the pencil is rendered still more divergent 
and the image is still more blurred and nearer. In consequence the position 
of minimum deviation for a near object differs from that for a distant one. 

Aberrations of a Prism. — Although, in a prism of small angle, the effects 
of aberration due to its form can be ignored, considerable distortion of the 
image is produced by a strong prism. 

The distortion of image, seen through a prism, is due in general to (a) vary- 
ing incidence of the light in a plane, (b) varying incidence in one plane as 
compared with another, and (c) varying incidence of different pencils. Chro- 
matism also plays a part in this connection, (a) is the origin of coma in a lens, 
(b) is the genesis of radial astigmatism, (b) and (c) of curvature, and (c) of 

Distortion increases with the nearness of the object, when light is very 
divergent; if the object is distant the light is parallel, so that (a) above dis- 
appears and (6) is not so marked. 

Distortion increases with the size of the object. If a narrow pencil of light 
from the centre of an object enters the eye through a prism, and suffers mini- 
mum deviation and but little aberration, the pencils from other points cannot 
do so; the peripheral portions of a large object are blurred compared with 
the centre. Size of object is also the main factor in thickness, which follows. 

Distortion is caused by the greater thickness of the prism through which 
oblique pencils pass from the extremities of an object. These pencils suffer 
more deviation than the central pencils, and therefore appear to come from 
points relatively more distant from the centre than those nearer to the centre 
of the object viewed. Thus a straight line, parallel to the edge, appears curved 
with its convexity towards the base. A square object has its two sides, 
which are parallel to the edge of the prism, concave to the latter direction. 

Distortion is caused, or increased, by abnormal position of the base-apex 
plane which causes pencils to have varying obliquity. If the base-apex line 
is vertical, say edge up, the vertical magnitude of a square object, whether 
near or distant, appears increased when the edge of the prism is nearer to it 
than the base, while the vertical dimension is lessened if the base is nearer the 
object. The effect increases with the inclination, as does also the total devia- 
tion of the image in both cases, unless the object is relatively near. 

If the prism be rotated around its base-apex line — i.e. if, say, a vertical 
prism, edge upwards, be rotated so that one side of the prism is nearer the 
object than the other — the image is lengthened diagonally, being drawn out 
more towards the edge than the base and more on one side than the other, 
so that a square object appears as a distorted parallelogram. 

Lens Aberrations of Form. 

Apart from chromatism, the image formed by a spherical lens suffers 
from five aberrations due to its shape, and these must be severally corrected 
before the lens is capable of forming a geometrically perfect image of an 



object. The first is spherical aberration, the second coma, the third radial 
astigmatism, the fourth curvature of the field, the fifth distortion. 

The first three errors mentioned are 'point aberrations, and lenses corrected 
for them are called stigmatic as distinct from astigmatic ; a lens corrected for 
spherical aberration is termed aplanatic. The last two errors are aberrations 
of a plane, and lenses free from them are termed rectilinear or orthoscopic. 
Form aberrations, in general, are lessened by (a) employing a stop or dia- 
phragm, (b) using some special form of single lens, or (c) using a combina- 
tion instead of a single lens. 

Spherical Aberration. — Since a lens may be regarded as consisting of an 
infinite number of prisms whose angles of inclination increase with the dis- 
tance from the axis, it follows that the deviation effected by the various zones 
of a lens depends on this distance. In a Cx. lens the varying inclination of 
opposite points on the two surfaces, in each meridian, causes parallel light 
to converge, in theory, to a point, but actually, the refraction of a spherical 
lens is such that light from a point is not brought to a focus at a single point, 
the rays transmitted by the marginal zones of the lens meeting sooner than 
those transmitted nearer the centre, as depicted in Fig. 234. 

Fig. 234. 

Each zone of a lens has its own focal length, varying from the principal 
focus F, for rays refracted in the zones immediately surrounding the prin- 
cipal axis, to a point where rays A and B passing through the most external 
zones, meet the axis. The inability to unite in a single point all the rays 
diverging from an object-point on the principal axis is called spherical aberra- 
tion, which is due, not to the fact that the deviating power is greater towards 

Fig. 235. 

the periphery, for that is a natural property of a lens, but to the fact that 
the deviating power increases too rapidly towards the periphery, with the 
result that wave fronts are not truly spherical after refraction. 

In Fig. 235 the opposite points D and E of the lens constitute a portion 




of a prism G K H, and the ray A D, incident such that its point of incidence D 
and its point of emergence E are equidistant from the edge, therefore suffers 
minimum deviation, this latter occurring .when the refraction of the ray is 
shared equally between the two surfaces. The deviation of the ray ABC 
proceeding from the same point, and refracted by the prismatic element B C, 
is not minimum, and is relatively more bent from its course than the ray A D. 
It is mainly owing to the departure from minimum deviation incidence of the 
light at the periphery that the deviating power there is unduly increased and 
spherical aberration produced. For parallel light the angle of incidence in- 
creases as the tangent of the angle, whereas for aplanatic refraction it should 
increase as the arc. 

Central and Peripheral Refraction. — When the peripheral part of a lens 
(Fig. 236) is blocked out only the central area of the lens is effective, and 
parallel rays, as a whole, meet slightly within F. When the central portion 
of the lens is covered (Fig. 237) and only the periphery acts on the light, 
the latter, as a whole, meets still further within F. 


Fig. 236. 

Fig. 237. 

Circle of Least Confusion. — When the whole lens is exposed to the light 
(Fig. 234), the converging circles of confusion from the central, and the 
diverging circles from the peripheral area, are of about the same mean diameter 
at C, the circle of least confusion; here the disc of light is of minimum size. 
At any point either nearer or further the disc is larger than at C, 
but the greatest concentration of light occurs at F, where the image of a 
luminous point is a bright spot, surrounded by a halo caused by the diverging 
light from the periphery of the lens. The true focus F is the most distant of 
the series of foci shown in Fig. 234, and is that due to refraction by that area 
of the lens immediately surrounding the principal axis. 

The distance of the image from a Cx. lens in the three cases where the 
periphery only, the centre only, or the whole of the lens is effective, can be 
shown by experiment, the object being a bright source placed behind a small 
aperture covered by a piece of yellow glass in order to make the light more 
or less monochromatic. 

Longitudinal and Lateral Aberration. — The distance between the ex- 
treme foci is the longitudinal aberration; the diameter of the confusion disc 
A B (Fig. 234), when the screen is in the theoretical focus, is the lateral aberra- 
tion. The lateral aberration increases more rapidly than the longitudinal 
with an increase in the aperture of a lens, the latter varying as the square 
of the aperture, and the former as the cube of the aperture. 



Influencing Factors.— The definition of an image depends on the small- 
ness of the circles of confusion of which it is constituted, and these circles 
are dependent on the degree of spherical aberration. The latter varies with 
the incidence of the light, the aperture, form, index, and thickness of the 
lens; as these factors are changed spherical aberration is increased or decreased. 

Via. 233. 

Fia. 239. 

Best Form of Single Lens. — Spherical aberration is least when the rays in 
general are, after refraction at the first surface, more nearly parallel to the 
bases of the virtual prisms of which the lens is formed, so that the total 
refraction is approximately equally divided between the tivo surfaces. 

As a general rule, for parallel light, the more curved the front, and the less 
curved the back surface of the lens, the smaller is the spherical aberration 
(Fig. 238); as the object is nearer the lens and the light becomes more and 
more divergent less curvature is needed for the front, and more for the back 
surface. In these cases an approach to minimum deviation at the periphery 
of the lens is obtained. A very high degree of spherical aberration results 
if the less curved surface is exposed to parallel light (Fig. 239), or the more 
curved surface to light diverging from the focus of the lens, for then a consider- 
able departure from minimum deviation for peripheral rays occurs. Since 
the incidence varies with the distance of the object, spherical aberration de- 
pends not only on the form of a lens, but also on the distance of the source 
from that lens. 

The plano-convex, or better, the crossed lens (having surface powers in 
the ratio of about 6 to 1), with its more curved surface turned to the light, 
is the form of single lens which gives the best definition for objects at extreme 
distances. The same lens turned the other way is the best for very near 
objects, while the double convex is the best when the incident rays diverge 
from twice the focal distance, for then, object and image being equidistant 
from the lens, the incident and emergent rays form equal angles with the two 
surfaces. If used for all distances the double Cx. is perhaps the best form 
of single lens. 

To obtain minimum spherical aberration in a single lens the radii of the 
two surfaces should be in the ratio of 1 + 2/u, and 1 - 2 ft +4:/ju. These quanti- 
ties, when/^^1'5, are as 6 is to 1, giving the crossed lens previously mentioned. 
When ^=1-686, the value of 1 -2ju+i/fx is 0, so that the one surface should 
be piano, and if the index is higher, this quantity being negative, the lens 
must be a meniscus. 



A Numerical Expression for Longitudinal Aberration is sometimes given, 
as below, for parallel light and thin lenses, where /.*= 1-5. The values are 
in terms of d % F, where d is the semi-diameter of the lens. 

A crossed Cx. with the more curved surface to the light 
A plano-Cx., with the curved surface to the light . . 
An equi-Cx. 

A crossed Cx. with the less curved surface to the light 
A plano-Cx. with the plane surface to the light 

These values vary with the index of refraction with the thickness of the 
lens, and for different distances of the source of light. 



Fig. 240. 

Least Time. — Since light travels in a straight line it takes the least pos- 
sible time to reach a given point, and this principle of least time holds good 
for refraction. Thus, various rays diverging from a point in air and passing 
into another denser medium must arrive at the same point, at the same 
time, if a point focus is to be obtained. With a lens, disregarding spherical 
aberration, this occurs because, although the distance from A toB, and thence 
to F, is greater than from A to C and F (Fig. 240), yet the distance traversed 
in the denser medium is greater in the case of A C F. The law of refraction 
fa sin i=(JL 2 sin r is in accordance with the principle of least time. If a lens 
is corrected for spherical aberration all rays diverging from an object-point 
must reach the same image-point and in the same time, no matter what course 
they take. In other words the optical length (which is the actual distance 
of travel multiplied by the yt of the medium in which this takes place) must 
be the same for all rays between the object and image points. 

Fig. 241. 

Let the distance of A from any point on the refracting surface (Fig. 241) 
be d v and the corresponding distance of F be d 2 ; then d 1 /n 1 +d 2 j.i 2 is the 


optical length of any ray diverging from A and refracted to F, so that for 
AX, AB and A C to meet at F it would be necessary that d x ju 1 + d 2 /u. 2 be 
a constant for any incidence of the light, i.e. A B (x l + B F fi 2 =A C / a 1 + 
C F /u 2 =A X (x x +X F ju 2 . As this cannot occur with spherical surfaces, 
spherical aberration may be said to be due to the fact that all the rays diverg- 
ing from a point on the axis cannot reach the same point in a given time, 
or rather that, within a given time, the rays reach different points of the axis. 
In the case of a lens the influence of the two surfaces has to be con- 
sidered, since each ray travels in three different media. If d x be its course 
in the first medium/^, d 2 its course in the second medium/^, and d z its course 
in the third medium fi v then d x jLt^ + d 2 jli 2 + d 3 /n s would need to be the same 
for each ray in order that all rays diverging from an object-point may meet, 
after refraction, at a single image-point. 

Fig. 242. 

Influence of Thickness. — A ray A B traversing a thick lens (Fig. 239) is 
retarded in the denser medium, and can only reach, in a given time, a point 
G on the principal axis which lies nearer to the lens than H, the point reached 
by a similar ray passing through a thin lens. Thus, spherical aberration 
increases with the thickness of the lens. 

Remedies. — A theoretical remedy would be found if the speed of the 
light could be increased, or the refractive power of the lens decreased at the 
periphery. This would necessitate the lens being made of a medium whose 
index of refraction decreases as the distance from the principal axis increases, 
which occurs in the crystalline lens of the eye. Or the lens would need to 
have less curvature at the periphery than at the centre, i.e. one having some 
curve other than spherical. 

The practical remedy for spherical aberration of a single lens is the em- 
ployment of a stop or diaphragm used in combination with the lens, the mar- 
ginal rays are then cut off and spherical aberration is consequently lessened. 
The same result is obtained by making the lens of small diameter. 

In general, spherical aberration is less as the number of surfaces sharing 
the refraction is increased. Thus two positive lenses may be employed in the 
place of one, for the same refractive power, or the positive and negative com- 
ponents of a system separated by an interval, a principle sometimes made use 
of in photographic and microscope objectives. As a rule an achromatic com- 


bination has little spherical aberration, or it may be eliminated altogether, 
the positive and negative aberrations of the component lenses neutralizing 
each other, as do their dispersions. In practice this method affords the only 
true means of correction. 

Aplanatic Lens. — A lens, or lens combination, corrected for spherical 
aberration is termed aplanatic, but no combination can be rendered entirely 
aplanatic for all distances of the object, nor can it be for other than mono- 
chromatic light; but by employing a stop, as is done in most optical instru- 
ments, and a judicious choice of combination and of the form of the individual 
components, it may be rendered so for practical purposes. A single surface 
may be aplanatic, also a single spherical lens, but only for one distance of 
object (vide Aplanatism at end of this Chapter). 

Positive and Negative Aberration. — Positive aberration obtains when the 
marginal rays come to a focus before the central, negative aberration if the 
central rays come to a focus before the marginal. 

Under and Over Correction. — A lens combination which partially neu- 
tralises the positive aberration is under-corrected, and if it more than neutralizes 
the positive, it produces negative aberration, and is said to be over-corrected. 
In photographic lenses it may happen that spherical aberration is com- 
pletely eliminated for the axis and periphery, while it may still occur in the 
intermediate zones. 

The Oblique Aberrations. — A beam of light diverging from a point on the 
principal axis would, on passing through a lens corrected for spherical and 
central chromatic aberration, meet again as a point on the principal axis. 
When, however, the luminous point is situated on a secondary axis, further 
aberrations are introduced by the oblique incidence of the light, these being 
the point aberrations coma and radial astigmatism, and the plane and line 
aberrations curvature of field and distortion. 

If a small bright source be placed obliquely below the axis of a lens and 
a white screen moved behind it, the image is blurred at all distances, assuming 
various comet-shaped, cup-shaped, and pear-shaped figures, which are the 
result of coma. If coma be reduced by placing a fairly small diaphragm in 
front of the lens and the screen is held within the focus, and slowly drawn 
away, the image is seen to form a symmetrical ellipse, and then successively 
a horizontal line, a horizontal ellipse, an irregular circle, a vertical ellipse, a 
vertical line, and finally broadens out into a blurred patch. These lines 
result from radial astigmatism. 

Coma is an aberration produced by the unequal refracting effect of the 
different parts of the various meridians of a lens, on an oblique pencil of light; 
it is spherical aberration for oblique light and is, of course, more pronounced 
as the axis of the incident pencil is more oblique. 

Instead of a point-image of a point-object, situated on a secondary axis, 
there results a blurred pear or comet shaped halo of confusion partly surround- 
ing a bright point, the latter being directed towards the axis. The halo 


spreads away from the axis because the aberration is caused mainly by the 
part of the lens nearest the source. 

The confusion disc produced by coma is asymmetrical, whereas the con- 
fusion disc of spherical aberration is symmetrical with respect to the axis 
of the beam of light. 

Fig. 243. 

Let d and e (Fig. 243) be rays proceeding from a distant point on an 
oblique axis A B. The ray e meets the surface of the lens sooner than d, 
and since e departs more from minimum deviation than does d, the ray e e' 
cuts the axial ray at e" sooner than does d d' at d" . 

Influencing Factors. — Coma is increased in direct proportion to the aper- 
ture of the lens. It varies also with the form and, in general, whatever tends 
to increase spherical aberration tends also to increase coma. 

Remedies. — Coma is reduced by the use of plano-Cx. and meniscus lenses, 
for the reason that less refraction takes place at the second surface. The chief 
remedy is the employment of a stop, especially if this be placed a short dis- 
tance from the concave surface of a meniscus. The effective aperture of the 
lens is thus reduced, the portions producing the aberration being practically 
cut out. 

The Sine Condition.---For coma to be eliminated, the sines of the angle, 
a and a' formed by an incident ray with the axis, before and after refraction 
should have a constant ratio; i.e. sin a/sin a'=a constant (Fig. 243). 

Radial Astigmatism is an aberration which results from the unequal refrac- 
tion of different meridians of a lens on an oblique pencil of light; it is, naturally, 
more marked as the axis of the incident pencil is more oblique. 

Instead of a point-image of a point-object situated on a secondary axis, 
there are two line-foci through which pass all the rays contained in the pencil. 

For every oblique axis there are two principal meridians or planes; the 
first is that containing the oblique axis and the principal axis; the second is 
that which, while containing the secondary axis, is at right angles to the 
first. * 

* The terras sagittal, and meridional, tangential and radial, used in the previous 
edition of " General and Practical Optics," have been dropped in favour of first and 
second bocauso the former terms were sometimes confused. 



In Fig. 244 let a pencil of light be incident on a lens from a distant point 
A, situated on the secondary axis AX; then S S' is the first and M W the 
second plane, in this case S S' being vertical and M M' horizontal. All rays 
in a first plane as g, and c, b and d, meet in points along the line T T', which 
is the first (tangential) focal line, whence, diverging in one direction and con- 
verging in the other, they continue to the second (radial) focal line R R'. 

Fig. 244. 

Thus the first line is the focus of the first plane, while the second line is that of 
the second plane, each focal line being at right angles to the plane of which 
it is the focus, and therefore corresponds in direction to the other principal 

T is the meeting-point of a and c, while T' is that of b and d in the first 
focal line; R is the meeting-point of c and d, while R' is that of a and b in the 
second focal line. 

In the second plane the light has to traverse a greater thickness of the lens 
than does an axial pencil; and the greater obliquity increases the angles of 
incidence so that the light is rendered more convergent, and has its focus 
nearer the lens than the focal plane. In the first plane the light has a still 
greater thickness to traverse, and is still more oblique as a whole than in the 
.second plane, and therefore its focus is still nearer the lens. Consequently 
radial astigmatism is due to the increased angles of incidence of oblique light, 
and increased effective thickness of the lens. 

The astigmatism is essentially the interval between the focal lines produced 
by the difference in the effective powers of the lens in the first and second 
planes of incidence. Between the two focal lines there is a position where 
the cross-section of the refracted light is most nearly circular, and this — 
the circle of least confusion — may be regarded as the mean focus of the oblique 
pencil of light. The calculation for the distances of T T' and R R' are shown 
in Chapter XXII., where they are termed ¥ 1 and F 2 respectively. 

To illustrate oblique refraction, let Fig. 245 represent the focal plane of 
a Cx. lens viewed from behind. Rays parallel to the principal axis, and 



directed before refraction to the points ab c and d, are refracted towards and 
meet in the point F. If the rays are parallel to an oblique axis, as in Fig. 244, 
a meets c in T and 6 in R', while d meets c in R and b in T', but 
T T', as stated, lies nearer the lens than R R f , and both are nearer than F. 

Fig. 245. 

Radial astigmatism has been illustrated with light diverging from a 
point on the lower edge of an object, so that the resulting first (tangential) 
focal line is horizontal and the second (radial) line is vertical. If the luminous 
point is to the right or left of the object, the first line is vertical and the second 
line horizontal; if the first plane is oblique both lines are oblique, there being 
a pair of astigmatic lines at right angles for each secondary axis. 

Fig. 246. 

The first and second focal lines on the numberless secondary axes 
constitute two curved surfaces T T and R R' respectively and (Fig. 246) 
both are nearer than F ; but at the principal axis they meet and form a point 
in the focal plane, where the two focal lines fuse into a point-image. The 
field of circles of least confusion form a surface 0', concave towards the 
lens, lying between R R' and T T', and this may be regarded as the focal 
plane of an ordinary lens (see Curvature of Field). 

Influencing Factors.— Radial astigmatism is greater as the lens aperture 
is larger. It varies also with the form of the lens, and the more nearly this 
is of double Cx. form the more marked it is. 

Remedies. — Radial astigmatism is lessened by employing a plano-Cx. 
or a meniscus, especially the latter, combined with a stop placed at some 
little distance — about a fifth the focal length — on the concave side. The 


stop cuts off extreme peripheral rays and so makes both focal lines shorter 
in length and more nearly equal. They are also receded so that the circle 
of least confusion lies more nearly in the focal plane. By still further 
displacing the stop away from the lens both lines may even be thrown 
behind the focal plane. 

By combining glasses of high refractive power and low dispersion with those 
of opposite quality certain conditions are fulfilled which, besides eliminating 
chromatism, correct astigmatism over a wide area. With the newer varieties 
of optical glass a degree of correction is secured which was not possible with 
the older kinds, wherein refractivity and dispersion were more or less propor- 

Sphero-Cyl. Lens. — The difference between the astigmatism of a sphero- 
cylindrical and the radial astigmatism of a spherical lens, is that the former 
is due to the varying curvature of the lens, the focal lines being formed on the 
principal axis; while the latter is due to the oblique incidence of the light, the 
focal lines lying on a secondary axis. Otherwise the general result, that is, 
the production of two focal lines instead of a focal point, is very similar in the 
two cases. 

Curvature of the Field. — As stated under Radial Astigmatism, if A be a 
point on the lower extremity of an object the light diverging from it, after 
refraction by the lens, forms two focal lines, and between them is situated the 
circle of least confusion, which may be regarded as the focus of the rays diverg- 
ing from A. On the surface containing the circles of least confusion of all 
the object-points, the sharpest image of the periphery of the object is formed, 
and since the effective power of a lens is greater as the light is more oblique, 
this surface forms a portion of a sphere with its concave surface towards the 
lens. This curvature of the field is partly due to radial astigmatism (see Figs. 
244 and 246). 

Radial astigmatism is, however, not the sole cause of curvature, for if 
T T (Fig. 246), the field of the first lines, were made to coincide with R R', 
that of the second, the combined suiface would still be curved. 

Again, even if all the peripheral foci were at the same distance from 
the optical centre (or second equivalent point) as the focus on the principal 
axis they would together form a portion of a spherical surface whose radius 
is equal to F of the lens, so that curvature would still remain. Thus, a sphere 
is entirely free from astigmatism, but the field is nevertheless curved. There- 
fore, if the image of an ordinary object formed by a lens is projected on to a 
flat screen, either the centre or the periphery may be focussed, but it is im- 
possible to obtain a good definition of both at the same time. The image 
of a convex object would be still more curved than that of a flat one, but a 
concave object might be so placed as to have a flat image. 

Remedies. — To flatten the field, radial astigmatism should be eliminated, 
and the oblique foci lengthened. 

For the former the remedies are as for radial astigmatism — namely, a 
meniscus lens with a stop on the concave side. 



A stop, by narrowing the beam on a secondary axis, causes the focus, 
represented by the disc of least confusion, to be formed at a distance, depen- 
dent on the form of the lens, at which curvature is a minimum. This, for 
single lenses, is generally about one-fifth the focal length on the Cc. side as 
for radial astigmatism. 

If a Cx. and a Cc. of equal power be separated to have convex effect, 
the distance can be so adjusted as to make the image flat. The oblique 
rays, after refraction by the convex, meet the concave nearer to the periphery, 
and the convergence is thereby lessened; therefore the final convergence is 
to a point further away, for oblique pencils, than would be the case after 
refraction by a single Cx. lens, whose power is equal to that of the combination. 

An almost perfectly flat virtual image is obtained with the Ramsden eye- 
piece where two equal plano-convex lenses have their convex surfaces facing 
each other. Or by the Huyghen eye-piece formed of two plano-convex lenses, 
whose respective focal distances are as 1 and 3, both curved surfaces facing the 
same way. 

Curvature is said to be under-corrected, or positive, when the image is 
concave towards the lens, and negative if, by over-correction, the image 
becomes convex. 

The Petzval Condition. — In order that a combination of two lenses may 
form a flat image, the condition which must be satisfied is that F 1 fa + F 2 fa 
=0, where ^ and F x refer to the crown, and fa and F 2 to the flint components 
respectively. In order that this shall not controvert the condition for achro- 
matism, which is F x v y +F 2 i' 2 =0, the crown, with less dispersion, must have 
a higher refractive index than the flint, a condition already referred to in the 
section on radial astigmatism. In this case v 1 /v 2 =fa/fa- 

A Flat Image obtains, if the focal length of each oblique pencil is equal to 
F/cos e, where e is the angle which the oblique axis makes with the principal 

Distortion is an aberration in the magnification of the image. It is chiefly 
due to spherical aberration which causes peripheral image-points to be formed 
relatively nearer to the principal axis than their corresponding object-points. 





*■ i . 

■«— • m 


1 i 





_. — . 



- ■-, 





P ! 






Fio. 247. 

Fig. 248. 

Fig. 249. 

Distortion increases as the obliquity of the light is increased, that is to 
say, the size of the image is relatively more out of proportion to that of the 



object as the object is larger and, therefore, its extreme points further from 
the centre. 

The real image formed by an ordinary Cx. lens is said to suffer from negative 
or barrel distortion, thus the image of a square (Fig. 249) is compressed rela- 
tively more at the corners, which lie furthest from the principal axis, than at 
the sides. The virtual image of a square seen through a Cx. lens is said to 
suffer from positive or pincushion distortion, as in Fig. 248, this being the 
reversal of the barrel distortion of the real image. The virtual image of a 
square seen through a Cc. lens has barrel distortion. Any arrangement of the 
stop, or separation of the components of a lens system, may produce distor- 
tion not otherwise apparent. 

Fig. 250. 

Fig. 251. 

Influence of a Stop. — A diaphragm used with a lens, or combination, 
diminishes spherical aberration, coma, astigmatism and curvature of field. 
This accentuates and brings into prominence distortion, so that rectilinear 
lines of the object near the margin appear curved in the image. 

When a stop is in front of a Cx. lens the effective area of the lens for an 
oblique pencil lies mainly on the opposite side of the principal axis to that 
of the object-point, so that the mean focus lies between R and R t (Fig. 250) 
nearer to the axis than if the whole tens were effective. Thus the natural 
negative distortion of a Cx. lens is enhanced. 

When a stop is behind the lens (Fig. 251) the effective area of the latter 
for an oblique pencil is chiefly on the same side of the lens as the object-point, 
so that the mean focus lies between R and R 2 more distant from the principal 
axis than if there were no stop. The consequence is that the natural nega- 
tive distortion of the lens is not only corrected, but positive distortion is 

The distortion is due to the lens and not to the stop, for if a combination 
be corrected for distortion the stop may be in front, of the lenses, between 
or behind them, and no distortion ensues. 

Remedies. — Distortion is eliminated by employing a combination of 
lenses with the stop placed between the two components. Then those oblique 
rays which pass through the one side of the front element must pass through 
the other side of the back element, and wee versa,[ao that the negative distorting 
effect of the front lens is neutralised by positive distortion of the back lens. 

Separation of the component parts of a lens system can te utilised for 



the correction of distortion, and in single lenses it may be reduced somewhat 
by altering the thickness and curves of the lens. 

The Tangent Condition. — A chief ray X C or Y C (Fig. 252) is one which 
passes through C, the centre of the stop. If it be prolonged forwards and. 
after refraction, produced backwards, the point of intersection p is a chief 


Fig. 252. 

When all the chief points thus formed lie in a plane perpendicular to the 
axis, i.e. the refracting plane, the refracted chief rays, produced back to the 
axis, meet in a single point C The lens is then said to be spherically corrected 
with regard to the stop. 

Each chief ray makes with the principal axis, before refraction, some 
angle b, and, after refraction, some angle b', and when the foregoing con- 
ditions obtain, tan Z//tan b—a constant for every chief ray; the image will 
then be uniformly magnified throughout, i.e. the image will be free from 
distortion when the tangent condition is fulfilled, as in Fig. 252. 

Aberrations in General. 

In the brief description of the aberrations contained in the foregoing 
articles certain points are worthy of special note. All the aberrations of a 
single lens are reduced by the use of a stop with the exception of distortion, 
which is generally increased, or anyhow made more apparent. The con- 
struction of a good lens also largely depends upon the use of meniscus com- 
ponents, without which a wide stigmatic field would be impossible, while, 
needless to say, crown and flint glasses are essential for achromatism. The 
nature of the corrections depends largely upon the use to which the lens is 
to be put, but on the whole, the designer of a photographic objective has a 
harder task than the maker of telescope and microscope objectives. Of all, 
perhaps, the photographic objective must be the most generally perfect 
since it is required to produce a flat, stigmatic and undistorted image over a 


wide field whose diameter is not infrequently equal to the focal length of the 
lens. To secure this a kind of compromise must be effected between central 
and peripheral definition, since the type of lens — the crossed and piano — 
giving the best central correction for spherical aberration and chromatism, 
is useless for eliminating the oblique aberrations. 

If a first-class photographic lens designed for wide-angled work be 
examined, it will be found to contain at least one deeply periscopic com- 
ponent, and in all rectilinear objectives both are of meniscus shape. For 
extreme wide-angle work the periscope type must be still further deepened, 
until we find, in the Hypergon of Busch, a lens consisting of two thin hemi- 
spheres with a stop at their common centre. Generally, therefore, the smaller 
the angular field the flatter are the curves required to produce it. 

In the telescope, prism binocular and opera glass only a narrow angular 
field — not exceeding a few degrees — is required, and therefore the oblique 
aberrations may be comparatively ignored, and all the attention centred on 
the correction of spherical aberration and chromatism, which may be done 
to an exceedingly high degree of perfection. Thus any good telescope or 
opera-glass objective will be found to be, as a whole, either plano-Cx. or 
bi-Cx. with the greater curvature towards the light, which is practically 
parallel in all cases. 

Rather more care must be bestowed on the microscope objective, since 
here some correction must be given to flatness of field and coma, so that it 
may be said to occupy an intermediate position between the telescope and 
photographic objectives, and, the object being near F, the bottom component 
of the objective is plano-convex, having its piano surface directed outwards. 

A plano-Cx. condenser is turned the one way or the other, according as 
the source is near or distant, and according as the beam of light projected is 
large or not. 

Spherical aberration is a defect of the image on the principal axis, and, 
therefore, for best definition it is necessary to distinguish between point- 
objects and objects of definite size. Thus the eye lens of an ocular is always 
plano-Cx. with the curved surface towards the object to be viewed, which 
is the real image formed by the objective, and notwithstanding that this 
obj ect lies in the focal plane of the eye lens. This is because the obj ect viewed 
is of definite size, and not merely a point on the axis, that is, spherical aberra- 
tion must be sacrificed to a small extent to allow of correction for distortion, 
which is really spherical aberration of peripheral pencils as a whole. 

Again, in visual optics, the deep periscopic spherical and toric are now 
recognised as being far superior to the doubles in that the field of sharp defini- 
tion is greatly extended by the elimination of most of the oblique aberrations. 

Aberrations of a Cc. Lens. — Although in the foregoing articles Cx. lenses 
have been used in diagrams and examples, it must not be forgotten that 
Cc. lenses suffer from precisely similar aberrations. They are, of course, 
opposite to what would be produced in the virtual image of a Cx., e.g. the 
distortion of the virtual image with a Cc. is barrel, whereas it is pincushion 



with a Cx., so that when two lenses are neutralised in the ordinary way 
their aberrations are also practically neutralised, unless the lenses are thick 
and together take a deep periscopic form. 

Aplanatic Refraction. — Refraction at a spherical surface is always accom- 
panied by more or less spherical aberration; it is possible, however, to con- 
ceive surfaces that are aplanatic, i.e. capable of producing a point-image of 
a point-object situated on the principal axis. 

It is convenient to apply the principle of least time in each particular case. 
As pointed out, the optical length of any ray is its actual distance multiplied 
by theu of the medium in which it is travelling and the condition to be ful- 
filled for aplanatism is that all the rays diverging from an object-point must 
reach the image-point at the same time. However, surfaces which are aplana- 
tic under certain conditions or for light of a certain wave-length are not so 
under other conditions or for other wave-lengths. 



Nj' / 

Fig. 253. 

Fig. 254. 

Aplanatic Cx. Surface. — Let/ X (Fig. 253) be a near object-point in air; its 
real image f 2 in the denser medium will be aplanatic if the distances d x + 
[i d 2 , d x " +/J, d 2 " etc. be equal. The light travels along d x d x " etc. at a velocity 
V v while it travels along d 2 , d 2 " etc. at a lessened velocity V 2 . The curvature 
of the surface, where d x +[_i d 2 is a constant, is that of a Cartesian ovjI. Hf 2 
were the object in the dense medium, and f x the image in air the same 
conditions apply. 

