Skip to main content

Full text of "An elementary introduction to The Nautical almanac, and astronomical ephemeris"

See other formats


This is a digital copy of a book that was preserved for generations on Hbrary shelves before it was carefully scanned by Google as part of a project 

to make the world's books discoverable online. 

It has survived long enough for the copyright to expire and the book to enter the public domain. A public domain book is one that was never subject 

to copyright or whose legal copyright term has expired. Whether a book is in the public domain may vary country to country. Public domain books 

are our gateways to the past, representing a wealth of history, culture and knowledge that's often difficult to discover. 

Marks, notations and other maiginalia present in the original volume will appear in this file - a reminder of this book's long journey from the 

publisher to a library and finally to you. 

Usage guidelines 

Google is proud to partner with libraries to digitize public domain materials and make them widely accessible. Public domain books belong to the 
public and we are merely their custodians. Nevertheless, this work is expensive, so in order to keep providing this resource, we liave taken steps to 
prevent abuse by commercial parties, including placing technical restrictions on automated querying. 
We also ask that you: 

+ Make non-commercial use of the files We designed Google Book Search for use by individuals, and we request that you use these files for 
personal, non-commercial purposes. 

+ Refrain fivm automated querying Do not send automated queries of any sort to Google's system: If you are conducting research on machine 
translation, optical character recognition or other areas where access to a large amount of text is helpful, please contact us. We encourage the 
use of public domain materials for these purposes and may be able to help. 

+ Maintain attributionTht GoogXt "watermark" you see on each file is essential for informing people about this project and helping them find 
additional materials through Google Book Search. Please do not remove it. 

+ Keep it legal Whatever your use, remember that you are responsible for ensuring that what you are doing is legal. Do not assume that just 
because we believe a book is in the public domain for users in the United States, that the work is also in the public domain for users in other 
countries. Whether a book is still in copyright varies from country to country, and we can't offer guidance on whether any specific use of 
any specific book is allowed. Please do not assume that a book's appearance in Google Book Search means it can be used in any manner 
anywhere in the world. Copyright infringement liabili^ can be quite severe. 

About Google Book Search 

Google's mission is to organize the world's information and to make it universally accessible and useful. Google Book Search helps readers 
discover the world's books while helping authors and publishers reach new audiences. You can search through the full text of this book on the web 

at |http : //books . google . com/| 

• • • • 












Cbarlbb Wilson, Lbadknhall St. 
Melling & Payne, South Castle St. 

it S3. 


The scheme of the following pages is to afford instruction without the aid of 
any other work than the ^'Nautical Almanac, and Astronomical Ephemeria/' to 
which it is professed they are an Introduction. 

Writers on Elementary Astronomy generally either reserve the information 
most eagerly sought hy the curious, or detail it on the supposition that the rea- 
der is a mathematician. Undouhtedly no great progress can he made in Astrono- 
my without the aid of the mathematics, hut there may he a medium between a 
perfect acquaintance with these abstruse studies and a sufficient knowledge to make 
astronomical data easy of comprehension. The Author, therefore, in pursuance of 
his plan has, he beUeyes, familiarised and introduced as many scientific explana- 
tions as may enable any student to comprehend the facts and complicated theories 
of the Celestial Phenomena. It will be immediately evident to the scientific rea- 
der that any attempt at such explanations beyond an outline would not be 
consistent with the scope of so small a work as the present. 

The alphabetical arrangement has been adopted for the convenience of reference* 
and care has been taken to give in every article the words to which the student 
must refer to complete his information on any one subject. 


Astronomy may be defined as the science which teaches the order, motions, dis* 
tances, magnitade,eolipses and appearances of the heavenly bodies, and their relation 
to the Earth. The study of this science consists of systematic observations of the sun 
moon, planets and fixed stars; and to assist these observations there are books and 
tables of general calculations, maps which delineate the apparent places of the starry 
host; and the celestial globe, on which we see the stars, not as they appear in the 
heavens, but reversed for the purpose of working problems. The stars on the celestial 
globe would present a picture of nature if the globe were hollow, the stftrs pierced 
through the shell, and we were to view these apertures from the centre instead of the 
circumference. The symbols and abbreviations used in Astronomy are the foUowingir 

The Run. 


Conjunction. Signs of the Zodiac. 


The Moon, 


Quadril. Hours of 



New Moon. 


Opposition. Riffkt 



First Quarter. 


Trine. Ascension, 



Full Moon. 


Sextil. r 

Aries. - - ^ 0° 


Last Quarter, 


Ascending Node. I 

Taurus. -. - 30 




Descendii^ Node. II. n , 

Gemini. - 60 




North. III. ffi 

Cancer, r - 90 


The Fiarth, 


South. IV. St 

Leo. . - - 120 




Ea-st. V. 1TJJ 

Virgo. - - 150 




West. VI. ^ 

Libra. - - 18U 




Degrees. VII. tn. 

Scorpio. - 210 




Minutes of degree. VIII. f 

Sagittarius. 240 




Seconds of degree. IX. Yf 

Capricomus. 270 




Hours. X. ns 

Aquarius. - 300 




Minutes of Time. XI. K 

Pisces. . -330 


The Georgian. 


Seconds of Time. 

B.A. Bright Ascension. 

Dec. Declination. Long. Longitude 

. Lat. Latitude. 

Greek characters to denote the magnitude of fixed stars in any particular constella- 
tion: a Alpha, First magnitude; /3 Beta, Second; y Gamma, Third; 8 Delta Fourth; e 
Epsilon, Fifth; f Zeta, Sixth; i; Eta, Seventh; S Theta, Eighth; i Iota, Ninth; k Kappa 
Tenth. These characters are sufficient to distinguish the principal fixed stars, but 
the whole of the Greek alphabet is used ,and, when exhausted> the Italian and Boman 
characters, and the common numerals are employed. When a Greek character and a 
numeral are both used they denote tht^t there is more than one star of the same mag- 
nitude in the constellation; as a* Geminorum, (Castor J the star Pollux being a^ 
Greminorum. a. Alpha, also signifies Ascension, and ^, Delta, Declination. 

€ AB. AC. AG. AL. 

ABERRATiON>(^a deviation.) Light occupies 8" 13" (8 minutes 13 seconds of time) 
in passing from the Sun to the Earthy and during this time the Earth has moved 
20'', (20 seconds of a degree, the entire orhit of the Earth round the Sun heing 
reckoned as a circle of 360 degrees) . At any instant, therefore, the rays of light 
which reach the Earth are those which left the Sun 8" 13* previous, when the Earth 
was in a different position with the Sun to that which it occupies at the time 
of observation. This phenomenon is called aberration, and the luminous circle which 
mi^ be seen around the real disc (face) of the Sun (caused by the aberration of 
the solar rays) is called the crown of aberration. And as the aberration of the 
Sun is owing to the motion of the Earth in its orbit, so the aberration of a Pla- 
net is due to the ownbiii^ moUofas of that Planet ahd the Earth in their respec- 
tive orbits. It is therefore said, that the. aberration of a Planet is equal to the 
geocentric ( See geocentric, ) motion of the Planet, or the space it appears to 
move ovef as seto from the Earth, during thi timb (^' light ocec^wes in piss- 
hxg {\rom the Planet lx> the Earth. ¥^ tiie method «f estinMiJig Ae amomil; cf 
abemAion see mens^ratiok. 

Acceleration. Either a real or ap^a^t iiitii^ase of Uhc veloctty dt cdlMltiifl 
bodies. It is idito applied to th^ difibrence belfweito a sblkr and sidereal di^, {ISeis 
TIME ) or the time by which th^ ttxed Hti*s art seen froih the Earth, oh €Btt9t 
arrival at some pbint, such as the mendMi point {iSf€^ MERii^rAiv) to anticipate !3ie 
anival of the Sun at the same point. A Star which i^ses with the Sun one day wW 
rise 3°* S6* Sooner than the Sun the sncceefing diay. This nebehraihn is caused: by 
the Eftrth revolving in its orbit round the Sun, so that we View the'^n StSy in it new 
point wit& relation to the Fixed Stars, which are at such an inxKmott'^ble distance 
that the entire circle of the Earth's path round the Sun ( the diaaiieter of the circle 
being 190 millions of miles, ) is but a speck when compared wiih idie imidensity of 
the Starry sphere. The acceleration of a Planet is a realintoveaiiib ofTielooity in one 
part of its elliptical orbit over its velocity in ichother part. The ddoelerMon of the 
Moon is a very slowly and gradually increasing motion of tke'MolDh Youkid the £arth> 
the cause of which is only attempted to be explained by mechanieal laws of great com. 
^lexity. Betardatixm is the term contrary to acceleration, and signxdes eiflier a real 
or apparent slowness of velocity at one time compared with anothsr. 

AcRONicAL, or AcrOnychal. a term given to the rising of a^itair above the ho. 
rizon as the sim sets, or to its setting below the horizon as the sun rises. 

Age of the Moon. See Moon. 

Altitude, is measured on the arc (of 90 degrees,) between the obser^r's zenith 
and horizon, {See angle, zenith and circles). Thus the Star in* the fimt diagram 
is at an altitude of 45^. ^ 

This apparent altitude differs firom the true td- S 

titude by the dip, parallax and refi'actum,(wkidh fil' 

loords see), and the allowance made for these differ- 
ences is called the correction of the altitude. 

When the apparent alti- 
tude is corrected the tme 

altitude is an angle between OhseriHr I J Sortie n 

two lines drawn from the centre of the Earth, one of them being 
the rational horizon. {See circles.) Cirhles t)f dtitude iwe at 
right angles with the horizon, and intersect each other at the zenith. IPorcffi^fo-of U- 
titnde are parallel to tlic horizon. 





AitfftiTUDB. W^ p^t of the <compm «t.iiir]Uch a jbefn^y b^dy rinses or ;^ts, or 
ibe Ai0t9»oe of tl^ jpvwiptl^m -tlie ^t'or W^t^^^t^nrar^ t^^ NqrOi^ Soutb. 

l>h»% m-.i^ 4iliginKm» o be^ng 4]ie position of the 

observer^ the am|Attt4eoftheStar.risipg|>r^isel7 

hdf way between the £iist and Nov|hjH>iQ^^will be 

45^N. (45,<il^a^ sN^orth) and thje amplitude of the 

West 4 A \ Easl other Star settiiig one quarter of the distance from 

the West to the South will be 22"" 30' S. (22 degrees 
30 minutes, or 22^ degrees South.) Amplitude may 
be called the horij^ontal azimuth. (See azimuth) . 
Circles of amplitude are at right angles with the 
horizon and ix^m&ct each other at the zenith. 

ANGiiSj (in Greometry)j is the incHnation or opening between two, straight lines that 
meot at one extremity. The point jwhere the lines meet is called the vertex or angu- 
lar p^t, and is taken for the oentre of a circle^ on the circumference of which the an- 
glejusoneasured m degrees and parts of a degree^ the whole circle b^ing divided into 
360?. The vBiie of ^-circle by whjich the angles are 
meas^ff^ is immaterial; the aras, or parts .of the cir- 
comference, of the largest and smallest circle described 
from ^ angular point, (that is drawn by one leg of a 
pair of compassesiwhile the other le^g is on the ai^2;ular 
pointy) and included between the lines forming the an- I 
g\e, being proportionate to each other. Thus one' 
fourth and one eighth of each circle in the figure are lii- 
•videdby the Imfis^ forming the angles 45° and 90° . 
iXhefigQrc^JieiNrQsento aiigles of 22^°, 45°, 90°aQdl35°, 
the ^e or radius forming in eadi caae one J^ of the 
.«n^^ jghile. tjbe measurement by degrees. is comn^on :to both drdes. It will be seen 
«itttajjghM|ce that an angle.cannot^y as 180°> the two.radji or lines 
^ from 0° and 180°.uotfoi]a9i^^rf^9]^}e« but becoming. one continued 
striught line. .Astranovucal.moQsurements.are performed by observing 
the angle included between any two points, as a Stiur and the nearest point 
of the horizon, a Star and the nearest point of the Moon's disc^; the eye 
of the observer being the angular point. In tig. 2. e. Leaad e. b, are the 
legs of the angle, e,a. the altitude, I, a. b. the base and e* the angular 
jpoint; the measurement of the angle taking place at the base or arc L a. b. 
Anomalistic Tear. See time. 

' An&s. When the Planet- Saturn is in sodi n position that we see the thin edge 
only of the Ring whidi suiTOunda him the term ofiMB is given to the Rii^ which then 
appears only as two horns or handles projedang fix>m each side of the IHanet. 

^ , , -fir Antbcedkmce. Although the FLgiets rise daily in 

the East r and. s^t in the West, an appearance owing to 
the rotation of the Earth on its axis, th^" are in reality 
pursuing the opposite course from West toE^t. There 
is an exceptipn to this rule however occasionally to 
be observed; the Fhmets appduring either to be sta- 
tionary among the Fixed Stars for a short period, or 
to retrograde towards the West. This is owing to the 
different positions of the Earth and Flanets with respect 



West to each other in different parts of their orbits. Thus, 


8 AP« AQ. ABu AS. 

With reference to the diagram, if the Earth proceed in its orbit, -from West iP 
Ea^ty whilst Jupiter is passing from W. to E. Jupiter will appear to he travelling 
westward, fot when the Earth is at West Jupiter is seen at W. towards the East, and 
when thg Earth is at East Jupiter is seen at E« towards the West. This apparent 
retrograde or hackward motion is called the antecedence, or motion in anteeedentia,w}ale 
the true motion is called the motion in eonsequentia or direct motion. 

Aphelion and Apogee. See Apsidcs. 

ApsitkES. As the orbits of Planets are elliptical, and the Sun not precisely in the 
centre, part of each orbit Is farther from the Sun than the opposite part, and the 
extreme points of the farthest and nearest parts are called the apsides. The most re- 
mote part is called the aphelion or higher apsis, oitBXa? 
and that part the most adjacent is the perihelion ,..-..•.—... — ^^^^ 
or lower apsis. The line of the apsides is drawn ..•'* \ . 
through the centre of the sun to the aphelion and ^'/\J» ^\ -% 
perihelion, as in the diagram. Instead of aphelion i!i / ^ CjWa '^\ ^T 

and perihelion the words apogee and perigee axe ^i\i; -.- ^J^aO' — v""'^!®*- 

used to designate the farthest and nearest points ^\^ **^if yuia^.j^. ^ 

of the orbit of the Moon round the earth, apogee '--^ ^/ ^ 

being the farthest and perigee the nearest point. '••.. y 

The Sun is also said to be in apogee or perigee q^' '^"5^ 

when the Earth is at the farthest or nearest point A P I«-A- ^ 

of its orbit round that luminary. 

Apparition. See Heliacal. 

Aippt^LSE. When two heavenly bodies can he seen at one view through the telescope. 

Aquarius, (the Waterman) The sign of the Zodiac which the Sun enters about the 
19th of January and leaves about the 16th of February. . . 

ARp. Part of the circumference of a circle. If at noon precisely an observer look 
towards the Sun and imagine a line in the heavens passing perpendicularly from the 
centre of the Sun to the horizon he will imagine an arc of his meridian. 

Aries, (the Ram.) A sign of the Zodiac which the Sun enters about the 21st of 
March andi leaves about the 19th of April. 

Asc&NDi^G. lUsing from the horizon. When a Planet's latitude {See latitude,) is 
increasing towards the North i^.is said to have an ascending latitude, hecause in the 
Northern parts of the World the Planet will appear to be proceeding farther from the 
Sorizon, and when a Planet's latitude is increasing towards the South it is said to 
have a descending latitude. The reverse of these terms would be appropriate in the 
houthem Hemisphere. The ascending node {See node) is that point of a Planet's 
orbit passing the Ecliptic towards the North. 

. Ascension. See Right Ascension. 

AscicNSioNAL Difference. See Right Ascension. 

Aspect, (ff Stars and Planets, is their situation with respect to the Sun or to each 
other. There are five aspects: Conjunction, when they are in the same degree ; 
Sextile, when they are 60 degrees distant from each other; Quartile, when they are 
90°, or one quarter of a great circle apart; Trine, when they are 120°, or the third 
part of a great circle asunder, and Opposition, when they are opposite to, or a semi- 
circle distant from each other. 






Astronomical Day. See Time. 

Astronomical Horizon. The Rational Horizon. See circles. 

Asteroids. Four Planets lately discovered; Juno, Ceres, Vesta and Pallas* See 


Austral. Soutliem. 

Augmentation. There is an apparent and cominonly observed increase of mag- 
nitude of the Sun and Moon when near the horizon, the cause of which is in dispute, 
but may be owing to the vast quantity of atmosphere through which we see those 
bodies when we look towards the horizon at them. A similar apparent increase of 
size takes place if ashilUng be put m a saucer with a small quantity of water, when 
the shilling will appear of its real size, but if the saucer be filled with water the shill- 
ing will appear much enlarged. We may consider the atmosphere as a large magni- 
fying power (or convex lens, as the optical term is,) weakest in the zenith, (See 
ZENITH,) towards which we look through the least quantity of atmosphere, and oPthe 
greatest power at the horizon, towards which we look through the 
greatest quantity. Thus to a spectator at a, of the Moon in the zenith M 

there is a much smaller quantity of atmosphere between the Moon and * ;' / \ 
his situation on the Globe than there is to a spectator at b. The ? A • 

figure will show how small the surface of the atmosphere, covered by Ij \ \ 

the reflection over a, is to that angular reflection caused by the rays 
proceeding to b. It vnUl be seen therefore that this apparent increase ^^0Si^?T? 
<of magnitude is only an optical illusion. The Moon, indeed, is decreetsed 
instead of increased in apparent diameter as she approaches the horizon 
from her greatest altitude. This is caused by the Moon being so much ff 
farther from the observer at b than from the observer at a. For the Moon being at a dis- 
tance of only 240, 000 miles from the Earth, and the distance from a toe, or one half 
the diameter of the Earth, being near 4000 miles, the observer at a is one sixtieth part 
of the entire distance nearer the Moon than the observer at b. The Augmentation of 
the Moon is 1 second of a degree when the Moon has an altitude of 5 degrees from 
the horizon, 10 seconds when at an altitude of 40°, 15" when at an altitude of 80°, and 
1 6" when at the zenith. 

Axis, of the Earth, An imaginary line conceived to pass through the centre of 
the Earth from North to South, and around which it revolves. 