If the object-point^ (Fig. 254) be at oo, again the condition for aplanatism 
is that d x +[i d 2 , d x +/u d 2 etc. be a constant; the curve must then be that 
of an ellipsoid, i.e. all points on a plane wave R T X must be retarded so that 
they reach the focus F 2 in the same time that each point would have travelled 
to R T X if uninterrupted. If the object be at F 2 , so that the light is pro- 
jected parallel, the same surface is required. 

Aplanatic Cc. Surface. — If/ 2 is the virtual image oif x (Fig. 255) it is aplana- 
tic if d x -fi d 2 , d x -jli d 2 etc. is a constant, and the curvature of the surface 
for this condition is also that of a Cartesian oval. If, however, d x =[i d 2 the 
curve is spherical. 

Aplanatic Cx. Surface. — If a luminous point be situated within the dense 
medium of a convex refracting surface (Fig. 256), a position on the axis can 
be found such that the virtual image is aplanatic. The distance of f x from 
the surface must be r + r//j,, or r (/j, + l)//u, and therefore the image/ 2 is formed 



at r +[x r, oir(/Li + l). As the distances of^ and/ 2 are respectively r//n and jur 
from C, the magnification isf 2 /f l =ju 2 . This principle is made use of in Abbe's 
homogeneous immersion objective employed in high-power microscopes. 


Fig. 256. 

In this case the bottom lens of the objective is a hemisphere whose plane 
surface is towards the object, and, when immersed in cedar oil of the same 
index as that of the glass, the whole forms a single refracting body as shown 
in Fig. 256. The object is then placed at/* p and its aplanatic image is formed 
at/ 2 , which in turn serves as an object for the remainder of the objective 

Fig. 257. 

Fig. 258. 

Aplanatic Lens. — If, in a Cc. periscopic lens (Fig. 257), the object at/ x 
faces the concave surface, the virtual image at/ 2 is aplanatic when d\=fj, d 2 . 
In this case r x the radius of the first surface must be/ x /(/i + 1), while that of 
the second surface must be [f x +t)/fi {t being the thickness), for then/ 2 lies 
in the centre of curvature of the second surface; uf 2 =fv ^ otn measured 
fiom the first surface. 

Example. — Let/ X =15 cm., t=2 cm., and ^=1-5; then 

/•j =15/(1.5 + 1)=6 cm., and r 2 =(15+2)/l .5=11-33 cm. 
After refraction at the first surface we have 

l-5// 2 = - .5/6 - 1/15= - 4-5/30 
Therefore - 4-5/ 2 =45, or/ 2 = - 10 

An aplanatic Cx. meniscus results when the object faces the Cc. surface 

(Fig. 258) if r 1 =f 1 and r 2 =/j,{f x +t)/{fx + l). In this case the rays from/ x 

are normal to the first surface, and d x is constant, as is also d 2 , for all rays; 

f 2 lies in the aplanatic point of the second surface corresponding to the value 

of/ x given in Fig. 256 illustrating the case of the single surface. 


Example. — Letj^=15 cm., t=2 cm., and^e=l«5; then r t = - 15 cm., 
r 2 =1.5(15+2)/(1.5+l)=25.5/2.5 

so that r 2 =10-2 cm. 

If there are two unknown quantities r 2 and t, values must be found for 
them so that jLif 1 =f 2 , both measured from the second surface. 

These are the only case where aplanatism can be obtained with lenses; 
there is no case for parallel light, nor for double Cx. and Cc. lenses, but, as 
explained under spherical aberration, this can be minimised by employing 
certain forms of lenses and a stop. 


Aberrations of a Mirror. — If the angular aperture of a spherical mirror 
be large, rays which diverge from a point on the principal axis do not meet 
in a single conjugate image-point after reflection, owing to spherical aberra- 
tion. Mirrors suffer also from coma, radial astigmatism, curvature of the 
field, and distortion, but not from chromatic aberration. 

Since reflection, from a spherical surface, is much more powerful than 
refraction by it, the spherical aberration of a mirror is greater than that of a 
surface having the same curvature. 

As stated in the chapter on Reflection, the aperture of a mirror should not 
exceed 20° at C, the centre of curvature if a point image is to be obtained of 
a distant point object. A parallel ray A B (Fig. 259) incident on a Cc. mirror 
at a point beyond such aperture is reflected to cut the axis at/1 nearer to the 
mirror than F. As the angle of incidence i increases so f approaches M, and 
when t'=60°, as with the ray D E, it is reflected to the vertex M, the aperture 
being then 120°. 

Let a be the semi-aperture of the mirror, and if taken as straight 

a/V=sin 6= sin i and a=r sin i. 

Thus, if t'=30 o , 45°, and 60°, a=-5r, -7r, and -866r respectively. 



In Fig. 260, b=i and C D=-5r, then -5r/6/=cos i, so that the distance 
Mf, at which any ray parallel to the axis cuts the latter, is in terms of i— 

M/=r=r/2 cos ?'=2F ~F/cos i. 

From the above a/r=sin i=\ 1 - cos 2 i; 

. < /^& A /4F 2 -o 2 . 

whence cos i= V 5- = v — ,^ Q 

r l 4F 2 

Substituting these values in the previous formula we get M/in terms of 
a, the semi-aperture 

M/W - ,- 2 /2Vr 2 -a 2 =2F - 2F 2 /a/4F 2 - a 2 . 

2F 2 

The longitudinal aberration— — ; =— ^ - F. 

V4F 2 -a 2 

The two astigmatic focal lines of a small oblique pencil of parallel light 
at an angle of incidence i, are distant F cos i and F/cos i from the mirror. 

Caustic Curve. — Those rays diverging from a point which are within a 
few degrees of the principal axis, unite in a point, which is taken as the focus. 
Those rays having larger and larger angles of incidence (Fig. 261), are re- 
flected to cut the principal axis nearer and nearer to the vertex of the mirror., 
and their intersection gives rise to a series of points of increased illumination 
which, together, form what is known as a caustic curve, the cause of which 
is spherical aberration. 

Caustics may, also, be virtual but are not noticed because the pupil of 
the eye acts as a small stop and limits the divergence of the rays. 

Aplanatic Reflection is simpler than refraction because the light before 
and after contact with the surface is in the same medium. 



Aplanatic Mirror. — For a mirror (Fig. 262) capable of producing an aplana- 
tic image, f 2 of some point/! within oo on the principal axis, if d x d x " . . . 
and d 2 ' d 2 " ... be the incident and reflected rays, d x +d 2 ' must equal d x " + 
d 2 ", and likewise for any other incident reflected ray. Thus, in general, d x + 
rf 2 =a constant, so that the mirror must be an ellipsoid of revolution with f x 
and /, as the foci. The object could, of course, be at/ 2 and the image at/ x . 


Fig. 262. 

Fig. 203. 

The mirror is, however, aplanatic only for these two points, aberration appear- 
ing immediately the object -point is displaced from either. For every pair 
of conjugates a different curve is needed, so that ellipsoidal mirrors have no 
practical utility, as their limited application never occurs. 

Spherical mirrors of any aperture are aplanatic if the light diverges from, 
or converges to, a point at the centre of curvature. 

If the object-point be at oo (Fig. 263) the curve of the reflecting surface 
becomes that of a parabola of which F is the focus. Here the directrix R T X 
represents a plane wave interrupted by the mirror, and in order that all points 
on such a wave may meet at a single point, they must be converged to F 
in precisely equal times, so that, as before, d x +d 2 =d x " + d 2 ", etc. If the 
object point be at F, the light is reflected as a parallel beam. 

Parabolic mirrors are employed in reflecting telescopes for bringing rays 
from an infinitely distant object, such as a star, to a sharp focus. Also for 
projecting a parallel beam of light, as in lighthouse and optical lanterns, 
searchlights, microscopic reflectors, etc. Such mirrors possess the advantage 

Fig. 264. 

Fig. 265. 

over refractors in that all light waves are equally projected, and therefore 
chromatic aberration does not occur. For this reason also they are preferred 
to refractors for the photography of celestial bodies. A Cx. spherical mirror 
cannot project a large beam which even approximates to parallelism. 


Let/i (Fig. 264; be the object-point, and/ 2 its virtual image; the latter is 
then aplanatic if dj'-d^, d x " - d 2 " etc. be a constant. This results if the 
curvature of the mirror is thai of a hyperbola, f x and/ 2 being the foci. If the 
virtual object- point be at/ 2 and the image at/ x the same curvature is required. 
Like the ellipsoidal, the hyperbolic mirror is of no piactical value. 

An aplanatic convex reflecting surface for a near object must be hyper- 
bolic (Fig. 265), while for parallel light it must be parabolic. 


Oblique Sphericals. 

Direct and Oblique Refraction.— Let Fig. 266 represent the face of a Cx. 
lens placed normally to the light. Let the effect of the refraction in the verti- 
cal plane be ignored and that of the horizontal considered by itself. Rays of 
light parallel to the axis passing through c c' would meet in a point behind, 
and in line with, ; similar va,ys incident at d d' and e e' would meet in corre- 
sponding points behind the lens, forming a vertical line focus parallel to B B' . 

/ \ 


/ i 

o \c ] 

B '.e' J 


Fig. 266. 

Again, considering the vertical plane by itself, the refracting effect is to 
produce a horizontal line focus parallel to A A'. The vertical line meeting 
its corresponding horizontal line, in the focal plane, they combine to form 
point foci for rays parallel to the principal axis. This is true also for any two 
planes at right angles to each other. 

When, however, the incidence is oblique the two lines do not combine, 
so that a point source gives rise to two focal lines. This, as an aberration, is 
called radial astigmatism (q.v.). 

Obliquity of Lens. — In Fig. 267 L is a Cx. lens whose principal axis is 
A D F. The line G D represents the axis of an oblique pencil whose image 
is F t . . . F 2 . The first plane contains the oblique axis and the principal 
axis; the second plane contains the oblique axis and is at right angles to the 
first. F x the first line is the focus of the first plane, and lies in the second plane. 
F 2 , the second line, is the focus of the second plane and lies in the first plane. 
Both lines are nearer to the lens than F, and F 1 is nearer than F 2 . The two 
lines are at right angles to each other, and each one is at right angles to that 
meridian of the lens to which the plane refers. In Fig. 267 the two planes are 




that of the paper, and that passing through C D, perpendicular to the 

Now the conditions obtaining for an oblique pencil of light and an upright 
lens as in Fig. 267, are the same for a direct pencil and an oblique lens as in 

Fig. 268. That is to say, if a spherical lens acts with an astigmatic effect on 
an oblique pencil of light, a spherical held obliquely to the incident light 
similarly acts as if it were a sphero-cylindrical lens. 

When a spherical lens is held upright, parallel to a screen, and at its focal 
distance, a luminous point on the axis will have a point-image on the screen. 
If now the lens be rotated around, say, a horizontal axis, the image becomes 
confused and drawn out as if a cylindrical had been added to the spherical. 
Two focal lines are formed on the screen hold at the proper distance for each. 
The second focal line is, in this case, vertical, and slightly within the focus 
of the lens; the first line is horizontal and still nearer to the lens. Thus the 
effect produced by obliquity of a spherical is that of a slightly stronger spherical 
combined xoith a cylindrical whose axis corresponds to the axis of rotation. The 
refraction is therefore increased in both meridians, but mostly in that at right 
angles to the axis of rotation. 

The increased power in the meridian of the rotation is owing to the fact 
that the light passes through a rather greater thickness of lens when the latter 
is oblique than when placed normally. The increased power in the meridian 
at right angles to the axis of rotation is due partly to the same cause, but 
still more to the increase in the angles of incidence of the light in that meridian. 

Fig. 269. 

Tilted Sph. — In Fig. 269 let a be the angle of rotation of the lens, F the 
focal length, and F x and F 2 the first and second oblique foci. A B is the 


principal axis of the lens, and C D is the secondary axial ray on which the focal 
lines are formed. The pencil of incident light is presumed to be parallel to 
C D, so that rays, as d and e, or d' and e', incident in planes parallel to the axis 
of rotation, meet each other to form the second focal line F z . Rays as d and d', 
or e and e', incident in planes at right angles to the first, meet each other to 
form the first focal line F v The angle of rotation a is that between G D and 
A B, and b is the angle of refraction at the first surface (i.e. /u sin 6=sin a). 

The distances of F x and F 2 are found from the following formulae, for the 
derivation of which see the works of Dennis Taylor and Percival. 

„ „ sin a- sin & „ (a -1) sin a 

F.,=Fx^-^ ^.=Fx 

sin (a - b) sin a cos b - sin b cos a 

F( j a-1) , .„ F(u-l)cos 2 a _ 

F =^ ^ — and F,=— ^- 7 — =F, cos 2 a 

jli cos 6 - cos a i u cos o ~~ cos a 

D (a cos 6 - cos a) D (a cos b -cos a) D 9 

or D 2 =- — =- — and D x =— _ = — — 

1 {JL-1 (ju - 1) cos 2 a co& A a 

For small angles of obliquity and ^=1*5, the following approximate 
formulae can be employed — 

„ ,,/ sin 2 a\ ,, ^, . _ _ ,/ sin 2 a\ _ D 

Examples. — A 10" Cx. lens is rotated 20°, then — 

F 2 =10 x (1 - .117/3)=9.61" F 1 =9-61 x .883=848". 
A + 6 D lens is rotated 30°, then— 

6 6-54 

Since D 2 does not vary greatly from D^ the increased or cylindrical effect 
produced by obliquity of a spherical lens is 

D _ D sin 2 a 
C=D, -D 2 = — ^- -D = - -=— =D tan 2 a 
cos* 5 a cos^ a 

If the two focal distances be measured, the angle of rotation of the lens 
can be found from the equations 

F 1 /F 2 =D 2 /D 1 =cos 2 a 

Table of the Sphero-Cylindrical Effects of Oblique Sphericals. 

The following table gives the approximate effects obtained by rotating a 
1 D Sph. lens; the effect on other lenses is proportional. The rotation is 
supposed to be around a horizontal axis. The effect increases rapidly with a 
greater obliquity. 



A ngle of 

. *1 






1 er. Mer. 

Hor. Mer. 

Ver. Mer. 

Hor. Mer. 







1-00 o 0-01 






1-01 O 0-03 






1-02 o 0-07 






1-04 o 0-16 






1-06 o 0-24 






1-09 o 0-36 






1-13 O 0-57 






1-16 O 0-84 






1-20 o 1-20 

Tilted Cyl. or Sph.-Cyl. — The effective power of a cyl. rotated around its 
axis is the same as D x and F x ; it is, in effect, a stronger cyl. If rotated across 
its axis its effect also is that of a very slightly stronger cyl. If a sph.-cyl., 
both powers being of similar nature, be rotated round the axis of the cyl., the 
cyl. effect is increased because T> 1 - D 2 is increased. If rotated round its 
meridian of greatest power, the sph. effect is increased, and the cyl. decreased 
because D x - D 2 is lessened. If the two powers are of opposite nature rota- 
tion in either principal Mer. increases the cyl. effect. A rotation oblique to 
the principal Mers. results in a new combination altogether. 

Wide-angle or Meniscus Lenses.- — The form of lens which allows of best 
vision over a fair range of, say, 50° or 60°, i.e. 25° or 30° on each side of the 
axis, is one which eliminates radial astigmatism and produces a flat field; 
the two do not necessarily accompany each other, and the former is the more 

The subject has been treated by Ostwalt and Wollaston, and more recently 
by Dr. Percival in his " Prescribing of Spectacles " and by Mr. A. Whitwell 
in the Optician. The calculations, which are complicated, are based on motion 
of the eye about the centre of rotation some 27 mm. behind the plane of the 
lens. The actual best form, as to the curvature of the two surfaces, varies with 
the power of the lens, with the ju, with the distance of vision, and with the 
distance of the lens from the eye ; it is, however, neaily always a deep meniscus, 
except for high power concaves. For ordinary power lenses, made of ordinary 
crownglass, a good form does not differ much from the ordinary commercial 
meniscus which has a surface of - 6D on the convex and a + 6D on the con- 
cave. Another series of best form has extremely high curvatures of some 
+ 20D or -20D. 

Oblique Cylindricals. 

Meridional Refraction of a Cyl. — Fig. 270 represents a Cx. plano-Cyl. bus. 
axis horizontal. If a lens measure be placed in contact with the maxi- 
mum meridian M it shows the highest possible curvature of that cylindri- 
cal. Along the axis the instrument would indicate 0, and between these two 
the recorded power varies. Suppose the two fixed legs are at d and d, then 



the sag of the central leg indicates the power, which is based on the formula 
r=d 2 /2 S (vide The Spherometer), and the curvature (7=2 S/rf 2 , where d is 
half the distance d d. Let the instrument be turned so that the legs lie on the 

If now the sag were the same as before 

meridian M' at an angle b with M. 

it is because the distance between the legs is greater, the curvature C in the 
Mer. at M' bearing to the curvature G in Mer. M the relationship C'/C== 
d 2 /d' 2 , where d' is the new distance between the central and one of the fixed 
legs in the meridian M'. But d'=d/co$ b, so that 


d 2 d 2 cos 2 b 

d' 2 

d 2 

= COS' 

b or (7=(7cos 2 & 

Now the dioptric powers D at M, and D' at W are directly proportional 
to the curvatures G and G' respectively, so that in the meridian M' the power 
of the lens D'=D cos 2 b, or what is the same, D'=D sin 2 a, where a is the 
angle between M' and the axis. Similarly it can be shown that in the meri- 
dian M" at right angles to M' the power D"=D sin 2 b, or D cos 2 a. If we 
consider the angle a between a given meridian and the axis of a cyl., its 
power' varies as sin 2 a; if we consider the angle b between it and the maxi- 
mum meridian, the power varies as cos 2 6. 

Although we thus refer to the refractive power of a cyl. in any oblique 
meridian, yet this latter does not cause a point focus. A cyl. brings incident 
light to a line focus, parallel to the axis, and if the meridian of maximum power 
be isolated by means of a stenopceic slit, so that the oblique meridians are cut 
off, the line is reduced to a point, because the curvature in that meridian is 
spherical, and the effective aperture of the lens, at right angles to the slit, 
being reduced practically to zero, the result is similar to that of an ordinary 
spherical lens. If the slit be slowly rotated the meridians successively un- 
covered are elliptical in curvature, and the point focus, first obtained, gradu- 
ally widens into a line parallel to the axis, showing that, although the effective 
part of the lens is oblique, the effective curvature is always that of the maxi- 
mum meridian. If the rotation be continued until the slit is parallel to the 
axis, the line reaches its maximum length just as though the whole lens were 
uncovered. Thus the only meridian capable of producing a true focus is the 
maximum principal meridan, which has a spherical curvature. It is, how- 



evci, useful to assume that the oblique meridians of a cyl. have certain powers 
relative to the maximum which contribute to the general power of the lens, 
and the following gives the necessary calculations; a distinction must, how- 
ever, be drawn between the incomplete line-foci of such powers, and the point- 
foci produced by spherical curvatures. 

Fig. 271. 

Fig. 272. 

Oblique Powers of a Cyl. — Fig. 271 represents a Cx. cyl. lens whose axis 
Ax. is vertical, and maximum power M horizontal. Let tiis lens be a +5 D, 
and the object be a point at oo. Any ray of light incident in the meridian Ax., 
central to the meridian M, suffers no deviation, it being normal to the lens 
at both surfaces. Any ray incident in Mer. M is refracted to an extent 
governed by its distance from the central point of Ax., such that it meets all 
other rays, incident in that meridian, in a point in line with, and 20 cm. 
behind it. Any ray, as b, incident in an intermediate meridian, say that of 
70°, is refracted to meet all other rays, incident in the plane b c a, in a point 
in line with c, and also 20 cm. distant. The deviation suffered by the ray b, 
refracted in an intermediate meridian, is less than that which occurs when 
refracted as e in meridian M, both being equidistant from the central point 
of Ax. The total image is a Ver. line. 

In the case of a sph.-cyl. (Fig. 272) a ray incident at b in an oblique 
meridian is refracted by the sph. to a point on the principal axis, and by the 
cyl. to a point in line with c, with the resultant oblique deflection in the direc- 
tion b', so that it meets rays incident in a plane b c a parallel to M in b', and 
those incident in a plane parallel to Ax. in c'; or if the lens be regarded as 
consisting of crossed* cyls., the deviation is towards both axes, resulting in 
an oblique deviation towards c' in the first, and V in the second focal line. 

Let D be the maximum power of a cyl., D' the power in a given Mer., 
and D" that at right angles to D'; let a be the angle between the axis and 
the Mer. of D'. Then the powers of a cyl. in any pair of given opposite meri- 
dians are, as previously stated, found from 

D'=D sin 2 a 


D"=D cos 2 a 

The power along the axis is 6, and at right angles it is D, so that the 
total power of this pair of opposite Mers. is D +0=D. Likewise the sum of 
the powers of any pair of opposite Mers. is equal to D, for sin 2 a + cos 2 a=l, 
so that D sin 2 a +D cos 2 a=D' +D"=D. 


Thus the powers of a + 3 D. Cyl. Ax. 180°, at 20° and 110°, are— 

D'=3 x .11696=.35 D. at 20°; D"=3 x -88303=2-65 D. at 110°. 

Let A Y and A Z (Fig. 273) represent the forces exerted, respectively, in 
the Hor. and Ver. Mers. by, say, a 3-5 D. Cyl. Ax. 60°. Let H be the hori- 
zontal and V the vertical effect. Now X Y=A Z=sin 60°, and X Z=A Y 
=cos 60°, whence H=D sin 2 a=3-5 x -75=2-625, V=D cos 2 a=3-5x-25 = 
.875, and 2-625 + -875=3-5=D. 

Fig. 273. 

In these calculations it is merely necessary to find either D' or D" since 
the other can be obtained by subtraction from D. Thus if V=-875, H= 
3-5 - -875=2-625, and vice versa. 

Following are the approximate powers of unit cyl. in different Mers. 
calculated as shown above. 

Degrees from Ax. 



















Proportional ) 
power . . / 



















Obliquely crossed Cylindricals— If two cyls. D and D' are placed with 
their axes corresponding in the Ver. Mer. their combined Ver. power=0, 
and the Hor.=D+D'. If one or both cyls. be rotated, they are equivalent 
to a combination of some two other principal powers. When the two axes 
are at right angles the combination is equal to a sph. if D=D', and to an 
ordinary cross-cyl. if D and D' are unequal. It should be particularly noted 
that, with any obliquity of the axes, two (or more) cyls. are always equivalent to 
some other cross-cyl. whose axes are at right angles, and are, therefore, also equiva- 
lent to some sph.-cijl. The sum of the two principal powers D l and D 2 is 
always equal to the sum of the individual maximum powers D and D', 
that is, 

D + D'=D X + D 2 

Not only the powers of the principal Mers., but also the sum of the powers of 
any pair of Mers. at right angles to each other=T> + D'. Rotation of the axis of 
one or both cyls. merely locates the refraction in varying quantities as 
regards each of any pair of opposite meridans, and does not alter the total 



Let b (Fig. 274) be the angle between the axes of two cylindricals D and 
D', of which D is the higher of the two. Let D x and D 2 be the two resulting 
powers, D x being the higher. Let c be the angle which the axis of D x makes 

Fig. 274. 

with that of D, and let d be the angle it makes with that of D'. Then angle 
&=c + d. Now J) 1 corresponds with the axis of D 2 , and D 2 with the axis of D L . 
From the foregoing we have D + D'=D 1 + D 2 

and D sin 2 c + D' sin 2 d=D v also D cos 2 c + D' cos 2 d^D 1 

Multiplying these together we get 

D X D 2 =D 2 sin 2 c cos 2 c + D' 2 sin 2 d cos 2 d + DD' sin 2 c cos 2 d 

+ D D' sin 2 d cos 2 c 

Now D 2 sin 2 c cos 2 c=D' 2 sin 2 d cos 2 d 

.-. D 2 sin 2 c cos 2 c + D' 2 sin 2 d cos 2 d=2D D' sin c cos c sin d cos d 

so that 

D X D 2 =D D' (sin 2 c cos 2 rf + sin 2 d cos 2 c) +2D D' sin c cos c sin d cos d 

=D D' (sin c cos d + sin d cos c) 2 

but sin c cos c2 + sin (7 cos c=sin (c + (2)=sin b 

therefore DJ^D D' sin 2 6 

and since D 1 + D 2 =D+D' 

we can, knowing the multiple and the sum of the two numbers, arrive at their 
difference C, thus 

C=D X - D 2 =V (DTD') 2 - 4D D' sin 2 ! 

Then we get in the resultant combination 

The higher power 

and the lower power 


D 2 


+ D' 

+ C 




D x is the spherical + the cylindrical ; D 2 is the spherical ; C is the cylindrical- 


The following relationships exist : 

C + D' - D 
D X -D=D'-D 2 = and C sin c cos c=D' sin b cos 6 

D 2 D /2 C 2 


sin 2 d cos 2 d sin 2 c cos 2 c sin 2 b cos 2 6 

Now C 2 sin 2 c cos 2 c=D' 2 sin 2 6 cos 2 6=D' sin 2 & (D' - D' sin 2 b) 

but D'^Di + Da-D 

so that C 2 sin 2 c cos 2 c=D' sin 2 & (D x +D 2 - D - D' sin 2 6) 

=D X D' sin 2 b + D 2 D' sin 2 6 - D D' sin 2 b - (D' sin 2 6) 2 

Substituting D X D 2 for D D' sin 2 b we get 

C 2 sin 2 c cos 2 c^D' sin 2 & +D 2 D' sin 2 & - D^ - (D' sin 2 b) 2 

Or C sin 2 cxC cos 2 c=(D 1 -D' sin 2 b) (D' sin 2 &-D 2 ) 

also since sin 2 c + cos 2 c=l, 

C=C sin 2 c + C cos 2 c= (D x - D' sin 2 b) + (D' sin 2 b - D 2 ) 

Then we deduce that 

C sin 2 c=D' sin 2 6 - D 2 and C cos 2 c=T> 1 - D' sin 2 b 

Csin 2 c D'sin 2 '&-D, , D, 

Now tanc=- — : — = ,. . . ■ , =tano 

C sin c cos c D' sin b cos b D' sin b cos 6 

«-, . . , D D' sin 2 b 

Substituting for D 2 its equivalent 

DD'sin 2 & 7 D 

tan c=tan b - _ ■ . . — — ~-=tan b - -- tan b 
D x D sin b cos 6 D x 

So that tan C J^A^1^± 

c is the angular distance of D x , the stronger resultant cyl., from that of 
D, the stronger original. We could find a formula for d, but it is unnecessary, 
since d=b-c. The distance d' of the axis of D 2 , the weaker resultant, from 
that of D', the weaker original cyl., is found from 

(D 2 -D') tan b 

tan d'- 

D 2 

Since (D 2 -D')=(D X -D), it is easy to confirm calculations, but care 
must be taken with the - signs. When D and D' are of similar signs d' is 
negative. The two resultant axes must be 90° apart — i.e. b- (c- d')=90°. 
A positive measurement is towards the other axis, and a negative one is 
away from it. 

To find b the angle between two cyls. D and D' in order to produce any 
two effects D x and D 2 , we have sin 2 &=D 1 D.,/D D', but of course it is possible 
only when D 1 + D 2 =D+D'. 


Unlike Cyls. — When the one cyl. is positive and the other negative, the 
same formulae apply, but c is negative, as also is d'. The calculation is 
rather more involved, and it is better, as suggested by Mr. A. Jameson, to 
convert the combination into one with similar signs. This is done by adding 
to the combination a Cx. sph., whose power is equal to that of the Cc. cyl., 
thus converting the - cyl. into a + cyl. Then ignoring, for the moment, 
the added sph. the calculation is made for the resultant of the two obliquely 
crossed Cx. cyls., and from the result the added sph. is finally deducted. 
This is illustrated in an example given below. 

Two Equal Like Cyls. — Here the calculation is simplified, for when 
D=D', c=d, so that it is unnecessary to calculate C or c. Thus 

7 7 

D x =2 D sin 2 - D 2 =2 D cos 2 - c=b/2. 

Two Equal Unlike Cyls. — Here also the calculation is simplified, for 

D=-D' D+D'=0 D x + D 2 =0 

D D' sin 2 6=0^2= - D 2 sin 2 6=D* or D; 

therefore D sin 6=D X , and-D' sin &= -D 2 . 

— cos ^ measured negatively from the Cx., for the resultant 

Cx., or from the Cc. for the resultant Cc. 

measured from the Cx. positively for the resultant 
cos b Cc, or from the Cc. for the resultant Cx. 

The two measurements=90°. C need not be calculated. 
Examples.— + 3 C. Ax. 70° o +2 C. Ax. 20°, D+D'= +5, 6=50°. 
C = V(3 + 2) 2 -4x3x2x-5868=Vl3-92=3-30. 

5 + 3-30 5-3-30 

D i=— 2~ = 4,15 D 2=-^— =-85 - 

tanc= (^-3)Xl^l8 =j3302=tanl8O18/ 


The combination is +-85 S. o +3-30 C. Ax. 51°42'. 

DD' sin 2 fc^DjLV i.e. 3x2x-5868=4-15x -85=3-52. 

The sum of the maximum powers of the two original cyls., in this example 
+ 5 D, is not changed by altering the position of the two axes with respect 
to each other, for the sum of the two principal meridians of the resultant 
cyls. is similarly -+ 5 D. That is, D 1 + D 2 =4-15 + -85=5 D. 


Two Unlike Cyls.— + 4 C. Ax. 20° o -2-75 C. Ax. 65°, D+D'= + l-25, 


C= V(4 - 2-75) 2 - 4 x 4 X - 2-75 x •5=V / 23-5625=4-85. 

1-25 + 4-85 1-25-4-85 

D 1= = ——=3-05 D 2 = 2 =-1-80. 

Tan C = (3 ° 5 " 4)Xl = - -311=tan 17° 15". 

The combination is 

- 1-80 S. o +4-85 C. Ax. 2° 45', or +3-C 5 S. o - 4-85 C. Ax. 92° 45'. 

D x + D 2 = +3-05- 1-80= +1-25. 

Here by calculation tan c is a minus quantity, and the angle is measured 
from the axis of D away from the axis of D' instead of towards it. 

By Jameson's suggested method, adding +2-75 D sph., we have +4 C. 
Ax. 20° o +2-75 C. Ax. 155° to deal with. 

C = V(4 + 2-75) 2 -4x4x2-75x-5=\ / 23-5625=4-85. 

6-75+4-85 6-75-4-85 or 

D,= -— =5-80 D 2 = — - - = -95. 

1 2 2 2 

T M ,^ (W0 - 4)xl -«i-toirin'. 

The combination is +-95 S. o +4-85 C. Ax. 2° 45'. 
Then, subtracting +2-75 sph. we get as above — 

- 1-80 S. o +4-85 C. Ax. 2° 45'. 

It should be noticed that C is measured towards the axis of the +2-75 C, 
which is 25° below the horizontal on the right. 

Two Equal Like Cyls.— + 4 D C. Ax. 10° o +4 D C. Ax. 60°. c=25°. 

D 2 =2x4x -1786=14288 D x =2 A X -8214=6-5712. 
The combination = +14288 S.O +5-1424 C. Ax.. 35°. 

Two Equal Unlike Cyls.— + 4 D C. Ax. 60° o - 4 D C. Ax. 120°. 6=60°. 

D x =-D 2 =4x -866=3464. 
The combination^ +3464 C. Ax. 45° o - 3464 C. Ax. 135°. 

Graphical Illustration of the Formulae. 

Draw A D (Fig. 275) in units of length = D, and A D'=D', making the 
angle D' A D=6. On A D mark off A H=D 1 - D, and prolong A D a 
distance D F—A H= D x - D so that A F= D v From E drop E H normal to 
H, and E H—i^D^ - D) tan b. From D draw D G equal and parallel to A E; 



connect E G and from G drop the normal G F to F so that G F=E H. 

(D x -D) tan& 

Connect A G. Then G A ¥=c, and G F=tan c= 


Fig. 275. 

Oblique Prisms. 

Oblique Powers of a Prism. — The power of a prism lies in the base-apex 
plane. At right angles thereto — in the axial plane — it possesses no deviating 
power, and at any Mer. intermediate to these two the power A' is — • 

A'=A cos r, 

where A is the power of the prism, and r the angle between the given meridian 
and the base-apex plane. Thus the effect at 40° of a 4° prism whose base- 
apex line is vertical, r being 50°, 

A'=4x -6427=2-57°, 

the power A" in the Mer. at right angles thereto is — 

A"=A sin r. 

Following are the approximate powers of unit prism at different Mers. 
calculated as shown above. 

Degrees from base-~\ 
apex plaue . . / 



















Proportional power 



















Indirect Prismatic Action. — If the base-apex plane is oblique the prism has 
not only its main power in that plane, but a Ver. and a Hor. effect as well. 
Let (Fig. 276) V represent the vertical and H=H' the horizontal effect of 
an oblique prism. Let A=P=0 Q be the power of the prism, and r the angu- 
lar distance of its base-apex line from the horizontal. Then, since sin r= 
V/A and cos r=H/A, 

V=A sin r and H=Acosr. 

Thus let the base- apex line of a 5°d prism be at 20° from the horizontal. 
Then V=5x -3420= 1-71°, and H=5x -9397=4-698°. 

If the base-apex line is at 45°, a 6A has 




Given a 4°d prism, the position of the base-apex line so that the Ver. 
efl'ect be l°d is sin r=l/4=-25=sin 14° 29' from the horizontal. 
Then V=4x-25=l°d and H=4x-9681=3-872°d. 

Fig. 276. 

If with a 6 A a Hor. effect of 3 A is needed, cos /-=3/6=-5=cos 60°, so 
that the base-apex line must be at 60°, V being -6x -866=5-2 A . 

If the angular distance=r' of the base-apex line be taken from the Ver., 

V=A cos r' and H=A sin r'. 

If a prism of 8 A has its base at 30° left eye,- its components are — 

V=8x-5=4 A base up; 
H=8x-866=7 A (approx.) base out. 

Obliquely Crossed Prisms. — The resultant effect of two (or more) prisms 
whose base-apex lines are oblique to each other is found as follows: 

Fig. 277. 

In Fig. 277 let A B and A C be of such lengths that they are proportional 
to, and represent the deviations caused by two prisms of A X =P X and A 2 =P 2 , 
whose base-apex lines are crossed at an angle a. To construct graphically 
the resultant deviation the rhombus A B G D is completed by drawing C D 
equal and parallel to A B, and B D equal and parallel to A C. Then AD 
represents in units of length the resultant deviation, and r is the angle it 




makes with the weaker of the original prisms. If a third prism A 3 were intro- 
duced, a similar construction between A D and A 3 would give the single 
resultant of the three prisms A v A 2 and A 3 , and so on for any further 

In Fig. 277 AD 2 =AB 2 + AC 2 + 2A B-A C cos a. 
But A D is the resultant prism A, and A B and A C the original prisms A x 
and A 2 respectively, so that the formula giving the resultant A of two 
prisms A x and A 2 obliquely crossed at an angle a, can be written — 

A=VA 1 2 + A 2 2 + 2A 1 A 2 cos a, 

A, sin a , . . 

and tan r= - , r being measured from the weaker original. 

A t + A 2 cos a 

Examples. — Two prisms of 6°d and 8°d respectively whose base-apex lines 
are 30° apart; then — 

A=V6 2 + 8 2 + 2x6x8x-866=Vl83-136=13-53°, 


and tan r 

6 + (8x-866) 

When A X =A 2 the formulae simplify to 


= •3091=- tan 17° 11' from the 6°d. 

A=2A cos - and r 



When the two prisms are at right angles to each other, the one Hor. and the 
other Ver., the angle a=90°, sin 90°= 1, and cos 90°=0, so that the formula? 
simplify to 

A=VH 2 TV 2 and tanr=V/H 

as given in Chapter XI. 

Oblique Decentrations and Decentrations of Oblique Cyls. 

As shown in Chapter XII., a Cx. lens causes the action of a prism whose 
base lies in the direction of decentration, and a Cc. lens has the reversed action. 

The prismatic power of a Sph. (Fig. 278) is governed, in any Mer., by the 
distance from the axis 0; thus the zone indicated by the dotted circle has, 







* i _ ... 


o r 








at any point, the same prismatic power. A decentration from to X or from 
O to Z has a prismatic action of A=D C, where C is the distance in cm. 

Fig. 279 shows a Cyl. axis Hor. Its prismatic power lies in the plane at 




right angles to the axis. At a point X, its action is the same as at X in Fig. 
278, but if decentered from to Z, its action is only Z'Z which is less than Z. 
Therefore the result of a decentration equal to X in the different Mers. varies 
from the maximum D C in the power plane to zero in the axial plane. Fig. 
280 shows a combination of Sph. and Cyl. axis Hor. Here, at the point Z, we 
have the combined actions of Z in Fig. 288 and Z'Z in Fig. 289. The two 
effects are of the same nature if the two components are also of the same 
nature, or contrary to each other if the one is Cx. and the other Cc. 

The necessary constants can be introduced into the following formula} 
when the prismatic effects are required in degrees or degrees of deviation, or 
the effects in A can be converted by the usual methods. 

Fig. 281. 

The Effects of Oblique Decentration of a Sph. — When a Sph. is decentered 
obliquely we have, in the meridian of decentration, A=DC, where A is the 
prismatic effect, D is the dioptral number of the lens, and C the decentration 
in cm. In Fig. 281 or represents an oblique decentration in a plane at an 
angle b from the Hor. When is moved to r, the Hor. displacement is oh, 
and the Ver. is ov=hr, and since o/j=cos o and ou=/jr=sin b, the Hor. 
effect H, and the Ver. effect V, of an oblique decentration A, are found by 
the equations 

H=A cos 6=D C cos b and V=A sin 6=D C sin b. 

Thus, if a +7 D sph. be decentered -6 cm. at 30°, 

A=7x -6=4-2 A H=7x -6x -866=3-637 A and V=7x -6x -5=2-l A 

When a Sph. is decentered in any plane M t its prismatic action in any other 
plane M 2 is D C cos b, where b is the angle between M x and M 2 . If 6=90° 
there is no effect in M 2 . 

Oblique Cyls. — If a plano-cyl., axis oblique, be moved horizontally, verti- 
cally or in any direction, an object viewed through it ivill appear to move in a 
direction across the axis, thus showing that the prismatic action is always at 
right angles to the axis, or in the meridian of maximum power. Indeed this 
result is only to be expected, since the virtual prisms in a Cyl. have their base- 
apex lines at right angles to the axis. Therefore no matter what decentration 
be made obliquely to that plane, the resultant effect is as though a smaller 
decentration had been made in the principal Mer. at right angles to the axis 
— that is, in the power plane. 



Oblique Cyls. Decentered in Prin. Mer. — The decentration of an oblique 
cyl. along the axis has no effect whatever. 

If it is decentered in the power plane, across the axis, the effect is, in the 
principal meridians, the same as with the Ver. and Hor. decentration of up- 

right cyls. This, however, produces Hor. and Ver. effects as well, because any 
single oblique action can be resolved into two components at right angles to 
each other. 

In Fig. 282 let xy be the axis of a cyl. at an angle a with the horizontal, 
and let x'y' be its position when the lens is decentered from o to r in the meri- 
dian of maximum refraction. The distance or=C, and the angle 6, which the 
power plane makes with the Hor., is the complement of a. The Hor. power of 
the lens is D cos 2 b, and the distance oh=c/cos b. The Ver. power is D sin 2 b 
and the distance ov=c/sin b. Therefore A, the main effect, H the hori- 
zontal, and V the vertical, are as follows: 


H=D cos 2 fcxC/cos 6=D C cos b. 

V=D sin 2 oxC/sin 6=D C sin b, 

or we can resolve the single effect or into two components od and oe=dr lying 
in the Hor. and Ver. planes respectively. 

Thus rod=b, od= cos b, oe=rd=sin b. 

Then H=D C cos b and V=D C sin 6. 

Thus, let + 4 D. Cyl. axis 60° be decentered 4 cm. at 150°; then 6=30° and 

A=4x4=l-6 A 

H=4x-4x-866=l-386 A , V=4x4x-5=-8 A . 

Oblique Cyl. Decentered Hor. or Ver. — Similar prismatic effects are obtained 
if an oblique Cyl. be decentered horizontally or vertically, the maximum effect 
A lying in the power plane of the Cyl. 

If the decentration is Hor. from o to 7i=C (Fig. 282), then or= cos b, 
and ov=cot b, so that 

H=D cos 2 b C A=D C cos b. 

V=D sin 2 6 C cot o=D sin b C cos b. 


For a Ver. decentration 

V=D sin 2 b C A=D C sin b. 

H=D cos 2 b C tan &=D cos b C sin b. 

If a +4 C. Ax. 60° is decentered -462 cm. horizontally, 6=30 

A=4x-462x-866=l-6 A 
H=4 x -75 x 462=1-386*, V=4 x -5 x 462 x -866=-8 A . 
If a +4 D Cyl. Ax. 60° be decentered -8 cm. vertically, 6=30° 

A=4x-8x-5=l-6 A 
H=4 x -866 x -8 x -5=1-386*, V=4 x -25 x -8= -8 A . 

These results, if compared with the last previous one, show that a 4 D Cyl. 
Axis 60° decentered -4 cm. in the power plane or -462 cm. horizontally or -8 
cm. vertically, has precisely similar prismatic actions. 

It should be noted that a horizontal or vertical effect alone can never be 
obtained by decentering an oblique cyl., and that is why it is inadvisable to 
decenter such lenses. 

Only if the power plane nearly corresponds to the line of decentering can the 
effects in other meridians be ignored. Indeed it may occur that the Hor. 
decentering of an oblique cyl. results in a greater Ver. effect, and vice versa. 
This is shown in the table below. 

The maximum Ver. effect of a Hor. displacement, and vice versa, results 
when the axis is at 45°. Also since sin 45°= cos 45°, the effect is equal in 
both directions, no matter how decentered. 

The Ver. effect of a Hor. decentration of a cyl. whose axis is at, say, 30° 
is the same as when the axis is at 60°, because although the Ver. displacement 
is less in the first case, the Ver. power is greater. 

To illustrate these effects let a +1 DC. be decentered horizontally 1 cm., 
the axis being respectively at 45°, 30° and 60°. Then 

With axis at 45° A=-7 A H=-5 A V=-5 A 

„ 30° A=-5 A H=-25 A V=43 A 

„ 60° A=-86 A H=-75 A V=43 A 

Hor. or Ver. Cyl. Decentered Obliquely. — Let A' be the effect in the power 
plane, and A" be that in the plane of decentration, then — 

A'=D C cos b A"=D cos 2 b C. 

In the axial plane there is, of course, no effect. 

The Decentration of a Sph.-Cyl. — Here we have to combine the actions of 
the two components as already indicated. In the following D is the power 
of the Sph. and D' that of the Cyl. 

Oblique Sph.-Cyl. Decentered in the Prin. Mers. — The effect of decentering 
an oblique sph. -cyl. in the principal meridians is the same as with Hor. and 
Ver. decentration when the axis is Hor. and Ver. respectively. 



If the decentration is in the power plane of the cyl. there are, besides the 
principal effect A, certain Hor. and Ver. effects introduced due to the oblique 
decentering of the sph. When o (Fig. 283) is moved to r there is a Hor. 

Fig. 283. 

decentration oA=cos a, and a Ver. one ov=rh=sh\ a. In this case a corre- 
sponds to 6 in Fig. 281, so that we can write as before — 

A=D C H=D C cos b V=D C sin b. 

Suppose a + 3 S. o + 2 C. Ax. 30° is decentered 4 cm. at 30° 

A=3x4=l-2 A 
H=3x4x -866=1-04 A , V=3x4x-5=-6-* 

When the decentration is in the power plane of the cyl. (Fig. 284) we have 
in the Mer. of decentration, and in the Hor. and Ver. Mers. the effects of both 
the sph. and cyl. In this case angle a is the complement of b. 

A'=DC + D'C=(D+D')C. 

H=D Ccos6 + D'Ccos6=(D+D')Ccos6. 

V=D C sin b + ~D' C sin 6=(D +D') C sin b. 

Here A' is used in place of A because, as will be shown later, the true pris- 
matic action is not yet disclosed. 

Thus suppose + 3 Sph. o + 2 Cyl. Ax. 30° be decentered -4 cm. at 120° 

A'=(3+2)x-4=2 A . 
H=(3 + 2) x -4 x -5=1 A , V=(3 + 2) x -4x -866=4-732 A 

Oblique Sph.-Cyl. Decentered Hor. or Ver. — If the lens is decentered 
horizontally, the sph. causes no Ver. effect, but the cyl. acts as does the plano- 
cyl. Let A' be the effect in the power plane of the latter. Then 

H=D C + D' cos 2 b C=(D+D' cos 2 b) C. 
A'=D C cos b + D' C cos 6=(D + D') C cos b. 
V=D cos 90° + D' sin 2 b C cot 6=D' sin b C cos b. 

If the decentration is Ver. the sph. causes no Hor. effect, but the cyl. 
acts as when not combined with a sph. 

V=D 0+D' sin 2 b C=(D +D' sin 2 b) C. 
A'=D C sin 6 + D' C sin 6=(D +D') C sin b. 
H=D cos 90° +D' cos 2 b C tan 6=D' cos b C sin b. 


Thus + 3 Sph. o +2 Cyl. axis 30° decentered -8 cm. Hor. 6=60°. 

H=(3+2x-25)x-8=2-8 A , V=2x-866x-8x-5=-7 A . 

The same lens decentered 462 cm. Ver. 6=60°. 

A'=(3 + 2) x 462 x -866=2 A 
H=2x-5x462x-866=4 A , V=(3 + 2x-75)x462=2-08 A . 

While a Hor. or Ver. prismatic effect can never be obtained with an oblique 
plano-cyl., this is possible with a sphero-cyl. by adjustment of the decentering 
so as to neutralise the unneeded effects introduced. Practically this is best 
achieved, if it be possible, by employing a prism for the marking as described 
in Chapter XII. It is always possible if the sph. is strong compared with the 

When the plane of decentration, although not precisely corresponding, 
does not differ much from that of the axis of the Cyl., the latter may be 
ignored as, indeed, it may also be if the Cyl. is very weak compared with the 

Hor. or Ver. Sph.-Cyl. Decentered Obliquely. — In the axial plane there is 
an effect A'" from the Sph. only. Let A' be the effect in the power plane 
of the cyl., and A" that in the plane of decentration. 

A'=D Cco8& + D'Ccos6=(D + D') C cos 6. 
A"=D C + D' cos 2 6 C=(D+D' cos 2 6) C. 
A'"=D C sin 6 + D' cos 90°=D C sin 6. 

To Calculate C. — If a certain prismatic effect is required, regardless of other 
effects produced, by a decentration, C can be found by equating the formula 
given for the given conditions. 

Actual Resultant Prismatic Effects. — An oblique cyl. decentered horizon- 
tally or vertically or in any plane M' always has its greatest prismatic effect 
in the power plane M, because if 6 is the angle between the two, the power 
diminishes from M to M' as cos 2 b, although the decentration increases 
from M' to M as 1/cos b, so that the result in M is D C cos 2 oxl/cos 6= 
D C cos b. Thus a 1 D lens decentered 4 cm. in M' a plane 60° from M, we 
have in M' (l x -25) x 4 and in M we have 1 X (4 X -5). 

With an oblique sph.-cyl. the effect in the power plane of the cyl. might, 
or might not, be greater than in that meridian in which the displacement is 
made, this depending on the relative powers of the two components ; and the 
actual resultant prismatic power lies between the two, if the powers of the sph. 
and cyl. are of the same sign, and outside them if they are of opposite signs. 

The Hor. and Ver. effects of a decentration of an oblique sph.-cyl. having 
been calculated the actual resultant effect A can be obtained from the formula?. 

A=VH 2 + V 2 and tanr=V/H. 



Suppose H=2-8 A and V=-7 A ; then 

A=V / 2-8 2 + -7 2 =V8 : 33=2-88 A tan r=-7/2-8=-25=tan 14° 

General Principles. — Although definite formulae have been given in the case 
of obliquely decentered cyls. and sph.-cyls., and for finding the Hor. and Ver. 
components and the main effects, they can be worked, in each case, from 
first principles, as indicated in the following. This may be necessary if the 
decentering is neither Hor. nor Ver. nor in the principal meridians. 

Decentration in any Mer. — If a cyl. be decentered in any Mer. its effect 
in the power plane can be calculated, and from this the component Hor. and 
Ver. effects. 

Thus suppose a + 2 D Cyl. Ax. 30° be decentered -2 cm. in Mer. 70°; then 
6=50° and 

A=D' C cos 6=2 X -2 y -6428=-26 A at 120°. 

Then H=-26 A cos 60° V=-26 A cos 30°. 

If + 6 S. o + 2 C. Ax. 30° be decentered 2 mm. upwards in meridian 70°, 
the prismatic effect due to the sph. is 6x -2=1-2 A base up at 70°, while that 
due to the cyl., as from above, is -26 A base in Mer. 120°. 

Therefore there are two prismatic effects crossed at 50° (120°-70°) and the 
resultant of these can be found from the formulas given on page 258. In this 

A=Vi-2 2 + -26 2 + 2x1-2x-26x-6428=VhX)87=1-38 

•26 x -766 

tan r=- 

= •14= tan 8° 

1-2 + -26 x -6428 

So that the effect of decentering + 6 S. O + 2 C. Ax. 30° 2 mm. up in 
meridian 70°, is 1-38 A base up at 78°. 

Further, this oblique prismatic effect may be resolved into its Hor. and 
Ver. components from the formulae given previously. 

Any possible case of decentration can be worked from general principles, 
as in the examples just given, provided, of course, that proper attention be 
paid to signs, etc., but, as can be seen, the procedure is complicated. 


\ X-3 / 

^\/ x ' 


— -t- 

Fig. 285. 

Fig. 286. 

Universal Formulge. — The effect produced in any Mer. B by decentering 
a cyl. in another Mer. A can be found as follows: M is the Mer. of power, 



x is the angle between M and A, y is that between M and B, and z is that 
between A and B (Fig. 285). 

Now for a displacement C in A, that in M —Q cos x, and in B it is C cos 
a/cos ?/. The power in B is D' cos 2 ?/, therefore — 

A B =D' cos 2 yX C cos z/cos y=T> cos y C cos a;. 

For a sph. the effect in B is D C cos z. 

Opposite Powers. — It is comparatively easy to learn the prismatic actions 
when both powers are of the same nature, but when they are of opposite 
natures this becomes complicated ; they may tend to augment or neutralise 
each other. 

Thus, suppose the lens in Fig. 286 be +3 C Ax. 45° o - 3 C Ax. 135°, 
and it be decentered to the right from to 0' ; the virtual base of the + com- 
ponent is to the left downward, and that of the - is to the right downward, 
as shown by the two arrow heads. Indeed, in such a combination a Hor. 

+ Cyl. whose power is 












5° to 85° 












95° to 175° — 






- Cyl. whose power is 







5° to 85° 






Ver. — 





95° to 175° 






Equal + and - Cyls. 
+ Power. - Power. 



R L 



0° to 45° 

90° to 135° 







U D 



45° to 90° 

135° to 180° 










90° to 135° 

0° to 45° 











135° to 180° 

45° to 90° 






deceleration produces no Hor. effect whatever, but merely a Ver. one, and 
vice versa. The arrow C shows the direction of the resultant effect in the case 

In order to be certain of the position of the base of the actual resultant 
virtual prism it is better to mark out that of each component separately, 
when the one power is + and the other - . 

The table on p. 265 gives the direction of the virtual base, E, L, U, and D 
indicating respectively Eight, Left, Up and Down. The directions of the 
Cyl. are those of the powers, as shown in Fig. 286. 


Apparent Magnification. — Hitherto we have dealt only with the ratio 
between the actual sizes of object and image (real and virtual), which ratio 
may vary to an indefinite extent depending upon the position of the object 
with respect to the lens. Here we deal with what is known as the apparent 
magnification of the object — or rather, its image — when viewed through a 
Cx. lens used as a simple microscope, loupe or reader. Apparent magnifica- 
tion is not subject to such great variations as the magnification mentioned 

Magnification is expressed by linear increase of size, the superficial magnifi- 
cation being the square of the linear. Thus x 3 implies an increase of three 
diameters, while x 1/3 expresses a corresponding reduction. 

The Visual Angle is that subtended by an object at the nodal point of the 
eye, and the retinal image subtends there a similar angle. It is, however, 
more convenient to consider distances from F x , the anterior focal point of 
the eye, where the object, and the retinal image projected to the refracting 
plane of the eye, subtend equal angles, as shown in Fig. 287. 

Distance of Most Distinct Vision. — When a person views a near object so 
as to get the best possible general view of it, he unconsciously holds it, not at 
his near point, where the demand on accommodation would be very great, 
but at the most convenient distance called the distance of most distinct vision. 
This distance varies considerably in different individuals, depending upon 
age, length of eyeball, etc. Thus it is theoretically farther away in 

Fig. 287. 

hyperopia and nearer in myopia; it is decidedly nearer in youth, when Ac. 
is active, than in old age. Consequently, for the purpose of establishing 
f ormulse, a conventional value of 10" is taken as the average or standard dis- 
tance of most distinct vision. In the following articles the distance will be 
reckoned as from F x , some 15 mm. from the refracting plane of the eye. 



Magnification. — In Fig. 287, A B is an object at a distance d from F v b a 
is its retinal image, and b' a' the projection of the latter on to the refracting 
plane. C D is the same object at a shorter distance d v dcis its retinal image, 
and d' c the corresponding proj ection on to the refracting plane. It is obvious 
that the sizes of d' c' and b' a' are proportional to the angles they subtend 
at F v which are also those subtended by the object in its two positions. 
These angles, in turn, are as d : d v so that — 

__ d'c' d 


b'a' d t 

Thus if d=10" and d 1 =2 // , M=5, provided the object could be seen clearly 
without accommodation at both distances. This, however, is not the case, 
because, in order to see an object clearly at any distance the emmetrope 
must exert accommodation, for example, 4 D at 10", which, by increasing the 
refraction of the eye, reduces the size of the retinal image as compared with 
that obtained if no accommodation were used. At 2" much more Ac. is 
needed, namely, 20 D, and the total refraction of the eye would be still 
further increased, and the retinal image still further diminished. Further, 
no ordinary eye could possibly exert anything like 20 D of accommodation, 
so that an object at a very near distance is quite indistinct, owing 
to the extreme divergence of the light from its various points. It is to 
overcome this light divergence that a Cx. lens is employed as a simple 

Thus, when a watchmaker fixes a 2" lens in front of his eye at the anterior 
focus, he sees a near object apparently larger than he would, without the lens, 
at 10", because, not only does the object subtend a greater angle, but also it 
is seen without accommodation. It might be said that a powerful convex 
lens does not magnify in the popular sense of the word, but merely allows the 
object to be brought within the limits of accommodation. If accommodation 
were possible at both points, i.e. 4 D for 10" and 20 D for 2", M would be 
about 4-5. 

The Pinhole.— If an O be viewed at a certain distance by means of 
accommodation, and is then viewed through a pinhole disc, placed at F x of 
the eye, its apparent size is increased because the diminishing effect of accom- 
modation is, to a great extent, eliminated. Again, if a very small object 
be held quite close to the eye it is either not seen at all, or very blurred. If, 
now, a pinhole be introduced between it and the eye, it becomes, clearly 
visible because the pinhole cuts down the retinal confusion circles, and makes 
accommodation unnecessary. There is, of course, enormous loss of light, 
and definition may be impaired by diffraction, but the object is seen with fair 

Let an O at, say, 10 inches be viewed through a pinhole held close to 
the eye, and then gradually be brought quite close; it is seen distinctly at all 
instances, without accommodation, and the apparent change of size due 



to that of the retinal image is easily observed. In these circumstances the 
ideal condition illustrated in Fig. 287 is realised, and the expression 




rendered exact. 

The Formula for Magnification. — To obtain the true apparent M. due to 
a Cx. lens we must compare the retinal image of the object, without and with 
the lens, with equal accommodation- used in both cases. In other words, it is 
necessary to find the distance f y of the object from the lens such that its 
virtual image be projected to 10" from F x of the eye or from the lens. There- 
fore the lens is presumed to be at the anterior focus of the eye. 

Fig. 288. 

Thus in Fig. 288 is the object at a distance from the lens/ x which is 
slightly less than F, and / is its virtual image at a distance/^ which is, by con- 
vention, 10". The lens being at F v we have — 



1 1 

f + kT 

10 + F 

10 F 



10 F 

To + F' 


™ I 10 

M= o= 7l ' 

substituting f or/ x its value in terms of F- 


10(10 + F) 10 4 F 10 

or 1 + 


10 F F " "B 

This is the usually accepted formula to express the magnifying power 
when the lens is placed so that its optical centre coincides with the anterior 
focus of the eye. 

In this case the accommodation used is the same without and with the 
lens. That is to say, if the object is at 10" from F x a certain amount of accom- 
modation is brought into action in order to see it clearly. With the lens in 
position at F x the object is at/ x and the light from it, after refraction by the 
lens, diverges as if proceeding from 10". The object at^ and its virtual 
image at 10" subtend the same angle at F x so that this formula expresses the 
ratio between the angles subtended by the image and object when both are at 10", 



as shown by the projection of the object back to the plane of the image in 
Fig. 288. There is no magnification due to the lens itself because, when 
at F r no matter what its strength, it cannot alter the. size of the retinal image. 
The only effect a lens, when used as a simple microscope, can have is to enable, 
the object to be seen under a larger angle by overcoming the extreme divergence 
of the light from a very near object. 

Thus with a + 2" lens M=I + 10/2=6. 

When the lens is very strong the formula may be simplified to 

M=10/F or D/4 

A 1/4" lens has M=10/£=40 instead of 1 +40=41. 

Since the distance of most distinct vision governs the magnifying power 
of any lens it is smaller for a myope whose distance of distinct vision is shorter 
than 10" and greater for the hypermetrope whose position of most acute 
vision is greater than 10". Therefore, in the preceding formulae, instead of 
10", there would be substituted some other figure if needed. Thus, for a 
hypermetrope, where rf=16, M=l + 16/2=9. For a myope, where d=6, 
M= 1+6/2=4. 

Combinations and Cc. Lenses. — The foregoing formulae apply equally to a 
combination of lenses like that found in an ordinary eyepiece, provided the 
equivalent focal length and position of the equivalent points be known. 

As magnification results from vision of a near object through a Cx. lens, 
because the angle under which the image is clearly seen is then larger, diminu- 
tion is obtained with a Cc. lens because the angle under which the image is 
seen is then correspondingly smaller. 

General Formula. — Now the most comfortable view of an object is 
obtained when accommodation is at rest. The emmetrope, when 
using a Cx. lens for magnifying purposes, places the object at F of the lens, * 
so that the light may be rendered parallel. The hypermetrope places it 
beyond F, so that he may receive convergent light, and the myope places it 
within F, so that the light may be divergent after refraction. In all cases the 
conjugate focus of the object distance is the conjugate focus of the retina 
with accommodation passive — that is to say, the image formed by the lens 
must coincide with the far point of the eye. 

Fig. 289. 

In Fig. 289 let e be the distance of the lens from F v and let/j and/ 2 be 
respectively the object and image distance from the lens. Let d be the con- 


ventional distance of 10" from F v and the object at 10". 0' is the same 
object so placed that its image I is at R, the far point of the eye. It also 
is measured from F v that is to say, it indicates the nominal error of refraction 
of the eye. a is the angle subtended by 0, and b is that subtended by I at 
F v Then 

I I 

a 0^ <y 0'(f 2 + e) f x {f z + e) 

d d 

But f x 

F/ 2 


F+/ 2 

W+/i) <*( F +/ 2 ) 

!%(/■ + «) Wz + e) 
But / 2 =R - e. 

d(F + ~R-e) 10(F + R-e) 



The value of R is positive in myopia and negative in hypermetropia. 
When the lens is at F v e=0, so that — 

10(F + R) 
M ~ FR ' 
In emmetropia 72= oo, so that — 


for all distances of the lens from F v 

In emmetropia, when F> 10", M is less than unity, any apparent magnifica- 
tion being due to suppression of accommodation, the result being an increase 
in the retinal image between that obtained without and with accommodation. 

A farsighted person whose R= - 20" (H.2D) uses a 2" lens at 1" beyond 
F t ; then 

„ 10(2-20-1) -190 • 

M= — -= =4*75 

2X-20 -40 

with the same conditions, the person being shortsighted with R=20" (M.2D), 

__ 10(2 + 20-1) 210 roK 

M= nn — -= ,^=5-25 

2x20 40 

For the emmetrope, M=10/2=5. 

It will be noticed that when e=F — that is, when the lens is at a distance 
equal to its own focal length from F x — the expression again simplifies to 
M=10/F. The magnification for any state of refraction is then constant 
and equal to that obtained by the emmetrope. 


The variation in magnification is the same for similar degrees of hyper- 
metropia and myopia, as represented by the correcting lens at F x , which 
is to be expected seeing that the decrease and increase, respectively, in axial 
length of the eye is the same for equal degrees of nominal ametropia. 

If the object be within the focus of the lens, and the eye withdrawn from 
the latter, the retinal image becomes smaller, but when the is beyond F, 
i.e. adapted for a hyperope, the retinal image increases in size as the eye is 
drawn back. Should the obj ect be exactly in the focal plane, the retinal image 
undergoes no change, since the emergent light is parallel. In all three cases, 
however, the field of view is reduced, less being seen of the object than when 
the eye is close to the lens. 

M for at a Fixed and Lens at a Variable Distance. — When an 
object is held, not near to the eye, but at, say, the reading distance, some 
16 inches, M varies as a Cx. lens is moved to and fro between the eye and the 
object. The calculation is based on the optical system of the eye and a Cx. 
lens at a variable distance, and is shown in " Visual Optics and Sight Testing." 
The formula is — 



Fx - xy + y 2 

where F pertains to the lens, F 1 is the anterior focus of the eye, x is the distance 
of object, and y that of the lens, both measured from F x of the eye. 

This is the expression that applies when a hand glass or reader is employed, 
and the lens moved about, as distinct from a simple microscope, when the 
object is moved in order to get the best view. 

This formula shows that M=l — that is to say, the lens has no magnifying 
effect — when y=o, so that the lens is at F 1 of the eye. Also M=l when y=x, 
so that the lens touches the object viewed. In both cases the formula simpli- 
fies to Fj/x, which is the same as when there is no lens employed. 

The formula also shows that the denominator has its minimum value, 
M being at its maximum, when y—x/2 — that is, when the lens is midway 
between F x and the object viewed. 

The same serves for a Cc. lens, which also has no effect on magnification 
when at F x or at the object. The denominator has its maximum value when 
y=x/2, showing that the maximum diminution occurs when a Cc. lens is 
midway between F x and the object. 

Therefore, for any position of the object, and for any Cx. lens, withdrawal 
of the lens towards the object at first increases the magnification, which 
reaches a maximum when half-way between the anterior focus and the 
object; M then decreases until, when the lens touches the object, the mag- 
nification is the same as what it was when the lens was coincident with 
the anterior focus, this being zero. This maximum, when a Cx. lens is about 
midway between eye and object, holds good in all cases, but is quite inde- 
pendent of the clearness of the image, which may either be blurred or sharp, 
depending upon the strength of the lens. Similarly the greatest diminution 



occurs when any concave lens is midway between eye and object, but in this 
case, provided there is sufficient accommodative power, the image is clear. 
These facts explain some of the phenomena in connection with spectacle 

Best Distance. — For an object to be seen at its best through a hand glass, 
it should be placed slightly within the focus. Firstly, because, owing to the 
curvature of the field, especially in strong lenses, only the central portions are 
clearly defined, the object having to be moved nearer to bring the peripheral 
parts into focus, whereas, if the edges are rendered clear by bringing the object 
within the focus, a slight effort of accommodation will render also the centre 
sharp. Secondly, it is difficult to view a near object without involuntary 
accommodation, and therefore its exertion to a slight extent renders the 
observation more comfortable. The same applies, more or less, to the simple 
microscope, but with the latter the object viewed is generally very small, 
and therefore the peripheral definition is not of so much importance; rather 
the highest magnification possible is sought, combined with the most com- 
fortable conditions — that is, with accommodation at rest. 