Azimuth. The distance of a celestial body from the North and from the East or 
'West points of the Horizon of any place. When the body is so far from the North 

« 1 


as to be near the South the Azimuth is sometimes 
reckoned from the South point; that is, the sup- 
plement {See SUPPLEMENT.) of the Azimuth is 
taken instead of the Azimuth itself; but this is im 
material, for the number of degrees between the 
North and South being 180 it is of the same im- 
port whether we say a celestial body is 1 70° from 
the North or 10° from the South. The Azimuth 
"VVest of a Star is technically described as an angle at 
the zenith (See ZENiTH,)of a spectator contained between his meridian (See merid- 
ian.) and the circle of altitude (See altitude.) pasang through the star. If we 
suppose the star.* on the circle of altitude in the diagram to be precisely half the 



10 BE. BO. tSA. CE. 

distance between the West and South its Azunuih inXL be N. 135° W, {Northf 135 
degrees West.) or S. 45° W. (Sautk, 45 degrees West.) When the circle of altitude 
or Azimuth circle cuts the Horizon at the East and West points it is called the 
Prime Vertical. The star at the Eai^ in the diagram is on the Prime Vertical. The 
Magnetic Azimuth differs* from the Tnce Azimuth according to the variation of the 

Beard of a comet. The rays of light around the nucleus or central body, distin- 
guished from the tall, or himinou^ appearance emanating from that part of the 
Comet opposite the Sun. 

Bissextile, or Leap Tear. "Rx^ty fourth year, when a day is added to the calen- 

dar> the twenty mnth of February, for the cerrectioil of time. But as the excess of a 
Solar year (See time,) is not quite the fourth part of a day above the 365 days of 
a common year, and as the adding a day to the calendar every fourth year would ex- 
eeed the amount of correction required by 44 minutes in 4 years, ( or 1 1 minutes 
annually,) it is arranged that eeerg hundredth year shall not be a bissextile year but 
only three of every four centesimal or hundredth years. The leap years of the pre- 
sent century ace easily found by dividing the number of years since 1800 by 4; if 
remain it is leap year; if 1,2 or 3 remain it is 1,2 or 3 years after bissextile.- Exam- 
ple: Is 1849 a leap year? Answer: 4 times 12 are 48 and 1 remains; consequently 
the year 1849 is 1 year after bissextile. 

BoREAf.. Nofthem. 

Boreal Sn&NB. Theses of the Zodiab North df the Equator, Aries, Taurus 
Gemini, Cancer, Leo and VirgOi m which the Sun is ntuated from the 2l8t. of March 
to the 21 St. of August. 

Calendar. An Almskiac. Fbr' an exphflHtioii of the **R^eipal Articles of the 
Calendar^', in Ate Naoiical Almduae, see T»f«. 

Cahcfr, the Crab-. The sign of the Zodiac which the Sun enterr about the 2rst. 
of June, and leaves^ about the 22nd. of July. 

Capricorntjs, the Goat. The sign of the Zodiac whioli the Sun enters about tlie 
22iid. orDecember andieaves abdut the 19th. of January. 

Cardinal Signs. The Signs of the Zodiac in which the Sun appears at the 
commencement of Spring, Summer, Autumn and Winter; Aries, Libra, Cancer and 

Catoptrical. Bielating*to catoptrics; the science of^reflected vision. See reflbc- 


Central Forces. The centripetal andcentriftigal forces, which are antagonis- 
tic to each other, and' by means of which the planetary motions are conducted. The 
centripetal force, if acting by itself^ would gravitate the MoOn and the other satell- 
ites to their primary Planets, and the primary Planets to the central Sun; but the 
centrifugal force, of equal power with the centripetal, and exerted in a conttary di- 
rection^ (that of repelling or scattering from the centre,) brings about an equihbriUm 
of motion. < The scattering discharge of mud from a coach wheel in motion is the 
effect of a centrifugal force, and the &11 of a heavy substiance to the ground^ ir cau- 
sed by the centripetal or gravitating force. 

Celestial EauATORi The Equinoctiid cirde in the heavens. (See circles.) 

Celestial Meridians. Great Circles in the heavens due North and South, 

and intersecting each other at those points of the heavens immediately opposite the 

CER. CIR. 1 1 

 '■■■■■ -  , . 

North, and South pales of the Ei^nth, wd termed the celestiAl poles. If -the reader 
will pla€e himself ^th his hack to thp Nprtb he wijl h»ve the West at his. right 
hand, the East at his left hai^d and he will look towardsithe. South* A line imogioed 
to he drawn under his feet towards the North and Squjt^ ^11 be his Meridia)i ob 
the Globe, and an arc in the heavens opposite this lii^e, fronji the zenith (the poinJi 
overhead, ) to the North or South will be an arc of his Celestial Meridiaft. The^uper- 
ior meridian of an observer is that ar<^ of his Meridi^ Circle which is above tho- 
elevated Pol^ (See poles,) the arc belqw the Pole beir^.his.ti^erMii' meridiaa* This 
distinction is nepessary when the transit of the Meridian, hj the celestial bodie3 is 
mentioned, as thpy all mal^e two trans^s of every Meridian Girdle da^y; one transit 
taking place at the superior or upper, arc of each Meridian and the other at the in- 
ferior or lower arc. 

Ceres. One of the four Spheroides. iS'e^ solar sx^TPMf 

Circles^ A^t^onome^s ims^^e ma^y Great Circles iu the heavens^ but three priu^ 
cipal ones, from whic^^ t^ey.fprm the bases of all observations ,of the heavenly, bodies. 
Every circle i? called Qreat the plane of which* passes thcough the -centre ot the. 
Earth. The j^^an^ of ^ circle is an .ii^ag^nary number of ra^u • HUingrUp. the circle: 
tjms the sppkes.of a.wh^^lare the, radii of the circle of the. wheel, and thexadii with 
the axle compose the j^/awe: the parchment of a dr^m is,th^ jo/a/ie of the circlex)n which . 
the parchment is stretjch^d. The, first of the three Great Circles is the Rational Hori- 
zon. That circle made round our field of view at. sea by the watpr apparently touching, 
thei heavens is called the apparent or visible^ horj^QJV a circle .drawn horizontally^, or per- 
fectly level, from th0 S-ElSr.Shl'B^lS; 

eye of an observer is "^ ^^i' 

the «e?m5/&,horizpn» i'^sSS^ — 
and a cirjcle whose '^ 
plane pas^e^ through 

the centra of the earth ' ^ . ^ . 

is the ra^ionc? horic B.A.TIOKAX, '^ T-IORi 7>OK^^ 

zon {See tfie figure, anc( the word de^resion) The sejcond Great Circle is the 
Equinoctial, or Celestial Equatpr, a circle of th^ heavjens, the plane of which 4s in 
continuation withthe plaae of the Equator of the Earth. The Sun is jon the Equi- 
noctial about the 2 1st. of March and '2 1st. September, when equal days imd nights 
are over the Earth. {See seasons.) The Equinoctial is traced by observing certain 
remarkable .Stars, to which the Moon in her course seems ta appxpach, and also. by 
observing the position of the Planets. The third Great Circle is the Ecliptic, or ap- 
parent annual path of the Sun, which also is traced by observing icertain .aremarkaUe 
Stars, the distance of which Jfrom the E^pty;. Jtia]^ i>^^ i^QHe«il%- fiae^iitaised^ Se^-r 
SEASONS and earth. 

Circles of the Sphiire. Th)BL appoB^j^^^e ofih^^^e^s^em^Bom. the Earth risgl^ - 
bular or spherical,, and any. circle in^agii^fsd in the heavens is a Circle of tiie Sphere* 

Circles of Altitude,.^, Am plitupe, Aziuvjn, DEeLiNATjoN, Lativude, 
Longitude. See, Altitupe ^c. 

Circles, Diurnal. Circle^apparently deserihed by the jb^eas^enly bodies in thei^ 
daily passage over the Earth frojji East .to West, 

Circles of Excursion. Circles par^-Uel to, simI at^uqh a distance (about 10 de- 
grees) from the Ecliptic as the boundmri^s ^of the excursions of the Plimets. 

Circles of Perpetual Apparition and. Perpetual Occultation. The in- 
habitants of the equatorial parts of the Earth have the whole of the Celestial Sphem • 




South Pole. 

North Pole. 

turned towards them every day, but those living North or South of the Equator see only 
a part of the sphere. This will be understood by imagining the globe in the first dia- 
gram to be revolving from W to E, when it will be evident that a person situated oa 
the Equator will have every part A 

of the Sphere presented to his 
view in 24 hours, but a person 
situated at the North or South 
Pole of the Earth would always 
have a Celestial Pole overhead, 
and all the Stars of his hemi- 
sphere (half a Sphere) perpet- 
ually describing circles around 
parallel to his horizon. The cir- 
cles D G would be diurnal cir- 
cles (See CIRCLES diurnal) of Stars seen at N; and A O would be the circle of 
perpetual apparition and perpetual occultation to N and S; the hemisphere from A 
O to the Celestial North Pole being in perpetual apparition to N. and in perpetual 
occultation to S and the hemisphere from A O to the Celestial South Pole being 
in perpetual apparition to S and in perpetual occultation to N. In all places distant 
from the Equator only one Celestial Pole is visible, or in perpetual apparition, the 
other being invisible, or in perpetual occultation. The second diagram represents 
the circles of perpetual apparition and occul- 
tation of an observer in latitude 45° North. 
The Globe must be imagined to be revolving 
from W to E., as in the first diagram, but, 
the observer being now at I instead of at the 
Equator the circle A B will be in perpetual 
apparition to him, and the circle C D in per- 
petual occultation; the extreme North point of 
his horizon {b of the dotted line) being always 
directly under some part of the circle A B, and 
the extreme South point {c of the dotted line) 
being always directly over some part of the 
circle C D. 

Civil Day. The day commencing and ending at Midnight. See time. 

CoLt7RE8. Two Great Circles of the hea- 
vens supposed to intersect each other at right 
angles at the Celestial Poles, and to pass 
through the Solstitial and Equinoctial points 
of the Echptic. The Solstitial points of the 
Ecliptic, are those points which are farthest 
from the Equinoctial, or Celestial Equator, 
and the Equiuioctial points are those points of 
the Ecliptic which intersect the Equinoctial. 
In the diagram, A A is the Equinoctial, B B 
the Ecliptic, P S P S the Solstitial Colure, ^ 
P N P N the Equinoctial Colure, P P the Ce- 
lestial Poles, S S the Solstitial points and N N 
the Equinoctial points. 



__ ) 

Comets. Wandering bodies, the nature and utility of which in the general scheme 
of the Universe are entirely unknown. In default of a better surmise however, we 
may consider them to be electrical bodies binding our Sun or Solar System to the 
other nearest Suns (or Stars ) by which means our System may not, even in an in- 
finite series of ages, float unchecked over the wide expanse of creation, and approach 
some other system so as to endanger the stabiHty and equiUbrium of our centripetal 
and centrifugal forces. (See central forces and solar system) t 

Complement. In Geometry, such an addition to an arc as will suffice to com- 
plete 90 degrees, or one quarter of a circle. In Astronomy it is the number of de- 
grees required to complete the 90° of an arc between the horizon and zenith, or be- 
tween a Celestial Pole and the Equator, &c. Thus, if a Star have an altitude of 
40° the complement will be 50°. 

Configurations. The relative positions of heavenly bodies with each other as 
seen from the Earth; principally appHed to the configurations of the satellites of Ju- 

Conjunction. The meeting of two heavenly bodies, which need not f^pear abso- 
lutely to touch each other for this term to be used: it is sufficient if they are in the 
same degree of the 360 of a great circle of the heavens. When the Sun is between 

^J2? lEarlA, 9,.- 

O • Mereunf 

a Planet and the Earth, or a Planet is between the Sun and the ^arth, then that 
Planet is said to be in conjunction with the Sun. When the Earth is between a Pla 
net and the Sun, the Planet is said to be in opposition with the Sun. In the diagram 
both Venus and Mercury are in conjunction, whilst Mars is in opposition. Conjunct- 
ion and opposition are sometimes termed the syzygy of a Planet. The apparent con- 
junction of two Planets is called a Grand Conjunction. 

' Consequentia. See Antecedence. 

Constellation. A series of stars near each other and supposed to form parts of 
some figure as a bear, a lion ^ The number of constellations is 91. See fixed 


CojJSTANT of Aberration of the Sun. The amount of aberration independent of 
the very small change produced by the variation in the dbtance of the Earth from 
the Sun. See Aberration. 

Copernican or Pythagorean system of astronomy. The system first propoun- 
ded by Pythagoras, and afterwards fUlly established by Copernicus, explanatory of 
the motions of the Earth and other Planets moving round the central Sun. 

Culmination. Stars appear, like the Sun, to describe portions of circles in the 
heavens; that is, they appear to rise daily in the East, and pass gradually towards 
the West after having risen above the horizon a certain distance according to their 
position in the Sphere. The greatest altitude a Star reaches is at the celestial meri- 
dian of the observer, and its transit of that meridian is called its culmination. But 
Stars within the circle of perpetual apparition of any place (See circle of perpet- 
ual apparition, ) do not set below the horizon, but appear to describe entire 






circles around the elev^ed pole; ( the celestifd pple 
mtihin tjus drclf; and consequently pexpetuaUj ^*®" 
Tated ahoye the horizon). Ii;i tl^e case of s\^ch Staxs 
when their transit of th,e meridian takes ph^ie above 
the pojje it is Cftljed tlj^e ugper culpoinatip^, aiid th^ 
passage or. transit heipw tl^ pole is caft^d the lower 
cijibuinatiop. If ij N, in the ac^D^p^nyuig e^^a^, 
be the northern Horizon of a place in north latitude, 
^ will be tfc celestid north I^ole, C t^A thp orcle 
of peipe^^f app^ Bf C i) D an arc of the^nj^e^ 
ric^ and' 1!^. P w^^ the arrows a cirde of th^* cefcs- 
tial sphere parallel to the Equator and circle of perpetual appaiition. Now the appa- 
rent d^ily motion of the sphere being in the direction pointed by the arrows the 
Mo6ti 'aud Stftf at 1\J; and'C are miking their upper culmination, and the Stars be- 
n&lh' the T61e E ai'e afeout to make their iower culmination; in the latter case one^ 
of the Stars being above and the other fteZou; the horizon. The -^Q Rf 2 q 7^ 
term^ u^pct aM tew^t teulniinAtion are flsb siised to Henote the 
irrivjfl of a Star at Ae MeiieEkii bimeatk the horizon of any 
place. Let the second diagram r^resent Ihe horizon of a place 
with its circle of perpetual occultation beneath it. The Star 
just below the horizo^ will then be making its upper culminfition^ and at the most 
depressed part of the circle another Star is making its lower culmination. The 
terms Culminating, Transit of the Meridian and Meridional Passage are synony- 
mous; and the word Southing is generally used in north latitudes for the culmination 
of the Moon. Moon culminating Stars are those Stars which on the day of obser- 
vation cilhmnate about the same time as the Moon; as the Star at C in the diagram. 
Cusps. The points of the illuminated horns of the Moon or Yenus. 
Cycles. See time. 
Day. See time. 

Declination. The distance of a heavenly body North or South from the Equi- 
noctial Circle. Degrees of declination are reckoned on th$ Celestial Mmdian* Cir- 
cles or parallels of declination are parallel to the Equinoctial. 

' Degree. The 360th. part of ^ cirde of any dimension. A degree is subdmded 
into 60 minutes/ and each minute into 60 seconds. A second is sometimes diyided 
into tepths, hundredths and thousandths of a second: 4° 16' 5 9"* 9 are read ^ 4 de- 
crees 16 minutes 59 seconds 9 tenths; -69 as 9 hundredths of a second, 'SOjS.j^ls 806. 
thousandths of a second. A degree of longitude varies in dimension at eveiy distance 
from the Equator, where it is 69-5- miles, to the Poles, where all the circles of longi- 
tude meet, and wherie, consequently, there is no longitude. A degree of latitude is a 
trifl^iess than a degree of lon^tude on the Equator; the diameter of the Earth at the 
Equator being gfeater than a diameter measured between the Poles. This fact is as- 
certained by the foUOi^in^ xo^thod of measuring the arc of a meridian. A Star is 
observed at one extremi^ of a kmg plaiie to have a certain altitude when on the 
meiidian of that place. The observer then travels Noith or South, so as to continue 
under the same itieridii^ until the altitude lof the Star becomes one degree more or 
less than at first. The exact distance the observer has travdled is a degree of terrestrial 
latitude, but it is evident that the measurement of some known part of a degree would 
answer the purpose equally as well as the measurement of an entire degree. Now, 
this actual measurement of degrees and parts of degrees has been accomplished in va- 


DEP. DlS. DIA. 15 

—  — .—  ----. .•■■ ■-- 

nous ktitades, and the rescdt is that tUe lengthLcf a d^ee^ oik the Eail^ Ikicreases 
"with the latitude^ being the greatest near the Poles and the le$^t. at jtbe Equator; 
from which fact it follows that the Earth's curvature is greater at the Equator than 
at the Poles, oV, in other words, the Earth is 
flatter at the Poles than at the Equator* 
Let F A represent a flattened arc of meridi- . 
an oh tlie GTobe, as at the Poles, (but pur- •^ 
{k>sely exaggerated for this explanatidn,} and \ 
P c s A an ate of meridian of greater curve, 
as at the Equator. The zenith of a place 
being precisely in a direction upwards in 
continuation of a plumb line hanging to- 
wards the centre of gfavi^, and the centre 
of gravity being varibd in t^e instances FA 
and c s according (but not corresponding) to the centres of the two curvatinre^ Z 
will then; represent thezenith of F on the flattened and of c oi| file curved . suiface, 
and Xwill represent the zenith of s on tibie curved^and of Aon tji^ flatt^^aed surfae^. 
The altitude of the Star * is the complement of its zenith distance, {See cojn ple- 
MENT aind ZENITH,] and, consequently, the Star wpuld have the sfucne altitude. at, F 
as at c, and itt s as at A, and the measurement of the curved and flattened, surfaces 
on the Globe coincident to the arc Z "^ X of the Celestial Sphere will be. dissimili^r, 
being the difference' between !]^ A and c s> the great cury^ure c s being of less extent 
in length than the smaller curvature or flattened surface FA.. 

Depression, or dip of thf horizon. An angle psntalned l^etween the ajyjtf^i^t 
and sensible horizons, aiid the eye of an observer. (jS^ee circles). In the diagram 
the line and riig\uhd,^r 
c represents a phmulaet 
showing^ the tf 1X6 per- 
pendicular; CA ik aline 
drawn horizontpUy to it 
^m the eyeofan obser ^ 
ver at c, and is the sensible horizon, whilstc B,a lin^ ^eddng appoint wluere the .sky 
and water appear to meet, is the visible hori^n^ ^d'A c b id the an^e of d^i£99tQ9i 
or dip. Again: the ship being the place of observation, and d the sensible horizon 
or a level line from the eye of an observer on, deck, whilst b is a line to the visible 
horizon, the angle between the observer's 0ye.and d » is. the depression. It- will be 
seen that the greater t^e 4titude of the place of observation the ferther the visible 
horizon is removed from the observer. 