Fig. 290. 

Fig. 291. 

Fig. 292. 

Special Forms oi Magnifiers in which spherical aberration is reduced. 

The Wollaston (Fig. 290) is a sphere cut into halves; these are reunited 
with a stop (of about F/5) between them. 

The Coddington (Fig. 291) is a sphere with a deep V-shaped groove so 
that the central area is reduced to about F/5, as by a stop. 

The Stanhope (Fig. 292) is a cylinder spherically curved at both ends; 
the object end being less curved than the eye end. 

To measure Virtual Magnification. — This is indefinite because it depends, 
with a given lens, on the distance it is held both from the eye and the object. 
It can be done roughly by viewing an object at 10 inches by the one eye and 
a similar object close to the eye through the magnifier. If the lens is after the 
style of a Coddington, which is not held close to the eye, the same object can 
be viewed at the same time through the lens and directly. The object 
should be, in both cases, a series of parallel horizontal lines some 5 mm. 
apart. Then the magnified image space will appear equal to so many spaces 
seen by the unaided eye. 



Polarised Light. — The beam of light transmitted by a homogeneous 
medium, such as air or glass, is ordinary in the sense that it consists of waves 
whose transverse vibrations lie in every direction across the line of travel, 
whereas the vibrations of polarised light are confined to certain directions 
only. The polarisation of light may be plane, circular, or elliptical. The 
plane of polarisation of plane-polarised light is that from which the vibrations 
are eliminated, the latter being executed at right angles to the plane of polari- 
sation. (Sometimes the plane of polarisation is taken as that in which the 
vibrations are executed.) 

Suppose a rope attached to a wall and vibrated at the free end; vibrations 
or waves will run along the rope in any plane. If, however, the rope be passed 
between two upright sticks all vibrations will be stopped except those in the 
vertical plane. The former illustrates ordinary unpolarised waves, and the 
latter plane-polarised light waves. 

Polarisation is said to be a proof of the truth of the generally accepted 
theory of the transverse wave motion of light. 

Fig. 293. 

Polarisation by Reflection. — At a certain angle of incidence, which varies 
with the ju of the medium, the reflected and refracted beams L and R 
(Fig. 293) from the glass surface A B are at right angles to each other. The 
vibrations of the incident light, which are perpendicular to the surface, 
penetrate it and are transmitted, while some of those parallel to the surface 
are reflected. The reflected beam is polarised, the vibrations being confined 



to a plane parallel to the reflecting surface, while the plane of polarisation 
(in accordance with the definition above) is perpendicular to the surface, 
and is therefore the same as the plane of incidence of the light. 

Only a small portion of the total incident light is reflected, but the 
amount is increased by increasing the number of surfaces, that reflected from 
the under surface of a plate being polarised in the same manner as that 
from the top surface. 

The angle of incidence necessary to obtain polarisation of the reflected 
beam is found by the equation i a=tan p, where p is the polarising angle. 
Thus p differs with the optical density of a medium, the polarising angle of 
water being 53°, that of glass about 57°, and that of a diamond 68°. Dif- 
ferently coloured rays have different polarising angles, so that white light 
is never completely polarised by reflection. The polished surfaces of metal 
have no polarising effect. 

Polarised reflected light can be best obtained from a sheet of black 
glass, and, of course, suitably placed with respect to the incidence of the 
light. The blackening prevents double reflection if a single beam of polarised 
light is required. 

Polarisation by Refraction. — The light, incident at the polarising angle 
on a transparent body, which is refracted and transmitted at right angles to 
the reflected beam, is partially polarised, the plane of polarisation being at 
right angles to that of the polarised reflected light. Pure polarised refracted 
light can only be obtained when a beam is transmitted obliquely through a 
bundle of thin glass plates bound together, so that, by repeated reflection, 
all light polarised in the opposite direction is got rid of. The proportion of 
light transmitted is less as the number of plates increases, while the propor- 
tion reflected is greater. 

Double Refraction. — Most crystals polarise light owing to double refrac- 
tion, notably calcite (Iceland spar), quartz, and tourmaline. A light wave in 
air or in any homogeneous body vibrates in every direction across its line of 
propagation, and its velocity is uniform and inversely proportional to what 
is termed the optical density of the medium. In a crystal, owing to its 
molecular structure, the retardation of waves, when incident obliquely to 
the axis of crystallisation, is greater in one direction than in another, so 
that the rays are transmitted along two separate paths, the one ray being 
called ordinary, and the other the extraordinary ray. 

The ordinary ray consists of spherical waves which obey the ordinary laws 
of refraction of light in homogeneous media, but the waves of the extraordinary 
ray are elliptical, and conform to no fixed law. The extraordinary ray is not 
at right angles to the wave front, nor does it lie in the same plane as the inci- 
dent ray and the normal to the point of incidence. Both rays arc polarised 
in planes at right angles to each other and travel at unequal speeds, except 
in the direction of what is known as the optic axis, where both waves have the 
same velocity and where no double refraction occurs. In planes at right angles 


to the optic axis there is also no double refraction in the ordinary sense, but 
the waves are retarded unequally, the one travelling more slowly behind the 
other. Thus doubly refracting crystals have two refractive indices, one foi 
the ordinary, and one for the extraordinary ray. 

Rock Crystal or Pebble.— Rock crystal or quartz is a pure, usually colour- 
less, crystalline variety of silica, which occurs in nature in the form of a 
hexagonal (six-sided) prism, terminating in a six-sided pyramid. Its mean 
index of refraction (^=1-54) is about the same as that of ordinary crown 
glass, but lower than that of flint glass, its dispersion ( / w H - / a A )=-014 being 
lower than either. When cut into a slab or ground to form a lens, it is usually 
styled a pebble. It is much harder than gla^s, more brittle, a better conductor 
of heat, and it transmits much more readily than glass the ultra-violet rays 
which lie outside the visible spectrum. Its density is 2-65, that of glass being 
from about 24 to 34. 

The relative scarcity and greater difficulty of working pebble makes it 
comparatively expensive. Its freedom from liability to become scratched 
is its sole advantage, so that pebble is not so good as crown glass for spectacle 
lenses, although perhaps for simple spherical convex lenses, which are fre- 
quently put on and off and therefore specially liable to become scratched 
in the centre, it is sometimes to be preferred. As lenses, the pebble 
should be quite clear and free from stria?, specks and flaws, and should be 
axis cut. 

Axis-Cut Pebble. — Axis-cut pebble is that which is cut into slabs at right 
angles to its line of crystallisation, so that when the surfaces receive their 
spherical curvatures, the axis of the crystal coincides with the principal axis 
of the lens. Axis-cut is more expensive than non-axis-cut pebble, because 
in cutting it there is not so good an opportunity of utilising those parts of 
the crystal which are free from flaws, as when the slabs are cut without 
regard to any particular direction. 

To Recognise Pebble. — Pebble is recognised by (a) feeling colder to the 
tongue than glass„{6) by the fact that on account of its hardness a file makes 
no impression on it, and (c) by the polariscope test. By the latter the 
difference between axis-cut and ordinary pebble can also be seen. As sup- 
plied to the optical trade pebble is usually quite colourless, and when in the 
form of a lens it has a sharper ring than glass. 

Double Refraction in Pebble. — Pebble possesses the property of double 
refraction, the refractive index for the ordinary ray being 1-548 and for the 
extraordinary ray 1-558, and since the index is higher for the extraordinary 
than for the ordinary ray, pebble is described as a positive crystal. It is 
because the difference in them's of the two rays is so small that double refrac- 
tion by a pebble spectacle lens is not appreciable, the images being too 
close together to be seen double, the more so since the substance of the lens 
is thin. 



Tourmaline. — Tourmaline cut parallel to its axis reduces an incident 
beam of light to two sets of polarised waves, the one in the plane of the axis 
of the crystal, the other at right angles to it. By a curious property of 
tourmaline the former (the ordinary ray) is absorbed almost immediately, 
and the latter (the extraordinary ray) only is transmitted, so that all the 
emergent plane-polarised light is vibrating in the plane parallel to the axis. 
The plane of polarisation of a tourmaline plate can be determined by analysing 
the light polarised by reflection from a plate of glass, as mentioned on 
p. 278. 

The Tourmaline Polariscope. — The simple polariscope consists of two plates 
of tourmaline cut parallel to their axes and suitably mounted. These plates 
are sometimes fitted to the ends of a wire spring like a pair of sugar tongs 
crossed, and called a pincette. If the two plates are placed in such a position 
that their axes are parallel, the plane-polarised beam of light transmitted by 
the first plate will traverse the second, and if a polariscope, so fixed, is looked 
through, green or brown light — due to the colour of the tourmaline — can be 
seen. The combination looks much more opaque than would pieces of glass 
of the same intensity of colour, because half the light received by it is 
quenched. The outer plate which polarises the light is called the polariser, 
and the second plate — the one near the eye — is called the analyser. If, now, 
the analyser be rotated, while still looking through the instrument, the light 
will be found to become less and less bright, until, when it has been turned 
through a quarter-circle, the two axes being then at right angles to one 
another, the plane-polarised beam transmitted by the polariser is stopped by 
the analyser. If the axis of the polariser is, say, horizontal, it can transmit 
only waves whose vibrations are horizontal, while the analyser can transmit 
only those whose direction is vertical ; consequently all the light is blocked 
out. So long as the two axes are oblique to one another, some light passes 
through both plates. 


Fig. 294. 


Fig. 295. 

Fig. 296. 

It is in the position of extinction of the two plates that the polariscope 
serves as a pebble tester, so that if required for that purpose, it should be 
looked through and the one plate rotated until the darkness is complete. 
Unless this is done it is useless for the work, although even if it cannot be 
made quite dark there is an appreciable difference in the quantity of light 
transmitted by glass and by pebble placed between the plates, as explained 
in the following article. Fig. 294 shows the two tourmalines with their 


axes parallel, Fig. 295 with their axes oblique, and Fig. 296 with their axes 
at right angles. 

A polariscope can be formed by two plates of black glass, arranged in 
planes at right angles to each other. The first receives the incident light at 
an angle of 57°, and the second receives the light thus polarised by reflection 
also at an angle of 57°. If the original light consists of a parallel beam total 
extinction at the second glass reflector will occur. 

A simple polariscope can also be formed by one piece of black glass and a 
single plate of tourmaline. Polarised light reflected at the proper angle 
from the glass may be intercepted and quenched by the tourmaline when the 
latter is held with its axis perpendicular to the plane of the glass, and at right 
angles to the reflected ray. In both cases, however, monochromatic light 
must be used if total extinction is to be obtained; with white light, owing 
to its constituents of varying wave-length, complete darkness cannot be 

Recognition oi Pebble by Polariscope. — If an ordinary glass lens, being 
homogeneous in nature, is placed between the two plates of the tourmaline 
polariscope, it has no effect on the plane-polarised beam of light transmitted 
by the polariser, and nothing can be seen through the instrument. A pebble 
placed in the instrument, by virtue of its double refracting nature, so twists or 
rearranges the vibrations of the beam transmitted by the first tourmaline 
plate that the light is incident on the second plate in directions other than 
at right angles to its axis, and part of it is transmitted. Hence with a pebble 
tester a pebble can be distinguished from glass, since, when a pebble is placed 
between the tourmalines, light is seen, while none is seen when glass is so 
placed. Also a slice of quartz, like most other crystals, when viewed through 
a polariscope, presents arrangements of colour which are characteristic of it. 

If a pebble cut parallel to the axis of the crystal (non-axis-cut) is placed 
between the dark tourmalines and rotated there are found two positions in 
which no light passes; the one is where the axis of the pebble is parallel to, 
or in the same line with, the axis of the polariser, and the other is where it 
bears thesame relation to the axis of the analyser. In either case, the polarised 
beam of light received by the pebble cannot be made to vibrate so as to be 
transmitted by the analyser. 

When the pebble is axis-cut a clear centre, surrounded by a series of 
coloured rings, is seen, and the light cannot be blocked out, no matter the 
position of the crystal between the two tourmalines. 

When the pebble is cut nearly, but not quite, perpendicular to its axis, 
coloured arcs of circles (incomplete rings) are seen; the light also cannot be 
blocked out, no matter what its position between the plates of tourmaline, 
because the axis cannot be made parallel to that of either the polariser or 
analyser. The intensities of the colours and the sizes of the arcs are both 
dependent on the nearness of the section of the pebble to that of right angles 
to the axis, i.e. on its nearness to axis-cut. 



Advantage of Axis-Cut Pebble. — Rock crystal which is axis-cut is prefer- 
able for lenses to that which is non-axis-cut, because in the former there is 
no double refraction for light parallel to the axis. 

Iceland Spar. — Spar or calcite, like quartz and tourmaline, has the power 
of double refraction, but since the ordinary wave has a higher index than 
the extraordinary, it is termed a negative crystal. The index of the ordinary 
ray is 1-659 and that of the extraordinary 1486, so that the comparatively 
large difference between the indices causes a corresponding high degree of 
double refraction, enabling the doubling of objects to be plainly seen through 
slabs only a few mm. in thickness. 

Fig. 298. 

The Nicol Prism Polariscope. — This is a device whereby a beam of pure 
polarised light is obtained by transmission through an arrangement of Iceland 
spar. The latter is cleaved obliquely to its axis, and the two segments re- 
cemented by balsam whose index of refraction is 1-54, or about midway be- 
tween the indices of the two rays. Now the angle of cleavage with the axis 
is so arranged that, when the ordinary ray is incident on the layer of balsam, 
it does so at an angle greater than the critical angle for indices of 1-659 and 
1-540, and is therefore totally reflected to one side. On the other hand, the 
extraordinary ray, whose index I486 is lower than 1-54, that of the balsam, 
is transmitted, and constitutes a plane-polarised beam of light which is, how- 
ever, only half the intensity of the original beam. The polariscope consists 
of two Nicol prisms, the one being the polariser and the other the analyser. 
On account of the scarcity of spar, Nicol prisms are now expensive to make, 
and are largely replaced by reflecting polariscopes of some form or other. 

Fig. 297 shows a rough outline of a nickel prism. ABD and BDC are the 
two portions cemented together by the layer of Canada balsam BD ; the axis 
is xx'. Light entering in the direction EF is divided into ordinary waves, 
which are totally reflected in the direction GH, while the extraordinary tra- 
verses the prism. 

The Wollaston Prism is used, as in the ophthalmometer, to produce double 
images. It is formed of two right-angled prisms of quartz ABC and ADC 
(Fig. 298), having their hypothenuse sides cemented together, thus forming 
a rectangle. The one prism ABC has its axis of crystallisation parallel to its 
edge A, while the other ADC has its axis at right angles to its edge C, and 
parallel to its suiface DC. Thus the axes of crystallisation are at right angles 


to each other, and for a ray of light X, incident normally on DC, the relative 
/Li of the two prisms at the surface AC is greater than unity in the one plane 
and lower than unity in the other, with the consequence that the ray is divided 
and bent partly towards the base BC and partly towards the edge A, the 
deviation in both directions being symmetrical and further increased at the 
surface AB towards Y and Z. 

The Colours of Polarised Light. — Circular and elliptically polarised light 
may be regarded as the result of two plane vibrations which are at right angles 
to each other, the circular having its vibrations equal and the elliptical 
having them unequal. The vibrations are not in the same plane, but the 
one is in advance of the other, and since the interval differs for various wave- 
lengths, the component colours of white light become separated and give rise 
to the colours seen when a crystal is viewed in the polariscope. The arrange- 
ment of the colours for each form of crystal is characteristic of it. 

A ray of light transmitted by quartz cut perpendicular to its axis (axis- 
cut pebble) is not bifurcated, but it possesses the property of rotating the plane 
of polarisation, so that the vibrations transmitted from the polariser are no 
longer at right angles to the axis of the analyser. The amount of twisting 
undergone by the plane of polarisation is proportional to the thickness of the 
quartz, and, provided monochromatic light is used, extinction could again be 
obtained by rotating the analyser through a sufficient angle. With white 
light, however, this is impossible, as the rotation of the plane of polarisation 
depends also upon the wave-length, i.e. colour of the incident ray, and there- 
fore the angle of extinction differs for each wave-length. The plane of polari- 
sation is rotated more for the short than for the long waves, and the analyser 
blocks out tho3e whose plane of polarisation is at right angles to its own, 
but transmits the complementary colour; consequently the arrangement of 
colours changes as the analyser is rotated. In addition, some of the light 
transmitted by the polariscope and the pebble must be oblique so that it 
suffers double refraction owing to the unequal oblique distances travelled 
by the two rays. A kind of interference is set up between the ordinary and 
extraordinary rays, and a series of brightly coloured rings, somewhat similar 
to Newton's rings, are seen (if white light be used) crossed by two dark brushes 
at right angles to each other. If the analyser be now turned so that its axis 
is parallel to that of the polariser, the rings will be seen to change to their 
complementary colours, and clear spaces are substituted for the dark brushes 
previously formed. A white cloud is the best source in these experiments. 

Unannealed Glass. — Glass which is unannealed, or has been subjected to 
pressure, strain, or twisting, polarises light and therefore acts in the polari- 
scope somewhat similarly to a pebble, in that light is transmitted; but the 
effects produced by unannealed glass can never be mistaken for those of crystal 
since the patterns, even if not irregular, as is generally the case, are totally 
unlike those caused by any kind of crystal . 



Interference. — If from two adjacent point sources P 1 and P 2 (Fig. 299) 
waves of light are propagated, the crests and troughs of the waves from P 1 
will coincide with those from P 2 along certain lines marked B, and reinforce 
each other, thus causing increased wave motion (amplitude). Along other lines, 
marked D, the crests from the one source coincide with the troughs of the 
waves from the other, with the result that the wave motion is neutralised 
owing to the interference of the one set of waves with the other. If the light 
is monochromatic, alternate lines of light and darkness, known as interference 
bands or fringes, are in this way produced. The light bands are along lines 
so situated that any point on them is a whole number of wave-lengths from 
P 1 andP 2 . The dark bands are along lines so situated that any point on them 

r o u_y h 


Fiq. 299. 

is one half wave-length farther from the one source than tlje other. The 
shorter the waves which interfere with each other, the less is the distance 
between the light and the dark bands. If, as in white light, there are waves 
of different lengths, the interference bands, instead of being alternately light 
and dark, are alternately red, blue and white, the latter occurring where the 
various colour bands coincide. 

In order to secure interference between the light from two sources, the 
latter must be exactly similar, giving out waves of precisely the same length, 
amplitude and sequence. For preference the sources should be the dupli- 
cated images of a single source and the smaller they are the finer are the inter- 
ference bands, also they must not be separated by too great a distance. 

The colours of thin films, such as soap bubbles, layers of grease on water, 
etc., are due to interference. Part of the light is reflected from the outer, 



and part from the inner, surface of the film, and the light reflected from the 
two surfaces is not in the same phase, a wave reflected from the inner surface 
has to travel over a greater distance than one from the outer surface. If the 
thickness of the film, therefore, be such that the inner wave emerges half a 
wave-length, or any odd number of half wave-lengths, behind the outer wave, 
they will interfere. Should the inner wave emerge in the same phase, i.e. a 
whole wave-length or any number of wave-lengths behind the outer wave, 
reinforcement takes place. 

Newton's Rings. — When two plane, or two similarly curved, surfaces, the one 
convex and the other concave, are placed in contact, the film of air contained 
between them is of equal thickness, but if the one surface is not truly plane, 
or of exactly similar curvature to the other, the film of air is of varying 
thickness, and colours, due to interference, as explained above, are exhibited. 
If a convex surface is placed in contact with a plane or another convex sur- 
face, the film of air contained between them is of gradually increasing thick- 
ness. At the centre the film is very thin, and, seen by reflected light, there is 
a central black spot surrounded by a series of alternately dark and bright 
rings if monochromatic light is employed, or by coloured rings if the light is 
white. If viewed by transmitted light the centre is bright and the surround- 
ing rings are alternately dark and bright, or of colours which are comple- 
mentary to those seen by reflected light. These are termed Newton's Rings. 

The width and regularity of the rings afford a delicate test for similarity 
between two curves, and is made use of for testing the surfaces of the com- 
ponents of high-class photographic objectives, etc. The standard curve is 
called a test plate on to which is placed the surface to be tested. The absence 
of coloured rings shows true contact over the whole of the surfaces, but the 
presence of rings proves a difference in curvature; complete absence of any 
rings is, however, rare, and the surface is considered satisfactory if the rings 
are wide and of dull colour. 

Diffraction. — When light reaches the edge of a body some of the waves, 
owing to their undulatory motion, bend round the edge of the obstacle and 
penetrate the shadow cast by it. This phenomenon is known as diffraction. 
If monochromatic light is admitted through a small aperture there is a series 
of alternate light and dark bands or rings, parallel to the edge of the shadow. 
These bands become less and less distinct as they are progressively farther 
away from the aperture, and they are broader in proportion to the length of 
the waves. If the light is white, the diffraction fringes of the different colours 
overlap and a series of coloured fringes are seen. The aperture must be 
narrow, or small, otherwise the diffraction effects are lost in the general 

Diffraction bands can be seen by looking at the sky through a pinhole, or 
through a narrow slit at, say, the filament of an electric lamp, parallel to it. 
If a hair or thin wire be placed between the light and a screen, a series of 
fringes can be seen both within and beyond the geometrical shadow. If the 



obstacle be circular, such as a small round patch on a piece of clear glass, 
the shadow is seen surrounded by alternate light and dark rings, or, if the 
source be sunlight, by a series of spectra which encroach on the shadow, at the 
centre of which a bright dot can be seen. Favourable conditions must be 
chosen to view diffraction bands. A star seen through a perfectly corrected 
telescope, and small objects seen by the microscope, appear bordered by one 
or more faint rings. Owing to diffraction, there is a limit to the possible 
magnifying power of a microscope, since the higher the power of the objective, 
the smaller the lenses, and consequently the more marked the diffraction 

The colours of many beetles and of mother-of-pearl are caused by diffrac- 
tion and interference phenomena, and are not due to pigmentation; here the 
wing-cases of the beetles, or the mother-of-pearl, are very finely striated, 
which causes them to act like irregular diffraction gratings. 

Diffraction Grating.— A large number of very fine equidistant lines — 
some thousands to the inch — ruled parallel to each other on a plate of glass 
or metal forms a diffraction grating. 

Diffraction Spectrum. — Dispersion can be obtained by reflection from, or 
transmission through, a glass diffraction grating, or by reflection from a 
metal grating; the transmitted or reflected light forms a series of spectra 
which can be thrown on a screen, or be examined by a telescope, and the 
finer and closer the lines the purer will be the spectrum obtained. 

The lines of the grating scatter a portion of the original waves into fresh 
and regular series, of which some are quenched by interference. Unlike the 
spectrum obtained by prismatic refraction, the colours as the direct result 
of interference are evenly distributed in accordance with their wave-lengths. 
The red end is not condensed, nor the violet end extended, so that the red 


R' fi' y' ltqy 




Fig. 301. 

and orange occupy more, and the blue or violet occupy less space than in a 
refraction spectrum; also the most luminous part is more nearly in the centre. 
Such diffraction gratings afford an accurate means by which to measure the 
wave-lengths of light and the relative positions of the Fraunhofer lines. 

Fig. 300 represents a portion of a highly magnified section of a glass 
grating, Q and R being the clear spaces between the lines. The distance 
Q R, equal to one ruling and one space, forms a grating element. 


Imagine parallel light falling on the grating from the direction L ; the 
bulk of the light passes through uninterrupted, so that an eye placed near 
L' will see the original source very much as it would through a piece of plane 
glass. On moving the eye to one side, so that the direction of view is oblique 
to the grating, colours will commence to appear, these being in the regular 
spectrum sequence from violet, which makes the smallest angle with the sur- 
face, to red, which makes the greatest. A short interval with no colour will 
occur after the red, but on increasing the obliquity of the eye to the grating, a 
second series of colours, in the same order as the first, but more drawn out 
and fainter, will be observed. This is shown diagrammatically in Fig. 301. 
The first, V G R, is the primary spectrum; V G' R' is the secondary spectrum, 
beyond which are others, provided the grating is not too fine ; usually only the 
primary and secondary spectra can be seen from a grating having about 15,000 
lines to the inch. As previously stated, it is by the reinforcement of the wave- 
lets diverging from the grating spaces along certain lines oblique to the sur- 
face, aided by interference, that the spectra are produced. 

In Fig. 300 consider a certain direction QP oblique to the normal L L' , 
making with the latter the angle a; or, conversely, suppose the grating itself 
be tilted through that angle with respect to the incident light. Then the 
wavelets diverging from Q and R will either reinforce or interfere with each 
other according as QP is an even or odd number of half wave-lengths — that is, 
as the difference in the paths of travel of the wavelets is an even or odd number 
of half wave-lengths. LetP Q be equal to the smallest possible even number, 
i.e. two, of half wave-lengths. Then in the direction P Q there will be rein- 
forcement giving rise, in the eye or observing telescope, to an image of the 
original source if the light be monochromatic, or to a spectrum colour, if white 
light be employed. Now 

PQ— QRsina, or w=E sin a, 

where w=P Q is one wave-length of the light in question and E=Q R is a 
grating element. The element E is known, and the angle a can be found by 
means of a revolving telescope as in the spectrometer {q.v.); therefore the 
wave-length w can be calculated from the above formula. 

Example. — Let the grating have 15,000 lines to the inch, and suppose 
the angle a for a particular part of the spectrum, say the yellow (D) line, to 
be 20°. 15,000 lines to the inch corresponds to 254/15,000 mm. to every 
grating element E, and sin 20°= -342. Therefore 

w=254x -34:2/15,000= -000579=579 mi. 

If the secondary spectrum be employed, w will represent two wave-lengths, 
so that w=E sin a/2, the result being the same as in the example given, but a 
would be rather more than 40°. 

It should be observed that no spectrum is formed when the eye or the 
observing telescope is normal to the grating, the various reinforcing and 
interfering wavelets overlapping to form white. The number of spectra 


formed is smaller as E is smaller, i.e. as the number of lines to the inch is 
greater, and vice versa. 

The most suitable source is a fine slit, brightly illuminated, placed parallel 
to the rulings, the spectrum consisting of an innumerable number of diffracted 
images of the slit ranged side by side, and representing practically a separate 
image for every wave-length. By the employment of metal gratings, special! y 
in the form of concave mirrors which focus the spectra direct on to a screen 
or photographic plate, increased intensity of light is secured. 

Luminescence is the general name given to the property of a body by 
which, without sensible rise of temperature, it becomes luminous. 

The luminosity of phosphorus, fungi and decaying vegetable matter is 
caused by oxidation. Chemical or physiological action is usually the cause of 
the light emitted by shell and deep-sea fishes, fire flies, glow worms, beetles, 
insects, animalculse, and the bacteria found in putrefying vegetable and 
animal matter. The brilliant light observed on tropical seas at night is due 
to numberless luminescent organisms. The light emitted by various insects 
is found of almost every colour in one or other species. Luminescence can 
also be produced by heating fluorspar, quinine, etc., by applying friction to 
quartz or cane-sugar in the dark, or by cleaving a slab of mica. Fused boric 
acid or even water when rapidly crystallised or frozen may exhibit this pheno- 

When a high-tension current is passed through a vacuum tube, Eontgen 
rays are produced, and the walls of the tube emit a greenish luminescence 
which is assumed to be due to minute electrified particles striking the wall 
of the tube with immense velocity and producing light and heat by their 
impact, the colour of the luminescence depending on the nature of the glass. 
Kadium is found to shine perpetually in the dark, and bodies exposed to the 
radiation of radium become themselves radio-active, i.e. luminescent for a 
time. Luminescence also includes the following phenomena : 

Phosphorescence is the term frequently given to the foregoing phenomena 
of luminescence, but it is more properly applied to the property of a body of 
being luminous in the dark after exposure to light. Some diamonds, fluorspar 
and various minerals possess this property; chloride or sulphide of calcium 
or barium, preserved from air in a sealed glass, will shine brilliantly for a 
long time. 

Phosphorescence is excited by rays of shorter wave-length than those which 
produce the phosphorescent light, although the latter may be found of every 
colour of the spectrum. It is supposed to be due to the absorption of light, 
and its later radiation, as light of longer wave-length, after the exciting action 
has been removed. When phosphorescence results from exposure to sun- 
light, the latter is termed insolation. 

Fluorescence. — Fluorescence is the property possessed by certain bodies 
of absorbing ultra-violet waves, invisible to the eye, and of emitting, by 
radiation, light of longer wave-lengths by which they appear self-luminous. 


This property was first discovered by Stokes in fluorspar, and so named by 
him fluorescence. The emission of light ceases immediately the original 
source of light is cut off, and in this fluorescence differs from phosphorescence. 

The phenomenon is not confined to the ultra-violet rays, for if a solution 
of chlorophyll be placed in a dark room and a beam of white light allowed to 
fall on it, the surface of the solution emits a red fluorescent light. A solution 
of quinine emits a pale bluish colour in the presence of daylight. The fluores- 
cence increases if the solution is held in the violet end of the spectrum, and 
is visible when held beyond the limits of the visible spectrum, the invisible 
ultra-violet rays exciting fluorescence and becoming changed into visible 
blue-violet rays. Similar effects may be seen with uranium glass, which 
fluoresces a brilliant green when placed in ultra-violet light. A thick plate 
of violet glass placed in front of a beam of light from the electric arc will 
cause the same phenomenon. iEsculine (the juice of the horse-chestnut bark), 
platino-cyanide of barium, and many other substances are fluorescent, and so 
are also the cornea, crystalline lens, and bacillary layer of the retina. 

It would appear as if sometimes the radiated light is of shorter wave- 
length than the original, so that fluorescence is generally taken to be the 
absorption of invisible light and its radiation as visible light while the exciting 
cause is present. It is said that the ozone of the atmosphere is fluorescent. 

Calorescence is the name given by Tyndall to the conversion of the in- 
visible infra-red waves into visible light. This he achieved by focussing an 
electric light, by a reflector, on to some platinum foil after passing it through 
substances opaque to visible, but transparent to infra-red light. 

Blueness of Sky. — If the air were absolutely transparent and of uniform 
density, light from the sun would reach the earth without any loss, and the 
sun, moon and stars would be set in a sky which would appear black both 
during the daytime and at night. The air, however, contains a great quan- 
tity of aqueous vapour, and the blue colour of the sky is said to be due to 
reflection from the minute particles of this vapour suspended in the higher 
layers of the atmosphere, and of so-called cosmic dust also held in suspension 
in the air. Tyndall showed that when mastic is thrown into water the minute 
insoluble particles of the mastic emit a deep-blue colour similar to that of the 
unclouded sky. If a cloud of smoke be blown into the air, the smoke particles 
reflect the short blue waves more freely, and the cloud assumes a blue tint, 
and if a white screen be held, in bright sunlight, behind the smoke, the screen 
assumes a reddish-brown hue. 

By some the blue of the sky is said to be due to polarisation by oblique 
reflection from particles of vapour, salt, etc., in the air; by others it is thought 
to be caused by fluorescence of the ozone. 

Aerial Perspective. — If two objects, one light, and the other dark, be seen 
at a considerable distance, they lose some of their contrast, the light object 
becoming darker by absorption of its reflected light by the intervening air, 
and the dark object becoming lighter by the superadded light diffused 



through the air. ' This causes what is known as aerial perspective. If the 
air is clear and the added light is blue, distant hills throw deep shadows of a 
purple-blue colour in bright sunshine. 

Eclipses. — A total eclipse of the sun occurs when the moon is so situated 
that some portion of the earth lies in the umbra of the shadow cast by it; 
the eclipse is partial to those portions of the earth in the penumbra of the 
shadow. An eclipse of the moon occurs when the moon lies in the shadow 
cast from the sun by the earth. 

Light Streams. — The stream of light seen reflected from the surface of the 
sea, or other body of water in motion, in bright sun or moon light, is due to a 
series of imperfectly formed images, of the sun or moon, reflected from the 
ripples of water so that they enter the eye proceeding from different points. 
If the water is quite smooth a definite image of the luminant is perceived. 


Fig. 302. 

Fig. 303. 

The Rainbow. — A rainbow is visible when the sun is behind the observer 
and a shower of rain in front of him, or it may be seen in the spray of a 
waterfall. Since the sun's rays falling on the raindrops are parallel, the 
course of light through all the drops must be the same, and it is therefore 
sufficient to trace the course of a ray through a single drop. Let a pencil of 
rays from the sun meet the drop at A (Fig. 302). On entering it is refracted 
and dispersed towards B and C at the back of the drop, thence reflected to 
D E, where it is refracted to emerge in the directions V R which make an 
angle with the entering ray. The emergent dispersed light thus diverges to 
the observer's eye, and the various colours, being unequally refracted, are 
projected back as R' V, so that the outside of the bow is red and the inside 
blue- violet. The extent of the bow depends on the position of the sun; when 
the latter is at the horizon the bow forms a semicircle to an observer at sea- 
level. As the sun rises the arc sinks so that its centre is below the horizon 
and is smaller. 

A secondary larger, broader and fainter rainbow is generally seen con- 
centric with the primary. The rays from the sun to a point A (Fig. 303) 
undergo refraction and are reflected twice at B C and B' C, and again re- 
fracted at D F. In the emergent light violet is below and red above ; these 
being reversed on projection, as V and R', the secondary bow is blue on the 
outside and red within. 



In Fig. 304 E is the eye and // the horizon, R is the rainbow. The semi- 
circular arc of the primary bow subtends at the eye an angle of some 42° for 
the red and 40° for the violet. The angles subtended by the secondary 
rainbow are about 54° for the violet and 51° for the red. 

Fig. 304. 

The Horizon. — When the sun is low down on the horizon its light has to 
pass through a thicker layer of atmosphere filled with dust particles and 
moisture; more of its blue and violet rays are absorbed or reflected, and it 
thus appears reddish, as for the same reason it appears red in a fog. 

Near the horizon, the sun and moon appear larger than when higher in 
the heavens because they are mentally projected beyond the horizon, as 
compared with terrestrial objects, whereas when seen in the zenith this 
cannot be done, as they stand alone; they are not really larger, as measure- 
ments with a telescope show. They also appear slightly flattened vertically, 
when near the horizon, and appear a trifle higher up than they really are, 
owing to the refraction of the air and the greater obliquity of the light from 
their lower edges. 

Refraction diminishes the dip of the horizon and so slightly increases its 
apparent distance. The distance of the horizon can be computed approxi- 
mately from d=Vl-5h, where h is the height in feet of the observer above 
the sea or earth level, and d is the distance in miles. For nautical miles 
d= Vl-3 h. The derivation of this formula is shown in " Simple Calculations." 

Mirage (Fata Morgana). — If the layers of the air are of markedly un- 
equal density, as is sometimes the case in hot climates, especially on a desert 
where the warmest layers are the lowest, the phenomenon known as the 
mirage may be seen. Light from objects above, on its passage to the earth, 
traverses layers of air which become gradually less refracting, the angles of 

Cool at/- 


Hot -aX j 


Hot sand 

Fig. 305 

warn e' at + 

Cold, water 

Fig. 306. 

incidence accordingly increasing so that the light becomes more and more 
parallel to the surface, until at length the critical angle is reached, beyond 
which refraction changes to reflection. The light is then reflected in the con- 
trary direction, and ascends to reach the observer's eye as if proceeding from 


a point below the ground, and objects appear inverted. This is shown in 
Fig. 305, where light from an object 0, on reaching the eye at E, appears to 
come from M below the level of the ground. 

If the lowest strata of air are the densest, as in Fig. 306, they give rise 
to the same phenomenon, but the mirage M is in the contrary direction, so 
that a landscape, or a ship at sea, may appear above the horizon. This occurs 
in very cold climates. 

Scintillation. — The twinkling of a star is due to irregularities in the atmo- 
sphere causing variations in the path of the waves, which partially interfere. 
This produces variations in the apparent brightness and colour of a source 
of light, subtending a very "small angle at the eye, such as a star. It is not 
observed in the case of a planet, because this has a real magnitude. 



Refraction and Reflection Compared. — A spherical mirror may be regarded 
as a dioptric system in which i tt 1 =/* 2 anc * therefore F 1 =F 2 . It resembles a 
single refracting surface in that the principal point is at the vertex of the curve, 
and the nodal point or optical centre is at the centre of curvature, but it 
resembles a lens in that F is equally distant from the principal and nodal 
points. F is midway between them in a mirror, and they are united in a lens. 
Also the mirror resembles the lens in that the first and last media have equal 
fi's, the source and its image are both in air, and therefore F 1 =F 2 . 

If light is incident on a plane-polished surface it is partly reflected and 
partly refracted. If r is the angle of refraction and r' that of reflection we 

fjL x sin i=ju 2 sin r=fi 2 sin r', 

but for the reflection /bi 2 =fj, v and therefore »•'=?'. The relationship between 
the angles of reflection and refraction is 

sin r' sin i /jl 2 
sin r sin r fi x 

If ^ 2 =i.5, suppose a ray with an angle of incidence of 9°; then r'=9° 
and r=6° approximately. The angle between the reflected and refracted 
rays is 180- (r + r') which becomes 180° when incidence is normal, and 90° 
when incidence is that of complete polarisation. 

With a curved surface by reflection and refraction respectively, we have 

112 , 1 

— = — r=- an d x-> 

F r/2 r 2r 

therefore reflection is four times as powerful as refraction, or six times as 
powerful, if compared with the posterior power of a surface. 

If the surface of a Cc. lens is used as a reflector, to find F, /u being taken as 
1-5, the dioptric F of that surface is four times as long as the catoptric F. 

If a Sph. mirror be placed against a lens measure scaled in diopters, 
F is 1/1 that shown by the scale. Thus if a mirror shows 2-5 D, its F is 100/ 
(2-5x4)= 10 cm. 

Figs. 307 and 308 show the difference in F when an incident beam of light 
is reflected from, or refracted by, a thin piano Cx. or Cc. glass lens of //=l-5. 
of which C is the centre of curvature. Light parallel to the axis, if reflected, 




meets at jR, which is half the distance of C from the poleP; if refracted it 
meets at F, which is twice the distance of C fromP. The thick lines represent 

Fig. 307. 

Fig. 308. 

the refracted rays and the dotted lines the reflected rays. A Cx. surface 
is a positive refractor and a negative reflector, while a Cc. surface is a negative 
refractor and a positive reflector, when it is adjacent to air. 

Refracting Reflector. — A lens silvered on its second surface so that refrac- 
tion and reflection occur is termed a Mangin mirror. 

Fig. 309. 

In Fig. 309 a lens of index /u has two surfaces A andP of radii of r x and r 2 
respectively; the surface B is silvered. A ray of light a, parallel to the axis, 
and incident on A, is refracted towards/, the posterior focus of that surface 
such that 


f Fi ' 

The ray on arriving at b on the second surface B is reflected and the power of 
the mirror is 2/r 2 , so that the convergence of the light becomes 




1 2 

- + - 

2/JW 1 + r t (jJi-l) 

[xr x r 2 /urfa 

This expression is the conjugate virtual object power \/f x with respect to 
the first surface A towards which the light is now directed, and from the 
conjugate formula for a spherical surface, when/ x is in the dense medium and 
f 2 is in air, 

1 ju - 1 jil 

fi~ r i fi 


Now/j is positive, since the light in this case is convergent, so that, sub- 
stituting for \ff x the expression \/f above 


Jjt 2 {fi- l)+2pr 1 

The value of l/f 2 is the ultimate convergence of the light after refraction at 
c, and/ 2 is the focus of parallel light due to the Mangin mirror, and therefore 
can be written 1/F. That is, 

1 _ 2r 2 (/n-l)+2jur 1 2(^-1) 2//_2( / u-l) 2(fi-l) 2 
F ~ i\r 2 r x r 2 ~ r x r 2 r 2 

AT 2(^-1) 1 ,2(^-1) 1 . 2(^-1) 2(^-1) 2 
Now r — =— and -^— — =„ also r + ^TL __'_ 

F x r 2 F 2 r x r 2 F' 

where 1/F X and 1/F 2 are the anterior focal powers of the two surfaces and 
1/F' is the power of the whole lens, so that the power of the Mangin mirror is — 

12 2 12 2 2 

-i — or — = — i- h — • 

F F' r 2 F Fi F 2 r 2 

These last formulae show that the convergence — or divergence — of the light 
received from a Mangin mirror, is precisely the same as if the metal constituted 
a mirror separated from the back surface of the lens, so that the light passes 
through, and is refracted by, both surfaces, is then reflected by the mirror 
and again refracted by the two surfaces of the lens a second time. 

The result is the same whether (a) the back surface is silvered, (b) the 
lens is backed by a mirror having a curvature exactly the same as that of the 
second surface, (c) if the lens is neither silvered nor has a backing mirror; 
in this last case, however, only a very small proportion of the light is reflected 

If the form of the lens, F' andyU are known, r 2 has to be calculated and F 
varies, if the two surfaces are unequal, according to which is silvered. 

For a double Cx. or Cc. — =— — — . 

F r 

1 2 a - 2 

For a plano-Cx. or Cc. with the plane surface silvered -=— 

1 x F r 

1 2u 
For a plano-Cx. or Cc. with the curved surface silvered -=— . 

F T 

The second surface of a lens is positive or negative, whether it acts as a 
refractor or a reflector, because, if Cx. towards the air it is Cc. towards the 
glass, and vice versa; and since the reflective power of a surface is four times 


as great as its anterior refractive power when / u= 1*5, we can write for the 

Mangin mirror 

1 2 6 

===== + w or D=2D 1 + 6D.„ 

F F t F 2 * 2 

where F t and D x pertain to the first surface, and F 2 and D 2 to the second. 

For a double Cx. all powers are positive and for a double Cc. they are all 
negative, and D of the. Mangin mirror is equal to 4 D of the lens. 

Thus with a lens of D x = + 1 and D 2 = + 2, we have D= + 14. 

If T> 1 = + 4 and D 2 = - 2, we get D = - 4 ; if this lens were turned the other 
way D=+20. 

The effect of a Cx. or Cc. periscopic may be positive or negative as the one 
or the other surface faces the light. 

In order that incident parallel light emerge as parallel it is necessary that 

-r x [A, r x fi 

[I - 1 fJL-l 

or approximately r 2 = - 3r v i.e. when the radius of the reflecting surface is 
equal to the posterior focal length of the first surface, parallel light retraces 
its own course; or the second surface must be of opposite nature to that of 
the first and of one third its dioptric power. 

The ordinary Cc. glass mirror is silvered on the back surface and has a 
positive F=r/2, the same as if the metal itself were exposed to the light. 
The light is diverged twice at the front surface, but a preponderating con- 
vergence takes place at the second. 

Optical Glass. — Glass is a hard, generally transparent or translucent sub- 
stance, made by the fusion of silica with potash, soda, lime, lead and other 
substances, such as pearlash, arsenic, manganese, saltpetre, chalk, etc. It is 
brittle, sonorous, ductile when heated, and fusible only at a very high tem- 
perature. It is usually not soluble, but is acted on by hydrofluoric acid, 
and is a very bad conductor of heat. There are many varieties of glass, and 
the process of manufacture, as regards the ingredients used and the treatment 
after complete fusion of the various components, depends on the nature of 
the glass to be produced. 

If suddenly cooled, glass becomes extremely brittle owing to the state of 
tension produced by the cooling of the outer portions while the inner are 
still in a molten condition; annealing tends to reduce brittleness. Glass 
used for optical purposes must be homogeneous, i.e. of equal density and 
refractive power throughout, and perfectly transparent; it is therefore care- 
fully mixed and gradually cooled. It should also be free from air bubbles, 
stria; and colour for spectacle lenses, although a few air bubbles, if small, 
may be of little or no consequence in a camera lens. The solid block of glass 
is usually polished on two sides, so as to allow of the detection of defects, 
and from it clear discs of appropriate size are cut. 



To detect strain a polariscope (q.v.) is required. To detect striae, bubbles, 
etc., the glass should be examined by the eye in the focus of a combination 
such as is constituted by an erecting eyepiece. The light diverges from F L 
of the first lens, is rendered parallel, passes through the plate to be examined, 
and is converged by the second lens to the examiner's eye. Striae, etc., are 
disclosed by patches or streaks which spoil what should be a uniformly bright 

Lenses are made of crown glass, which contains lime, or of flint glass, 
which contains lead. Flint has generally a higher refractivity and chroma- 
tivity; the greater the proportion of lead in the glass the greater, usually, 
are the refractive and dispersive powers. It is denser, heavier and softer 
than crown, and is almost perfectly colourless. Crown glass has the advan- 
tage of lower dispersion and is harder, so that it does not so easily become 
scratched, but it is more brittle than flint. It has sometimes a decided 
greenish tint, due to the presence of iron. The pinkish tint found in some 
glass results from the admixture of manganese. 

According to its component ingredients and manufacture, the indices of 
refraction of glass vary for the various lines of the spectrum, the mean jn of 
crowns being, say, 1-52, and of flints 1-62. 

The following may be taken as very rough examples of the proportions 
of the materials entering in the manufacture of optical glass: — 

Flint Glass (100 parts). — Silica 50, lead 30, potash 10, other in- 
gredients 10. 

Crown Glass (100 parts). — Silica 70, soda 10, lime 10, other in- 
gredients 10. 

In the following table some examples (not actual kinds) are given to 
illustrate the refraction, dispersion and specific gravity of different kinds of 
optical glass, and the method generally employed in arranging them in the 
order of their v values or efficiencies. 









C - F= Sft 

A-D D-F 



Very light crown 




0-0050 00055 



Light , , 




0-0055 0-0065 



Ordinary ,, 




00060 0-0070 



Heavy ,, 




0-0065 00075 



Very heavy ,, 




00070 0-0085 



Very light flint 




0-0075 0-0090 







0-0085 0-0095 



Ordinary ,, 




0-0095 0-0115 



Heavy ,, 




0-0105 0-0130 



Very heavy ,, 




0-0185 0-0280 








Water (distilled) 




Absoluto alcohol 

Oil of bergamot 

Olive oil 


Gum arabic 


Bisulphide of carbon 



Rock salt 

Salt solution . . 



Chroma to of lead 

Canada balsam (liquid) 


. . jWd = 

. . flo = 

.. fl D = 

• • /** = 

.. /X B = 

. . /x D = 

. . jU D = 

. . ^ E = 

. . fl D = 

. . jU S = 

. . /1e= 

. . [X D = 

. . fl v = 

■ . /i D = 

• • ^D = 

• • / «E = 

• • A*D = 

• • ^D = 

2-500 to 


Canada balsam (hard) 

i«D = 


Oil of cassia 


Oil of fennel 



Anilin oil 

i"D = 


Oil of cloves 

A*D = 


Oil of cinnamon 

A« E = 


Cedar oil (lens immersion oil) 

A'd = 



^B = 



M E = 


Rock crystal, pebble (ordinary 


A*D = 


Rock crystal, pebble (extra 


^D = 


Tourmaline (ordinary ray) . 

f^D = 


Tourmaline (extraordinary) . 



Iceland spar or calcito (ordin 

ary ray) 



Iceland spar or calcito (extra 





jUe = 



flu — 




YeUoiv (D). 




























Discs for Lenses. — When a lens of certain power and diameter has to be 
worked, the thickness of the blank should be such as to avoid undue grinding 
down (if too thick) or failure to obtain the finished lens (if too thin). The 
necessary calculation is based on the simplified spherometet formula, writing 


Fig. 310. 

t for the required thickness in place of S, the sag in the original. Then £= 
fZ 2 /2r for each surface, where d is half the longer diameter of the finished lens. 
For the whole lens, t for the one surface must be added to that of the other, 
as in Fig. 310. 



With sufficient accuracy the radius of a plano-Cx. or Cc. lens is half the 
focal length, and that of a double Cx. or Cc. is equal to the focal length. If, 
say, a lens of 10 cm. F were needed in plano-Cx. form, r=5 cm.; if the lens 
were double Cx. each r=10 cm.; therefore T, the total thickness, is precisely 
the same for both forms of lenses. Also we can use C, the total diameter 
of the lens, in place of d, the semi-diameter; that is, d! 2 /2/=C 2 /8r, and since 
we take 2r=F we can write as a general formula for thickness of disc 


C 2 

This formula serves for all lenses no matter how the powers are distributed 
provided both surfaces are Cx. or both Cc. For periscopics the surface of greater 
power only need be reckoned for. The long diameter of an oval lens must be 
taken for C and F and C must be in the same terms, preferably mm. The 
total T, thus obtained, is the minimum and allows only for a knife-edge Cx. or 
a wafer thin Cc. ; generally an additional thickness of 1 mm. is needed for the 
bevel of a Cx. lens or the central thickness of a Cc. For diopters T=C 2 D/400, 
all terms being in cm. T for a cylindrical surface is calculated as for the 
same power spherical. 

Thus for a + 20 D. DCx. lens of 37-5 mm. diameter, that is, ordinary test 
case size. Then F=50 mm. and 


37-5 2 
= 4x50 

= 6 mm. and 6 + 1 = 7 mm. 

For a curved protector of r=20 cm. and diameter 30 mm. 

30 2 
T= 20Cb<8 = ' 56 mm ' ° r Say 2 mm ' 

For ordinary spectacle lenses the approximate thicknesses are 

1 eye 
00 eye 

1+300/F, or 1+-3D. 
1+400/F, or 1 + 4 D. 

eye . . 1 + 350/F, or 1 + -35 D. 
000 eye . . 1 + 450/F, or 1 + -45 D. 

Lens Sizes. — American standard eyes, with their axes, and length of wire 
needed to make a standard eye wire in mm., are given in the following: 














34 x26 

35 x26 







41 x32 



46 x38 



The numeration, based on peripheral measurement, as given in the next 
table applies to all shapes, the ratio of the long to the short axis of the oval 
being approximately 1-3 to I, and that of the long oval 1-5 to 1. 




Length of Periphery. 




Long Diameters. 






\ Oval. 



92-5 mm. 









94-5 „ = 92-5+2 









97-5 ,, = 94-5+3 









101-5 ,, = 97-5+4 









100-5 ,, =101-5+5 








112-5 ,, =100-5+6 







Power of Cement Bifocals. — The power of the segment or wafer in a cement 
bifocal is that which, added to the main lens, gives the power required for 
reading. The index of refraction of the Canada balsam, by means of which 
the wafer is joined to the main lens, is practically the same as that of the glass, 
so that it need not be considered. 

The free surface of the segment must be the total reading power less the 
power of the free surface of the main lens. The power of the contact sur 
face of the segment must be that of the contact surface of the main lens, but 
of opposite nature, so that they neutralise each other. Suppose the two 
powers be +2 for distance and +3 for reading (Fig. 311). If the main lens 








Fig. 311. 











Fig. 312. 

Fig. 313. 

Fig. 314. 

is double Cx. with + 1 on each surface, the segment would need to be - 1 
on the contact and + 2 on the free surface. If for the same powers the main 
lens is periscopic Cx. the two surfaces would probably be +3-25 and - 1-25 
(Fig. 312). The wafer would then be +1-25 on the contact surface, and 
- -25 on the other, the wafer being placed on the Cc. side of the main lens. 
If placed on the Cx. side, the contact surface of the wafer must be - 3-25, 
and the free surface + 4-25 D (Fig. 313). 

If the main lens is - 5 D Cc. and the reading power is - 2-5, then the 
segment requires to be a + 2-5 on the contact surface and piano on the 
other (Fig. 314). If the main lens is -7 periscopic Cc. with, say, +1-25 
on the one surface, the segment, if placed on the Cc. side, is +8-25 on the 
contact, and - 6-25 on the free surface, for a reading power of - 5 D. 

When the main lens is a plano-cyl. the segment is attached to the plane 


surface. When the main lens is a sph.-cyl. the segment is attached to the 
spherical surface. Thus with, say, + 3 Sph. o + 2 Cyl. with an addition 
of +2 for reading, the wafer must have powers of - 3 and +5. 

Centering of Cement Bifocals. — The added segment is always Cx., the 
lower part being weaker if the upper is Cc, and stronger if the upper is Cx. 
If the wafer is itself centered, the prismatic effect due to decentration of the 
main lens remains. For a properly centered lower, the segment of the bifocal 
must have a prismatic effect contrary to that of the main lens where they 
are united. This is obtained by decentering the segment to the requisite 
extent. When the main lens is Cx. the prismatic effect of its lower portion 
is base up, so that the wafer must be base down, its thick part being at the 
edge of the main lens. If the latter is Cc. its prismatic effect is base down, 
and therefore the segment must be base up, i.e. its thin part must be at the 
edge of the main lens. 

In Fig. 315 A is the geometrical and optical centre of the main lens, and 
B is the optical centre of the reading position; the distance A B is usually 
about 8 mm., but may vary. Let D x be the total power of the main lens, 
and C x be the distance A B. Let D 2 be the power of the segment by itself, 
and C 2 its needed decentration in cm. Now, in order that there be no pris- 
matic effect at B it is necessary that D x C 1 =D 2 C 2 , so that the formula for 
calculating the needed decentration of the segment is 


D x is the power of the spherical, or the vertical power of a cyl., or sphero- 
cyl., whose principal meridians are vertical and horizontal. 

Let the upper be +4-5 D. and the lower +6; the segment is +1-5, so 

C 2 =4-5x-8/l-5=24 cm., the thick part down. 

Let the upper be - 3-5 and the lower - 1, the segment being +2-5; then 

C 2 =3-5x-8/2-5=l-l cm., the thick part up. 

The amount of decentering is often very large, and demands either that 
the blank from which the segment is taken be of extra large dimensions, or 
the segment be ground on a prism. 

It is necessary to place the optical centres of the lowers each 1-5 mm., or 
so, inwards in order to allow for convergence when reading. If the main 
lenses are Cx. their prism action is base out, and that of Cc.'s in. To neutralise 



this the segments must be decentered in if the main lenses are Cx., and de- 
centered out if they are Co., such horizontal decentration being considered 
for the centres of the reading portions which are in from those of the uppers. 
The difference between the position of the optical centre of each eye for 
distance and for reading varies, but 1 -5 mm. is a good average. In all cases 
the actual amount of decentering of the wafer required, so that the lowers may 
not be decentered when used for near work — the required position should be 
marked by a dot — can be obtained by sliding the segment over the main lens 
while viewing the small crossbar as described for centering. 

Inset or Fused Bifocals are made by inserting a segment of high curvature 
and high^ into a depression made in a main lens of low ju. 

To calculate the curvature of the segment, let D x be the distance power 
of the whole lens, and D 2 the reading power; let^ be the index of the main 
lens, and /u 2 the higher index of the segment. The radius of curvature of a 
surface, separating two dense media, when the focus is finally in air, is 

r=F( / M 2 - ; a 1 ) or r= 1Q0( fa- fiJ/D 

It is necessary to find the tool which, made for producing a certain dioptric 
power D when the index isjn v shall give to the internal surface of the segment 
of ^ 2 tne necessary power D 2 , after allowing for the powers obtained from the 
two outer surfaces D 4 and D 5 (Fig. 316). Let D 3 be the outer power of the 
surface containing the segment, D 4 the outer power of the segment, D 5 the 

Fig. 316. 

power of the surface not containing the segment, and D 6 the power of the in- 
ternal segment surface between the two glasses. Then 

D 6 =D 2 -(D 4 + D 5 ). and D 4 =D 3 (// 2 - l)/(/"i- !)• 

The lens may be of various forms, as shown in Fig. 316. 

D ^ D 6 (^ 1 -1 )_(D 2 -D 4 -D 5 )(^ 1 -1) 

/ W 2 _ i M l f J '2~f J 'l 

Now D 4 being of higher /u, although of the same curvature as D 3 , which 
is known, is of greater power such that D 4 =D 3 (^ 2 - l)/^- 1). Therefore 

D 3 (A*, - 1)~| / ^ 1 -l \ (D a -D 5 )(^ 1 -l)-D 3 (A* 2 - 1) 

D -r P .-D.-^<^- l >i(ft=i) 

l /iri j y 2 -/v 


The values of D 2 , D 3 and D g and those of the two^t's being known, this 
equation serves for all forms, whether Cx. or Cc, shown in Fig. 316. For a 
sph.-cyl. form A is used and D 5 disappears from the equation; for a plano-cyl. 
form B is employed and D 3 disappears. Thus for a plano-cyl. of form A 
having T> 1 = - 1*5, and D 2 =0, them's being 1-52 and 1-65, we find 

_0x (1-52 - 1) - [- 1-5 (1-65 - 1)]_ + -975_ 
D= 1-65-1-52 13 ~ 

LetD 1 = +-5 and D 2 = +2-25, made periscopic so that D 3 = +1-25 and 
D 5 = - -75; using form (D) we get 

[ + 2-25 - ( - -75)] -52 - (1-25 X -65)_ -7475 
1-65-1-52 ^l3" : 

If them's are 1-52 and 1-65, D=4 (D 2 -D 5 )-5 D 3 for forms G, D and 
E; D=4 D., - 5 D 3 for form A ; D=4 (D 2 - D 6 ) for form B. 

If them's are 1-5 and 1-6, D=5 (D 2 - D 5 ) - 6 D 3 for forms C, D and E; 
D=5 D^- 6 D 3 for form A ; D=5 (D 2 - D 5 ) for form B. 

The disc selected must be rather thicker than for ordinary lenses, especi- 
ally if the segment is of high power. 

Having insets of known powers the selection of a suitable blank and the 
curvatures of the two outer surfaces are as follows : Let the two^'s be 1-65 
and 1-52 so that for a given curvature producing D 3 we have D 4 =5 D 3 /4, 
i.e. D 4 is 1/4 stronger than D 3 , and D 4 - D 3 =D 3 /4. Now part of the additional 
power for reading is obtained from D 4 - D 3 , and part from D 6 , i.e. D 2 - D x = 
(D 4 -D 3 ) + D 6 ; therefore the powers needed on the two surfaces are D 3 = 
4 (D 2 - D 4 - D 6 ), and D 5 =D 4 - D 3 . 

It is preferable to select a disc such that D 6 is higher than the addition 
needed for reading, and in that case D 3 is Cc. if D x is Cx. 

In all cases it is advisable to calculate two or three combinations in order 
to arrive at the most suitable. 

If a Cc. curvature is given to the surface of D 5 there is danger of working 
through to the segment. 

If D^Djj-Di the surface D 3 is piano; therefore for sph.-cyls. select 
D 6 --=D 2 - 1-25 D l5 the cyl. being to the side of D 5 , and the sph. to that of D 3 . 

The proportional increase of power of D 4 over D 3 is found from 



so that if the two /u's are other than those given above, the factor 4 in the 
value of D 3 would vary accordingly. 

As examples, for B l = +2-25, and D 2 = +3-5 select D 6 =l-5; then 
D 3 =4x (1-25- 1-5)= -1, and D 5 =2-25 + l= +3-25. 

ForD^-3-5, and D,= - 2-25 select D 6 =2-5; thenD 3 =4x (1-25-2-5) 

= - 5 and D 5 = - 3-5 + 5= +1-5. 


For +6 S. o -2 C. with +8 S. for reading, D 6 = +8 - 1-25x6= -5. 
For - 10 S. o - 3 C. with - 7 S. for reading, D c = - 7 + 1-25 X 10=5-5. 

To Construct Test Types after Snellen. — Each letter is a square block and 
at a certain distance d for which it is designed, it subtends an angle of 5'. 
Each limb of each letter is one fifth of the total diameter and subtends an 
angle of 1'. 

The general formula is 8=d tan V, where S is the size of the letter, d 
is the distance in mm., and V is the visual angle. Tan 5'= -001455 and tan 
1'= -000291, so that the diameter of each letter is 

S=1000x -001455=1-455 d (d being in M. and S. in mm.). 

The diameter of each limb is similarly obtained from -291 d, but the letter 
dimension divided by 5 gives the limb dimension. 

The diamete-r of any letter in inches=12x -00145=-0174 d (d being 
in feet). 

Thus for 6 M. the types are 6x1-455=8-75 mm., those for 12 M. are 
17-5 mm., and so on for every other distance. 

If the visual angle is other than 5' the size in mm. is 

S= -000291 x visual angle in minutes of arc X distance. 

The size of the types can also be calculated from circular measure. The 
ralian=57-3°=3438'.; if an angle is smaller the arc, subtending it, is propor- 
tionately smaller, so that 

V/3438=S/rf or S=V rf/3438. 

Suppose the types be required for 18 M. under a visual angle of 4'; then 

S=4x 18000/3438=21 mm. (approx.). 

Mirror for Reversed Test Types. — The necessary size S of the mirror 
depends on the size C of the chart, and the distances d' between the mirror 
and the chart, and d, that between the subject and the mirror. The mirror 
should be just large enough to be filled entirely by the image of the chart. 

S d n Cd 

or S= 

c d+d' d+r 

If, as is generally the case, d + d' =6 M., the subject and the chart being 
at the same distance, i.e. 3 M. from the mirror, the latter is just one half the 
size of the chart in both dimensions. 

To Construct Tangent Scales. — With quite sufficient accuracy the spacing 
S of a tangent scale for use at a distance d is 


where K=l for A , K=l-75 for °d and K=-9 for degrees of prism. Thus for 
prism diopters the card must be scaled so that each division shall be 1 cm. 
for each M distance at which it is used. Each division is for 20 ft., a one 


hundredth part of 20 ft. multiplied by the constant pertaining to the notation 

On a scale, shown in Fig. 132, used at 2 M. the numbers indicate degrees 
of deviation, at 3-5 M. they indicate prism diojiters, the divisions being each 
3-5 cm. Thus if a given prism at 2 M. indicates, say, 4 it is a 4°d; if held at 
3-5 M. it will indicate 7 A , which is the equivalent of 4°d. 

In order that equal divisions should indicate accurately equal increase of 
angular deviating power of prisms, the scale should be on an arc at the centre 
of which the prism is held. This is the basis of the Centrad notation which, 
however, owing to the inconvenience of such an arrangement, did not come 
into general use. 

On a flat surface the divisions should be d tan 1°, d tan 2°, etc., where d 
is the distance at which the chart is used; that is, the successive spaces should 
increase in size, since tangents increase more rapidly than do the angles of 
deviation. For small angles, however, it is sufficiently accurate to make 
each division in cm. = 1-75 d, where d is the distance in metres. Thus for use 
at 3 M. each division would be 3x1-57=5-25 cm. approx. 

Ii/u is taken as 1-5 the divisions for degrees should be -875 cm. for each M. ; 
if ^=1-52, they should be -9 cm.; if/^=l-54 they should be -94 cm. In prac- 
tice the A scale serves for degrees. 

Artificial Sun. — Practically a collimator (q.v.) constitutes an artificial 

sun, but the best conditions are obtained if the aperture subtends at the lens 

an angle of 30'. The aperture is at the focal distance of the lens employed, 

Fx -5 

so that its aperture a= =F/114. That is, a: F as -5°: a radian. If the 

1 57 

lens is of 150 mm. F (6 inches) the best aperture is of 1-3 mm. diameter. 

Pinhole Apertures. — Since light travels in straight lines, if that from a 
candle flame be allowed to pass through a small aperture on to a white screen, 
an inverted image of the flame is formed on the latter. The relative sizes oi 
image and object are as their respective distances from the aperture; thus 
they are equal in size when the two are equidistant from the aperture. The 
image is smaller if the screen be brought nearer to the aperture, or if the 
candle be moved farther away, and vice versa. Generally the smaller the 
aperture, the sharper but less bright is the image. 

In order that a distinct image of a flame may be seen on a screen, it is 
necessary that the rays from each point of the luminous body should not, 
on the screen, overlap those from adjacent points of the source. This may 
be said to occur practically when the light passes through a minute aperture, 
because then only a very narrow pencil of light — the cross section of which 
is similar in shape to that of the aperture — from each point can reach the 
screen, and for the same reason the image thus formed is faint. 

The shape of the small aperture does not materially affect the shape of the 
image, nor its distinctness. Thus when the sun shines through the gaps in the 
foliage of a tree, each of these gaps varies in size and shape, but the luminous 


images of the sun form bright discs on the ground, all identical in shape unless 
the gaps are large. 