Depressed Pole. The opposite Celestial Pole to that which is elevated. (See 

Descension. The apparent passage of a cdlestial body from its greatest altitude 
towards the western hbriion either in a Right or Oblique Sphere. (See Right As- 

Diameter. The appd.fent diaiiieter of a celestial' body is the an£ile xa^det which 
it appears when viewed from the Earth. (5^^^ angle.) A' great circle of the heavens 
(See circles) being divided into 360 degrees, aud each dejgfee into 60 minutes, fis 
many minutes or parts of a minute of this circle as are covered by the celestial body 
will be the apparent diameter of the disc. 

16 PIS, 

DiOPTKiC, Beating to tl 

Dip. See otnanov. 

Disc. He Tuible part o 

X of redacted raioB. See BcnucnoK. 

T &m of the Son, the Mood or a Planet, as seen &om 

Distance. J9e« mehsubatiom. 

DiUBNAL. B«Utiiig to a day. The dtnraal motion of a Planet is its real daily mo- 
tion from Wetl to Eatt in its orbit roond the Sun. llu dinmal tranat oi a nanet 
ia ttt qiparent daily paasage from E<ut to Wett, caused by the rotalioa of the Earth, 
during which the Flanrt deseribes ac arc erf' the sphere wbicb i* called the Planet's 

Dominical letter. See time. 

Dkagon'b bead and db.agon'b tail. Tiro Astronomical characters; Q Dragon's 
Head, signifj'ing the ascending node, and fs Dragon's Tail, the deaeending node. 
See MODE. 

Dynamic^ Part of the aaemx of Mechanics; naed in Astrooomy >s it conUins 
the theory and mechanical laws of bodies in motion. 

Eakth. {See also bolab btsteh). The Earth is divided by ge<^Taphers into 
lire zonei; one torrid, tvo frigid and two temperate. 
The torrid it that division to part of whicli the Sim ia 
perpendicular at all times. It extends 23° 28' (nearly) 
on eadi side of the Equator. The northern limit of this 
tone is called the Tropic of Cancer becanse the Sun, 
when perpendicular to it, is in the sign Cancer, and the 
southern limit is cslled the Tropic of Capricorn for a ri- 
milAr reason. The frigid zones, or Arctic and Antarctic 
circles, are 23° 28' from each Pole, the Arctic being at 
the North and the Antarctic at the South. The tempe- 
rate zones he between the frig^ and the torrid xones. 
The imagioaiy divisions of the Earth which have a n 
tronomy are i ~ 



e particniar relation to As- 
, the Equator, a great circle equally distant from the Poles, and di- 
riding the Earth into the northern and aonthem hemispheres. A celestial continu- 
ation of the plane of the Earth's Equator is the Celestial Equator, or Equinoctial, 
which divides the heavens into the northern and southern 
hemispheres, ii. Meridian tines, or hour circles, passing 
through the Equator, from Pole to Pole. (See Fig.2) A 
Meridian on the Earth is a semi-circle, alt the ' places on 
which have the same longitude, which is reckoned on the 
Equator from some particular meridian, as Greenwich or 
I Paris. In this diagram the meridian lines or semi-circles 
I are drawn through every 15° of longitude, which number 
8 equal to one hour of Time, or one twenty fourth part 
of the circumference of the Earth. Reckoning from the 
East, every place on either of these semi-circlea will have 
noon one hour earlier than the places on the next semi-cir- 
cle to the 'WeBt. The perspective of the meridian hnes m this diagram would be in- 
correct if the Earth were to he conceived at rest; but the student must imagine the 
Earth revolring, a-.d each meridian semi-circle to be passing separately under his 
view. Tlie word meridian has been derived from mid-da'j. The Sun is SMd to be in 

""-Hi ■^.o' 




the meridian when he touches the highest point of the arc he appears to describe 
daily in the heavens, that arc being pecuhar, or existing only in respect, to the 
place where it is observed, iii. The Ecliptic, a more imaginary circle over the 
Earth than the Equator, or the meridians, and, therefore, more difficult to be con- 
ceived. Let the flame of ' the candle A represent the Sun, and let B C be a string 

strained oh supports, behind which string place a ball or globe, inclined as in the dL 
agram, and let the upper part of the ball represent the North. N will then represent 
the North Pole of the Earth and S the South, and the wires at N S the axis of the 
Earth. Then turn the ball or globe on its axis and you will perceive that the string 
will every instant divide the globe in a different manner to the previous instant, but 
will always maintain the same relative position to the whole globe. Such is the 
Ecliptic when imagined as the hue of the Sun*s annual path over the whole Earthy 
projected, or depicted on the globe. As the globe revolves the circle E F will be 
turned to the flame of the candle, and the Northern Hemisphere will have more of 
the hght and heat than the opposite; but remove the candle to B and the reverse will 
be the case, and if the candle is placed at H it will be parallel with the Equator O Q 
in every part of a revolution of the globe. This explanation will assist in familiar- 
ising the phenomenon of the Seasons. (See Seasons). The line from F to A will 
. represent the radius vector of the Ea^h when the Sun is at C, and if the Moon he 
imagined at B, the line from B to I will represent the radius vector of the Moon. 


East. The exact point where the Sun rises at the times of the Equinoxes; that 
is, at the times when the Sun, in his apparent diurnal course, passes over the Equa- 
tor of the Earth, the Equator being at an equal distance from the North and South 

Eccentric. Out of the centre. An eccentric circle is a circle the centre of which 
is not concentric with, or on the centre of, another circle. The eccentricity of a Pla- 
net's orbit arises from the orbit being elliptical and the Sun not being in the centre. 

Eclipse. The passage of the Moon over the Sun or any of the Planets; of the 
Planets over the satellites; and of the shadow of the Earth over the Moon. Figure 1 



represents an eclipse of the Sun; the Moon being observed from A, on the Earth, to 

18 EL^ EM^ ER 

pass between the Earth and the Sun. Figure 2 represents an eclipse of the Mooui 

Ficr 2 


V^cLvO.xi^ ) o Moon 

the Earth passing between the Sun and Moon, and throwing its shadow on the 
Moon. An a«;i?//flrr eclipse of the Sun is when the centre of the Moon appears on 
the centre of the Sun, and a ring of the Sun's disc appears entirely round the 
Moon's disc. An annular eclipse occurs when the Moon is at her greatest distance from 
the Earth, her apparent diameter then being not so great as when nearer. A central 
eclipse occurs to an observer when the centres of the eclipsing and eclipsed bodies aj>- 
•j • 3 pear exactly to coincide. Tlie echpse in Fig. 1. is annular, and Fig. 3. 
^ ^ represents an eclipse of the Sun both annular and central. Calculations 

of the ecHpses appear in the Nautical Almanac, and the echpses of Ju- 
piter's Satellites by Jupiter are of much service in determining the 
longitude of places on the Earth. 

Ecliptic. (See circl-es, zodiac and earth). The Echptic has its name 
from the circumstance that all the eclipses of the Sun and Moon are performed either 
actually in, or very near that circle. 

Elevation of the Pole. The distance of a Celestial Pole from the zenith of the 
place of observation, by which the exact distance of the place from the Pole of the 
Earth and from the Equator can be ascertained. For, if the North Pole of the hea- 
vens is obsened to be 40 degrees from the zenith of any place that place will be in 
SO*" of North latitude; 50° added to 40° completing the 90° from the Pole to the Equa- 
tor. When the North Pole is below the horizon of any place that place is in South 
latitude. The elevation of the Pole is said to be the complement of the elevation of 
the Equator. Thus if the Pole be ascertained- to be 35° from the zenith, the Equator 
will be 55° from it, 55° being the complement of 35°; that is, the two sums added 
complete the 90° from the Pole to the Equator. 

Elliptical. Relating to an ellipsis or oval. See kepler's latvs. 

Elongation. The difference in motion between ^^-^ J^lamet 

the swiftest and slowest of two Planets, as seeif from . 
the Earth, or the space one has passed over be- 
yond the other. The word elongation is also used to 
denote the apparent distance of a Planet from the 
Sun. The angle of elongation is contained between 
lines drawn from the centres of the Sun and Planet to 
the centre of the Earth, as in the diagram. 

Emersion. When a Planet or a satellite has been "Xi&rlTfu 

eclipsed by a heavenly body, and appears to^ come 

out from behind that body it is said to emerge, and the fact itself is an 
emersion. Immersion is the commencement of an Eclij)se, when the body is immers- 
ed, or sunk within the influence of the eclipsing body. 

Epact. See time. 

EO EV^ FA^ FL 19 

Ephemeris, Astronomical. A diurnal account of the situations ^c. of the heav- 
enly bodies. 

Equation of Time. See time. 

Equation of the Equinoxes. As the equinoctial point (the first point of Aries,) 
is continually shifting its place on the EcHptic (See precession,) the places of the 
heavenly bodies referred to the Equinox, that is, their Longitude, or their Rigkt AsC' 
ension {See these terms,) is also continually shifting. The diiference between the true 
and mean place of the Equinox is a quantity termed the Equation of the Equinoxes. 
Equation of the Centre. An allowance for the difference between the true 
place of a Planet and its mean (average) place in its elhptical orbit. 
Equator. See earth. 

Equinoxes. The times when there are equal days and nights over the whole 
Earth. The Equinoxes are two in number, the Vernal and the Autumnal; named so 
to correspond with the Spring and Autumn Seasons of the Northern Hemisphere, 
But the Vernal (Spring) Equinox to us in the North is the Autumnal Equinox to the 

South. In the North, the Sun appears daily 
to describe in the heavens an arc, such as 1, 
in June, a smaller arc, 2, (the Equinoctial} 
during the Vernal and Aatumnal Equinoxes, 
and the smallest arc, 3, in December. While 
these appearances are presented to the North 
the contrary are presented to the South, and 

the phenomena at the Equator are very dissimilar For, when the Sun describes 
to the North the arc of the Equinoctial, as depicted in the figure, the Sun at 
the Equator is vertical, passing directly overhead; when the arc 1 is described 
to the North the ascension as seen at the Equator is only 23 j degrees North from 
the Equinoctial, and when the arc 3 is described to the North the ascension at the 
Equator is only 23^ degrees South from the equinoctial. 

Equinoctial. See circles and earth. 

Equinoctial Colure. See colure. 

Equinoctial Points. The first points of Aries and Libra. See Colures. 

Equinoctial Time. See time. 

EvECTioN. When the Sun is in Perigee, (nearest the Earth) in January, the Sun 
has a greater, and the Earth a less, attractive power over the Moon than in July, when 
the Sun is in apogee (farthest from the Earth). As the Earth's attractive power dimi- 
nishes, and the Sun's power increases, the Moon recedes from the Earth and her orbit 
is enlarged, the effect of which is seen in her periodic time of performing a lunation, 
which in January is 35 minutes longer than in July. The greater the dilitation 
(enlargement) of the orbit the longer is the period in which a revolution is perform- 
ed in it. 

Facul^e. Spots on the Sun, which are brighter than other parts of the disc. 
MaculcB are spots less bright, or even dark. 

Fixed Stars, (the Suns of other Systems) are at such an enormous distance from 
the Solar System that scarcely any perceptible change is made in their relative posi 
tions as seen from the Earth. There is no doubt however that they move, but as our 
Sun,, and all the Planets, occupy but an inconsiderable speck in creation, auJ the near- 


est of what we call the Fixed Stars is at least 200,000 times farther from us than the 
Sun is, the change of position of a few only of the Stars is perceptihle even by the 
most careful and accurate observations. Although their number, when view- 
ed through powerful telescopes, appears infinite, yet the naked eye can ne- 
ver see more than 500 at one time. The Stars of the first magnitude are 
only 20 in number, those of the second, 7^, and those to the sixth magni- 
tude inclusive, only 3128. For the purpose of arrangement, most of the Stars 
are supposed to be situated within some figure, called a constellation, the remainder, 
not included within any figure, being termed informed Stars, Twelve of the constell- 
ations are in the Zodiac, 34 at the North, and 45 at the South of the Zodiac, The 
Stars, called fixed, have first, an apparent motion over the Earth in 24 hours, an ap- 
pearance caused by the rotation of the Earth on its axis;, secondly, a very small ap- 
parent motion in Right Aseenaion and Declination, caused by the Precession of the 
Equinoxes, Aberration and Nutation, (See the explanations to these terms,) and, 
thirdly, some of the Stars are seen to have a real, or proper, although very slow mo- 
tion, by which they not only change their relative positions sUghtly, but become of 
greater or less magnitude at one period than at another. We infer indeed that every 
Star (including the Sun) has some progressive motion, but the inconceivable distances 
at which they are placed preclude our appreciating the motion except in a few in- 
sauces, and, as we accompany the Sun, his very gradual change of place, distributed 
as it is over thousands of years, becomes perceptible only in respect to a period like 
that occupied by the precession of the Equinoxes. If the small circles jS^ S, in the fi- 



gure be taken to represent the circuits performed by any two Stars in an indefinite 
number of thousands of years, and the circle E a circuit performed by tlie Sun and 
Solar System in 25,000 years, it can be readily imagined that the angles under 
which we shall view the Stars in different parts of their circuits, *S S, will be percep- 
tible only of a very minute change in any short period. 





To find the constellations Ursa Majoris, (the Great Bear J and Ursa Minoris, 
(the Little Bear,) is the first lesson in the study of the Fixed Stars to those living 
in the Northern hemisphere. The following diagram contains the principal Stars 


^ *- 

"^ ^ $ 

or- ^ *• ^ ^^ 

JPi;U Star . -^^ 

in these constellations, the most important of whieh is a Polaris, or Alruccabah, 
the North Pole Star or Cynosure, in the constellation of the Little Bear. The 
student who for the first time essays to find these stars must bear in mind the 
daily revolution of the Earth, and must not, therefore, expect to find them always 
in the situation they appear to the reader of this page; for although their relative 
distances from each other are always the same, yet each hour produces an evident 
change in the positions of the constellations when compared with the horizon or 
zenith of an observer. The Great ^ear, for instance, which at one time may be 
seen emer the Pole Star, as in the above delineation, will, six hours after, be to the 
left or west of it, six hours more will be under it, and in another six hours will be 
at the right or due east of the Pole. These constellations, and others which surround 
the North Pole of the heavens, never set below the horizon to observers in the nor- 
thern p^ts of Europe, America and Asia, and never rise to the inhabitants of many 
of the southern parts of the world. The constellations surrounding the South Pole 
never set to the inhabitants of South America, Africa and Australia, and are never 
seen from Europe, Asia and North America. (See circles of perpetual appari- 
tion.) The Great Bear is sometimes vulgarly called the Waggon and Horses; the 
tail of the Bear becoming the horses, and the Star Duhhe the hind wheel of the wag- 
gon. Bearing this in mind it is easy to remember that Dubhe and the other Star 
forming the back of the waggon become the Pointers to the Pole Star. The follow- 
ing map may be taken for lesson the second. It contains several principal Stars, an 
acquaintance with which will form a good foundation for pursuing the subject with 
the aid of regular celestial maps. 



* »(.^^ ,y * * 


* * ^ J 






*Alcle-rci//nv^C^ ■* 


. jy^yic!? or ^^ 

•* '^ ^ 


^ * 

* > 

^ Pi 











^7 .'- . 

j9^;^. ^1^ ^ 






a UroL^ca 



* * 



The Pleiades, or Seven Stars, are in the constellation Taurus; Caput Medusae, 
Algol and Algenib in Perseus; Capella in Auriga; Castor and Pollux in Gemini; Al- 
maach in Andromeda; Schedir in Cassiopeia; the Pole Star in the Little Bear; 
Dubhe, A'lioth, Mizar and Benctnasch in the Great Bear; Seginus in Bootes; a Draco 
and Rastiban in Draco; Deneb or Arided in Cygnus; and Alderamin in Cepheus. 





The Nautical Almanac contains the Apparent Place8(the Right Ascension aad De- 
clination,) of 100 Fixed Stars, an Ephemeris of the Moon Culminating Stars, ( See 
EPHEMERis and CULMINATION,) and a Tahle of the Phenomena of the year, parti- 
cularly the conjunctions of the Planets and Fixed Stars. By a frequent reference 
to these parts of the Almanac, and hy comparing the Phenomena therein desclibed 
to their actual occurrence in the heavens a gradual progress in the study of the Fix- 
ed Stars may be made. 

FoRMULii.. A form, rule, or method, of working a problem or ealcnktiim. 

Galaxy or Milky Way. There is a white (milky) broad belt df Mght over the 
heavens which is ascertained to emanate from an innum^raMe host of Fixed Stars, 
only visible through the most powerful telescopes. A very slight observation of the 
heavens on a clear night will serve to recognise this belt, in a very small part of 
which 258,000 Stars w^ere once observed. Its breadth varies from 4° to 20°. 

Gemini, (the Twins.) The sign of the Zodiac which the Sun enters about the 
1st. of May and leaves about the 20th. of June. 

Georgium Sidus, Urantjs, Herschell. Three names of the Hanet discov- 
ered by Dr. Herschell. See solar system. 

Geocentric Place. The position of a Planet as viewed frem the Earth. Hclio- 
xi-rsi poUt^ centric longitude and latitude of a Planet is its 

position supposing it to be viewed from the Sun. 
In the diagram the geoeentric piece of the Planet 
(omitting its decliBation,) is, R^ht Ascension 
14** 30', and its heUocentric lon^tade 165^. (See 
declination, right ascension and longi- 
'^ >fj TUDE CELjnsTiAL). For, as the circle with the 


First Point of Aries represents the circle of 
Right Ascension, divided into 24 hours, or 360 
degrees, the geocentric place of the Planet, or 
that point of the circle in which the Planet app- 
cars when viewed from the Earth is 14^*30°* (14 
hours, 30 minutes of Right Ascension,) from 
the First Point, and, at the same time, that point of the circle in which the Planet 
would appear if viewed from the Sun is 165° (degrees) distant from the ^irst Point. 
The Roman numerals, VI. XII. XVIII. denote three of the hours of Right Ascen- 
sion, and the figures 90. 180. 270. three points of the celestial longitude.' 

Gibbous. A term appUed to one of the phases of the Moon. See moon. 

Gravitation, See central forces. 

Heliacal. Stars, when they approach too near the place of the Sun, are lost 
to sight by the superior effulgence proceeding from the solar luminary, and are said 
to rise and set heliacally. When a Star emei^es from the influence of the Sun's rays 
it makes an heliacal apparition or appearance; and when immersed in the solar rays 
it makes an heliacal occultation or obscure position. The Moon rises and sets helia- 
cally when 1 7° distant from the Sun. 

Heliocentric. See geocentric. 

Hemisphere. The half of a sphere, orb or globe. The great circuit of the hea- 
vens visible at any time is the Celestial Hemisphere. The visible discs of the Sun 

24 HO. IM. - JU, KE. 

and Moon are the Solar and Lunar Hemispheres turned towards us. Any half of 
the World is an hemisphere: thus we say the northern and southern^ or the eastern 
and western hemispheres. 