If the number of apertures be increased, the number of images will 
similarly increase with the number of holes, until the images will so overlap 
one another that it is impossible to distinguish them separately, and there is 
a general illumination of the screen. 

Although the smaller the pinhole the better is the image defined, yet if 
the aperture be too small the image is blurred by diffraction. Hence the 
aperture should be theoretically that diameter which is too small for diffusion 
and too large for diffraction to blur the image. The aperture is found from 
V4:f 2 A., where f 2 is the distance of the screen from the aperture, and A is the 
wave-length, this being -0001 for photographic and -0006 for visual effect. 
A (the aperture), f 2 and A are expressed in mm. If A be a constant -0004, 
and f 2 be in inches, we can simplify the above to A=-2\/f 2 , the value of A 
being in mm. The intensity of the light is A/f 2 . The respective sizes of 
object and image O/l—ij/i^, where f x is the distance of the object. 

Transmission and Opacity. — The transmissiveness of various transparent 
media to different parts of the visible and invisible spectrum varies consider- 
ably. Thus crown and flint glass are comparatively opaque to heat rays and 
equally transparent to light rays, but while crown is rather opaque to the 
ultra-violet, flint is still more so. Most crystals, as fluorspar and pebble, 
are exceedingly transparent to the ultra-violet, and fluorspar also to the infra- 
red rays. Kock salt and iodine are very transparent, while alum is very 
opaque, to the infra-red rays. Crookes' glass absorbs infra-red and ultra- 
violet, and the darker shades some of the visible light as well. 

The cause of opacity may be said to be due to the restraining influence 
exerted by bodies — or rather, their composition — on the passage through 
them of waves of certain lengths. The light is not, however, lost, but is con- 
verted into some other form of energy — perhaps generally heat— but the rise 
in temperature would be slight. Moreover, a rise due to opacity to ethereal 
vibration must be distinguished from that caused by the nature of the sur- 
face, i.e. its absorptive power, which has a much more powerful influence in 
raising the temperature of a body. It is due to the infra-red or heat radia- 
tions accompanying light that an opaque body becomes markedly heated 
when exposed to general radiation. Thus polished and blackened metal may 
be equally opaque, but the latter would be rendered much the hotter by free 
absorption of light. It would be difficult to eliminate the factor of absorption 
in the measurement of a rise of temperature produced by opacity to light. 

Some bodies transmit light and not heat or chemical rays, and others the 
reverse. Bodies which transmit the invisible heat rays without becoming 
quickly warmed themselves are termed diathermanous ; those which do not 
are termed athermanous or adiathermanous. 

Confusion Discs. — The size of a disc of confusion C (Fig. 317) bears the 
same relationship to that of the lens aperture A as its distance b from F does 
to/, the distance of the lens from F; thus C/A=b/f, or C=A b/f. 



For instance, with a +4 D lens the disc of confusion C at 15 cm. from the 
lens, is 25 - 15=10 cm. from F, therefore C= 10/25 of A. It would be the 
same size at C if 35 cm. from the lens, and also 10 cm. from F. If C is 40 

Fig. 317. 

cm. from A, then C'/A=15/25. The source of light is presumed to be 
distant so that the light is parallel; if it is near, the conjugate distance / 2 
must be taken instead of F. 

If a screen be held close behind a Cx. lens facing a distant bright source, 
the emergent light is similar in size to the lens aperture, and it becomes 
smaller as the screen is receded, the minimum being reached at the focus, 
after which it again increases in size. 

With cylindrical lenses the two diameters must be calculated, the con- 
fusion disc being elliptical. These two dimensions C and C" at any distance 
are found from 

C=A a/F x and C'=A b/F 2 

where a and b are the distances respectively from F 1 and F 2 . 

Thus the size of the confusion disc formed at 30 cm. by a +4 S. o 
+ 2 C. Ax. 90°, the diameter of the lens A being 5 cm.? Now F 1 =16-66, and 
«=30 - 16-66=13-33 cm. ; F 2 =25, and Z>=30 - 25=5 cm., so that 

C=5x 13-33/16-66=4 cm. and C'=5x 5/25=1 cm. 

The disc is 4 cm. horizontally and I cm. vertically. It is difficult to show 
the two different diameters in one diagram, but a separate one for each clearly 
shows the principles involved. For the combination above we find at 20 cm. 
both dimensions to be 1 cm. 

For a near point source, the confusion disc, in the focal plane, d=- 
a(fo- F)//;=aF// 1 , or d=a¥ 1 /f 1 where F 2 and F 2 differ. 

Fig. 318. 

To find the circle of least confusion (Fig. 318), as in spherical or chromatic 
aberration, when F x and F* are the foci of the periphery and centre, or of the 


blue and red light, respectively. The calculation, similar to that on the 
interval of Sturm, is as follows: 

B/A=6/F 1 =o/F 2 ; ¥ 2 -¥ x =a + b; FJF^b/a 

a=F 2 - Fj - 6=F 2 - V t - aF x /F 2 or a(F x + F 2 1=F 2 (F 2 - V L ) 

That is, a=M^t Similarly, &= F f^ 

„ Ao A(F,-F,) , ' ,. 1T> „ , 2F 1 F 2 

Then B= „- = - j; 2 A ' - and the distance AB=F X + 6=,- ' 

F 2 F 1 + F 2 1 F 1 + F 2 

Thus, let a lens be of 3" aperture, Fj the focus of the periphery is 19", 
while that of the centre F 2 is 20". The disc of least confusion is 

3x(20-19) r ,..,.. • 2X20X19 

B= 20+19 = f3 and ltS dlSt9nCC 1S 20TT9" =1948 

Images Formed by Cyl. Lenses and Mirrors. — The formation of images by 
cyls. has only been considered so far as the production of focal lines from 
point sources is concerned. Nevertheless, a plano-cyl. can produce an image 
of sorts, although naturally very ill defined and distorted, from an ordinary 
object; such images, even when real, are best examined by the eye, because the 
pupil of the latter acts as a stop, and cuts down the excessive confusion caused 
by the absence of point-foci. 

The real image produced on a screen by a plano-Cx. cyl. is made up of 
focal lines approximately equal to the axial diameter of the lens; in conse- 
quence the real image is an infinite number of streaks parallel to the axis. 
Viewed from behind by the eye, the image seen is partly real, partly virtual, 
it is not altered in size along the axis, and may be diminished, magnified, or 
of the same size across the axis. With the axis, say, horizontal, the image 
is not laterally reversed, but is inverted ; with the axis vertical the image is 
reversed but not inverted. When the object is within F the image is wholly 
virtual, there is neither reversal nor inversion, there being unit magnification 
along the axis, and enlargement across it. 

In the case of a Cc. cylindrical the image is always virtual, is equal in 
size to the object along the axis, and diminished across the axis. There is 
neither reversal nor inversion. 

A Cc. cyl. mirror acts similarly to a Cx. cyl. lens, and a Cx. cyl. mirror to a 
Cc. cyl. lens. What has been said above with regard to lenses applies equally 
to mirrors. 

The Flame. — A flame (Fig. 319) consists of three cone-shaped portions, 
viz. : — 

(A) The dark central portion surrounding the wick is the cone of genera- 
tion or obscure cone. It is of low temperature and composed of gaseous 
products holding in suspension fine carbon particles which have not yet 

become incandescent. 



(B) The luminous part surrounding A is the cone of decomposition or 
luminous cone, in which the carbon is in a state of intense incandescence, and 
in which luminosity is greatest. 

(C) The thin external envelope, light yellow towards the summit and light 
blue at the base, is the cone of complete combustion giving but little light, 
and is the main source of heat. Here the temperature is high and combustion 
complete on account of the free access of the oxygen of the air. 

Fig. 319. 

The flame in general is brighter at the top where the light predominates, 
and darker towards the base where heat is in excess. The outer envelope, 
being mixed with oxygen, is called the oxidizing element, while the inner 
cone, consisting mainly of unconsumed gas, is called the reducing element of 
the flame, since there metals may be reduced from their compounds. 

A flame is produced by the incandescence of carbon particles which have 
been brought to a high temperature, the combustion, when once started, 
being continued owing to the heat produced by the chemical action itself. 
In a lamp or candle flame the material consumed is drawn up by capillarity 
through the wick. 

Heat being produced by combustion, and luminosity being the result 
of the incandescence of unconsumed particles of carbon, the luminosity of a 
flame is low when combustion is complete, as is the case with the flame of 
some gases and of alcohol. It is high in a coal-gas flame, or in that produced 
by the combustion of oils and fats, where a considerable quantity of incan- 
descent carbon is present. If the combustion be intensified by the intro- 
duction and intimate mixture of a sufficient supply of oxygen, as is done in 
the ordinary blow-pipe or Bunsen burner in which coal-gas is consumed, 
luminosity is decreased and heat is increased : the flame produced is then of 
a faint blue instead of the usual yellowish colour. The oxyhydrogen flame 
also gives very great heat, and yet is of a pale bluish colour and almost 
invisible; but when made to impinge on a lime cylinder, it renders it white 
hot at the point of contact, giving rise to an intensely brilliant spot of light, 
so that the temperature of a flame is neither indicated by the luminosity nor 
by the colour alone. To obtain maximum luminosity the supply of air must 
be neither too large nor too small. If too large the carbon is consumed too 
quickly, and if too small the carbon passes off unconsumed as soot. 


On the other hand, although the temperature of the Bunsen flame, or any- 
other source of complete combustion, is very much higher than that of 
luminous or incandescent sources, yet its power of radiation is considerably 
less. This can be illustrated by means of an experiment with a Bunsen 
burner and a thermopile, the latter being an apparatus exceedingly sensitive 
to radiant heat and its detection when placed some distance from a source. 

With the complete combustion flame practically no rise in temperature 
is indicated by the thermopile, but when the oxygen is cut off and the flame 
becomes luminous, the index of the pile immediately shows a higher reading. 
Thus, for the production of radiant heat, the source must consist of rapidly 
vibrating incandescent particles capable of transferring their energy to the 
surrounding ether. For local heat, from conduction and convection air 
currents, the highest temperature is produced by complete combustion, 
where little energy is wasted in agitating the surrounding ether. 



The Spherometer is a mechanical instrument for determining the radius 
of a spherical surface. The most usual form consists of three fi,xed legs, 
arranged so that their points describe an equilateral triangle around a fourth 
leg in the centre which moves up and down, by means of a fine screw. The 
head of the screw supports a round horizontal plate, which has its edge almost 
touching a vertical scale divided into mm. or '5 mm. as the case may be, 
and the plate itself is usually divided into 100 parts. The elevation or depres- 
sion, therefore, of the central leg, from the plane of the other three, can be 
read with considerable accuracy. Generally the pitch of the thread is so 
arranged that two complete revolutions of the plate lowers or raises the central 
leg 1 mm., and as the plate itself is divided into 100 parts, the elevation or 
depression of the leg can be read to an accuracy of -005 mm. 

Fig. 321 shows a plan of the instrument, C being the central leg, and 
X, Y and Z the three fixed legs. 

S, the sagitta, or sag (Fig. 320) of the curve for any particular chord A B, 
is measured by the central leg of the spherometer, and d by the distance 
between the central leg and an outside leg. The radius of curvature, r, is 
found from the formula below. 

Fig. 321. 

If two chords of a circle intersect at right angles the products of their 
respective parts are equal. Thus in Fig. 320 A B and C D are at right angles, 
and the line A B is divided into two equal parts d and d, so that 

Sxa=dxd=d 2 
But a=2r - S, so that d 2 =S (2r - S) 

<Z 2 + S 2 





The distances C X, C Y, C Z (Fig. 321)=rf, and the angles X C E and 
ZC E are each 60°. Let E be the distance between any two of the fixed 
legs, say X and Z; then 

E/2=d sin 60°, or E^— — =dV% or d=- 1 =. 
1 2 V3 

Substituting in the previous formula the value of d in terms of E we get 

(E/V3) 2 + S 2 '_ E 2 /3 + S 2 E 2 + 3 S 2 
r== ~2S "" 2S = 6S 

This latter formula serves when the distance E between two adjacent 
fixed legs is taken instead of d, the distance between a fixed and the central 

When the sagitta S is very small compared with r (as is nearly always the 
case), the quantity involving S 2 in the formulae may be neglected, and they 
become respectively 

r=d 2 /2S and E 2 /6S 

As an example, suppose the distance between the movable and a fixed leg 
be 24 mm., and all four legs are in contact with a Cx. surface when the central 
leg is elevated 2-5 mm. Then 

24 2 + 2-5 2 582-25 


or neglecting S 2 

2x2-5 5 

24 2 

= 116-45 mm. 


=115-2 mm. 

The Lens Measure, used in the optical trade, is a mechanical instrument 
based on the construction of the spherometer. Projecting from the top of a 
small watch-like case are three metal pins, the central one projecting beyond 
the other two, and is movable. This latter acts on a spring connected with a 
pointer which indicates on a dial the dioptral number (or F) of a lens. The 
dial is graduated from known curves whose powers are calculated on a given 
index of, say, 1-52. 

When the surface of a lens is pressed on the pins, until arrested by the 
two side ones, the central pin becomes depressed, and causes the pointer to 
revolve and indicate the power of the lens (as represented by its curvature) 
in diopters. Care must be taken that the plane of the lens is at right angles 
to the plane of the pins. The surface is sph. if, on rotating the lens, while 
pressed against the pins, the index remains stationary, and it is a piano if 
zero is indicated by the pointer. 

If the index moves to different positions, when the lens is rotated, it 
indicates a cyl. or toroidal surface, the maximum power being shown by the 
highest number attained. The axis of a cyl. is indicated when the index 


points to zero, while the base-curve of a toric is indicated by the lowest power 
registered. The maximum curvature of a cyl., and the highest and lowest 
curvatures of a toric, are, of course, spherical ; the intermediate curvatures, 
although elliptical, are indicated as if they were spherical. 

If the lens has a cyl. element, the power of each surface is distinct from the 
other. When both surfaces are sph. the power of the one is added to that of 
the other to obtain the dioptral number of the lens; thus with - 3 D on each 
surface, the lens is -6D. If the one surface is +2-75 and the other - 1, 
the lens is +1-75 D sph. 

Surfacing tools or discs are those employed for grinding the curvature 
of lenses; they must, of necessity, be gauged for some given refractive index, 
usually, 1-52. 

Accuracy of Spherometer, Tools, etc. — The pointer of a spherometer or 
lens measure should indicate zero when a plane glass is applied to it. 

To test the accuracy of the scaling, lenses or discs of known curvature can 
be measured by the instruments. 

To test the accuracy of surfacing tools, templates of known curvature are 

Changed jli. — A lens measure or a surfacing tool can be gauged for one 
refractive index only, and should the measure be used on a lens not having 
an index for which it is graduated, the power registered will be wrong. Simi- 
larly, if a surfacing tool is used on glass whose index is higher or lower than 
that for which it is calculated, the lens produced will be respectively stronger 
or weaker than the indicated power. 

Jjetju x be the index for which the measure or tool is made, and /u 2 be the 
index of the glass employed. Let D be the power indicated by the measure 
or tool, which would be correct if the index were^, and let D' be the true 
power of the lens, the index being /u 2 . Then 


Thus suppose the reading is 5 D on a lens measure made to ^=1-52, but 
the lens made of glass of //=l-56. Then the lens is stronger than 5 D, and is 

D'=5x —=54 (approximately). 

If a +5 D surface is ground on a tool made for ^=1-52 and the glass 
employed has ^=1-56, the power produced is 54 D as above. 

The dioptral tool D that should be employed to produce a given surface 
power D', when the glass is of /u 2 and the tool is gauged for ju v is 

D=D' ( ^i ) 




Thus suppose the tools are made for glass of / a 1 =l-52, and a lens of 10 D 
has to be made of glass of// 2 =l-54, we should employ a tool of 

If focal lengths are indicated we have F^ - 1)=F'(//.- 


Fio. 322. 



The Astronomical Telescope consists of two unequal convex lenses (Fig. 
322), separated by a distance d equal to the sum of their focal lengths, 
so that parallel light incident on the one lens emerges parallel from the other, 
but inverted and reversed. The lens of longer focus — the objective — receives 
the light, from the object, and forms a real inverted image in the focal plane 
of the second lens — the eyepiece — so that a normal (emmetropic) eye behind 
the latter sees, without accommodation, a magnified, inverted image of the 
object. As the name implies, this instrument is used for viewing celestial 
bodies, where the inversion of the image is of no importance. Light-gathering 
power is the essential feature of the Astronomical Telescope. 

When the separation d=¥ 1 + ¥ 2 the telescope is said to be in normal 
adjustment. For a hypermetrope, who requires convergent light, d is slightly 
more than F x + F 2 , and for a myope, who requires divergent light, d is slightly 
less than F x + F 2 . 

In Fig. 322 let Q be the optical centre of the objective, andP R the extreme 
axial rays of the object at oo, the one extremity P being assumed to be on the 
principal axis Q of the telescope. Then P Q R=a, the angle subtended 
by the object at Q, and S T is the real image formed in the focal plane of the 
eyepiece, of which is the optical centre. The angle under which this image 
is seen is b. The magnification therefore is the ratio between the angle b, 
under which the image is seen when the telescope is in use, and the angle a, 
under which the object would be seen by the naked eye, Thus 


Now b and a' are small and subtended by the common perpendicular 
S T, so that 


But T Q—F v that of the objective, and T 0—F 2 , that of the eyepiece 



Thus if F x =5 in., F 2 =2 in., and d=7 in., M=5/2=2|. If the combination 
is reversed, so that the stronger lens faces the light, M=2/5. 

The Ramsden Circle B' A' (Fig. 323) may be defined as the real image of 
the aperture A B of the objective formed by the eyepiece, and represents that area 
through which passes all the light which traverses the telescope. It is some- 
times called the exit pupil, and may be seen by turning the telescope towards 

Fig. 323. 

a bright source, as a lamp, and focussing the circle on a piece of translucent 
paper placed close to the eyepiece. It marks the position where the pupil 
of the observer's eye must be placed in order to obtain the largest possible 
field of view; the latter is contracted if the eye be withdrawn or advanced an 
appreciable distance from that position. Usually the Ramsden circle is 
within an inch or so of the last surface of the eyepiece, and consequently the 
telescope must be placed close to the eye. Sometimes this is impracticable 
or dangerous, as with sighting telescopes on ordnance, the recoil of which may 
injure the eye of the layer, in which case the instrument is so designed that 
the circle is farther back at, say, 3 inches from the eyepiece. 

The significance of the Ramsden circle is the same for the terrestrial tele- 
scope and for the prism binocular, described later. 

The aperture of the objective is sometimes called the entrance pupil, and the 
following ratio holds good : 

r Diameter of entrance pupil A B F, 

M= = =— 

Diameter of exit pupil B'A' F 2 

The Field of View varies directly with the aperture of the eyepiece, and 
inversely with the magnification. It is independent of the diameter of the 
objective as such and, as stated, is a maximum when the pupil coincides 
with the Ramsden circle. The field of view is about 1° to 3° for small 

The Illumination varies directly with the diameter of the objective, and 
inversely with the magnification. To observe faint celestial bodies, such as 
stars of tenth or twelfth magnitude, telescopes with very large objectives are 
essential, the whole of the light falling on the latter being passed through the 
Ramsden circle and into the eye, provided the pupil is at least as large as the 
circle itself. In this sense the effect of the telescope is virtually to enlarge 
the pupil of the eye to an extent equal to the magnification. 



Correction of Aberration, on account of the comparatively small angle of 
view, is necessary only for spherical and chromatic errors, for which, however, 
the obj ective must be well corrected. The correction of the eyepiece is carried 
out in a manner described later. 

Resolving Poiver — that is, the ability of a telescope or other instrument 
to render fine details apparent — depends upon the diameter of the objective. 
Thus with a certain telescope a particular star may appear as a single point 
of light, whereas with an instrument having a larger objective the star proves 
to be double. It is a question of diffraction. 

Fig. 324. 

The Terrestrial Telescope demands an erect image. For reinvertingthe 
inverted image I (Fig. 324) formed by the objective L, of a distant object, an 
erector R is inserted between I and the eyepiece E. By means of the erector 
a second real image /' is formed in the focal plane of E and this is erect. 
Then the final virtual image, seen by the observer, is also erect. 

The erector consists of two strong Cx. lenses between which, usually, a 
stop is inserted so as to reduce spherical and chromatic aberration. Accord- 
ing to its position and formation, the erector may increase, decrease or leave 
unchanged the magnification. In this connection it may be taken as part of 
either the objective or the eyepiece and the equivalent points and focal length 
of the combination would need to be calculated in order to apply M^Fj/Fa 
in the ordinary way. 

Compared with the astronomical telescope, the illumination of the terres- 
trial is poor, owing to the introduction of four extra refracting surfaces, 
and perhaps of a stop. 



Fig. 325. 

The Prism Binocular is identical in principle with that of the terrestrial 
telescope, except as to the method of causing erection of the image. Total 
reflection prisms are used for this purpose, and Fig. 325 shows a typical 
arrangement of the optical parts. 



L is the objective, E is the eyepiece, andP x andP 2 are the reflecting prisms. 

The convergent beam of light from L falls on P 1 which is a right-angled 
isosceles prism having its edge horizontal. The light is totally reflected, in 
the vertical plane, at the two inclined surfaces successively, and so it is 
vertically reversed as if proceeding from an inverted object. A second 
similar prism P 2 , but having its edge in the vertical plane, and therefore at 
right angles to that of P v then receives the light and reflects it twice in the 
horizontal plane without affecting the vertical inversion caused by P v A 
real upright image is thus formed in the focal plane of the eyepiece E. 

By this arrangement the volume of light transmitted is little inferior to 
that of the astronomical telescope. Also the magnification, which depends 
on the distance between the objective and ocular, is very high for the length 
of the instrument, which is about one third that of a telescope having the 
same magnifying power; the transmitted light traverses the body three times 
before reaching the eyepiece. 

There is theoretically no limit to the magnification of the prism binocular, 
but for all-round use the best M is 6 or 8 times; if higher, it has to be held 
very firmly indeed to prevent unsteadiness of the image, while if only a low 
magnification is required the Galilean is perhaps to be preferred. 

The instrument is compact, easily made in binocular form, and presents a 
single image whose stereoscopic effect is enhanced by placing the objectives 
wider apart than the natural interpupillary distance. 

The field of view varies from about 3° to 12°. 

Fig. 326. 

The Galilean Telescope or Opera-Glass consists of a Cx. lens, L (Fig. 326), 
placed in front of a Cc, E, of higher power, at a distance equal to the alge- 
braical sum of their focal lengths, so that the lenses neutralise each other 
by separation. Although the rays of each pencil from a distant object 
emerge parallel after refraction by both lenses, yet the pencils themselves are 
deviated so that the image is seen under a larger angle. 

Let R be the axial ray of a beam from the extreme point of a distant object 
subtending the angle a. Were E not interposed a real inverted image I 
would be formed, but with E placed at a distance from / equal to its own 
focal length the pencil is again refracted as a parallel beam. The angle under 
which the image is seen is b, so that 



The angles a' and b are small, and / is the common perpendicular, so that 


But IQ=F V that of the objective L, and /0=F 2 , that of the eyepiece E. 
Therefore, as with the astronomical telescope, 

M=F 1 /F 2 . . 

Thus, if F x =5 in., F z =2 in.,. and rZ=5 - 2=3 in., M=5/2=2|. If the 
combination is reversed so that the Cc. is to the front, M=2/5. 

The Ramsden Circle A' B' (Fig. 327) in the opera-glass is the virtual 
image of the aperture of the objective and is therefore situated in front of the 


Fig. 327. 

The Field of View is therefore contracted, as the pupil cannot be placed 
in the imaginary circle, and on looking through an opera-glass the field is 
bounded by the blurred Ramsden circle, which moves in the same direction 
as the observer's eye, as this is displaced from side to side, thus disclosing 
different portions of the field. 

The field varies directly with the aperture of the objective and inversely 
with the magnification, and so marked is the contraction in the higher powers 
that the glass is rendered practically useless. Thus M is rarely greater than 5, 
and more usually is 4 to 2. The utmost diameter of objective cannot exceed 
some 63 mm., which is the average distance between the eyes. The field 
varies from about 2° to 6°. For the notation of small telescopes see p. vi. 

The Illumination is good because, the image being upright, no erector 
is needed and the refracting surfaces are a minimum. The night-glasses used 
for marine work are Galilean telescopes having the largest possible objectives, 
and of moderate magnification. 

Correction of Aberration is only for spherical and chromatic errors, the 
angle of view being even smaller than in the telescope or prism binocular 
for the same magnification. In high quality glasses both the objective 
and eyepiece are corrected, but in the medium and lower qualities only the 
obj ective. 

The distance d between the lenses is equal to F x + F 2 when the emergent 
light is parallel, as foi a normal eye. For divergent light d <F 1 + F 2 , and 
for convergent light of>F 1 + F 2 , as is needed by the myope and hyper- 
metrope respectively. 



Comparison of Galilean and Prism Binoculars. — The Galilean is superior 
in illumination; its great disadvantage is the contracted field of view for 
equal magnification. 

With no instrument is the intrinsic brightness of the image increased, 
but lather reduced by reflection at the various lens surfaces, except in the 
case of a star, which has no magnitude under any conditions. 

Measurement of Magnification. — A practical method for measuring the 
magnification, of any form of telescope, is to view a fairly distant object 
having regular spaces, such as a brick wall, through the telescope with the 
one eye and directly with the other eye. With a little manipulation the two 
images can be made to overlap, and the magnification is given by the number 
of bricks, seen by the unaided eye, that are contained in a single brick seen 
through the telescope. 

Since the entrance and exit pupils of a telescope, having a positive eyepiece, 
can be measured, the ratio between their sizes gives the magnifying power. 

The Reflecting Telescope, sometimes used for astronomical purposes, con- 
sists of a long focus parabolic concave mirror of large aperture forming the 
objective, and the usual eyepiece to which the light is reflected by a small 
secondaiy mirror or prism. Its entire natural freedom from chromatic 
aberration renders it very valuable for some purposes. 

The Compound Microscope (Fig. 328) is used to obtain a magnified view 
of a small near object. It consists of two unequal strong Cx. lenses, the 
front one L, the objective, being a very strong combination, while the second, 
E, the eyepiece, is also strong but less so than L. The distance d between 
them is much greater than F x + F 2 and is governed by the available length of 
the instrument which is usually 10 in. — the conventional distance of most 
distinct vision. Some instruments, however, have a tube length of 8 in. or 
even 6 in. 

Fig. 328. 

The object to be viewed, A B in Fig. 328, is placed just beyond F of the 
objective L and a real inverted highly magnified image B' A' of it is formed 
in the focal plane of the eyepiece E when the microscope is in normal adjust- 
ment. An eye placed behind E then sees an enlarged virtual image of the 
first real image. Hence there is magnification due to both the objective 
and to the ocular, and it can be very approximately calculated as follows: 
Let N denote the position of B' A' on the axis. 

The magnification due to the objective is 

M 1= B' A'/AB=QN/QP. 


But Q N may be taken as the tube length of the microscope, which is 
usually 10 in., while QP is practically equal to F x — that of the objective. 
Thus M x may be taken as tube length/F 1 =10/F 1 . 

The magnification M 2 of the eyepiece can be expressed as d/F 2 =10/F 2 , 
where F 2 is the focal length of the eyepiece, and 10 in. is the conventional 
distance of visual projection which, in this case, corresponds approximately 
to the actual distance of the original object. 

The total magnification is, therefore, 

Tube length Projection distance 10x10 100 

M=M X M,= _ 8 X — J — = — — = — =- 

1 - F x F 2 F X F 2 FjF, 

where all terms are expressed in inches. Thus suppose F x =^ in. and 
F 2 =2 in., then M=100/-5=200. If all terms are in cm. the numerator of 
the above term becomes 625. 

The above formula is only approximate but is quite sufficiently exact 
for practical purposes. Q P is not actually equal to F v nor is the distance 
of projection always 10 in. While N is taken to be at F. 2 for the emmetrope, 
it would be beyond for the hypermetrope, who needs convergent light, and 
within for the myope, who needs divergent light. The microscope has a 
coarse adjustment so as to vary the distance between L and E, to suit the 
individual eye and distance of object, and a fine adjustment for the more 
exact disposition of these parts in order to secure the clearest possible view. 

The Ramsden circle has the same significance as in the astronomical tele- 
scope, and is denoted by x y in Fig. 328. 

Aberrations — spherical and chromatic — must be fully corrected, especially 
with regard to the objective, which, if of high class, is a complicated combina- 
tion of lenses. Coma also over a certain area must be corrected. The posi- 
tive eyepieces are the same as used in telescopes. 

Resolving power is a most important consideration in microscopy, and 
depends entirely upon the angular aperture of the obj ective. For the examina- 
tion of very small objects, such as bacteria, an objective of very large aper- 
ture must be used. A special type is the immersion objective, with which 
a drop of cedar oil produces a homogeneous medium from the object to the 
lower lens. 

Fig. 329. Fig. 330. 

The Angular Aperture a is that of the cone of light from the object that 
can enter the objective. The numerical aperture N.A. expresses the light 
gathering power and is given by N.A.==a sin a/2 where /u, pertains to the 
medium in the space between the object, or the cover plate, and the bottom of 



the objective. This medium (Fig. 329), with a dry objective, is air, and /u= 1 , 
so that the N.A. cannot exceed 1 . 

With an immersion objective (Fig. 330), however, the medium is water 
of ^=1-33, or cedar oil of ^=1-512. Thus the N.A. or the effective aperture 
of the objective, on which the resolving power depends, is increased by the 
employment of an oil immersion objective. 


Eyepieces generally consist of two uncorrected separated lenses so arranged 
that refraction is shared more or less equally between all four surfaces. 
Spherical aberration for the narrow pencils produced by the objective is thus 
practically eliminated, and as the final image is virtual the effects of chromatic 
aberration are inappreciable. 

The Ramsden eyepiece consists of two equal plano-Cx. lenses having their 
curved surfaces facing each other, and the separation is usually 2/3 F of 
either lens. 


• *~7 



■ ■* A 



Fig. 331. 

Fig. 332. 

In Fig. 331, showing the Ramsden system, L x is the field-lens and L 2 
the eye-lens. P and Q are convergent pencils from the objective forming the 
real image A B from which they diverge and, after refraction at both lenses, 
finally emerge as parallel beams. The Ramsden circle is x y. 

This eyepiece is said to be positive because its principal focal plane is 
outside the lenses — i.e. AB'm Fig. 331. It is therefore a convenient type 
where cross wires, micrometer scales, etc., are required to be used, as these 
can then be placed in the plane of A B, the magnifying effect of the whole 
eyepiece being equally exerted on both wires and image. 

The Huyghen eyepiece is usually employed where high magnification is 
required. It consists of two plano-Cx. lenses, each curved surface being 
turned the same way in the direction of the objective. The eye-lens is the 
more powerful, such that F 1 =3F 2 , the separation being (F x -|- F 2 )/2. 

In Fig. 332 L x is the field-lens, L 2 the eye-lens, and convergent pencils 
fall upon L x before the real image is formed at AB, the focal plane of the 
eye-lens. For this reason the Huyghen eyepiece is said to be negative, the 
principal focal distance on the one side being situated between the lenses. 

The Kellner eyepiece, now little used, consists of two equal plano-Cx. 

-lenses with both curved surfaces turned towards the objective, and separated 

by a distance equal to F of either. The real image from the obj ective is formed, 

therefore, in the plane of L v which is the focal plane of L. 2 . In this eyepiece 


L x has no influence at all on the magnification, and its great disadvantage is 
that any dust or scratches on L x are as conspicuous as the image itself, being 
situated in the same plane. 

In every eyepiece the utility of L v the field-lens, is to increase the field 
of view. 

Other Optical Instruments. 

The Camera consists, in principle, of a light-tight box, having a positive 
lens at one end, and a sensitive screen — the plate or film — at the other, upon 
which is received and recorded the real image of an external object. 

The Aperture- Ratio or F/No. is an important factor in the photographic 
objective, because on it depends the duration of exposure and, to some extent, 
the definition of the image over a certain area. The No. is found by dividing 
the equivalent focal length by the effective aperture of the lens; for example, 
a lens of F=6" with an aperture of 1 Jin. is said to work at F/4. This figure 
4 denotes the maximum ratio for which the objective is designed — it may 
work at any smaller aperture down as far as F/64 by the use of a variable 
iris diaphragm. A certain series of these F/Nos. usually are engraved on the 
mount, and are so arranged that a change from one to the next higher generally 
requires a doubling of the exposure. 

Principal Types. — The lenses employed in photography may be roughly 
divided into four main groups: (1) for portraits, (2) for landscapes, (3) for 
architecture and copying, and (4) for all-round work. 

Portraiture demands critical central definition over a relatively small 
area, the more peripheral portions of the picture being immaterial as regards 
sharpness. Spherical and chromatic aberration must therefore be fully cor- 
rected, the oblique aberrations being relatively neglected. The working 
aperture must be large in order that indoor photography with artificial light 
may be done without prolonged exposure. The focal length should also be 
long in order that distortion of perspective may be as small as possible. The 
Petzval system is a good example of the portrait lens, working at an aperture 
of, say, F/4. 

For landscapes fair general definition over the whole plate is necessary, 
but a high degree of correction for any aberration is unnecessary because the 
size of aperture is not important. For the latter F/8 to F/16 is generally 
sufficient. The lens may be of the single achromatic form, or any of the other 
types, except the purely portrait objective, may be employed. The front or 
back component of a modern high-class lens may be suitable for this work. 

Where freedom from distortion is essential, as in architectural studies, 
or in copying and process work, what is known as the rectilinear lens is largely 
employed. This consists of two equal components having a diaphragm 
placed midway between them so that any negative distortion of the front 
lens is neutralised by the equal positive distortion of the back lens. Such a 
lens is usually designed for an aperture of about F/6 to F/8, rapidity of expo- 
sure not being an important factor. 



The all-round type of lens, such as the anastigmat, really combines all the 
advantage of the others; it is one especially well corrected for astigmatism, 
and has a large flat field. Its working aperture is large, from F/4-5 
to F/6, and it is essential where rapid exposure is a necessity, and a large 
variety of subjects has to be covered. Such lenses are used in high-class 
hand cameras. It represents, jDerhaps, the highest skill of the optical designer, 
and one or both components may, in many cases, be used separately for some 
classes of work. 

Fig. 333. 

Fig. 334. 

The Stereoscope. — The stereoscope consists of a box so arranged that there 
is presented to each eye a view, of the same object, obtained by photography 
from slightly different positions. 

The photographs are taken simultaneously by a camera, having twin- 
lenses, placed slightly farther apart than is the distance between the two 
eyes, and the photographs obtained are reversed, so that the right and left 
eye sees the picture taken by the right and left lens respectively. The two 
pictures are mentally fused, and the single picture seen with stereoscopic 

The most usual form of stereoscope is that of Brewster (Fig. 333). Each 
division has a Cx. spherical lens whose F is equal to the normal depth of the 
box, so that light from the pictures enters the eyes in parallel beams. The 
lenses are combined with prisms whose bases are out so that light from the 
centres of the pictures, which are farther apart than the eyes, may enter the 
latter without their having to make any movement. 

In Wheatstone's stereoscope (Fig. 334) there are two plane mirrors at 
right angles to each other. The two pictures are to the side of the box and 
are seen by reflection from the mirrors, which can be adjusted so that the two 
images may be fused. This adjustability takes the place of the prisms in 
the Brewster model, while the greater distance of the pictures renders Cx. 
lenses unnecessary. 

The Optical Lantern is employed for projecting on to a screen a highly 
magnified real image of, usually, a transparent or translucent qbject such 



as a positive, printed from an ordinary photographic negative. The slide, 
as it is called, is strongly illuminated from behind, and placed just beyond 
F of a positive lens, resulting in a real, magnified and distant image inverted 
with respect to the slide. The slide is therefore placed in the carrier upside 
down, so that the image projected on to the screen may be upright. 

Fig. 335. 

Fig. 335 illustrates diagranmiatically the optical princ'ples. L is a power- 
ful source, such as an electric arc, and G a large compound condenser which 
concentrates a wide pencil of light on to the slide AB placed just outside F 
of 0, the objective, B'A' being the resultant real image. 

C is designed to produce the least possible spherical aberration, and that 
shown in Fig. 335 is known as the double D condenser. A still better result 
may be obtained with a combination of double and meniscus Cx., the latter 
being placed with its concave surface facing the source. It should be observed 
that to secure the most intense and even illumination the real conjugate focus 
of L formed by C is coincident with the centre of the objective 0. The modern 
kinematograph projector is based on the same principles. 

The objective must be highly corrected for chromatic and spherical aberra- 
tion, but the field of critical definition need not be large. For this reason 
portrait lenses lend themselves very well to projection work, the Petzval 
system in particular being used. 

Fig. 336. 

The Spectroscope (Fig. 336) is used for viewing and comparing spectra 
produced by prisms, and consists of a horizontal circle, mounted on a stand, to 
which are attached a telescope T and a collimator C, both of which can be 




rotated around the circle. The collimator is a tube having at one end a 
Cx. lens and at the other a narrow slit parallel to the refracting edge of the 
prism P. The distance between the slit and the collimator lens is equal to 
F of the latter, so that light, from the slit, is rendered parallel by the lens 
before reaching the prism. In the centre of the circle there is a small table 
B on which the prism is placed. 

The Spectrometer is a spectroscope with the addition of a scale of degrees 
on which the position of the movable telescope can be indicated, and to 
which, for accurate readings, a vernier and reading microscope is attached. 
This enables the principal angle, the deviating angle, and the dispersion of a 
prism to be measured. 

Fig. 337. 

A Direct Vision Spectroscope (Fig. 337) is formed of a train of, say, three 
crown and two flint prisms mounted in opposition in a tube. The prisms are 
such that there is no ultimate deviation for yellow light, while there is a con- 
siderable separation of the red and violet. A is a slit aperture parallel to the 
prism edge, and at the other end is the eye aperture at which a telescopic 
arrangement is sometimes used. 

The Sextant (Fig. 338) is used to measure the angle subtended at the eye 
by the sun and the horizon, from which the angular elevation of the sun 


Fig. 338. 

can be calculated. It also serves to measure the angle between any two in 
ac3essible objects. 

A small mirror M x revolves about a horizontal axis to which is attached 
a pointer G moving over a scale of degrees. M 2 is a small fixed mirror of 
which one )mU ig silvered and t'h? Other half is clear, and is so inclined that 


when M x and M 2 are parallel the pointer indicates zero on the scale. T is 
a small telescope so directed forwards that it receives at the same time light 
from the horizon by direct transmission through the clear part of M 2 , and by 
reflection, from the silvered part, of light which has been reflected to M 2 
from M v 

Let L 3 be a ray emanating from the sun, and L 2 a ray from the horizon. 
Then to an eye E the image of the sun along the path L z will apparently 
coincide with the image of the horizon seen directly along L 2 . The angle 
which L 3 makes with L v which is parallel to L 2 , is the angular distance 
between the sun and the horizon, but G, the pointer, only moves through t, 
which is half this angle; therefore the scale over which G moves is divided 
into half degree spaces, which, however, are numbered as whole degrees 
in order that direct readings may be taken from the scale, to which also a 
vernier {q.v.) is attached for greater accuracy. 

An artificial horizon is formed by a bowl of mercury whose surface becomes 
a truly horizontal plane. The angle between the position of a telescope 
when an object is seen thiough it, and its position when an image of the 
object is seen by reflection from the mercury, is twice the angular altitude of 
the object above the horizon. 

The Kaleidoscope. — The principle of the kaleidoscope depends on the 
multiple reflection caused by two inclined mirrors. The mirrors are placed 
lengthways in a tube, which is closed at one end by a disc of transparent glass, 
beyond which is one of frosted glass. Between these two glass discs there are 
a number of small coloured objects, or fragments of coloured glass. Looking 
through the open end of the tube an image is seen consisting of a certain 
number of images, the whole forming a more or less symmetrical figure. The 
usual form of kaleidoscope has three mirrors inclined to each other at 60°, 
and the figure is symmetrically hexagonal. The whole central figure, as seen 
in a kaleidoscope, is surrounded by others formed by repeated reflections of 
the light. 

The Vernier. 

The Vernier is an attachment to instruments where great precision of 
linear or angular measurement is required, and it obviates the necessity of the 
division of the main scale into very minute parts. It consists of a short 
scale V (Fig. 339) which slides along the main scale $ to which it is attached. 

V is the same length as a definite number of divisions of S, but contains 
one division more, so that if V is divided into 10 parts, these equal nine divi- 
sions of S, or if V has 30 divisions they correspond to 29 of S. Thus each 
division of V is smaller than each of S by a fraction whose denominator is the 
number of divisions of V, viz., I/10th or l/30th, respectively, in the examples 
quoted. The greater the number of divisions of V the more accurate are the 
readings, but also the more difficult is its use. 

The scale itself may be divided into whole terms of measurement, as 
mm. or degrees, or more commonly into main fractions of such terms as 



\ mm. or \ degrees. 

Such whole terms, or main fractions thereof, are read 
from S itself, the measurement being the last beyond which the zero of 
V has passed. The minute measurement is obtained from V by finding that 
division mark of V corresponding to, or in exact line with, a division mark of S. 




* j i* > 

IN I I I 1 I I I I I I I I I I K 

Fig. 339. 

Fig. 340. 

Thus, if 10 V=9 S, and the third division mark of V is in line with one of S, 
the exact measurement is 3/10 more than the whole number indicated on S 
itself. If V has 60 parts and the 33rd is in line with an S division, the frac- 
tional reading is ££ plus the reading on S. 

Fig. 340 illustrates a reading on a scale S directly divided to inches and 
tenths of inches with a vernier V whose 10 divisions=9 of the scale. The 
length of an object whose one extremity is at zero of S is -65 in., the 5th 
division of V coinciding with a division of the scale. The *60 in. is read from 
the scale itself, where the right-hand extremity of lies between the 6th 
and 7th divisions of S; the balance -05 in. is read from the V. The limit 
of accuracy is y^ in. 

As another example, let the scale be divided to inches and tenths of 
inches, and let 25 F=24 S. If the zero of V showed 5 in. and six spaces 
of yo m -> P^ us a cer tain distance when the fourth division of V is in line with 
a scale mark, the total measurement would be 5+tV+^lir or 5-616 in. 
The accuracy of the reading is carried to ^^ in- 

For an instrument such as the altitude barometer, the vernier is made 
with the V divisions longer than those of S, so that, say, 9 F=10 £. The 
V divisions are then on the near side of the zero, and are read backwards. 

Verniers for fine straight rules are usually made so that 10 V—9 S, thus 
measuring to T V mm. For box sextants and small surveying instruments 
30 F=29 S, so that £° divisions are subdivided to minutes. For barometers 
the readings are usually taken to T \ mm. when 10 F=9 S, or to ^\ „ in. when 
25 F=24 S. For marine sextants and theodolites 60 7=59 S, measurements 
being taken to 1/60 of 20' or of 10', giving limits of accuracy of, respectively, 
20" or 10" in the case of these two instruments. 



In order to grasp the various formulae and the theories underlying them, 
the student should perform for himself the simpler experiments connected 
with general optics. Most of the following can be done with quite rough or 
improvised apparatus, and a complete optical bench, meeting all require- 
ments, can be obtained at a very moderate cost. 

The Optical Bench. — An optical bench should preferably be scaled in 
cm. and mm. and be about 2 M long, thus enabling fairly weak lenses, mirrors, 
etc., to be tested. There should be — 

(1) A frosted lamp at the zero end of the scale. 

(2) A collimator consisting of a pinhole fixed in the focal plane of a Cx. 
lens, the lamp being placed behind the pinhole when in use. 

(3) A screen of ground glass and another, interchangeable with it, of 
opaque stiff white card having a central aperture equal in diameter at least 
to the collimating lens. The latter is used with mirrors. 

(4) A plate with an aperture of definite size, say 20 mm., with fine cross 
wires, to serve as an object, when the lamp is behind it. 

(5) Three or four carriers for lenses and mirrors. One should be universal 
and capable of holding any lens from the smallest up to say, 3" diameter. 

(6) Two or three clips on a single stand capable of taking lenses in con- 
tact or combinations of separated lenses. This should also be capable of a 
horizontal rotation round the support as a vertical axis. 

(7) A small horizontal astronomical telescope with adjustable eyepiece. 
All should be on movable stands and adjustable as to height, since axial 

alignment is essential in most experiments. 

Parallax is the term applied to the apparent displacement of an object due 
to the observer's position. We generally employ the term to indicate the 
apparent change in the position of one object, in relation to that of another, 
when the observer changes his point of view. Let an object A be in front 
of an upright pencil P, and another object B be behind P, and all three in 
the same straight line in front of the observer. Now on moving the head 
to, say, the right, a gap will be visible between P and A and another between 
P and B ; also A will be to the left of P, and B to the right of P — that is to 
say, a near object moves apparently against and a distant one with the 
observer's head. 



Parallax Test. — If there are two comparatively near small objects P and 
X, seen close together in the same direct line, the distance of the one P being 
known, if the head be moved sideways — (a) X is actually in the same plane 
as P, i.e. coincident with it, if no gap between them results; (6) X is nearer 
than P if X has apparently moved in the opposite direction to the observer's 
head ; (c) X is more remote than P if X has moved in the same direction. By 
placing P respectively nearer, or farther away, a position can be found for it 
such that parallax between them is said to be destroyed, since no apparent 
separation results from any degree of movement on the part of the observer; 
the distance of P then equals that of X. This principle is utilised for locating 
the position of virtual images formed by mirrors and lenses and will be referred 
to in some of the following articles. 

Plane Surfaces 

Movement. — A piano-spectacle glass can be determined with sufficient 
accuracy by observing an object (preferably crossed lines) through it while 
rotating and moving the glass. If the glass has no power due to curvature 
the image will appear stationary; moreover, if the surfaces be true planes 
no distortion or irregular movements can be detected. If there is no prismatic 
power, there is no rotation of the cross on rotating the glass. If the glass be 
held obliquely to the eye, so that the direction of vision forms a small angle 
with the surface, any unevenness of the surface becomes more apparent. 

Contact. — If one surface be a plane, this can be determined by applying 
to it a straight-edge, or another piano-glass, and observing whether there is 
contact throughout when holding the applied surfaces against a bright 
background. Real contact between two surfaces is also quite easily felt, 
and they will adhere to each other if slightly moistened by breathing on one 
of them. 

Spherometer. — A plane surface is shown by the spherometer or lens- 

Whitworth Plane. — By contact with a Whitworth true plane surface, 
which has been smeared with some red putty powder, and observing whether 
all portions have or have not taken an impression. 

Newton's Rings. — The absence of interference phenomena between a 
known plane surface and one tested is the most accurate method. 
See also Reflection tests and Telescopic tests. 

Reflection Tests. 

A plane surface can be distinguished from a curved one by viewing the 
reflected image from a bright source of light. If a plane, it acts precisely as 
a plane mirror, while if a sph. or cyl., the image is altered in size or distorted. 
If the object viewed is a square, then a Cx. surface will cause it to appear com- 
pressed vertically, i.e. in the direction of view, so that it has the appearance 
of a horizontal rectangle, while a Cc. surface causes vertical extension, giving 



the appearance of a vertical rectangle. In every instance the lens should be 
held as close and oblique to the eye as possible. 

As the lens is rotated, while still viewing the reflected image, there is no 
change in the appearance of the latter if the surface is sph. or plane, whereas 
if cyl. the image does change. If the object viewed be of some definite shape, 
say a vertical window bar, it is seen quite distinctly when the axis of the cyl. 
is in line with the direction of view, whereas it is indistinct when the axis 
is oblique to, and most indistinct when the axis is at right angles to, the line 
of vision, the general image being, drawn out if the surface is Cc, and com- 
pressed if Cx., as with sph. surfaces. This is an extremely delicate test for 
locating the axis of a cyl. 

Fig. 341. 

Fig. 342 

Focal Length of Cc. Mirrors. 

Direct Focalisation. — On the optical bench parallel light is obtained from 
the collimator C (Fig. 341), and passed through the perforated screen S on to 
the mirror M whose focal length is to be measured. The mirror is slightly 
tilted and moved to and fro until the image of the pinhole is thrown sharply 
on to the screen at F. The distance M F is the required focal length. 

Conjugate Focalisation. — If the cross wires be substituted for the colli- 
mator such that a real conjugate image be formed on the screen S, we have 
l/¥=l/f l +l/f 2 , where f x is the distance of the cross wires, and f 2 is the 
conjugate distance M S of the screen, to the mirror. This being the same 
as for Cx. lenses, the examples given serve equally well for Cc. mirrors. 

Symmetrical Planes. — An especially rapid and accurate way to find F is 
to use the cross wires and the disc containing them as both object and screen. 
The mirror is advanced towards S until the image of the wires appears sharply 
on the surrounding disc, which must then be at the centre of curvature. 
The radius of curvature is thus directly measured, and equals 2 F, i.e. F=r/2. 

Parallax. — If an object be placed within F, the virtual image can be 
located as described under convex mirrors, and the focal length found from 
the conjugates, care being taken to reckon the distance of the image as a 
negative quantity. 

The Spherometer. — See this method for Cx. mirrors. 

Focal Length oi Cx. Mirrors. 
Projection Method. — Arrange a collimator and perforated screen (Fig. 
342) as for a Cc. mirror, the screen being between C and M. On S describe 
a circle N concentric with the central aperture and of twice the diameter 



of the collimator lens. The action of the mirror being divergent it will 
reflect the parallel beam as a cone apparently diverging from F. Move the 
mirror to and fro until the projected area of illumination on S exactly fills 
the circle N. Then the distance of screen to M equals F of the mirror. 


Fig. 343. 



Fig. 344. 

Parallax Method. — Take two stiff wires or knitting needles (Fig. 343) 
and place onePj represented by the arrow in front of M such that its virtual 
image is /, seen on looking into the mirror from the same side asP r Behind 
M place a second needle P 2 such that it approximately coincides with I seen 
in the mirror. Now move the head from side to side, and if there is apparent 
separation between the virtual image I oiP 1 and the actual pinP 2 the latter 
must be moved towards or from the mirror until all parallax disappears. 
Then if P 1 M bef v andP 2 M be/ 2 , we have, since/ 2 is a negative quantity, 

l/F=l//i+ (-!//■). 

Convergence towards C. of C. — Set up the cross wire D (Fig. 344) and in 
front of it place any convex lens L so that the latter projects a real image 
at a distance L C greater than the radius of the mirror; the distance L C is 
measured. On interposing M and moving it to and fro a position will be 
found where the image of the wires is received back on to the disc D. 
When such is the case the convergent light from L must be incident on M 
directed towards the centre of curvature C because it has returned along its 
own path. Then the radius of the mirror is the distance M C, between the 
mirror and the real image formed by the lens, and M C = L C -L M. M 
must be slightly tilted to throw the image to the one side of the disc contain- 
ing the cross wires. 

Spherometer (q.v.). — The radius of the reflecting surface of a Cx. (or Cc.) 
glass mirror can be found approximately with the spherometer, but the 
results are uncertain on account of the coating. If, however, it has parallel 
surfaces and is thin, the radius of the front surface may be taken to be that 
of the second or reflecting surface. The latter is slightly shorter in a Cx. (and 
longer in a Cc.) mirror than the front surface measured. 

Bench Focalisation of Thin Lenses. 

Focalisation is direct when the unknown lens is measured by itself; it is 
indirect when another lens is combined with it, for the purpose of focalisation. 


Indirect Focalisation. — The procedure is to combine, with the unknown 
lens D, another known lens D'; find the power D" of the combination, and then 
deduct D' from D". Thus 

D=D'-D< or ^=1-1 

where F" andD" are, respectively, the focal length and the power of the two 
lenses combined, F' and D' those of the added lens, and F and D are those 
of the unknown lens. The approximate power to be added can be found 
experimentally. For great accuracy it is better to divide this power between 
a pair of lenses, placing one on either side of the lens to be measured. 

Fig. 345. 

Cx. Sph. — The power of an unknown Cx. sph. lens can be obtained by 
measuring the distance between the lens and its principal focus. Set up 
the collimator C (Fig. 345), from which parallel light emerges, and in front of, 
and near to it, place the unknown lens L. On the other side of L place the 
screen S, and move the latter to and fro until the image F of the collimator 
aperture is sharpest possible; then L F is the principal focal length; the image 
is a point. This method serves for Cx. lenses between, say, 2D and 10D; 
if weaker or stronger indirect focalisation is to be preferred or becomes 

If F=30cm.,D = — -=3-25. 

Cx. Cyl. — If the lens is a Cx. Cyl. the procedure is the same, but the image 
on the screen is, for the plano-Cyl., a line paraUel to the axis. With the Sph.- 
Cyl., there are two lines at different distances, and at right angles to each 
other. The more distant one is at the focal distance of the sph., the nearer 
one is at the focal distance of the united powers of the sph. and cyl. ; and is 
parallel to the cyl. axis. By finding these two lines, and measuring the dis- 
tance between the lens and the screen for each, the focal length and powers 
of the two principal meridians of the lens can be learnt. 

If F=16 cm., the lens is a + 6-25 D Cyl. 

If F x =16 cm. and F.,=30 cm., D^-25 and D =3-25— that is, + 3-25 
D Sph. o + 3 D. Cyl. 

Weak Cx. Lens. — The image formed by a weak Cx. lens is large and difficult 
to decide where sharp ; also it may be so distant as to be beyond the limits of 
the bench. Therefore, whether Sph. or Cyl. or Sph.-Cyl., an additional Cx. 
lens of, say, 2 D or 3 D should be employed for its focalisation. 



The added lens D' = + 3; the combination D" has F=27 cm. 


D=D"-D'= — =3-75 -3 = + -75. 

D' = + 3 and D/=25 cm. and D 2 "=30 cm. 

Then D x =4-3=:+l and D 2 =3-25 - 3= + -25. 

Strong Cx. Lens. — If F is very short, the exact distance is hard to determine 
with accuracy; for instance, whether F=2 in. or 21 in.; but if the lens be 
focalised with, say, a 3 in. Cc, the difference between the one and the other is 
then about 1 in. Therefore, for its measurement, a strong Cx. lens should be 
combined with a Cc. lens of sufficient power to lengthen the focal distance to a 
reasonable extent. 

The added lens D'= - 13; the combination D" has F=20 cm. 



20 : 


Cc. Sph. — Since a Cc. lens does not form a real image, it must be combined, 
for its indirect localisation, with a stronger Cx.-Sph.; for preference one 
which is about 3 or 4 D stronger. 

The added lens D' = + 8; the combination has F=40 cm. 



: 40 

=2-5 -8= -5-5. 

Cc. Cyls. — With a negative cyl. a Cx.-sph., of sufficient power, must be 
added to render the combination positive so that the two principal powers 
may be found. 

D' = + 8; the combination has F 1 =12-5 cm. and F 2 =16 cm. 




D 2 = -8=0 and D 1 = — -8= - 1-75. 

2 12-5 ~ l 16 

D' = + 8; the combination has F 1 =16 cm. and F 2 =30 cm. 

Then D 1 = — - 8= - 1-75 and D 2 = — - 8= - 4-75 

Fig. 346. 

Conjugate Focalisation.— Instead of finding on the optical bench the 
principal focal distance F, it is often more convenient to find the power of a 


lens from a pair of real conjugate foci. The latter may be used to check 
the former and two or three pairs of conjugate distance can be found to check 
one another. 

The object is the cross-wires D (Fig. 346) placed, in front of the lamp, at 
zero of the scale of the optical bench. Alternatively the object may be the 
small aperture of the collimator, the latter being reversed and placed with the 
lens towards the lamp of the bench. The aperture constitutes a small 
brilliant source from which the light diverges. 

In Fig. 346, D is the cross-wires and L is a Cx. lens placed at a reasonable 
distance from it, so that a real conjugate image may be formed on the screen 
S. If the distance of the object from the lens hef v and the distance of its 
image on the opposite side be/ 2 , then the focal power of the lens is 

11 1 

It is, however, much more convenient to use dioptric measure — that is, 
the distances/^ andy* 2 are converted into diopters so that 

Thus if/ x =25 cm. and f 2 =20 cm., instead of calculating that 

11 1 

F = 20 + 25 

100 100 
we write D=d , + d = — -+ — — =5+4=9D. 

20 25 

This method can be employed directly with medium power Cx. lenses, the 
image on S being, when the aperture object is used — 

A small circle if the lens is a Sph. 

A line parallel to the axis if it is a Cyl. 

Two lines at different distances if it is a Sph. -Cyl. 
To use the cross- wires with a Cyl. lens it is essential that the principal meridians 
of the lens should be exactly Hor. and Ver. This is achieved by rotating the 
lens, in the carrier, until the confusion disc of light formed on the screen is 
exactly Hor. or Ver. Then one of the cross-wires will be seen sharply at F x , 
and the other at F 2 . If the principal meridians do not correspond to the 
cross- wires no definite images are obtained with a Cyl. lens. 

Indirect conjugate focalisation is necessary for a strong Cx. lens, adding a 
Cc. for its measurement; also for a weak Cx. or for a Cc. lens, adding a 
suitable Cx. lens. 

Symmetrical Planes (Donders). — This method depends on the principle 
that when image and object are identical in size, the distance of each from the 
lens is 2 F, and the total distance between them is four times the focal length 
of a thin lens. It is a special case of conjugate focalisation. 

The lens is placed between D and S, which are moved towards or away 


from the lens until the image on the screen is sharp and of the same size as 
the aperture of D. The experiment is made more accurate if the screen is 
scaled. If the lens is weak it should be placed between a pair of Cx. lenses, 
if very strong between a pair of Cc. lenses, in order to obtain the symmetrical 
conjugate foci. The calculation is as given in indirect focalisation. 

It should be remembered that 4 F is the shortest possible distance between 
an object and its real image. 

Notes on Focalisation. — To focalise a periscopic Cx. lens, the distance from 
the lens to the screen should be taken first with the one face, and then with 
the other, turned towards the source of light. The mean of the two distances 
is the true F measured from the optical centre. The distance between the 
symmetrical planes divided by 4 gives F of a thin periscopic Cx. lens. 

With ordinary periscopic spectacle lenses, however, the distance of F, 
from the lens itself, is sufficiently exact in practice. 

Instead of the collimator, any distant bright source, as a window or arti- 
ficial light, can be employed for fairly strong Cx. sphericals, but this is 
uncertain for weak or very strong lenses, and practically useless for cyls. 

On the ordinary optical bench the easiest conjugates to measure are those 
of about 3 to 5 D. 

Sometimes the one power of a Sph.-Cyl. is more easily measured without 
and the other with an added lens. 

In conjugate focalisation the one conjugate d 1 should be selected as a whole 
number — that is to say, the lens should be placed at, say, 33 cm. or 25 cm. 
from the object, thus making d x =3 D or 4 D respectively. The lens should not 
be placed so that d x has a fractional power as it would have if it were placed 
at 30 cm. or 22 cm. The procedure is as in the following example. 

The lens being weak an added + 7 D is employed, and the lens is placed 
25 cm. from the cross-wire. 

(a) d x =i and d 2 is at 15 cm. =6-5 D. 

Dj=4+ 6-5=10-5 - 7= + 3-5 D. 

(6) (Z x =4 and d 2 is at 45 cm. =2-25 D. 

D 2 =4 + 2-25=6-25 -7= --75 D. 

(c) The combination is --75D o + 3-5 D which, by transposition, is — 

- -75 D Sph. o + 4-25 D Cyl. 

or + 3-5 D Sph. o - 4-25 D Cyl. 

Alternatively D 2 is the Sph. and D x - D 2 is the Cyl. 

Thus +6-25 D. Sph. o (+10-5-6-25=) +4-25 D. Cyl., and from the 
Sph. the added lens is subtracted. Thus the Sph.=6-25 - 7= - -75 D. 

Separation Method — Cc. Lens. — This is an optical bench measurement 
and is very useful if a strong Cc. has to be measured, and there is only a 
weak Cx. Sph. available. Light from the collimator is refracted by a Cx. 



lens L (Fig. 347) to come to a focus on a screen at F. The lens should be 
shifted about so that F is at some definite position, say the 100 cm. mark on 
the bench; the screen is then moved some distance back. In the cone of con- 
vergent light A F B the convergence is, at any point G, equal to the dioptral 

Fig. 347. 

distance G F. Therefore if another lens is placed at C it is as if it were com- 
bined with a Cx. lens of F=C F. Let G be 8 cm. from F, then the convergence 
equals 12-5 D ; if, now, a Cc. lens be placed at G, the light is rendered less con- 
vergent and the screen is moved about until the image is sharp thereon at, 
say, 114 cm. Then C #=22 cm. =4-5 D. Therefore the Cc. lens is, expressed 
in diopters, 

D=C S - C F==4-5 - 12-5= - 8 D. 

The cross-wires or the luminous point can be used instead of parallel light. 
This method serves also for Cyl. lenses, the image being a line or two lines as the 
case may be. 

The distance G S can be fixed and screen and lens moved about until the 
image is sharp but, of course, the selected distance must be appropriate. The 
combination of separated Cx. and Cc. lenses causes the image on S to be large 
so that it is difficult to decide when it is sharp. 

Fig. 348. 

Telescope Tests. — More accurate results can be obtained with lenses if 
the telescope be employed in their focalisation. This is really the reverse of 
the usual procedure, as will be seen from Fig. 348. The collimator G is 
reversed, so that its lens faces the lamp and the pinhole P is away from it. 
The telescope is adjusted for parallel light by pulling the eyepiece well out, 
and gradually pushing it in, until some distant object is seen sharply through 
it; the eyepiece is then fixed and the telescope T replaced on the bench. 
The lens to be measured is placed in a clip between P and T and moved to 
and fro until the image of P is seen sharply through T. Then the distance 
L P, from pinhole to lens, will be the focal length of the lens, since only 
parallel light can have emerged from L to enter the telescope and give rise 
to a sharp image therein. With a cyl. the image will be a line; with a sph.- 



cyl. there will be two line images at different distances. As in other tests, 
a known sph. must be added, if the unknown lens is too strong, too weak, 
is negative, or the difference between the principal powers insufficiently 
marked to give accurate results. The smaller the pinhole used in this experi- 
ment the sharper will be the lines obtained. 

Fig.: 350. 

Another method. Light from the pinhole P is brought to a focus at A 
by D, a Cx. lens. A is marked. The telescope T adjusted for oo is placed 
a convenient distance behind A. The lens L to be measured is then introduced 
between T and D and moved about until the image of P is seen sharply. Then 
the distance L A is F of the lens L which, if Cx., must be placed between the 
marked point A and T (Fig. 349), and if Cc. between A and D (Fig. 350). 
This method is good only for fairly strong lenses. 

For plane surfaces the telescope is adjusted for infinity. A beam of light 
rendered parallel by a collimator is allowed to fall obliquely on the surface 
to be tested and is, after reflection, received in the telescope. If now, on 
looking through the telescope, the image seen of the source of light is sharp, 
the surface is a plane. If the surface is Cx., the eyepiece of the telescope must 
be pulled out, and if Cc, pushed in, in order to get a sharp image. If the 
surface is irregular, a sharp image cannot be obtained at any spot. The 
presence of astigmatism, whereby one portion of the image is better defined 
than the other, is the surest proof of convexity or concavity of a surface. 

*f-~ . 





Fig. 351. 

Fig. 352. 

Focal Length of Cc. Lenses. 

Parallax Method. — This is similar to the method for Cx. mirrors, except 
that object and image are on the same side of the lens, while the observer is 
on the opposite side. A pinPj (Fig. 351) is set up, and its virtual image I is 
observed through the lens. A second locating longer pin P 2 is now taken 
and moved to and fro until, on moving the head, there is an absence of parallax 
between them, P 2 , seen above the lens, apparently coinciding with / seen 
through the lens. Then, if P x to L hef v andP 2 to L be/ 2 , the latter being 
negative, l/F=l//;+(-l// 2 ). 


Locating the virtual image with a Cc. lens is more difficult and confusing 
than with a Cx. mirror because the observer sees two objects and two images. 
It should be remembered that the more distant image must be made to coincide 
with the nearer object pin. The pinP x seen above the lens, and the image of P 2 
seen through it, must be ignored. 