Hour Angles^ and Horary Circles. See time. 

Horizon. See circles. 

Horizontal Parallax. See parallax. 

Immersion. See emersion. 

Inclination^ Angle of. See noi>e8 and obliquity. 

Inclination of Moon's Orhit. See Moon; 

Inequality. Unequal motion: a deviation in the motion of a Planet or Satellite 
from its mean motion. 

Informed or Unformed Stars. See fixed stars. 

Ingress. The entrance of the Sun into any of the signs of the Zodiac. 

Intercalary Day. See bissextile. 

Juno. One of the Asteroids. See solar system. 

Jupiter. See solar system. 


Kepler^s Laws. Three laws respecting the motions and positions of the celes- 
tial hodies of the Solar System^ first announced by Kepler and since demonstrated 
by the calculations of Newton: they are considered the foundation of Astronomy. 
To explain the first law recourse must be had to that part of Geometry called Conic 
Sections* a knowledge of which is essential in many parts of Astronomy. 

Conic Sections are curved lines formed by the intersection of a plane and a cone. 

A plane, or plane surfiice is one perfectly fiat and even. 

A cone is a solid body of the shape of Fig. 1, circular at the base A and angular 

or pointed at the^ vertex B. A straight or right line drawn from the vertex to 
the centre of the base, as D C, Fig. 2, is the axis of the cone All right lines 
as D E, D F, Kg. 2, drawn from the vertex to the circumference of the base, are 
sides of the cone. If a cone be cut by a plane parallel to its base, as P P, Fig 3, 
the section will be a circle, because the base is a circle. If it be cut so that the 
section be parallel to a side, as 1 1, Fig. 4, is to L L, the section will be a parabo- 
la. If it be cut perpendicularly to the base, and so that the plane cutting it, as H H, 
Fig. 4 if extended upwards would meet an extension of a side, as L N, the secti- 
on is an hyperbola. If it be cut from side to side obliquely (not parallel,) to the 
base, as I O, Fig. 4, the section is kd. ellipsis. Figure 5 is a parabola^ Fig. 6 an 
hyperbola and Fig, 7 an ellipsis. 

KEPLER'S LAWlg.' 25 

- — 

The orbits of all the Planets^ and some of the Comets^ are elliptie, whfle other 
Comets are supp osed to describe parabolic and hyperbolic eurves round the Sun 
nerer to return. 

A curvilinear figure is composed of curved lines, as the ellipsis^ The Periphery 
is the circumference of an ellipsis, or any other regular curvilinear figure. The 
axis of an elHpsis is a right line dividing it into equal parts, as A B, the longest 

axis, and D E, the shortest axis of the ellipsis. Fig. 8. 
The longest is called the transverse or major axis ; and 
the point C, where the longest and shortest axes inter- 
sect each other, is the centre of the ellipsis. The foci 
of an elUpsisare two points in the longest axis. To 
find the foci of an ellipsis draw the longest and short- 
est axes, take half the longest in your compasses and 
and set one foot in the shortest axis, at an end joining the periphery, as e. Fig. 8: 
the other leg will then intersect the longest axis in either focus, 6 or h. This 
latter explanation will serve to elucidate Kepler's first Law : - 



The Second Law is as follows : - 



In explanation, first see solar system and radius vector. Then, if A B C D 

Fig. 9, be the orbit of a Planet, and S the Sun in one- of 
the foci, the motion of the Planet, in its orbit at A, near 
the Sun, is greater than at D, remote from the Sun, and 
the Radius Vector will sweep over the surface, or curve, 
from D to B, or from C to D, in the same time as it 
will describe the surface, or curve, C A, or A B. 

The Third Law requires an explanation of the terms 
^ squares and cubes, besides that of Major Axis of an 

Ellipsis. (The latter has been already given in the explanation to Fig, S.) 

Squares, or square numbers (in Arithmetic,) are the product of numbers mul- 
tiplied by themselves : the square of 2 is 4 and of 6- 36. 

Cubes, or cube numbers, (in Arithmetic), are formed by multiplying any num- 
bers twice by themselves : the cube of 6 is 216 ; thus algebrically produced : 6x6 
= 36. 36x6 = 216. (6 multiplied by 6 are equal to 36, and 36 multiplied by 6 
are equal to 216.) The Third Law, then, is thus announced: 



- - • » ... 

The consequences deduced from these three laws are demonstrated to be, that 
the force {See central forces) acting on the Planets is directed towards the 
centre of the Sun, and regularly decreases in amount as the distance from the Sun 
is increased, (or, more properly expressed, is in the inverse ratio of the square of 
the distance of the centres of the Planets from that of the Sun ;) and, lastly, that 
the force is proportionate to the mass. From all these consequences it results 
that the Sun is the centre of an attractive power, that all the Planets revolving 
round the Sun are, like him, endowed with the power of attraction ; and that in 






the SoUr Sjrsttm all thd particles ^i matter mutually attract each other with a 
forde proportkmate to their masses. 

LAflTyoi!, CetiitiaL The distance of a celestial body fh)m the Ecliptic 

North or South. The Sun's latitude is a very 
slight variation of his apparent place, as seen 
from the Earth, caused by the Earth being at- 
tracted towards the Moon. If the Earth, at- 
tracted by the Moon, be at A, on one day of 
the month,the Sun will be seen in the heavens 
at D, and, on another day of the month, the 
Earth being attracted by the Moon to B, the 
Sun will be seen at C. This di£Perence, how- 
ever, is not so great as the diagram makes it 
appear to be, and but rarely amounts to l'^, 
which is less than the millionth part of a great 
circle. The Sun's latitude is technically eeilled 
the angular distance of the Sun's centre from the plane of the Ecliptic, North or 
South. The latitude und dscUnatum of a celestial body are likely to be confounded 
by the student unless it be impressed on his mind that Latitude is the distance from 
the EoUpttei and Deolination the distance from the Celestial Equator or Equinoctial. 
Circles or paraUels of latitude are circles parallel to the Ecliptic. 

LfiAP YfiAR. See BtSSEItTtLE. 

Leo (the lion). The Sign of the Zodiac which the' Sun enters about the 23rd. of 
July and leaves about the 22nd. of August. 

LtSAA, (the Balance or Scales). The sign of the Zodiac which the Sun enters 
about the 23rd. of September and leaves about the 22nd. of October, 

LtBUATtoN. See NtJTAfioN and moon. 

LtMii. A word applied to one part of a heavenly body when it is necessary to 
distinguish it from another part. Thus, we say the upper or lower Limb ; the east- 
em or western Limb of the Sun or Moon, in allusion to the upper or lower, the 
eastern or western part of the Sun or Moon as seen from the Earth. 

LiMtTiND Parallels. A term used to denote those parallels of celestial latit- 
ude beyond which an occultation of certain Stars by the Moon cannot possibly 
occur. See occultation. 

LoOAtiiTBM of the Radius Vector of the Earth. An artificial number 
representing the length of the Radius Vector, or the distance of the Earth from the 
Bun. Logarithms are artificial numbers used for £EMnlity of calculation where tl^e nie- 
thod with the common arithmetical characters would be tedious and full of com* 

LoKGiTUii«> Ceteetiat. The distance of a celestial body from the Equinox or 
first point of the sign Aries^ measured on the Ecliptic. The celestial Longitude 
and the Right Ascension are likely to be confounded by the ttudent, who must im- 
press ou his mind that the longitude is measured on the EeUptk in degrees, minutes 
and seconds of space ; while the Right Ascension is measured on the Equator in 
hours> minutes and seconds of time, and in degrees, minutes and seconds of 
space. Circles of Longitude are synonimous with meridian circles. 

Longitude Stars. Those Fixed Stars which are generally selected for ascertain- 
ing the longitude of places on the Earth by comparing the observed distance of the 





Moon from one of them with the Greenwich time at which a Lunar Distance ia pre* 
dieted in the Nautical Almanac to occur* 

Lunation and Lunar Distance. See. ^ooif . 

Mars. See system. 

• Mean Time, Mean Solar Day, Mean Noon. See timk. 

Mean places of Fixed Stars. When the apparent Biffht Ancmmon and JD#- 
clination of a Fixed Star are corrected for Precession^ Aherratimi and Nuiationt(S€€ 
the erptanations of these terms,) the product is the mean ^i/ac(?. 

Mensuration. The act or art of measuring lines, Buperftci©8, (surfao^if) and 
solids. Under the word angle will be found the astronomical method of mensara- 
ting by the arc of a circle, and under the word pegrxs the method of measuring 
the arc of a meridian. In this place will be explidned the iystlpms adopted for esti- 
mating the progressive motion of light, and the distances of the Sun imd Planets 
from the Earth. The student is first requested tp read the articles ASBRRATioir, 


The method of aseertafadng the distaooe and magaitude of 

the Sun or a planetary body is by obserrations of the paralU 
ax, and may be thus Atmiliarly explained. Let A B repres^t 
an arc of any meridian on the Earth, 6 » an arc of the celestial 
sphere and P a Planet. To an observer at A the Planet ap- 
pears at a, and to an observer at B the Planet ai^pemrs at b i 
half the arc a & is thereft^re the parallax rf the Hwiet. Now, 
the angle A P B is equi-angular, or similari to the angle a V b, 
and as the base A B of the angle A P B can be measured so 
the altitude, P C , of the angle can be ascertunedi and this al- 
titude is the distance of the Planet from the centre of the 
Earth. The distance beii^ thus found, the magnitude of the 
celestial body is calculated by observing ttie angle subtended, 
or drawn under the disc of the Planet to the eye, M d C d, C 
in this instance representing a place on the circumference of 
the Earth, P the Planet §een at the horigon of that place, and 
d d the base of the Angle subtended. In the case of the 8urii 
for example, the distance being 95 millions of miles, and the 
angle subtended from his disc being, on an average of the entire 
year, 23' 3" (a little more than half a degree, ) the base of the 
angle is the diameter of the Sun, 882,000 miles. An aa|le to 
represent this might be drawn in a field 800 feet long, in which, 
every inch being reckoned as 10,000 miles, the dtitttde of the 
angle would be 791 ft. 8 in., and the base of the angle^ repres^ting 
the diameter of the Sun, 7ft. 4*2 in. It will be immediately evi- 
dent that tmce the distance of the Earth from the Sun is the di- 
ameter of the Earth's Orbit, 190 millions of miles. Aaother me- 
thod of measuring the parallax of the Sun, and consequently his 
distance and diameter, is by observing the transit of the Planet 
Venus, or Mars, across the Sun's disc. This problem is rendered 
complicate by the motion of the Earth and Planet during the pro- 
gress of the observations; but the principle may be thus e^plaincdi 
Let S (l^g,2.) be the Sun, Y Vpnus and A B an arc of the 





ctrcqmfeience of the Earth. An observer at A ^11 see Venus projected on the 
disc of the Sun at a, the same instant that an observer at B will see the Planet pro- 
jected at h, And iht angle a Y 6 is equal to the angle A Y B. 

Again : let a b, Fig. 3, be an arc of the celestial 
sphere, S the Sun, Y N Yenus in two points of her 
orbit, and E R the situation of two observers on the 
Earth. WTien the observer at E sees the Planet pro- 
jected on the centre of the Sun, Yenns will be at V, 
and when the observer at R witnesses the ' same phe- 
nomenon Yenus will be at N. The sidereal time occu- 
pied by the passage of the Planet from Y to N will be 
equivalent to the celestial arc a I, as the great circle in 
which the Sun appears is divided into 24 hours. If 
then the obser^^ers duly note the separate instants when 
the Planet appears to them to occupy the Sun's centre, 
the interval between the two observations can be con- 
verted into space, and will become the measurement 
of the angle V S N, which is equiangular with a • b the angle measuring the Son's 

In explanation of the method of ascertaining the progressive motion of light, let 
S, Fig. 4, be the Sun, J, Jupiter in his orbit, and E e two 
positions of the Earth in its orbit. When the Earth is at 
E, Jupiter is seen in conjunction with the Sun, and when 
at e we see Jupiter in opposition. The diameter of the 
Earth's orbit E ff is upwards of 190 millions of miles. If ] 
then we note the time of an immersion of one of Jupiter's i 
Satellites when at E, and another when at e, and calculate 
the time elapsed between the two, and theji again note the 
time of an immersion when at e and one when again at E, 
and calculate the time elapsed between the two last, we 
sjiall find that the two last were performed in a greater pe- -^ ^S ^ 

riod than the two first, because between the two last the Earth receded from Jupiter 
190 millions of miles, and between the two first immersions the Earth advanced the 
same space nearer Jupiter. The exact difference would be IC minutes 26; thus 
showing that light occupies that time in traversing the diameter of the Earth's orbit, 
and half that time is the amount of the aberration of the Sun. But a plainer expla- 
nation may be afforded if we conceive an imaginary case. Suppose the Sun and Ju- 
piter to be stationary, the Earth to perform a circuit from E to e. Fig. 4, in six months^ 
and an eclipse of a Satellite of Jupiter to take place at noon daily. Then, if froni 
the Earth at e, we observed the immersion at the instant of noon, we should not 
witness it at E, 190 millions of miles farther from Jupiter^ until 1G"» 26' past noon. 

Meecxjry. See solar system. 

Meridian. See circles and earth. 

Minor Planets, or Asteroides. Ceres, Juno, Pallas and Vesta. See solar 


Month. Sec time. 




THE MOON, ^gi 

Moon. Next to the Sun the Moon is, to us, the most remarkable of the heavenly 
bodies. She is an attendant Planet, or Satellite of the Earthy to which she affords 
light by reflecting the light of the Sun; and she revolves from West to East, and to 
the same point of the heavens from which she monthly sets out, in ap average period 
of 27 days 7 hours 43 minutes and 1 1 seconds of mean solar time ; {See time,) 
which revolution is called fiL periodical month; but from New Moon to New Mpon 
again, the month consists of 29 days 1 2^ 44" 3", called the Synodical month or 
lunation. To perceive the cause of this variation it must be considered that while 
the Moon has been traversing her oihit round the Earth, the latter has been ad- 
vancing near a twelfth part of its orbit round the .Sun. The Moon, therefore, to be 
in the same position after a revolution, not .only has to pass once round the Earth, 
but has to accompany the Earth in the twelfth part of its orbit. The .diameter of 
the Moon is 2,200 miles; her mean distance from the Earth only 240,000 miles; 
A distance not much more than thirty times the diameter of .the Earth. Her orbit 
is elliptical (oval,) and the inclination of the plane of the orbit ^Kt an oblique angle 
with the plane of the Equator, and nearly coinciding with the EcHptic. The word 
lunar signifies pertaining to the Moon. A lunation is a lunar or synodical mbntii,or 
one complete revolution of the Moon round the Earth. A lunar year is twelve 
synodical revolutions of the Moon. A lunar day is the time occupied between the 
Moon's leaving the meridian of any place and arriving at the same point again the 
succeeding day ; which apparent daily passage is performed in 24^ 48°^ 46' of 
mean solar time, so that a lunar day is 48*" 46' longer than a solar day. The ap-^ 
parent daily passage of the Moon over the Earth (from East tp West, and contrary 
to her true motion,) is caused by the daily revolution of die Earth. Lunar distance 
is the distance of the Moon from the Sun or any of the Planets or Stars, as seen 
from the Earth; the measurement of which by instruments, with the aid of ca}cu« 
lations to be found in the Njiutical Almanac, will determine the longitude at sea 
within about 15 miles. The calculations in the Nautical Almanac relating to the 
Moon are of the following phenomena^ i. The sefni-diameter, or measurement of 
half the diameter of the Moon, in minutes, seconds and tenth parts of a second of 
a degree for noon and midnight of every day in the year. The apparent diameter 
of the Moon is daily undergoing a change in size, on account of her distance from 
the Earth being variable, ii. The Horizontal Parallax, (See parallax), hi. The 
Longitude, {See longitude celestial), iy. The Latitude, (See latitude 
celestial), y. The age of the Moon in days and tenth parts of a day, at meaa 
noon of Greenwich, reckoned from the time of the New Moon, that is, from the 
time when the Sun and Moon are in conjunction, or have the same longitude, yi.' 
The time of the Moon's meridian passage at Greenwich. (See guliwinatign). yii. 
The Bight Ascension of the Moon's bright limb, (See right ascension), yiii. 
The Declination of the Moon's centre in the heavais. North or South ^om the 
Equinoctial or Celestial Equator, from which she is never distant more than 26 
degrees, ix. The sidereal time qfthe semidiameter passing the meridian, (See 
TIME, SEMIDIAM1STER luid MERIDIAN). X. The mean longitude of the MotnCs as- 
cending node, (See nodes), xi. The Moon's daily motion, the velocity of which 
is continually undergoing a change, xii. The occultation of the Planets and Fixed 
Stars by the Moon, (See occultation). xiii. Moon Culminating Stars, (See 
culmination). XIV. The mean time of the greatest libration of the MoovCs appaj 


rent di$e. The ]ibrati(m of the Moon is a motion she has [See nutation] by which 
ike disc generallj presented towards the Earth is partly remoyed from sights an- 
other part occupying its place. The Moon always presents the same hemisphere 
towards the Earth, and the libration is the only change of the Moon's disc. "We 
have now only to explain the pheues of the Moon^ and other phenomena therewith 
connected ; for which purpose we use the diagram, page 31, requesting the student 
in the first place to bear in mind that the Moon is at an insignificant distance from 
the Earth, compared with the Moon's or the Earth's distance from the Sun, 
This diagram represents the positions and {)hases of the Moon for every 
day, from the third day of the lunation in November to the New Moon of Decem- 
ber 1844, The positions on the first two days are omitted to prevent confusion. 
This lunation has been chosen because there is a partial Eclipse of the Sun within a 
few hours of its conclusion. 

The dngiam also represents ; i. The circle of Right Ascension (See right Ae-> 
CBiraiON). II. The first Point of Aries, from which the Bight Ascension is reck^ 
oned in hours nmmtes and seconds, iii. The Rational Horizon of Greenwich at 
tke ietting of the Sun on the Idth. of November, and 9th. of December 1844 ; the 
Horizon at the Smi's setting on the intermediate days lying towards some points 
betwcCT the two lines, iv. The Bight Ascension of the Sun on the Idth. of Nov- 
ember, and 9ih. of December 1844; the apparent change of the Sun's position being 
caused by the actual variation in the position of the Earth in its Orbit, v. The 
Bight Ascension of die Mooa each day from the 13th. of November to the 
^, of December 1844. On the 13th. of November, at the setting of the Sun at 
Greenwich, an observer will have the Sun in R, A. (Ritfht jheensionj 15^ IG'^yand 
the Moon, the age of which will then be 3 days, in R. A. 18^ 31°*. The difference 
between the R. A. of the two bodies will be 3^ 15"*, and the Moon will set about 3^ 
15°* after the Sun. The limb of the Moon nearest the Sun will, at this time, be 
slightly illuminated, and this illumination, in the form of horns, will increase until, 
on the 17th. of November, the Moop's age being then 7 days, half the disc will be 
iiluminated ; this is the termination of tjie first quarter. Aflber this the dark part of 
the Moon will appear homed, the illuminf^tion being then called gibbous, until ou 
the termination of the second quarter, on the 24th. of November, the Moon's age 
being 14 days, the Moon will be full or completely illuminated. The Moon vrill 
then pass through the third and last quarter, and pesent the phases as in the dia- 
gram, until the 9th. of December, when the Sun's R. A. being 17^ 7^ 30", and the 
R, A. of the Moon being 17^ 10°* 10", the Moon will have completed a lunation, the 
whole of her disc will be dark, or only reflecting the feeble light afforded her by the 
Earth and Stars, and, between 18°* past 6, and 44°* past 9, of Greenwich Mean 
Time, the inhabitants of the greatest part pf North America, and of the islands in 
the North Pacific Ocean, will witness a partial Eclipse of the Sun. If the path of 
the Moon were precisely in the Ecliptic [the apparent path of the Sun,] there 
would be an Eclipse every month, on the occasion of new moon, but as this is not 
the case the Moon, when in conjunction with the Sun, is generally a little to tlio 
North or South of the great luminary and an £clip6e only occasionally takes place. 



jl«f ^ 

*^^ 0^^* 









Nodes. Those points of the orbit of a Planet which cross the Ecliptic. That 
point where the Planet passes from South to North is called the ascending node, and 
the other is the desceTiding node. The angle which the plane of the Ecliptic makes 
with the plane of the Planet's orbit is the angle of inclination, as A B, Fig. 1. A 
line from one node to the other is the line ofnodea, as in Fig. 2. The nodes of 
a Satellite are those points of a Satellite's orbit which cross the orbit of its primarv^ 
as the orbit of the Mooa crossing the orbit of the £arth. In the case of the Mood^ 
the nodes are continually changing their positions on the EcUptic, and there 
are calculations in the Nautical Almanac of the longitude of the MooifCs ascending 
node, that is, the distance at any time of the ascending node from the Equinox 

A. JB^ 


Jig 3 

or first point of Aries, the line of the Moon's tioctes making an etitire reTolution 
round the Ecliptic in 18^ years. If E C, Fig. 3, be an arc of the Ecliptic, E the 
place of the Equinox, or the place of the Sun on the 21 st. of March, and the Moon 
be observed in one lunation to cross the Ecliptic at a, towiards the North, a will be 
the place of the Moon's ascending node, and the longitude of the node will be 
E a. But the next lunation, the Moon, instead of crossing the Ecliptic at a, will 
cross at b, and the node is therefore said to shift from a to 5, from which, during 
the following lunations it will shift to c &c. until the whole circuit of the Echptic 
will in turn have received the nodes. The Equinox also (See precession,) is 
gradually shifting its place, and the correct longitude of the node will be the 
mean longitude of the Moon's ascending node from the mean Equinox. The longi- 
tude of the (L's ascending node for 1 Jan. 1843 is 281° 34' -1 ; for 1 Jan. 1844, 
262° 14' -4 ; for 1 Jan. 1845, 242° 51' -5. 

Nutation. A motion the Earth has in its annual revolution, by which the axis 
is twice slightly inclined towards the Ecliptic and as often returns to a positioii in 
which it is not so inclined. The Moon has also a similar motion called its libration. 
These phenomena appear to be connected with the precession of the Equinoxes. 
(See OBLiauiTY and precession.) A ''Term of Nutation involving 2 }>" is the 
amount of Nutation occurring in two months. 


OPP. . 



Nebulous, cloudy. The nebulous Stars are of the sixth magnitude, which show, 
a dim hazj light, and are scarcely visible to the naiked eye; but all Stars of this mag- 
nitude are not nebulous. See Nebula. 

Nebuljs. Misty congregations of matter observable throx^h the telescope aronnd 
some Stars, and also in many parts of the heavens apparently distant from any Star. 
In the constellation Andromeda a nebula can be seen with the naked eye, the app * 
earance of which has been described as that of a candle shining through horn, the 
condensation being greatest in the centre where the greatest brilHance is observed. 

Nucleus. A body around which other matter is gathered, as the .central body, 
of a Comet. 

Obliquity of the Ecliptic. . The angle which the EcHptic makes with the 
Equinoctial, which varies slightly in different years and different times of the year. 
Thus the obliquity on the 1st. of January 1843 will be 23° 27' 36" -58 ; on the 1st., 
of January 1844, 23° 27' 33" -02, and on the 1st. of January 1845, 23° 27' 34'''24. 
This change of obliquity is called the obliquity of the obliquity of the EelipHe. ' 

Occultation. [See heliacal.] The word occultation is principally applied 
to the obscuration of. Jupiter's SateUites within the illumination around that 

Opposition. See conjunction. 

Orbit. The path in the heavens of the Earth, or any of the Planets or Comets 
round the Sun, or of a Satellite of a Planet round that Planet, as the path of the 
Moon round the Earth. 

Pallas. One of the four Spheroides.' ' Siee solar system. 

Parallels of Altitude . See ai^titude . 

Parallels of Declination. See declination. 

• * 

Parallels of Latitude. jS^ee latitude. 

Parallel Latitude. A similar latitude. 

Parallel Sphere. See sphere. « 

Parallax. The apparent difference of posi- 
tion of a heavenly body by its being seen from 
different parts of the Earth, or at different heights 
above the horizon. Thus the Moon M, if seen from 
A will appear among the Stars at E. The Moon 
cannot be seen in her true place unless she is in 
the Zenith, or as seen from S, when an imaginary 
line drawn from the centre of the Earth wiU show 
to the spectator at S the Moon among the Stars at 
C ; S bemg then the nearest point of the Earth to 
the Moon. The angle, or difference, between C. 
and E is the Moon's Parallax to the spectator at 
A, and the angle, or difference, between D and C 
is the Moon's Parallax to the spectator at B. 
When we have to look horizontally at the Moon 
she has an Horizontal, or the greatest Parallax,, 
and it is evident by the diagram that when in the 
Zenith she has no Parallax. It will be seen that centre. 


Fualla^ makes a odestial body appear too low ; the calmlation for it is therefore 
added to an tqipareiU ahitode, Tlie Rxed Stars hare no Parallax ; even the Sun 
and Planets (excepting Mercory and Yenns) hare Terj little ; it is considerable only 
with the Moon, owing to that body being so near the Earth, and, conseqaentlyy at 
an enormoos distance from the story sphere in whidi she appears to shine. The 
Parallax of the Bfoon at the horiaon, or the Moon*s horiiontal Parallax, is upwards 
of a d^Sree ; the Son has an hoiiaoulal PtoaDax of onhf 8^ *5. 

PAKALUkx, Ankval* The ang^ whidi the Earth's Orbit makes with distant 
parts of the heavens* "When we conader that the orbit of the Earth is 190 millions 
of miles in diameter .we mig^t caqiect that, from different parts of the orbit, points of 
the heavens woold be seen under different angles. Let the circle A B represent 

the oibit <rfthe Earth, Now, if the Pked Stars were proportionate^ as near to 
onr orbit as the * * in the diagram are to the drd^ they would subtend the ang^e 
20^ at B, and the angle subtended by the same Stars at the opposite part of die 
orbit. A, would be 8^, {See angle). If a variation of the angle, or annual parallax 
of the fixed Stars amounted to only one second, or the 216,000th. part of a degree 
the distance would be fiurieem millume of naUume of miles; but it is doubtful if 
even thu small variation has been estabhshed by observation. The distance is so 
great that the entire orbit of the Earth is but a point in comparison. 

Parhslion. a mock Sun, occasionally seen and apparently owing to the reflec- 
tion of the Sun's l^t on thick and frozen clouds. 

PSNUMBRA, A partial shade between the perfect shadow and the full light of a 
heavenly body under an eclipse ; the time occupied by the rays of light in reaching 
us preventing our seeing the eclipse at any one instant precisely as we should do if 
there were no aberration. {8ee abbrration.) It is certain that the Sun is eclipsed 
to the full extent of the penumbra before that partial shadow is visible i^t the Earth. 

Perigxe. See apsides. 

Perihelion. See apsides. 

Pertxjrbations. Certain irregularities in the motions of the Earth andPlanetSi 
such as the Nutation of the Earth and the Libration of the Moon {See nutation), 
the *' obliquity of the obliquity '' of the Ecliptic {See OBLiauiTr), the Precession (tf 
the Equinoxes (iSfee precession), the Acceleration of the Moon (fi^etf accelbra<« 
tion), ^. 

Phases. iS^eeMOON. 

Phenomenon. An extraordinary appearcqice [phenomena, appearance8|] ii} 
Nature. Every Astronomical occurrence is a pb^pQipenon. 

PLA* POL. PEE. »5 

Pisces (the fishes). The sign of the Zodiac which the Sun enters aboat the 
19th. of February and leaves about the 20th. of Mardi* 

Planets. See solar system^ 

Plane. See circles. 

Poles. There is a Fixed Star in the North which appean always to bear the 
samey or telry nearly the same relative position to the Earth ; the Pole Star^ which 
shiiies with a steady, but dead hind of light, a little less than 2 degrees from the 
true North Polar point. Whilst all the other Fixed Stars appear, like the Suti, to 
describe diurnal circles in the heavens, (an appearance owing to the daily revolution 
of the Earth,) the Pole Star but slightly changes its position, and indeed appears to 
remain stationary. Instrumental observations, however, show that the Pole Stiur 
describes daily a small circle of 3^ diameter, and that therefore it is 1^^ degreeist 
from the polar point, which is the centre of the circle. At the North pole of the 
Earth the North pole of the heavens is immediately in the zenith. At the Equator 
the North and South poles of the heavens both appear at the horizon, and to be 
parallel to the centre of the Earth. Half way between the Equator and the North 
pole of the Earth, (or in 45°North Latitude,) the North pole of the heavens is el^ 
vated, or at an altitude of, 45°, and appears half way between the zenith and the 
horizon. The poles of the Ecliptic are points in the heavens 90° from every part 
of the Ecliptic drcle, and about 23^° from the poles of the Equator, or North and 
South poles. 

Precession of the EaviNOXES. To enable the student to have any cenoqptioB <f[ 
this interestmg subject he must first have a clear impression of the motion of the 
Nodes of a Planet, or Satellite, as attempted to be explained in the instance of the 
Moon, under the word nodes. Now, the Precession of the Equinoxes, (or the 
Becemon of the Equinoctial Points, as the phenomenon is called by some Astrono* 
mers,) is analagous to the motion of the Nodes of the Moon , but with this differ* 
ence to commence with, that whereas the Nodes of the Moon complete a revolution 
about the EcHptic in 18|^ years, the revolution of the Equinoctial Points about the 
Ecliptic occupies no less than 258 centuries ! If, when the Sun arrives, about the 
21s»t. of March, on the Equinoctial, his distance from some Star, measured on the 
Ecliptic, be accurately ascertained, and compared with an observation taken on the 
same day of the previous year, it is found there is a differencCi or increase of the 
Star's Longitude, amounting to 50" '1. This difference, so small for a single year, 
becomes great when accumulated, so that in a century it is 1° 23' 30" , and in about 
25,800 years the difference will be 360^, or the entire circle of the Ecliptic. Jjet 
A B C D , Fig. 1 . represent different positions of the Sun with respect to the Fixed 
Star S, at the Sun's rising above the horizon of an observer at the Equator ; the ho- 
rizon, in each case being depicted by horizontal waves. Let A be the position, at 
sun rise of the Vernal Equinox, the diurnal direction being A E. BCD will then 
represent the Sun rising on other days of the spring months, as the Sun, in his an- 
nual course, is seen to advance in a northerly direction, A being due East, and *the 
diurnal direction of the Sun bemg B G, C H, DI. The line P A B C D wiU be an 
arc of the Ecliptic ; the Sun, A, will be in the First Point of Aries, on the Ecliptic, 
and the Star S, being referred to the Ecliptic, (by a line drawn perpendicularly from 
the Ecliptic to the Star,) will have no Longitude that year ; the Longitude being 
reckoned from A in the direction BCD. But on the next occurrence of the vem* 


PRECESSION OF TWIg v qnii^ry^c^ 
1 H G iE 

"■«»— •■^•B 

d eqnmox the Srni will have receded, or not have advanced as ftr as A. by 50' -1 

Tl' -La^^^^ *^* P'*^** «f *•>« Equinox, or the First Point of Aries .nTrtl 
l^onptude ofthe Fixed Star S. wiD be P A. or 1°23' 30*. ft Sh tii^Sf t! 

fteJS^ td SIT' fn^^ °*« P»»t» of theEdiptic^ be likewis/kwS 
tneu- piaoes, and the constellations of the Zodiac, after which the Sinis of the Edin 

^et: ^e "Zfmr. f .g-eoincide with those Signs. Snchirf^tsIS 
Ari^dl^J^ilZ i ^'^' 2«00 y^ ago. ^ in the stellar constelh»tion 

kSn o?S,V 7 J^ ^ ^ ®r """ ^ *" """^ "l"^"" t-* »»««« in that const^U 

lation of the Zodiac ) bnt from the effect of Precession it is now in the co^. 

lataon Rsces, and. 2000 years hence, will be in the constellation A^^Z 

S^E^'.^fT'^ the original Signs although their positions no lom^i^^^'w^ 

the same cause, is a slow movement of the celestial 
poles, or such a motion of the poles of the Earth 
as to make them point successively, in about 25,800 

r^' V r^ P"* °^ » '^«''«' ^»^g the. pole of 
• ^S'S, " * *^*'*'' ""* *h« <*^eter of which . 
" J .V ^ °'' *^** *h® ""g^® between the Ecliptic 
and the Equator. See Fig. 2, in which • within the 
«rele IS the pole of the Ecliptic, P the position of 
the present Pole Star and North Polar Pomt, and L 

attraction by the Planets of the protuberance o7^ir^' "^ ^^ ** ''""^ 
Equator. («e* degree.) P^nioerance, or redundancy of matter, at the 






P. L. of difF. Proportional logaritliin of difference. (See hOGAKtruu,) 

Primb Vertical. {See azimuth.) 

Radius Vector. A radius of the elliptical orbit of a Planet or SateUite, as in 


the figure^ in whicli all the lilies diveiging from 
the body near the centre of the orbit are the radii* 
The radius vector (or traveUin^^ radius^ ) of the 
Earth measures its distance from the Sun, which 
varies so that at one peri9d of the year, ( the 
winter of the Northern, and the summer of the 
Southern hemisphere,) the Earth is 3 milUons pf miles nearer the Sun than when at 
the most remote point. Calculations of the length of the radius vector of each 
Planet, for every day in the year, are in the Nautical Almanac. : . , 

Reduction of Stars. The correction of the Right Ascension and Deelination 
of the Fixed Stars for Precession, Aberration and Nutatidn« ^See these terau.) . 

Reflection, of the raye of Light. The rebounding of -the' rays, or the Angle 

they make with a reflecting' surCice^ such as wa« 
ter, 6r a polished surface of metal or glass. It is 
said that the angle of inddenoe is eqtial to the 
angle of refleotiotf . Thus, in the figure, a rAy of 
light from Af after striking a reflecting surfabe at 
8y will rebound, or reflect to JB ; ^ iS^ 22 is, then, 
the angle of incidence and B 8 H the angle <^ 
' reflection ; these angles being of similar extent; 
In like manner, a ray from C will be reflected to DiiC 8E being the an^e of inci- 
dence mdDSHihe angle of reflection. A ray falling perpendiculaiiy on ft reflect- 
ing surface/ as from' E to iSf, will be reflected back in precisely the same, direction *; 
the incidetice making no angle neither will the/ reflection^ 

RIbfraction; of the rays of Light. An oj^tical illusion, which makes a heavenly 
body appear at a greater altitude thiiui it wot^ld be seen at^ thc^e- were no aitoos^ 
phere over the Earth. Light deviates frohi a^stniight line according to the densifyi 

« « M t 

I ' 


•I / 1 1 

« ji 

t!..^**:- .• 


5 A. R- T jj 

or quantity, of atmosphere throng wjfiich it passes. When the Sun is seen to rise 
or set the quantity of atmosphere, through which his rays proceed to an observer, is 
much greater than when the Sun has ascended fi considerable (dtitude. This wUl be 
seen by the diagram. The Sun, when at 8^ sends Ins rays several thousand miles 
throng the atmosphere frpm ^ to J{ to ^ei^^J^^an qbjservei; at B ; but if the Sun be 
in or near the zenith , as z , the, jcays bftve imly tp ^penetrate the atmosphere a few 
miles, or. the altitude of the atmosphofe above the jB^rth > aj^ frqo^ D fo E9. ^ I'cach 
an observer at E% When we look at the Sun rising or setting we look through such 



an enonnoot quantity of atmosphere that we are enabled to gaze at him with eur 
naked eye ; but if the Sim be at a eonaiderable altitude the quantity of atmosphere 
we look through is so mueh less that we ate then only enabled to bear the fieiee 
glances of the solar rays thn^h a darkened or colored medimn. These remarks 
are necessary previooa to giting an explanation of the term refraction, which is the 
new direction the rays of light move id after passing, in an oblique direction , from 
one medium or element into another. In passing from a rare into a dense medium 
rays of light are refracted towards the perpendicular. J B , Fig. 2. , represents 
a ray of light passing through a rare mediunf ; B G the 
same ray continued through adense medium, and D £ J> 

a perpendicular line ; the ray at B G being refraeteJ ^^-^^^^^^^ I 

toward$ the perpetuUeular. On the eotitrary, a ray of ~ 

light passing from a dense into a rare medium is refrac- 
tedyWisi the perpendiculaf. If a ray proceed from C, 
Fig. 2. and emerge at B, from a dense into a rarer me- 
dium it wiUbe refraefced towards A, from the perpendi- 
cular. Beverting to Fig.I, a ray from the Sun 8, after passing through tlie rate s^micc 
between the Sun and £arth» will be bent on arriving at the dense atmosphere, owing 
to which an observer at B will see the Sun, by refraction, before that kumnary has 
actually risen above the horizon^ Befractioa is (noncy) at the zenith, aiid 34' (34 
minutes of a degree,) at the hcmzen. When the Sun just appears to rise or set his 
centre is 34' below the rational horizon. {See circles.) Since refraction, therefore, 
causes a celestial body to«ppear too high the amount of refraction has to be snb- 
traeted from the apparent altitude to correct it for the true altitude* 

Bstardahon. iSee AccsLBRATioif • 

Rbtolvtion. The movement of a Planet, Comet or Satellite from one ftitA 
until it returns to the same again, as the annual revolution of the Earth round the 
Sun : or it is the movement of a body on its axis, as the dhimal revolution of the 
Earth. The revolution of the sphere is the apparent daily passage of all the celes- 
tial bodies over the Earth, from East to West, an appearance caused by the Earth's 
diurnal revolution from West to East. 