Projection Method. — This is similar to the projection method for Cx. 
mirrors. A parallel beam from C (Fig. 352) is allowed to fall on the unknown 
Cc. lens, and is diverged by the latter as if proceeding from F. If now S be 
moved back until the luminous area exactly fills the marked circle M N — 
which is twice the diameter of C — then the focal length of the lens is equal 
to L S, the distance of lens to screen. 

This method can be utilised for a sph.-cyl., the luminous area being twice 
the diameter of the lens, in each principal meridian measured separately. 

Reflection Method. — The Cc. surfaces of a negative lens may be employed 
as positive mirrors for measuring their radii of curvature. The object is the 
cross- wires, and its image is reflected back to the disc containing them, so that 
the distance of lens to disc is equal to the radius of curvature. Each surface 
should be calculated separately since the lens may not be a double Cc. sph. 
The refractive F of a lens surface is approximately = 2r. 

If parallel light is employed we get F by reflection/or each surface, and it 
is I of F by refraction. For example, if with parallel light F is found to be 4" 
for the one surface, and 8" for the other, the lens is 1/16+ 1/32=1/10 nearly. 

This method can be employed for a Cc.-eyl. surface, the projected real 
image being a line. 

F of Thick Lenses and Combinations. 

The position of the image, formed by a Cx. lens., is more accurately deter- 
mined by using as the screen a thin transparent glass plate, having a small 
dark spot on its front surface. The real image is formed on the screen and 
viewed from behind. The image and spot are in the same plane if, on moving 
the head sideways, there is absence of parallax. Adjustment to this position 
is obtained by moving the screen to and fro. The test is improved by using 
a fixed magnifying glass. 

Thin Lens Method — Positive Combination. — If a single thin lens is found 
which gives on a screen an image equal in size to that formed by a combination, 
the focal distance of the former is that of the latter; also the place at which 
the single lens is situated determines the second equivalent point of the com- 
bination. If the latter is turned so that the original back lens faces the light, 
the spot at which the single thin lens must be placed in order to give an image 
similar to that of the combination fixes the position of the first equivalent 

Thin Lens Method— Negative Combination.— Put up a, say, 6 inch Cx. lens 
and, at some 10 inches behind it, a screen. The unknown Cc, combination is 



placed some short distance in front of the Cx. and moved about until a sharp 
image of a bright distant object, as a window, is formed on the screen. The 
size of the image is carefully marked on the screen, the Cc. combination is re- 
moved, and a known thin Cc. is found that gives an image of equal size. F of 
the combination equals F of the thin Cc. 

Symmetrical Plane Method — Positive Combination. — To find ex- 
perimentally the equivalent focal length of a thick Cx. lens or combination, 
it is necessary to locate the equivalent planes, since the focal distances are 
the distances between these planes and the principal foci. 

Fig. 353. 

Let the system of lenses be suitably mounted (Fig. 353). Parallel light 
from the collimator G is refracted by it, and the principal focus F B is formed 
on the screen S, whose position on the bench is noted. Now substitute the cross- 
wires D for the collimator and move them about until its image formed on 
S, drawn back to S', is the same size. Then S' is the second symmetrical 
plane, and is therefore at 2F from some plane — the 2nd equivalent plane — not 
yet located. But the distance between 2F and .F B , i.e. the difference in the 
bench readings of the position of S' and S, is F, the equivalent focal length. 
Therefore measuring from S' towards the lens a distance equal to 2F, the 
second equivalent plane E 2 is located. Then a similar measurement of 2F 
from the cross- wires determines the position of E v the first equivalent plane. 
In some combinations E ± and E 2 are crossed, as illustrated in Fig. 353. 


Fig. 354. 

Rotation Method — Positive Combination. — This is, perhaps, the quickest 
and is a most accurate method for finding the equivalent focal length and 
equivalent points of a combination, such as a photographic objective. 


The secondary axes govern the position and size of the image, and since 
they pass through the second equivalent point, if the combination he rotated 
horizontally around a vertical axis immediately beneath E 2 the image from 
originally parallel light will remain stationary. If the system be rotated 
around any point other than E. 2 , the image will move. Light from the colli- 
mator (Fig. 354) falls on the lens so that the screen S locates F B . The com- 
bination is mounted in a special carrier capable of longitudinal adjustment 
from and towards S, and also rotation round the vertical axis A. Then, by 
lateral swing and longitudinal movement of the lens, a position is found where 
the image on S is motionless. Adj ust S to secure the sharpest possible image ; 
then the distance from A to S on the bench is the equivalent focal length, 
and the prolongation of A upwards locates the second equivalent plane E 2 . 
By reversing the combination in the carrier E l can be similarly found. It 
may be necessary in some cases to rotate the combination or lens on a point 
outside, as with periscopic single lenses. 

This method is especially suitable for photographic objectives having a 
wide angle of sharp definition; with uncorrected lenses, however, only a small 
rotation is possible before the image becomes confused from oblique aberration. 

Rotation Method — Negative Combination. — Rotation also serves for a 
negative combination, but in this case the virtual image formed of originally 
parallel light must be observed. The combination is placed between the 
telescope and the collimator. Focus carefully on the virtual image formed 
by the lens by drawing out the eyepiece, and get the image on the vertical 
cross-wire of the telescope. Rotate the combination as described for a posi- 
tive combination until the image seen through the telescope is stationary and 
sharp. Remove the combination from the carrier and bring up some object 
until its image is also seen clearly in the telescope. Then the distance of this 
object to the standard which originally held the Cc. system is the focal length 
of the latter. 

Approximate F of Small Strong Cx. Lenses. — Put up a scaled screen at 
10 inches from the lens and on the other side a small obj ect of known diameter. 
Adjust this so that its real image is formed on the screen, and note the mag- 
nification. Then F of the lens=10/M. Thus if M=5, F=2"; if M=40, 
F=l/4, etc. 

Fia. 355. 

Conjugate Method — Positive Combination. — Since F Z =A B, where A and 
B are the distance of and I beyond F, respectively, on the one and the other 




side of the lens system, this enables the focal length to be experimentally 
determined. Thus focus parallel light on the screen, and mark P 2 (Fig. 355) ; 
repeat the process on the other side and similarly mark F v Then place the 
cross- wires at a convenient distance^ and its image is at/ 2 ; measure F^^B 
ai&o f 1 F 1 =A, then F=\/AB. 

This should be checked by finding a second pair of conjugates A' and B'. 

Laurance's Method — Positive Combination. — Focus sharply for parallel 
light to locate the principal focus F B ; then move the screen back to/ 2 (Fig. 
356) which is n inches from F (say 1/3 of its focal length). Move the cross 

Fig. 356. 

wires in front of the lens "until its image is "sharply focussed on the screen at 
f 2 and mark its position P. Again withdraw the screen to/ 2 ', which is exactly 
one (or more) inches farther back, so that it is now n' inches from F; shift 
the wires toP' until the image is again in focus at//. Measure the distance 
PP' through which the object has been moved; call it d. 


F= V 


n —n 

If n' be exactly 1 in. longer than n, then n' -w=l, and therefore need not 
be regarded. Further, if w=l and n'=2, the calculation simplifies to 
F=V2 d. This is the true focal length, since it is independent of the posi- 
tion of the equivalent planes, which can be found by measuring the focal 
distance backwards from the principal focus. Thus supposing d=3'5", 
F=V2x 3-5 =2-65" approx. 

The Gauss Method for a Positive Combination. — Let u be the angle sub- 
tended at the lens by any two distant objects (Fig. 357) A andP, one of which 
B is situated on the principal axis. This angle can be measured by means 
of a theodolite, and therefore the angle u' subtended by the image B' A' at 
the second equivalent point C is also known, since it is equal to u. Then 

tan u'=h'/C B' or C B'=F=A'/tan u' 

The image h' can be measured directly on the screen. Since this method 
is independent of the position of the equivalent planes, these are not shown 



in the figure, being the 2nd equivalent point. If w=45° (Fig. 358), then 
tan 45=1, and F=h', i.e. the size of the image B' A' is equal to the focal 
length of the lens. 

Fig. 357. 

Fro. 358. 

Dallmeyer's Method for a Negative Thick Lens.— Take an achromatic 
positive lens and focus the image of the cross- wires on a screen; measure the 
size of the image formed and let it be m (Fig. 359). Place the negative lens, 

Fig. 359. 

whose focus is to be found, a short distance within the convergent beam of 
the positive lens, i.e. between it and the screen. Focus tin image formed 
by the combination and measure its distance D from the back surface or 
flange of the negative lens; measure the size m x of the image f »rmed. The 
size of m x compared with the size of the image produced by the positive lens 
alone is M=m 1 /m. 

Now move the negative a little nearer the positive lens (which latter 
must be kept in a fixed position) and focus a second time on the screen; 
measure the distance D' of the screen from the back of the negative lens or 
its flange. The size of the image m 2 compared with the size of m is W =m 2 /m. 
Then the focal length F of the negative lens is 




If M can be made equal to 2, and M' to 3, then F^D' - D. 



This equation is independent of the position of the equivalent planes, 
and therefore will hold true for any negative combination of lenses. 



Fig. 360. 

Fig. 361. 

i = 


Fig. 362. 

Fig. 363. Fig. 364. 

Small Strong Positive Lens — Dr. C. V. Drysdale's Method. — The focal length 
of small lenses can be found by means of a microscope which has a jDortion 
removed from the tube so that light, from a distant source placed at the side, 
enters the aperture and falls on a transparent reflecting surface M inclined 
at 45°, so that part of the light is transmitted down the tube as shown in 
Fig. 360. The eyepiece is arranged for parallel light by separation of the 
components, the adjustment being made by turning the reflector so that 
the light admitted is reflected towards the eyepiece. 

Employing no objective in the microscope and a plane mirror behind the 
lens to be tested, this mirror is moved to and fro until the image is sharp in 
the field of the eyepiece. The mirror is then at the focal length of the lens, 
the light converged by the latter being reflected back and refracted again as 
parallel. The lower focal point is thus found, as in Fig. 361. 

Replacing the objective (Fig. 362), the lens is moved farther back to such 
a po3ition that it is at its focal length behind the focal point of the objective. 
Then the light converged by the objective and refracted by the lens is parallel, 
and falling on the mirror, is again reflected as parallel, to be refracted by the 
lens to meet at the focal point of the objective, by which it is again refracted 
as parallel light. The image is sharp in the field of the eyepiece, and the upper 
focal point is found. 

The two focal points being marked, the back surface focal lengths are 
obtained. If, now, the mirror be moved a given distance A downwards, and 
the objective moved upwards by a distance B until the image is clear, we 
obtain the equivalent focal length from F B =VAB, where A and B are the 
distances of the conjugates beyond F B on each side. 

Dr. Drysdale has also made an experimental microscope in which the 
lens under examination can be oscillated around its second equivalent point. 
This enables the focal length to be determined, and further, by this means, 
aberrations can be easily detected. . 


Curved Surfaces. 

Dr. C. V. Drysdale's Method. — Dr. Drysdale's method of determining the 
radius of curvature of small surfaces as follows: Part of the light, received in 
the tube of the microscope, as described in the last article, is reflected down- 
wards towards, and through, the objective, by which it is brought to a focus 
at F as in Fig. 360. If, then, the reflecting surface of a mirror or lens is placed 
at the focus of the objective, the light is reflected back and seen by the observer 
in the field of the eyepiece, as an image of the source. This position or dis- 
tance of the objective from the reflecting surface is then marked on some part 
of the microscope. The tube of the latter must be racked upwards, if the 
surface examined is Cc. (Fig. 363) or downwards if Cx. (Fig. 364), until the 
image can again be clearly seen. The focus of the objective now coincides 
with the centre of curvature of the reflecting surface, for the light passing 
through the objective is incident on the reflecting surface normally and is 
reflected back along its original course. The distance between the first and 
second positions of the microscope objective, when the image is clearly seen, 
is the radius of curvature. The curvature of any zone of the surface can 
be obtained by using a suitable diaphragm. 

A later improvement made by Dr. Drysdale on the arrangement of the 
instrument used in the above method consists of an illuminator immediately 
above the microscope objective and a lens above the illuminator, which serves 
as the objective of the telescope and obviates the necessity of separating the 
eyepiece lenses. 

Telescope Method. — If the object be sufficiently distant compared with 
that of the image, as is the case with mirrors of small radius, when the object 
is, say, a metre distant, then the radius r of the curved surface bears to the 
distance of the image from the pole of the mirror, the relationship of r=2F, 
where F is the focal distance and the distance of the image. Let h x and h 2 
be the sizes of, respectively, the object and the image, and/ x the distance of the 
object from the mirror, while/ 2 is its focal length. Then 

/a=/iV^ and r=2/ 2 
The radius of curvature, of strongly curved lenses and mirrors, whether Cx. 
or Cc, can be measured by employing an instrument like the ophthalmometer. 
The distance between the two objects being known, that between the two 
images can be measured by a micrometer scale placed in the focus of the 
eyepiece of the telescope. f x is the distance of the objects from the curved 
surface, \ is the distance between them, h 2 is here the distance between the 
two images, as measured by the micrometer, and F is the distance between the 
objective and the micrometer. The relative size of the image formed atj^ 
and that formed at the micrometer is a,af x : F, so that the above formula 
must be multiplied by/j/F, and we then obtain 


Reflection Methods — On the Cx. surface (Fig. 265) to be measured, mark 
two small spots A and B, a convenient and known distance apart. At some 
convenient distance D E arrange two small white objects P and Q, so that 

Fig. 365. 

on sighting directly over each their virtual images P' and Q' are aligned, 
respectively, with A and B. Then the radius of the surface C A,C B, can be 
calculated from the following — 


EC~ED + DC~PQ ° r D PQ^AD 

Gauges. — The radius of small convex lenses can be determined by accur- 
ately made gauges, or more generally by glass cups of known curvature, 
usually known as test-plates. When the curvature of the lens does not corre- 
spond to that of the cup, interference rings are exhibited, while these are not 
shown if the two curves exactly correspond; or they are faint, and of slight 
brilliancy of colour, if the curves nearly correspond. A total absence of colour 
is, however, in practice, rarely found. 

The Refractive Index of Solids. 

The Spectrometer Method is the most accurate, that of the microscope 
being fairly exact; the others are more or less approximate. 

Spectrometer Method. — P the principal and d the deviating angles being 
measured, as described in Chapter XX., 


^~ sin(P/2) 

d must be the minimum angle of deviation. If P is not too large and the 
light falls normally on to one surface, the formula becomes simplified to 
^t=sin (P+ (Z)/sin P. If white light be used a spectrum will be formed, but 
the index for any particular colour can be obtained by bringing the cross- wire 
of the telescope over that particular colour. The mean index is calculated 
from the yellow (D line) and the mean dispersion from the difference between 
the indices of blue-violet (F line) and orange-red (C line). 

For example, a prism whose principal angle P is 59° 57' and whose 
angle of minimum deviation d for the D line is 40° 21', then 

P+tf 59° 57'+ 40° 21' n , , P n , 

— - = =50° 9' and -=29° 58' 

2 2 2 

sin 50° 9' -7677 , Bmn 

so that u=- — n „„ ,= ,^„=1'536. 

r sin 29° 58' -4995 


Microscope Method. — With a thin plate and a low-power microscope, ii 
fine line is focussed and the plate is then placed above the line. Now the 
microscope must be raised in order that the line be clearly seen, since the rays 
proceeding from it are divergent as if from a point nearer to the objective. 
The distance that the microscope objective has to be raised equals the distance 
between the real position of the line and its apparent position when seen 
through the plate. Let t be the thickness of the glass, and d the distance that 
the objective has to be raised; then fx=t/{t- d). The necessary measure- 
ments can be made fairly accurately by means of a mm. scale, some point 
on the tube being taken as the index pointer. A fixed scale, with a vernier, 
attached to the microscope, or the scale on the millhead of the fine adjusting 
screw, gives more exact readings. Thus, if the thickness of the plate be 
1 mm. and the object-glass has to be raised -38 mm., ^t=l/'62=l*6I. 

Fig. 366. 

Bench Method. — The medium being in the form of a block with two parallel 
surfaces. Take any Cx. lens L (Fig. 366) of convenient strength and project 
an image of the cross- wires D on to the screen S, such that $ and D occupy, 
approximately, symmetrical planes; note the position of D. Then introduce 
the medium M , whose index is to be found, between L and D, when the image 
on S will be found out of focus owing to the apparent vertical displacement 
of D. In order again to secure a sharp focus on S the disc must be drawn 
back to some point D' whose position is also noted. Then, if t be the thick- 
ness of the medium and d the distance between D and D'— the apparent dis- 
placement — we ha,veju—t/(t - d). The image on S must be well defined, and 
therefore an achromatic lens should be used. 

Block Method. — The refractive index of a transparent body, such as glass, 
can be roughly found as follows :— Make a dot d (Fig. 367) on the back of the 
block of glass; its image is d', nearer to S; then find such a position for a pin 
P, placed vertically in front of the glass, that on moving one's head from side 
to side the virtual image P' of the pin, by reflection from the front surface, 
appears to be behind that surface at such a distance that, owing to absence of 
parallax, P' coincides with d'. Then the apparent thickness of the glass is 
P' S=PS, a,nd/u=dS/PS. 

Plate Method. — A parallel plate (Fig. 368) of the medium, say glass, is 
placed on a sheet of white paper on a drawing-board or other smooth surface. 
A pin P x is then stuck in any position and a second pin P z is placed close to 
the plate and sufficiently to the left of P x so that a line P l P 2 makes a fairly 
large angle i with the normal N N'. Now observe, through the plate, the pins 



P 1 P 2 , which will appear displaced towards the right. Stick two more pins 
P 3 andP 4 in the board such that all four appear in one straight line. Draw the 
trace of the plate with a fine pencil, remove it and the pins, and with a 
compass, withP 2 as centre describe any circle — the larger the better, provided 

/ ! 








Fig. 367. 

f" 1 

i f ! 

Fig. 368. 

it falls within P 3 . Where this cuts the course of the ray in Q and M drop the 
perpendiculars Q N and M N', which are the sines of i and r respectively; 
ihen/Li=Q N/M N'. This method is only approximate unless carefully done 
and therefore three or four readings for different values of i should be taken 
and the mean result extracted. 

Critical Angle. — Should it be possible to measure C, the critical angle of 
a medium — generally this is neither easy nor accurate — ju=l/sm C. Such 
a method might be suitable for a substance like butter for which other methods 
are not. A special apparatus — a refractometer — is required. 

Polarising Angle. — This may be the most convenient method for an opaque 
body, for ju—ta,n p. 

The polarising angle can be found by an arrangement of a small source 
of light and a piece of tourmaline from a pebble tester, the axis being vertical. 
Then on raising or lowering equally both source and tourmaline from the sur- 
face of the medium to be tested a position will be found where the reflected 
image of the source is cut off. Measure the distance d from the point of reflec- 
tion on the surface of the medium to the point on the surface immediately 
beneath the tourmaline, also the height h of the latter above the surface. 
Then^^tan p=d/h. 

Prism Method. — If a spectrometer is not available, the value of P and d 
can be found roughly as follows : Place the prism (Fig. 369) on the drawing- 
board with the apex towards a window; look into the surface A B, which acts 
as a plane mirror, and select the image of a vertical window bar; get the image 
as near as possible to the apex A and put the pinP x in position so that it is in 
line with A. Do the same with the other surface A 0. Make a trace of the 
prism, remove it and the pins; then the angle formed by the lines P X A and 
P 2 A (i.e.P! A P 2 ) is twice P, the principal angle. P x A P 2 is measured with a 


To find the deviating angle d, erect, in any convenient position, two 
pinsP x and P., (Fig. 370), place the prism with one side in contact withP 2 ; 
then on looking through the prism somewhere in the direction V, the pins 
will appear displaced towards A. Secure minimum deviation by rotating 

the prism both ways, and finally erect two other pins P 3 and P 4 such that all 
four appear in one line. Then, by making the necessary tracings and con- 
nections with a fine-pointed pencil, the angle of minimum deviation d can be 
marked and measured on a protractor. 

Lens Method. — If the medium be in the form of a thin lens, its F and radii 
can be measured, and// calculated from the lens formula. 

The fi of Metals. — By making exceedingly thin prisms of less than one 
minute of arc, Kundt successfully determined the refractive indices of a 
number of the metals. The results showed that silver, gold, copper, mag- 
nesium, and sodium have an index less than that of a vacuum, and this, no 
doubt, accounts for the absence of a polarising angle in these substances. 
The red rays in some cases were found to be more refracted than the blue, 
so that metals form good examples of anomalous dispersion. The refractive 
indices of the metals were found to be proportional to their electric conductivi- 
ties, i.e. those metals which were good conductors have a low refractive index, 
and vice versa. 

The Refractive Index of Liquids. 

The jli of Liquids. — In general, the methods for solids can be employed 
for liquids, but the arrangements differ in some instances. 

Spectrometer Method. — The liquid is placed in a hollow glass prism whose 
sides are thin and with quite parallel surfaces. 

Microscope Method. — First focus the bottom of a small tank, and then its 
image when the liquid has been poured in. Finally focus the surface of the 
liquid, which should have some conspicuous dusk specks floating on it. The 
difference between the third and first readings gives the real depth, and that 
between the second and third the apparent depth. 


The critical and polarising angle methods are the same. The bench, block, 
plate, and prism methods are also applicable if the liquid be enclosed in a 
suitable plane glass box or prism. For the block method (q.v.) the liquid can 
be in a bowl with d at the bottom and P held above the liquid. 

Lens Method. — Take a small quantity of the liquid and place it between 
a thin plate of glass and a Cx. lens of known radius and focal length F x ; the 
liquid then forms a plano-Cc. lens. If now F of the combination be found, 
that of the Cc. F 2 can be learnt from 1/F 2 — 1/F- 1/Fj. Its radius is also 
known, it being that of the Cx. lens, so ju can be calculated from /j, - 1 =r/F. 


Those numbers in heavy type indicate chapters or main articles an particular subjects. 
subheadings to the articles serve as further guides. 



• • • • 


Coloured body . . 

.. 203 

Aberrations in general . . 

. . • • 


,, light 

25, 204 

,, oblique 

• • . . 


,, glass 

27, 205 

,, of colour . . 

■ • . • 



. 225, 230 

,, of form 

. . 


Compound systems 

. 180, 184 

, , plane 

. . . . 


Confusion discs 

.. 303 

,, point 

. . 



. . vii 

Achromatic calculations 

.. 215 


Convention, optical 

.. 79 


• • 



.. 169 


• • • . 


Cornu's method 

.. 5 


. ■ • • 


Crown glass 

.. 294 

Analysing card 

. . 



.. 275 

Angle, critical . . 

i « 



.. 193 

,, ,, table of. . 

• . ■ ■ 


,, of field 

. 225, 234 

,, deviating 

59, 127 


,, system 

.. 193 

,, dispersing 

. • 



. 104, 118 

,, notation.. 

• • • ■ 


, , polarising 

. . . . 



.. 138 

,, principal 

59, 127 



.. 133 

Angular aperture 

. . 


,, resultant.. 

.. 141 

Aperture ratio 

• . 


,, oblique . . 

.. 258 

Aplanatic reflection 

. . 



.. 3 

,, refraction 


Deviation, minimum . . 
Dichroic bodies 

.. 60 
.. 213 

Back focal distance 

■ ■ • ■ 



.. 282 

Bifocals, cement 

. . . . 



.. 13 

, , fused 

. . 



51, 207, 212 


■ • ■ • 


,, angular 

.. 214 

Bougie decimale 

. . 


,, anomalous . . 

.. 213 

Brewster's stereoscope. . 

. . 


,, irrationality of 

.. 222 

Bunsen photometer 

. . 


,, index of 
,, of prism 

.. 207 
.. 210 


. . . . 


, , table of indices of . 

.. 208 

Camera . . 

. . 


Dispersive power 

.. 209 


. . 


Displacement, by refraction . 

.. 54 


• • ■ ■ 


,, lateral . . 

.. 56 


• • • • 



. 225, 235 


. . 


Caustic curve 

• • • . 



.. 287 

Change of medium 

. . 


Effectivity of lenses 

.. 143 

Chemical rays 

. • • • 



.*. 152 

Chromatic aberration . . 

• • • • 


Equivalent focal length 

.. 152 

,, difficulties . . 

. . 


,, points 

. 152, 180 


207, 210, 




Circle of least confusion 11 

)8, 217, 226 


Experimental work 

.. 325 

Coddington lens 

• • • • 


Eye and lens 

.. 157 

Colour . . 



,, in dense medium . . 

.. 57 

„ mixing . 



Eyepiece, erecting 

.. 147 




Eyepiece, Huyghen 
, , Kellner 
,, Ramsden 

Fata morgana . . 

Fizeau's method 


Flicker photometer 

Flint glass 


Focalisation, notes on 


Foot candle 

Foucault's method 

Fraunhofer's lines 

Gauss equation 
Geometrical centre 
Glass, optical . . 
„ unannealed 
Glasses, optical, table of 
Grating, diffraction 
Grease-spot photometer 
Greek alphabet . . 


Hefner- Alteneck standard 



,, artificial 

Iceland spar 
Images . . 

,, multiple 
Inverse squares . . 
Inversion, lateral 

Joly photometer 


Least time 

,, aberrations of colour 

,, aberration of form 

,, achromatic 

, , addition . . 

, , af ocal 

,, aplanatic . . 

,, apochromatic 

,, back focal length 
best form of 


147, 156, 318 
147, 157, 318 
147, 157, 318 














. . 275, 279 
13, 28, 79, 305 
28, 46 
. . 18 
. . 30 

. . 24 



79, 80 





147, 150, 168 

225, 230, 240 


'.'. 146 


bounded by different media 182, 184 
Cc. aberrations of . . . . ■ 238 

characteristics of . . .. ..84 

combinations 146,152,160,172, 

177, 184, 222 

Lens combinations, measure of 
conjugate foci 

cylindrical . . 104, 

crossed cylindrical 
cylindrical, oblique powers 

,, reversion of 

discs for 
in dense medium . . 
forms of . . 
magnification by . . 
numeration of 
oblique cyls. 
obliquely crossed cyls. 
optical centre 
piano-cylindrical . . 
prismatic action . . 
rectilinear. . 
results of separation 
sizes of 

,, measurement of 
thickness of 
thin, measurement of 

toric or toroidal . . 
value of . . 

absorption . . 10, 26, 


colours of . . 6, 199, 



frequencies of 


linear propagation of 




recomposition of 





transmission . . . . 10 



Lummer-Brodhun Photometer 


.. 335 
.. 169 

94, 175 

.. 107 
.. 250 
.. 124 
.. 295 

143, 146 
.. 169 
.. 152 
.. 318 
.. 181 
.. 81 
.. 267 
.. 309 
81, 248 
.. 119 
.. 92 
.. 248 
.. 251 
.. 83 
.. 225 
81, 248 
.. 106 
.. 134 
.. 225 

155, 159 
.. 17 
.. 296 
.. 225 

106, 234 
.. 161 
.. 335 
.. 163 
.. 328 
.. 245 
.. 115 
.. 85 

206, 303 
.. 12 

204. 207 
.. 12 
.. 12 
.. 12 
.. 12 
12, 223 

274, 280 






, 26, 303 
. 3 
. 19 
. 285 
,. 24 



I'Ai : E 





56, 209 

Luminous bodies 



.. 274 


.. 277 

Magnification . . 

39, 43, 74, 99, 175 


.. 277 

Magnifying power 


Practical work 

.. 325 

Mangin mirror . . 





81, 248 

Principal points 

.. 180 


105, 110, 121 

Prism binocular 

.. 313 

Meridional plane 



.. 129 


.. 213,295 

Prisms . . . . . . 58, 

127, 194 


.. 316 

,, aberrations of . . 

.. 223 


.. 288 

,, achromatic 

.. 215 

Mirror . . 

28, 29, 195, 301 

, , chromatism of . . 

.. 210 

,, aberrations of . 


, , false images of 

.. 65 

,, aperture of 

. . 44 

,, indirect action of 

.. 256 

, , aplanatic 


,, measuring 

.. 129 

,, concave . . 

. . 33 

,, neutralisation of 

.. 124 

,, convex . . 

. . 34 

,, notation of 

.. 127 

,, conjugate foci . 

. . 38 

,, oblique . . 

.. 131 

,, curved . . 

. . 33 

, , oblique powers of 

.. 256 

,, cylindrical 


,, obliquely crossed 

.. 257 

,, inclined . . 

. . 32 

,, reflecting 

.. 53 

,, measurement of 


,, resultant 

>. 131 

,, parallel . . 

. . 32 

,, rotary (variable) 

.. 132 

,, plane 

. . 29 

, , rotation of 

30, 44 


.. 275 

Miscellaneous . . 


Neutralisation . . 


Radial astigmatism 

,, line 
Ramsden circle 

225, 231 
.. 231 
.. 287 


,, thick lenses . . . . 177 
Newton's formulae . . . . 44, 78, 101 

,, rings.. 
Nicol prism 
Nodal points 
Numerical aperture 

. . zsz 
. . 28 


Reflection . . . . 10, 28, 
diffused (irregular) . . 

tests. . 
,, total. . 

1, 80 

241, 290 

.. 10 

.. 326 

.. 51 

Object 13, 79 

Oblique refraction and deviation . . 245 


, , double 

46, 290 
.. 275 

Opera glass 

,, ,, notation . . 

10, 303 

Refracting reflector 

. . 291 

150, 158, 169, 314 

Refractive efficiency . . 
, , index 

.. 208 
.. 46 

Optical bench . . 
, , centre . . 

83, 133 

,, ,, measurement of 
,, indices, table of . . 

.. 342 

51, 295 

,, instruments 


Resolving power 

.. 317 

, , lantern 


Rock crystal 

.. 276 

signs .. 


Romer's method 


. . . . 13 

Rumford photometer 

.. 22 



Sagittal plane 

.. 231 

Parallel media 

. . 57 


.. 289 


. . 274, 276 

Scissors movement 

.. 123 




.. 322 


14, 16 

Shadow photometer 

.. 22 


. . 3 


.. 14 

Perspective, aerial 


Simmance-Abady photometer 

.. 24 

Petzval condition 


Sine condition 

.. 231 

Phenomena of light 


Sines, law of 

.. 49 




.. 286 

Photometric standards 


Slab photometer 

.. 24 




.. 322 


. . 268, 302 


.. 211 




.. 321 

Plane surface . . 

. . 193, 326 

,, direct 

.. 322 




. 7, 9, 210 

Telescope, astronomical 147, 156, 311 

,, diffraction . . 

.. 283 

Galilean ..150,158,169,314 

,, invisible 


,, reflecting . . . . . . 316 

, , irrationality . . 

.. 213 

,, terrestrial .. .. .. 313 

,, lines, table of 

.. 7 

Telescopic test . . . . . . . . 333 


. 118, 170 

Test types 301 

Spherical aberration . . 

.. 225 

Tories 110,115 


. 308, 310 

Toroid 118 

Stanhope lens 

.. 273 

Tourmaline 275, 277 

Steinheil cone 

.. 169 

Translucency . . . . . . . . 10 


.. 320 

Transmission . . . . 10, 26, 206, 303 

Sturm, interval of 

.. 107 

Transparecny . . . . . . 10 


.. 196 

Transposing . . . . . . . . 110 

,, aplanatic 

66, 239 

,, conjugate foci 

.. 74 

Umbra 14, 16 

,, curved 

.. 66 

Unofocal lens . . . . . . . . 148 

,, measurement of 

.. 341 

,, plane 

46, 193, 326 

Vernier 323 

Surfacing tools 

.. 310 

Violle 22 



Visual angle . . . . . . . . 267 

,, artificial 

.. 302 


. . viii 

Wave front 2, 47, 194 

Wave-lengths 8, 199 

Tangent condition 

.. 237 

,, ,, measurement of .. 284 

,, scale 

. 129, 301 

,, ,, table of . . . . . . 8 

Tangential line 

.. 231 

Wheatstone's stereoscope . . . . 320 

Telephoto lens 

.. 150 

Wollaston prism . . . . . . 279 


.. 311 

lens 273 


J. & H. TAYLOR, 

Dioptric Works, Albion St., BIRMINGHAM. 

J. & H. TAYLOR (London) Ltd. 

Dioptric Works, Red Lion St., Clerkenwell, 








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