Right Ascension. An observer situated at the £quator sees all the Fixed 
Stars rise and set perpendicularly to his horizon ; those rising due East passing over 
his zenith and setting due West, and those rising 45^ from the East setting 45^ from 
the West, after reaching an altitude of 45^ in the heavens. These ascensions, perp- 
endicular to, or at right angles with, the horizon of an observer at the Equator, are 
Bight Mcensunu of the heavenly bodies , (See Fig. 1 . ) and their ascensions at any 


With Arcs of Ascension of the heavenly bodies at right angles with it« 





ftt 45° North Latitude, 
With Arcs of Ajceniisn nt Oblique Aisles with it. 

other horizon than one on the Equator will be ohl^i. See Fig. 2. in which N the 
North Pole, is in the centre ofthe circle of Perpetual Appariton,- (See circle ftc) 
The angle, or difference, between the celestial meridian of a body and that put of 
the Equinoctial which rises with the body is the aeeentional differenee. Thus , in 
Kg. 3., P H being the same circle of Perpetual Apparition as in Kg. 2., Jtf E the 
celestial meridian of the Star S; £ £ Q the EquinoctiB], and U S the Horixon, tiis 
the point L on the Equinoctial has risen with the Star 8, and £ £ is the ascensional 

But the term BJght Ascension has a much more extended eignificadon than that 
iucloded in the above explanation of the pherumtenm which the term espresses. 
Technically the R. A. or A. R, (Right Ascension,) of a heavenly body is said to be 
an arc of die Equinoctial included between the First Point <^ Aries and the celestisl 

meridian of the body. Thus if Q, Fig. 3, be the First Point of Aries, sad N E the 
celestial meridian of the Star S, Q E will be the Star's Right Ascension, or titat 
ar^jular cUstance of the Star fron the First Point of Aries seen at any place on the 
globe, and without refweaee to tlie fact of the Star having made a Right or ao 
Oblique Ascension from that place ; the lUght Ascension having been made, as al- 
ready observed, at the Bquator. 

For the purpose of measuring the apparent distances of celestial meridiana frpm 
the First Point of Aries, the Equinoctial is divided into 24 parts, ta hoUra, by 24 
horary circles, all meeting at the South and North Poles of the heayens, as ip Kg-'|. 
which with its explanation will be found in the svtcceeding page. 



• In this diagram S is ike South Pole, and the circle described from it is the Equi- 
noctial.. The Sun.i^ i:epresented to be in R. A. 0^ 0" 0', {m distance from the First 
Point of Aries, and consequently an that Point) : 5 represents the position of the 
Planet M^cnry in.R. A.'23^ 1™ 37", (as near as the size of the figure will permit) ; 
% Jupiter in ». A. 29" 6°^ 22% Tj Saturn in ». A. 20^ 28«» 42% g Vesta , in R.A. 
19^20°K)», and ^ Ceres, in R. A. 15^>30'"0% all. these "Right Ascensions" being 
the appjorent distances of the celestial meridians of these bodies. Easterly, from the 
First Point of Aries, for the 20th. of March 1844 ; their distances from the Equi- 
noctial being their declination. On the day mentioned, the Moon and the Planets 
Venus, Mars, Juno and Pallas will have North declination and are, therefore, exclu- 
ded from this diagram, which only represents the horary semicircles of the Southern 
celestial hemisphere* If the line from 23 to 1 1 in the diagram be taken to represent 
the Southern Horizon of any place on the Equator, on that day, then the Sun is I'' 
of R. A, from the Horizon, in the East, as he will be one hour before sunrise, 
whilst Jupiter and Mercury are just skimming the Horizon, and Saturn is seen to 
have risen 2^^ hours, Vesta 3 hours 20 minutes and Ceres 7\ hours previously. 

Right Ascension is onie of the most important elements in Astronomy ; it divides 
the entire sphere of the heavens into 24 parts; it connects space in the heavens with 
time on the Earth. As we know that die ,Sun is in R. A. 0^ 0°^ 0', or on the First 
Point of Aries, about the 21st. of March, and that l^e passes over the great qrde of 
R. A.' m twelve months, we can form an instant concepticm of the Sun's place 
(nearly,) in the heavens at any time by allowing 2^ of R. A. for the Sun's apparent 
motion, from West to East among the Stars, for every month elapsed sinc^ the 21 st. 
of March. For example , on the 22 nd. of April 1844, the Sun's R. A. will be 2^, 
on the 23 rd of May 4^, and on the 21st of June 6^. When we learn that the Sun 
is in R. A. 6^ and the Moon in R« A. 18^, (that is, 12^ distant,) we can immediate- 
ly infer that the two luminaries are in opposition, and that, about the time when 

MN. SAT. SEA. - 41 

i» 0«i*> 

the Sun is rising in tlie East, the Moon is setting in the West ; and if we leam that 
the hours of R. A. of the Sun and Moon are equal we are at the same time informed 
that the Sun and Moon are in conjunction, that the Moon is just completing or 
commencing a lunation, and that she will rise and set with the Sun. In the N. A. 
(Nautical Almanac,) the R. A. of the Sun is given for every day, with the differ- 
ence for every homr ; and the R. A. of the Moon for every hour of every day, with 
the difference for every ten minutes. 

Ring of Saturn. See solar system. - 

Sagittarius, (the archer). The sign of the Zodiac which the Sun mters about 
the 23rd. of October and leaves about the 21st. of November. 

Satellites. Attendant, or secondary planets, as our Moon and the Moons, or 
Satellites, of Jupiter. See solar system. 

Saturn. One of the Planets. See solar system. 

Seasons. The phenomena of the Seasons are caused by the poles of the Earth 
bang always directed towards the same points of the heavens, and the axis of the 
Earth being inclined 23^ degrees from a line perpendicular to the plane of the orbit, 
as in the first diagram, in which X is a line perpendicular to the plane of the Earth's 
orbit, p a pole of the Earth, and P the direction of a celestial pole. The celestial 
pole, if placed in conformity with the size of the orbit in the diagram, should be sev- 
eral feet from P, in the direction jp P, so that in whatever part of its orbit the 
Earth may be conceived, the angle between a line from a pole of the Earth to a pole 
of the heavens and a line perpendicular to the plane of the orbit may only slightly 

*'•-... ^' 



vary. There is in reality a very small variation at different periods, for an account 
of which see nutation and precession. 

The second diagram represents the Earth in the four positions it occupies , with 
respect to the Sun, about the 21st. March, 21st. June, 23rd. Sept. and 22nd. Dec. 
If we imagine the Earth, in each position in this diagram, to lie revolving on its 
axis, it will be seen that, about 21st. March, the Earth will present, in the course 
of its diurnal revolution, the entire circle of the Equator directly towards the Sun. 
In this position, the Earth having the Sun vertical (perpendicular,) to the Equator, 
and at an equal distance from its two Poles, equal days and nights are over the 
Earth the Poles being in the boundaries of light and darkness. On the 21st. June 
the Earth, having progressed over one quarter of its orbit, in its daily revolution, 
turns its Northern hemisphere towards the Sun. The Sun then shines without 
setting on the North polar circle, the inhabitants of the Northern hemisphere are 










Svd^iuica <)i« 






c.— ••*• 

sec; . mar .sol. 43^ 

theh'^y tll^8ttn!Mer^86Ml0e;f^tt]|<l'tlK>te of^^ Soitth have th«ar/^l%iler; ike 
S6\iW|Kfflli^c&ti[^ bdiBg 'iisr diirkti^si. Oil tkil 2Sti. of September ih» Eaitb has 
reiU;%er'a'ipoifit'lRMeK'ib»''E Bgiiiitiiniri^difeedjr towaids tiie Sun , and' 

e^ikaPdiy^ aii^^n^S'arA'o^ir th^ EarA; Thk is the second Sunnier at the 
Etftmsfr, tH&'Atmt^taA IS^sp^^mx ^t' th« Kortii, imd tlie Vernal^ or -Spraig, Eqwnoix 
a^'tte Sbttm? The EM&'tkentMissesoiittfthfcfciifrti^ positiM ddineated in die 
di^rt^; wfeSdi ooMM abotit the* 22nd. Decenber, ^en the Ettdi pvesents its son* 
tl^ faifi&S^{«iiT« tl^ the gl^t Itin^ It is then the Summer 'sdstiee at 
thb^ S^Ch'taidthe' ^Winter sobtiee at the Nivth $ the North polsr ciieie^heinKin* 
dMOimt ItS^^Ptkb^l^ 8eei» thittMMrls only one day and night at' the fblea 
tUtoiighefvtrth^y^iu!^ Ute SM's rqrs^oldy r6aeh W from that pokt^if the Eatth 
wfxere titti SubI iai viltiea]^ alid'odfy'illuMttat^ hatf tlie ivoildat^ one time ; and aa 
the Poles are 90® from the Equator, it is nig^tf«f the N«»th Pole when the Sun is 
South of the Equator, ^which continnDil 'diftiiig half the year,) and day when the 
Sah ii Nbite' oft6i&1B^t6rVth% lte¥mft oNhk o^SOHfing at the Sooth Pble; Ti» 
orbit of the Earth is ellii^cal, and that jtet'of the t»rbit in whieh the Earth is sku- 
ated during the Winter of the Northtttt h^iieiS|)here is 3 millions of miles nearer 
^e" ]^BAh^ tUhif 'tli aj^diti^' paH. Thi^ elll^feity is searoely peiveptible in so 
itiiWf iP f^sm' as' tluf diigMh ;it attiomi^ to a dMefre^ee of only a parts in 190, 

l&cuLAR TiWW, TSiorioyi&A'KctEttiiA^io^* An indefinite time, motion or 
acc^eleration. Thl? Secular weeterdtum of tlUMa&iif^ Me&n mibtioH is a slbw and' con- 
tiiiuai increase of the' speed of the l^ooii over the Earth, eomjfared with her motion 
oi sbmVcehinneis pfeVibus, dtused by her gradually approaching the Earth. If con- 
tinued, for an immensity of ages, the Moon would at Ust comie in contact with the 
Earth, but it is theoretically shown tUat thd acceleration has its bounds, although 

BsuttiAMinUR. JSjBit a diameter. By the term "senudiameter^' of the Sun or 
Moon it ^erally understood half the horizonial diameter of 
tfther body slipaitated by a'Uiie drawn perpendicukr to the eye 
of die sj ^ ta tOi vMiu ^^ amiexed figare. The semidiametm 
of the' Sun aifd M6otf are eontinnany undeigoing a change of 
n^ypAietitaiie 6n aoeocbft eff t^eir vuying distanees from the 
EAtii. The dilidtdiKDieter of the Stmiagivenin the Nantical 
itimanad foi^ every dtty, and the seinidiameter of the Moon for 
ereiy nd9n and Audn%ht# To the senaidiameter of the Moon, thus given, a correc- 
tion has to be applied for augmmiaHon. [See augmsmtatiom and viamstkr.} 

E(ii8M]^i8; (Oie dctii^ioiij. ¥be si^ o^the Zodiac vHifeh the Sun enters about 
ltier23^<$. ^b^W, tend MM tiibout Oie 21st. of Noyembef. 

8iDEiipAi«, SiD^RAL, SiDEREAN. Starry. l^Sidtreal Time of the Sun's Semi- 
dianjieter facing the Meridian is the sidereal time occupied by a semidiameter of 
Ihe^un, on any particular ttay^ in passing a meridian point, lliis time is variable 
ap^rding to tne greater or smaller distance of the Sun frokd the Earth and the po- 
sition of the Earth in its elliptical orBi^ \See time, semidiameter and meri- 

Soi«AR. Relating to the Sun. 



Solar Systsm. The Solar S^stfunis Omt purt of the UmTone.wliich has the 
Smi for its centre^ and includes the Eerth and.oUier Planets which reyolve anmnd 
the great luminary ; the Comets heing periodicslaiidoceaaionalTisitoi^s of theSystem. 
The diagram which represents the .Orbits of each Planet does not. truly depict the 
sixe of each body. To approximate towards a correct representation would, require 
a drele of more than a milq and a half in diameter, on the droumferepee of which 
Uranus or the Geor^an would be .of the size of a cheery or. small plum, Saturn a 
«nall orange on a drde four fifths jof n mile in diameter, Jupiter a moderate sized 
Qrange on acirde nearly halfa mile across* A globe 2 feet ip diameter, placed in 
the centre would represent the Sun, Metciuy would only be* of the ease of a grain of 
mustard seed, 81 feet ftom the Sun, Venus* a pea, 141 feet, th^ Earth, also a pea, 
214 feet. Mars , a large pin's head, 326 feet, Juno, Ceres, Vesta and Pal]as,.grains 
of sand, 500 to 600 feet ftom the Sun» 


revokes on liis axis in 25|- days. His diameter is 882,000 miks, fi^ii he fills a 
space twice as huge as the orbit of the Moon* 


Nearest the Sun revolTes the Planet Mercury,, a small stai: wi^ a Teiy bri^i 
bluish li^t. He is distant from the Sun 37 mUUcns (Smiles, but^rom the Earth 
he appears so near the solar luminary as only pocasioiially visilj^le, a littlf be- 
fore sunrise or a little after sunset. He never appears more than 20^. from the Sun, 
or one ninth part of the visible sphere from East to West. During a Solar Eclipse 
he is sometimes seen ; and he is also observed to pass between the Sim and the 
Earth, traversing the Sun's disc. His diameter is about 3100 miles, and he revolves 
arpund the Sun in 88 days*. 


is the most beautiftd Star in the heavens, and is* called the Evening and the Mom« 
ing Star. When towards the West of the Sun she rises in our horizon before the 
Sun in the Morning, and when towards iheEast she shines in the Evening aft» 
the Sun has set. She never appears more than 29^ (or one taxHh part of the 'visi- 
ble sphere) from the Sun. She is to the East and West of the Sun 9 or 10 
montiiis alternately. When a morning Star she is sometimes called Phosphoms or 
Lucifer, and when an evening Star Hesperus, or Vesper. ' She has phases, like the 
Moon, sometimes homed and sometimes gibbous, and like Mercury is seen to trav* 
erse tlie Sun's disc, which proves that her orbit, as well as that of Mercmy, .is be> 
tween the Sun and the Earth. Distant from the Sun 69 millions of miles, and 
travels round the Sun in 225 days, at the rate of 76,000 miles an hour. Diameter, 
7,900 miles. Revolves on her own axis in 23 hours. 

Venus and Mercury are called the inferior Planets, their orbits being .within, or 
inferior, to that of the Earth. The other Planets, whose orbits are exterior to, or 
larger than that of the Earth, are called the superior Planets. 

THll EARTtt 

is distant firom the Sun 97 millions of miles, and travels round its orbit in 365^ 
days. Mean diameter, 7,900 miles ; its diameter from Pole to Pole being 26 miles 
less than at the Equator. Circumference 24,850 miles. Revolves on its axis from 
West to East in 24 hoursi and, like all the other Planets, (with the exception of the 
Satellites of Uranus,) pursues its orbital course round the Sun from West to East. 
Velocity in its orbital revolution 58,150 miles an hour, or 150 times swifter than a 
cannon ball. 

The Moon and the Satellites, or Moons, of Jupiter, Saturn and Herschell are 
called secondary Planets to the primary Planets around which they revolre. 

JU f *' 




jtok>^- ^ ^"^ 




the' ^tXft St^TfiM.' 


is « secondu; FUnet to her primary the Earth, tnm which she ia distant only 
236,847 mileB. Diameter, 2,160 miles. She makes one rerolutioii on her siis ia 
27^ days, and rerolveB around the Earth in nearly the ssaie period of time, invaria- 
bl; turning the same hemisphere towards oa. 


gives a duller light than Venna, and ia of a dniky red colour. Distant from the 
Sun 145 milHona of nules. Travels ronnd the Sun in 687 days, and revolves on 
bis own axis in 25 hours. Diameter half that of the Earth, 4190 niles. 


are fonr Planets generally called Asteroids, only lately diswvered, and never viable 
to the naked eye. Kameter of Pallas 2,090 miles, that of Ceres 1,600 miles, of 
Jnno, 1,425 miles, that of Vesta is not known. Ceres is 260 millions of miles from 
the Sun, Juno, 300 millioni, Vesta, 226 millions of miles from the Sun. The orbit 
of Pallas is very excentric and crosses the orbits of the other Asteroids. 


thelai^est and most splendid of the Planets, ia diatant from the Sun 493 millions 
of miles, travels round the Sun in 11 years 314 days, at the rate of 25,000 miles aa 
hour, and revolves on his own axis in 10 hours. Hisdiameter is 90,000 miles j his 
bulk 1300 times greater than the Earth, and he has 4 Satellites, each larger than our 
Moon. These Satellites are of conuderable importance in Astronomy, aa they re- 
rolve so rapidly around their primaiy that their transits over tlie disc of Jupiter, 
or an eclipse of one of them, is almost a daily occurrence, and the exact Greenwich 
times when these pheugmena are to take place are foretold in the Nautical Alma- 
nac. By a comparisoQ of tlie time at Greenwich when a transit or eclipse ia to be 
seen, with the time when it is observed at any other place, the longitude of that 
place from Greenwich is immediately Inferred without any fruiher calculation. 
For instance, if an eclipse be foretold to occur at Greenwich at twelve at Noon, and 
it is actnally observed at some other jiace at oAe F. H, that place will be distant 
from Greenwich the twenty f^iHth part of the drcumference of the Earth easterly 
from Greenwich, or in longitude .15°£. The observers at this place and at Greenwich 
will both be witnessing, the phenomena at the same minute, but it will only be twelve 
o'clock at Greenwich, when it is qae o'clock at the place 1^° easterly. Jupiter is re- 
markable for an appearance of l^^ts over his disc, snppoaed to be caused by his 
atmosphere being lesa dense ,at hi^^ Bquator than at his Poles, and, consequently, 
varying the luminous appearance of the planet. 


Sfttnm, when licwed by the naked eye, is of a dull leaden lustre, and is hardly 

T ^ SOlAR ^YSTEM, ^\ 7 

22,000 mOes an hour, and rev6^^6^'o8PE^^t)^ k^^iPldi^dm^'tlki fb^KKM^f 

the Bings does pot exceed^lM unless hut .iheir.4»r^l3i 4joggdOf»T «| j^^jt^ ^es ; 

:th$. ^te]^o;i4ianictter jo(:th^ extmof ,^ipgis i76^0pP| t^mte betveen^tb^la- 

net and interior Ring beipg, jPj^QpO^l^s, wfd the intoryS*^ betw^n tliie^ tw 'fijxxgi 

IfBDO miles.-.^Thfi Bing does i^iot^.f^nrays present the appearance asi in^the^oure : 

.,when the thin ease is turned to us it appears only as a very fine sTrai^rht line. The 

^ Nautieeu Almanaq contains predictions^ of the position, magnitude ana appearance of 


meter is about '35.000 jpiiles, ipi^ its quli 80 limeslthat oTthelBar^.^it is'cer^iinly 

:U ._„.._.".,. ■" 

round its orbit in 84 jedrs. 

The Ephemeris of the Planets occupies 164 pages of the Nautical Almanac, and 

contains for each Planet, for Greenwich Mean Nooff'df'^i^^'dl)^ id^the'^l^^ the 

apparent Geocentric Bight Ascension Aid U^KftdftV»r$^t^etkiis^'Of Ait^Mertiian 

Paaaage ; and the Logarithm of the true distance ftsmi Ae Earths th^: Heli^omtric 

Longitude and Latitude, and the Logarithm of the Radius Fee tor t^ It also contains 

for each Planet (with the exception of the Asteroicls,) at its transit over the M^rid* 

ian of Qreenwich, the apparent Bight Ascension and' Declination, and fhe variation 

. of B^t ABoenaion 8nd DddiintiDn lb¥ OB^ttour^f L6ri^tud4> tfi» SSderealtSQi»« of 

the Semidiameter passing the Mmffi£^» A^togtd$p['VieBMimA&ai:cfi^ 

.. eter. and the Horizontal ParaUax* Vpr an. explanation of each of these terms in 

Itais's^ fhS rfespeAive wordts; ' ' " ''' ^'^ ''-' ' - ^'^^ "' ^'- ^ — ^ 

M The nature of Cometa (hair^ Stars) hvKkt known. . It is cerUdn, howerer, that 
. they' are occibiotial Tisitiira^f the 'Sobt^ Systefn^ ! .(See^Cfhanm)*^.'fTlaUKkWBM)et 
also is not detennined,' and milj three httvefaad thrilr penodicalv^titmft^dc^^ 
first of these {Halle^js Comet t>t the Ck^m^t of ir&9*>^ppe4riiigi«¥eiyn76£ /^, 
the second^ (Ekcke's Comet) ey^ry thi^ee years and H tiUid^ Md tiber:tlM«( (Bi^ 
I C6ntet) every six y^ars and thrte quartfelm.:. Tbe-nuHMs^^s^ASom^ is ttte^ototial 
pdnt, or b6dy, liround wbi6h tibtere is anebulouiS' a|^earanee'eailed*tilMtiitei|yv«r.^e 
Mdeus'and hair fbgethfer form the hifodi^' tki.'Coiket. - Te^'tlub^id' ^eiiettll^,'r'btit 
not alwayd, atisadied a luminous tram called tHe tail,' fieme>Ckntetir iutveHad 
aevisral'(one of them as miny as sixdistsnctyiaibi and the'diramrions of thetegas- 
, eons 6r electiric appendages hai^ odeasioiiaUy beelr'abtdluildte NaiitioiKlAitna- 

nae fat the yiears wheii these' Coiiiefir lire ei^eeted^ IsoMifastHBi Ephe»iSfis'4f their 
last appearance, edqiprising the geocentxicBa^t Ascension ^attd}DeeUnalioii %atii:the 
variations in one hour, the time of the Comef s daily passage -of* th^'Mimidbntmd 
the logatitfasis of its Sisttoeed from AelEkuf aiidldBaMii *. - r «u«r T^:r» . t^l 

' • - tv *4> • ', «» J> 

48 SUP. tAU, TIP. 

i,    ii   — - — ' ** ' — : — *^ 

Solstices. Those points of the Ecliptic the most elevated above, or at tfie 
greatest distance from^ the Equinoctial ; so called because the Sun, when arrived at 
Qkemajipeara to stay or stop a short time. . See colures. 

SuppLXMXMTf (in geometry). Such an addition to the arc of a circle as will 
suffice to complete 180^ or a semicircle. In Astronomy it is the number of d^e^ 
required to oomplete 180^ Irpn^ North to South ^c. * , 

Sox«8TiOB8> SoXfBTirrAt Points. 8t& colitrbs and sxasoks, 
SovTBiKO. A term given to the approach of the Moon to the southern iute of 
the celestial meridian of a spectator. iSf«e culmination. . t 

SraERis. .The Celestial Sphere is flie concave or arched fece of the heavens, 
as seen from the Earth. A right Sphere of the Sun or a Star is one in which either 
body rises or siets in a perpendicular line to the horizon, while an oblique Sphere is 
one in which it continues parallel to the horizon. The Celestial Sphere at the Eqnk- 
tor is always a right Sphere for the Fixed Stars, as they all rise and set at right 
angles with the horizon. At the Poles the Sphere is always a parallel one ; the Sti^ 
never rising or settiiig, but those visible describing complete drcles, parallel to the 
horizon. ' At all other parts of the world the Sphere is more or less oblique for the 
Fixed Stars, but some parallels of latitude near the Equator have ar^ht Sphere Jor 
the Sun and Planets at some seasons of the year luscordin^ to the periodical changes 
of those bodies. See. also bight ascensiqn. 

Stars, See vixed stars, 

Stbllail Starry ; relating to the Stan. 


Stnodical MoNtB. See moon. 
Syzygy. See conjunction. 

Taurus, (the bull). 1%e sign of the Zodiac which the Sun enters, aboat the 
20th. of April, and leaves about the 20th. of May. ' 

Tides. The rotation of the Eai^ on ifs axis, combined with the attractfoti of 
the Sun and Moon exerted on the fluid portion of the globe, occasions the pheno- 
mena of the Tides. If the Earth were at'irest between the Sun and Moon the 
waters immediaA^y under the two luminaries would be raised hy their attraction 
and remain permanently elevated; hut as die relative positions of all three bodies 
are continually nndergoing a change, so the attraction on thewaters is continually 
shifliiig in position ; the attraction of the Siln and Moon being exerted in the same 
direction when the Moon is New and Full, (or in conjunction widi and opposition 
to the Son,) forming the high or spring tides, and the attraction bdng divided in 
amount between that due to the Sun and that due to the Moon when the Moon b in 
her, first and third quarters .; the tides being then neap or low. The devation of the 
tide due to the Sun is 2 feet and to the Moon 5 ^t ; when^ iheivfbre, Jboth the at- 
tractions are exerted together the tldid wave near the Equinoctial line, where the 
attractioii is greatest, is 7 ft. high, and when the Sun and Moon are in quadnittge, 
(one four& of a great celestial drcle apart,) the height is about 3 ft;^ heSng-the dev- 
atidn due to the Moon lessened by the attraction of the waters, in anangnlar dbee^ 
tion, duie to. the Sun. f 

Tina explanation (to a certain extent only,) contains the theory of what is. ealled 
tibe Chreat Tidal Waves^ which flow daily from East to West under the Sun and 



Moon ; that of the Sun bemg sometimes superposed on, or coincident with, that of 
the Moon and sometimes being independent. But there is this difficulty immedi- 
ately occurring in connection with the phenomena, that there is not merely one 
high tide per diem (each day,) but two ; or, in other words, the waters are not only 
elcTated under the Moon but at the same time are heaped up on the opposite side 
of the globe. To receive an explanation of this difficulty it must first be conceived 
that the tendency of the solar and lunar attractions is to bring the waters of the 
globe towards the Equinoctial line, thus causing a protuberance over the Equatorial 
rfigions and a consequent diminution of convexity, or height of the waters, at the 
Poles. Then, with reference to the following diagram, A c B d represent the 
waters, P a Pole of the Earth, and M the Moon. Let the effect of the Moon's 
attraction be conceived to be exerting itself on the waters immediately under that 
Satellite^ causing high water at A, and we shall immediately perceive that the influx 
of water at A must cause a great flux of water from c and d, which flux, or flow, of 
water, if continued long enough, would equally lessen the waters at B ; but, before 
this latter effect can take place, the attraction has shifted its position by the Earth 
revolving from A to d, and the waters at d, being then under the Moon, receive part 
of the waters which flow from A and B, another part falling towards c. The great 
body of water at A, when no longer under the perpendicular attractive influence of 
the Moon, falls nearly as much by the force of gravitation to c as it does by the 
oollateralj or sideways, attraction of the Moon to d. 

Again : let A represent high water of the superior tide, (the tide next ensuing 
after the transit of the Moon,) B high water of the inferior tide, (the tide opposite 
the superior) ; c and d low water and M the Moon. Conceive the Earth revolving 
from D to A : thjen, when d is opposite the Moon, A and B will become low wa- 
ter, c and D high water, d being the superior and c the inferior tide. 

To view the subject clearly two forces must be conceived constantly' in action ; 
the force of attraction which raises the waters towards the Moon or Sun, and the 
force of gravitation which exerts a constant effort to equalise the height of water, 
but with only partial effect on account of the superior force of attraction. 

But this outline of the cause of the GretU Tidal Waves delineated in the diagram 
has to be considerably modified to bring about any conception of the phenomena 
witnessed at different places on the globe^ The actual occurrence of high water at 
differ^it places would indeed agree with the theory were the land only formed into 
two continents. North and South, and the whole of the Equatorial regions covered 
with water, allowing an uninterrupted flow of the element, from East to West, to 
follow the afyparent da£[y course of the Moon ; but as this is not the case , as Africa 
and America, running North and South, are barriers, interrupting the free progress 


of the wave, and as some great seas are in unfavorable situations for reeeiving an 
influx of water from the great oceans^ or for parting with any, the whole theory is 
modified at every locality. In the Mediterranean, for instance, there is scarcely any 
tide, the entrance at the Straits of Gibraltar being small, and the Baltic Sea, which 
is still more remote and separated from the ocean, has no perceptible tide. At An- 
napolis, in the Bay of Fundy, the tide is said to rise sometimes upwards of 100 feet, 
and at Bristol the difference between high and low water is 50 feet. This division 
of the subject is so diversified that every part of the world, every bay, inlet and 
river, might justly demand a separate treatise to account for the local variation of 
height, and time elapsing, between the transit of the Moon and the rise of the wa- 
ters : in this place, therefore, it cannot be attempted. 

In the Nautical Almanac there are directions for ascertaining the height of high 
water at a great number of Ports, but the method exhibited only approximates to 
correctness* To predict the times of high water, and height of the tides, with the 
greatest accuracy which our present knowledge of the subject will permit, requires a 
series of tables depending on the following data, and constructed expressly for the 
latitude and local peculiarities of a Port. 

I. The Time of the Transit of the Moon. 

II* The Moon's Horizontal Parallax. 

III. The Declination of the Moon. 

iv. The Sun's Horizontal Parallax. 

V. The Sun*s Declination. 

The necessary explanations to this part of the subject will be given in the regular 
order of the above numerals. 

I. The time of the transit of the Moon is necessary to help us to an approxim- 
ate, or nearly accurate, time of high water at any place, which we arrive at from 
previous recorded observations. Let us take, for instance, the day of the New 
Moon« when we know that she is passing the meridian with the Sun at noon. A se- 
ries of observations will show us that the tide in the open sea continues to rise 3 
hours after the Moon has passed, and that at any particular l^ort the lunitidal in- 
ervaly or time elapsing between the transit of the Moon and the high water next fol- 
lowing, is always the same on this day of the lunar month, wind and other atmos- 
pheric changes permitting ; and the time when this lunitidal intertal expires is 
called the Establishment of the Port. 

Let us suppose, for example, the ^'Establishment of the Port'^ to be 12 hours 45 
minutes» and that we have a table before us containing the time of the transit of 
the Moon for every day in the month. Add 12 hours 45 minutes to the time of 
transit at New Moon, namely noon, and we learn that the approximate time of flood, 
or high water, next ensuing atler the Moon passes, is 45 minutes past 12 at night. 
After this the ebb tide, or flowing out of the water, commences. 

Between two floods, or two ebbs, about 12 hours 15 minutes elapse at New 
and Full Moon, and 12 hours 30 minutes at the quarters. These effects are 
called the Priming and Lagging of the tides, and are produced by the gremt 
tidal wave being the result of two operations, or , in other words, they are to be 
accounted for by the theoretical existence of two waves, one solar and One lunar^ 
which when they are superposed (brought one over the other) effect the/}ni»tng, 
and when separated produce the lagging of the tide, because their jmnt height has 
its maximum (greatest height) at some point immediately between than, and that 


connecting point becomes, in fact, the apex (top) of the two wares when considered 

as one. 

From a previous explanation it ^11 be seen that the highest or spring tides occur 
once a fortnight. The highest spring tides are due to the Moon being in perigee 
(nearest the Earth), and the smallest spring tides to the Moon being in apogee (far- 
thest from the Earth). 

II. The first correction of the approximate time is for the Moon's horizontal 
parallax. {See paralu^x.) The Moon's parallax increases in amount as she ap- 
proaches the Earth to be in perigee, and this correction is, in feet, one for the in- 
crease or decrease of attraction caused by the Moon advancing towards, or receding 

from, the Earth. 

IH. The second correction is for the Declination of the Moon, (5^^ declina- 
tion), which latter, when compared with the latitude of the Port, gives us the cor- 
rection due to the Moon southing near or remote from the zenith. The nearer the 
Moon is to the zenith of the Port the greater will be the attraction she will exercise 
on the waters, and the tide will arrive quicker and be higher in consequence. 

IV. The third correction is for the Sun's Horizontal Parallax, the explanation to 
which is similar to that given at ii, and the same may be said of : - 

V. The fourth correction, for the Sun's Dedination, the explanation to which b 

similar to that given at iii. 

All these corrections, tabulated expressly for the latitude of the Port, enter into 
the calculations, both for height and time, but the tables for some latitudes scarcely 
need embrace the corrections of the height for the Sun's Horizontal Pandlax and 
Declination, these corrections being too trifling in amount for any practical ad- 

Having thus ^ven an outline of the most scientific method, at present in use, of 
calculating the time and height of high water, it may be only necessary, in fcondu- 
sion, to add that the predictions, when accurately calculated, are sufficiently near 
for every practical purpose, although separate calculators, adopting the same theory, 
may, by the construction of their tables, deviate from each other several minutes. 
The author of this work having constructed a series of tables precisely according to 
the formulce adopted by the Admiralty for their annual publication "Tide tables for 
the English and Irish Ports " was, at first, surprised to find a difference between 
the results from his tables and those issued by the Admiralty, and on comparing the 
tide tables published in Liverpool he found a similar difference between each of 
them, in some instances amounting to 6 and 7 minutes in the predicted time of 
high water. The cause, however, soon appeared to be in the number of corrections 
required, which, if estimated in minutes only and not in fractional parts of a minute, 
would easily permit a number of small differences to creep in, accumulating to sev- 
eral minutes. The following is a specimen of the calciilations, from four hands, 
of the time of high water at Liverpool. 


p.M P.M. P.M. P.M. 

H, M. H. M. H. M. H. M, 

19 24 19 17 

56 11 55 54 

1 32 1 38 1 31 1 30 

As the theoretical eonstmction of thi^tables may be presumed tg be similar in all 
lour instances these results may be consideied curious* 

62 TIME. 

Time. Time is divided into periods, cjcles, years, months, weeks, days, hours, 
minutes, seconds and fractions of a second. A Grand Celestial Period, or Platonic 
Day, consists of about 25,800 years, during which takes place the Precession of the 
£quinoxes. (See precession). A cycle of the Sun, or Solar cycle, consists of 28 
years, at the conclusion of which (with an exception on account of Leap year, see 
bissextile), the days of the months return in the same order to the same days of 
the week as in the previous cycle. A cycle of the Moon, pr Lunar cycle, (called also 
the Golden Number^ as deserving to be written in letters of gold), .consists of 19 
years, after which the New and Full Moons return on the same days of the months 
as during the previous cycle, but 1 hour and 28 minutes i^ooner. There is an ex- 
ception to this rule respecting centesimal years, (years completing a century). The 
two last mentioned measurements of Time are among the six cycles in the Nautical 
Almanac. The other four are, 1st., the Epact, 2nd. the Pominical letter, 3rd. the 
Roman Indiction, and 4th. the Julian period. 

I. Epacts of years and months are terms applied to th& liifpon's age on the first 
day of the year and the first day of the month. The Epact of a year is a number 
expressing the excess of time in the Solar above the Limar year. The Solar year, 
or time the Ea^h occupies in making pAC complete revolution over its orbit round 
the Sun, is 1 1 days longer than the- Lunax year, or time occupied by the Moon in 
making twelve complete revolutions round the Earth. On the first year pf the Lunar 
cyde the Solar and Lunar years commen,ce together, (thatis^ the first day of the 
year is also the first-day of the Moon's age), and the epact is called 0. On the se- 
cond year of this cyde the Lunar year has. commenced IT davs previous to the 
Solar year, (that is, the Moon is 1 1 days old on the 1st. JT^i^ry)^ .$nd the epact is 
called 1 1 . The third year the epact is twice 1 1 =: 22 ; the fourth year, 3 X 1 1 = 33, 
but, (deducting 30 for one montjii .completed), the true epi^ct is ^caU,ed 3^ and so 
on to the end of the «ycle. The^paqt of a montn expi^.e^ses ^the ^oq^'s age on the 
first day of the month. The. epact of the month being IsQoynij the M9on*s age on 
any particular day of the mon^th can be easily aacextained. 

II, The Dominical Letter is a. letter answering to the ^st I)oj{iinus, pr Lord's day 
[Sunday] of the year. The seven first letters. of the alphabet, bging applied to the 
seven first days of the year, the letter answering to the first Sunday is the dpmini- 
,cal letter of the year. If Sunday be the first 4ay of the y^r the dominical letter 
for that year wiU be A ; if Monday be the fir^t^day, the (femii^cal letter will be G. 
Qut in Leap year there are two dominical lettws ^ed,.pai9.ely;» pne letter found as 
above, to be used only during January^md Eeljyuiarj;, jmd the ^ext j^revipus letter to 
be U3ed during the remainder of the year. The .Qf the year 1844 (a Leap 
year) happens on a :Mond4iy and the doioinical letters ,are G.; F. ' 

XII. The Bpman Indiction is a cycle of 15 j^eps hy -^ich ihjs^ ^mp^i^rprs of Rome 
ordered public acts to be .d^ted. The Poxiiitf j^jPQjpe) ^conti^^ic^ th(^,use pifit. 

IV. The JuUan Period is a cycle of 7,980 ye^rs,'^ made Jby,^rftfpl^g the cycles 
of the Sun, Moon and Bpinan Indiction together, 28xl9xlS =7^966/ 'fins 
period is found by* adding 4^713 to the year of the Christian era.' 

The three last articles aire not used in modem Astronomy ; but bdna; found in the 
Nautical Almanac an explanation maybe desirable, to remove any expe^tion of their 
utility to the nautical student. We now proceed Ifp explain Astr<^omical, Civil 
and Mean Time, and Hour Angles. 

An Horary Circle is a gircle ofany conea3rabkjSi8se,.bfti[i9g:;ei^h^r.Qf tJkQ ^P^lesof 
the Equator for its centre. When we:make.the South £ote.^jD^MKi9f:ttbilimcIe 

TIME. 53 

we read the hours from left to right as on a watch dial, but when we have the 
North Pole for the centre the hours are reversed and we read from right to left. 
To prevent confusion of the terms Horary Circle and the circle of Bight Ascension 
(both being marked by hours, minutes and seconds)^ the student must be careful to 
identify them as entirely distinct ; Bight Ascension being measured by the division 
of the Celestial Equator into 360° or 24 hours, commencing with the first point of 
Aries, (which in this place we may consider as an immovable point in the heavens), 
and being reckoned from" West to East, or the contraiy way to the apparent daily 
course of the Snn, whilst the Horary circle is moveable and answers to the 24 
hours of a Solar day, the point on it marking noon of any place being precisely on the 
meridian of that place, and the numerals marking the hours rising from the East 
and falling towards the West like the apparent course of the Sun. An Hour Angle 
or Horary Angle, called also meridian distance, is an angle contained between a Pole 
of the Equinoctial, (the North or South Pole), the meridian of the place of observa- 
tion, and the celestial meridian of the objeet to which the angle is referred. The 

accompanying diagram represents an Hour Angle from the North Pole, where the 
hours are read from right to left, (the West being' to the left). The Stars A and B 
have no hour angle, their celestial meridian being represented as coincident with the 
meridian of the spectator, but the meridian of the Star c makes an angle with the 
meridian of the spectator of 6^ W. (6 hours West) and has culminated (See culmi- 
nation) 6 hours previous to the Stars A B. The line, or radius, from the Pole, 
or centre, of the Horary Circle to the circumference, passing through a Star, ia the 
celestial meridian of that Star. 

For the explanation of Sidereal, Solar and Lunar Time, we use the accompanying 
large diagram, representing an Astronomical clock of a novel character, the circular 
dial of which, having the principal Fixed Stars of the Southern Hemisphere repre- 
sented on it, must be supposed to revolve once from East to West in 23 hours 56 
minutes 4 seconds of mean Solar, or clock time. This revolution will truly describe 
Stdereal time, or that apparent daily revolution of all the Fixed Stars which is owing 
to the daily revolution of the Earth on its axis. The dial has represented on it the 
two great circles of the Ecliptic and Equinoctial, the months and (is supposed to 
have) the days of the year. On the EcHptic is marked the twelve signs of the Zodi- 
ac, and on the Equinoctial the degrees and hours of Bight Ascension. (S^ee right 
a^scension). There are also two hands proceeding from the Pole, or centre of the 

TIME. 65 

Eeliptic, to describe the motions of the Sun and Moon on and near the Ecliptic, the 
Sun being always on that drde, and the Moon never distant from it mudi more 
than 26^. The Solar hand, S , which makes a daily revolution with the dial (or 
sphere of the heavens) in the direction of the hours surrounding the dial, will de- 
scribe a Solar day, or the apparent daily course of the Sun over the Earth, from 
East to West ; accompanying the Fixed Stars to a certain extent, but having an inde- 
pendent daily motion fh>m West to East, (in the direction January, February, 
' March, &c.,) which will cause it to occupy about four minutes longer in revolving 
firom noon to noon than the time occupied by the Stars in performing the same re- 
volution. This small independent motion, accumulating day after day, will cause the 
Sun to advance in the Ecliptic at the rate of one twelfth part of the circle of the 
Ecliptic in a month, or entirely over the circle in a year. When the Sun has arrived 
at precisely the same point on the dial froin whence at the commencement of the 
year he set out, 'the Sidereal year of 365 days, 5^ 48™ 10* is completed. The diff- 
erence between the Sidereal and the Solar, or Tropical year, (the latter a year of 
four complete seasons), is only 20°* 20", the Tropical year being 366 days, 5^ 48" 
50". When the Sun arrives at either an Equinoctial or Solstitial point he finish- 
es a Tropical year, and when he arrives at the same Fixed Star from which the year 
previous he set out, he finishes a Sidereal year. The AnomalisHe year is 365 days, 
5h > 13m 49«, The Tropical varies from the Sidereal year by 20" 20», a quantity 
equal to the recession of the Equinoctial point, (See precession) and the Anomal- 
istic year has a still smaller variation of 4" 39% being the difference between the 
completion of a Sidereal year, and the arrival of the Earth at its perihelion (nearest 
point to the Sun) from which the previous year it set out. All these data are 

in Mean Solar Time. 

The Sun appears to make 365 revolutions over the Earth while the sphere makes 
366 , but at the conclusion of the 365 Solar days, [say at noon,] the Sun has not 
arrived at the exact point of the heavens whence he set out at noon the 365th. day 
previous, but will occupy about 6 hours more to accomplish it. We therefore say 
there are 365 j- days in the year, and nearly every fourth year (See bissextile) we 
add one day to the calender, called an intercalary day, so that our calculation of a 
Tropical year may be kept correct. If this regulation were not adopted we should 
advance about 25 days every century in reckoning our seasons, and in 700 
years Spring would not commence until September, nor Summer until Decem- 

It will be observed that that part of the Solar hand of the clock which represents 
the Sun will always be on the Ecliptic, and twice a year also on the Equator, the 
yearly motion being oblique to the Equator. The Sun will be North of the Equator 
from the 21st. March, or the Vernal Equinox, to the 21st. September, and South of 
the Equator from September to March. (See seasons). It wiU also be observed 
that the hours are marked from to 24^ an Astronomical day being measured from 
noon to noon through 24 hours. Those points where the Ecliptic and Equinoctial 
intersect each other are the Equinoctial points. The point of intersection in March 
is the first point of Aries, from which the Eight Ascension is reckonedon the Equi- 
noctial, and the Celestial Longitude on the Ecliptic. The Solar hand in the dii^ram 
shows the month to be December and the time of the day noon ; that the Sun is in 
Yf Capricorn in R. A. 18^ or 270°. A Solar day is not performed in the same in- 
variable time, like a Sidereal day, [the apparent daily revolution of the Fixed Stars, 
which is perfectly uniform] but the length of the Solar days throughout the year is 

56 " TIME. 

t w » i h ^ * I 9 i 1 * 1" T V ^ g ' " • » t. ' .   a ;; '■ : * '  .";  '■   )  ■* !■■  p '  m  « *■  j i n m 

v^miB^Mtli owiiie^tDtiii^dliptkai fond of the aiibU of tlie Earth (which ouiMi 
the Eai^th to vary in its distance .fiom the 81m 3 inil]ioii8.df Bules)^ the obliqwtjr of 
the£diptie» {Sh fiE^AOKtf) and the variaticm \m the obhquity of the Eeliptic. [See 
onutaiiltt:.) A calculation for the meqnaHty in the length of solar dajs isins^ted 
in thb Nai|tk»l Ahnanacnader the title of the Equation ^ Time, The caleidation 
ia pf ft '4jiQBiaiitf which added to^ or subtracted from. Apparent Time makes Apparent 
h^ Mean Timiitt €i Mean into Apparent Time. Apparent Time is reckoned from 
the> tramit of the Son .oTer the meridian of any plaee, and b the unecpial time of a 
a4K)laf dffjT* -A Son dial describes Apparent or Solar Time« To fiuaUtate the men- 
tion of Mean Tixne in certain cases Astronomers imagine a ** Mean Sun " ttaveisiiig 
the heavens, and describing Meaiv or average^ Solar Time. What is.meant» for in- 
stance, by the instant of the Mean Sun being on the first paint of Aries is, the is* 
stant that the True Sun would be on that point if the Sun kept eipaJ time. Mean 
l^ime, then, is an average time deduced from all the unequal lengths of the selar 
days in the year, and is ike standard of the measorement of Time by dock work. 
Examples in the Equation of Time:- . . . 

I. ,0n the 1st. February .1844 the Sun will pass the meridian of Oreenwiph .13°^ 
49' ;76 (13 minutes 49 seconds and. 7^ hundredths of a second) after the ^^ Mean 
Sun ", or irfter the mean noon as shown by a well regulated dock. The time of tcan- 
sit of the meridian by the True Sun is the apparent noon, and the Equation of Time 
(i3°* 49* *76 according to the precept in the Nautical Almanae) has to be added 
to this noon to convert it into mean noon. 

Ex. II. The transit of the Sun over the meridian of Greenwich, on the Ist. No- 
vember 1844 will take place \6^ 17" -23 previous to the "Mean Sun '*, and 16°» 
17' *23 will have to be subtracted from the Apparent Time to convert it into 

The second hand of the dock depicted in the diagram is to describe the revolu- 
tion of the Moon, as seen from the Earth. Like the other hand, this is carried 
round from East to West by the daily revolution of the dial, and it also has an in- 
dependent movement urging it over the dial in a contrary way to that of the diaTs 
revolution, or froin West to East, by which it passes round near the Ecliptic in 27 
days, 7^ 43™ 5% which is called 2k periodical month, but as. during this time the Sun 
has also l^en advancing in the same direction, (West to East,) the Moon occupies 
29 days, 12'»44™ 3" in performing a revolution from one of her conjunctions with 
the Sun (the time of NewMoon^ to the next conjunction^ This latter ^period b 
called a synbdicdl month. The Lunar hand in the diagram shows the Moon to be 
in or near II Gemini, and in Bight Ascension about 3^, or 55^. 

It innst be wdl borne in mind by the student that the movements of this clock 
^ ouly represent the apparent revolutions of the Sun and Stars. He must remember 
' that the Stars and the Sun must be considered as having fixed places in the heavens, 
that their daily transit over the Earth, from East to West, is owing to the revolution 
of the Earth on its axis, and that the yearly p^issage of the Sun in a contrary direc- 
tion, from West to East, over the Ecliptic is due to the revolution of the Earth in its 
orbit round the Sun. The Moon, however, is actually passing over the Earth, but 
in a direction contrary to her apparent motion from East to West, tn reality she is 
proiceeding swiftly from West to East, her apparent daily transit from East td West, 
like the apparent daily transit of the Sun and Fixed Stars, being the effect of the 
Earth's rotation on its axis. A Lunar day is the tune elapsed from the instant the 
Moon leaves the meridian of any place to her return to the same point tfgain, the 

TIME. 57 

I ^1  !!■■  ^i»<— 4»..*— iM^— ■— ^ — ■Ill I I . I -I   II m Will  — mMM—  

next day. This iime is more variable than that measnred by the apparent passage 
of the Son over the Eatth, but averages 28^ 48°" 46* of Mean Solar Time. 

Greenwich Time> or Greenwieh Date, is tihedate, or day of the year, and the 
exact Mean Time at Greenwich when placed in comparison with the exact Mean 
Time at some other place. 

The Astronomical year commences on the 1st. Jannary at ^oon^ twelve hours 
-aUber the commencement of the Civil year, which is reckoned from midnight. During 
a voyage ronnd the world, or only over half the world, a curious effect of Time has 
to be allowed for in the calculations of a navigator. As soon as he passes longitude 
180^, (precisely halfway round the world from Greenwich,^ bis apparent noon will 
be simultaneous with the midnight of Greenwich, and his Astronomical day will 
have to change its term, according to his having proceeded to this longitude from 
the East or.from the West. If he sailed easterly, or the contrary way to the appa- 
rent daily pro^ss of the Sun over the Earth, Lis time will be twelve hours in 
iulMnee of the Greenwich time, and if he sailed westerly his time will be twelve 
hours later than the Greenwich time, and he will have to change his date (the day 
of the year according to his log book,) by adding to or subtracting from his previous 
date twelve hours, so that tiie d^te of his noon may be of the same term as the date 
at Greenwich. Suppose, for instance, a navigator has sailed easterly from Green- 
wich, and on the 1st. January, (according to his log book,) he passes from 1 79^ £. 
lon^tude to 179^ W. longitude. His noon will then be 12^ 4°* in advance of 
Greenwich Mean Time, and both his astronomical and civil date wiU be different to 
that at Greenwich. For whilst his log-book has reckoned his time as noon of 
the 1st. January of a new year, the time at Greenwich wants 4 minutes to the previ« 
pus midnight, tiie completion of the old year. Civil Time ; or 12^ 4™ to the comple- 
tion of the old year. Astronomical Time, and the date at Greenwich will be 31st. of 
December. On the contrary, if the navigator sail westerly, and pass from 179^ W. 
to 179° East lon^tude, he will have lost upwards of 12 hours on Greenwidi Mean 
Time, and the midnight of his 31st. December will actually be the noon of the Ist.^ 
January at Greenwich. Without care, therefore^ in altering his date after passing 
the 180th. degree of longitude the calculations a navigator would take out of the 
Nautical Almanac would be erroneous. Navigators making a voyage round the 
world will either lose or gain an entire day from the time of their setting out, accor- 
ding as they proceed easterly or westerly. And as an entire circuit of the globe, 
or tiie complete circle of longitude, 360^ from any one meridian to the same again 
is equal to 24 hours of Mean Solar Time, so every degree lying due East and West 
is equal to 4 minutes. It is noon at Greenwich 11°* 55" before it is noon at Liver- 
pool (Longitude from Greenwich 2° 58' 55" W.) ; 25°» 22'» before it is noon at Dub- 
lin (Long. 6° 20' SO^W.) ; and 4^ 56"» H" previous to the noon of New York, 
(Long. 74° 3' 31" W.). It is noon at Greenwich 19" 53» later than the noon ot 
Amsterdam (Long. 4° 53' 15" E.) ; 2^ 1°* 10* later than the noon of St. Peters- 
burg (Long. 30° 17' 33" E.) j and 7^ 32» 56» later than the noon of Canton (Long. 

Mean Equinoctial Time is the Mean Solar Time elapsed since the Mean Solar 
Time of the Yemal Equinox. [See seasons]. The instant wh»i the ''Mean Sun'* 
arrives at the Yemal Equinox it wiUbe on some particular meridian, and the Equi- 
noctial Time at places under that meridian will correspond with the Solar Time 
throughout the ensuing Equinoetiid year, while the Equinoctial Time at all other 
places will be quantities oorresponding to their longitudes frron the meridian at 

as TBO. VIR. URA. 

iR^ueb i|i0> Meaa \iisroti EqpNnoK iook ]^\9Mk B^^f^iim^ SinnV fit the ^emmfm 
of the nei^t VtBnti Skpism ift ^ith^ meridifla tbmt 89? fttrftiar tor* i^: ws(fiwr4* 
tfaefmiinuil vev^latioiia of ibe. .Simi iiviing tiie Eipuno^liBl jr^ar hemg ,3(*& 4^& 
•2412217 (3^d: 4qrt u4 249217 frftctiotw ^ «. iii9}i«^» Tfap fifi^iieoa^) 'Sim 
is then reckoned from that meridian. Examples :- The ^'UmASmf^ BktiM T^tfmw 
Umh 22nA. 1841 is <mt]i« tomOiw 4^ 34! W 'StStW^ of <^^mm^ mik.ibfi 
fniotM»n of the ]SqK»oqtkl Tiaae^^ Oraeufri^ f^ ei^^ihgr-t^nfimmfyt t|K^^«|it- 
siiii^ Bqmooetid^yfW, '809580^ At th^liqim^JIbetiih '']Mt4|i 

Sob" i^i on tba meniim 10^ ^ 4![ 'h& WtH-(£ (^nemnAm^lMimti^^ 
£qi|iaootial Tiaie fyp Qn^tm'vk^htwBin^ 'J»^7^m^ of'U%%\7 Im tlM^ ttoi of tin? 
Pluvious 3mir« At, t^e JBqimosrof Maidi 21Mr. 1843 ibf &M]«fti.ift 'iW^ 
('J242217 1^ dum 4ie:pr^('kHiSrfTaclion9>tlie itmw^ ^m^i D^fMsbii^ 7^ 

48f 7^ *9S iSul <rf^<Sf>e^wiKih| Aod'en Mnreb 21^. 1844 mtm6Mi9t ^08282^^ 
(-24221 7i^^aiii).tlia m«fidte of tiie Vmial Eqsuii^s^bmg !>" SS^ 20^' '4ft)fi^ 
Aftw th4i }re«r tbe Vtfimit^'^glm^i^ ^]Mri4i«A/ti^4iiul^ 9W<Nf;£lf»^r 

iri^h^' Theutiiify of£qw»»ti4ll^)N^ As««9i^ 

ngi^Sk but it is.]^ xftiMbiiiMdi 

T&iMsnv Fusioigorer; or tauten Wken^oetestisl^bedf app^aM>to'crMB4lie 
diseof.tbB8im;or>«nir'Of tbe^tittttiy 80t*Aft< sr^VfiM))' or^ to^ ereib 

.the metidittB,! or the rptitxie -v^KJioalj it ia> ^idMi & tnmsK.^ (fi^^ : AfistM^ara^ G«i.iif «• 
HAjTUMf mnd^ MifikittfAM;): ^b* IMWMff 4^fM^jfir9tfpoiHi i^Jriea is a tienn^ a^^pWS 
to tfaaiBSlant when tlMttpncdtft^pdlttt of tbeh6arre(B8'Whete.tii^ i!<il(>iie^8nd'£4»i* 

^Aiiaotmt die eateulstfen^f tbt^ tM&ste is f^ tb^ m^tidiaa 4>f :>G)MsiMriebL liife 
^&teKff>(/kt (Sbft#/fifi^iis<»t«^)«i9ageoTeii^-lt9.priuaiyPlSiMt^ i|S^Meft^irom4il»'Sftiili^ 
as Jjht drsAsfitst of^Japker^ft ISbiM^M oi^-tbe diso^if Oi^ilw^ 

• ¥tN0Si • S^'e^ B&Uktt fiird^EsM. 

Vl AGO, ' (l^e >vvt^j . tW s^ ^f tiie IkfBttc which #te Sim ^t^s abM^ the 
2drd. of An^fia^dteai^aboatthe 22ndi of Septcfmber, IHhefoBbwiMgfiAerbe 
tjomsiitted to membrf th67i]ifff-{>mre oonVe^efnf for cafiing to- mind thddi^s 'of 
'^ months on whidi the Sun estters i^e signs of the Zodite. 1^ nkontfas ^mKy 
^aeiily be-^und by remembering tSiilt (Aries answers io Mftrch^ antil; the otSieriSgHi 
^ liieJo^ev^moAthsinsaceesstmi^ftiDm Ariesaad Mardi* (iSte page5,'inwMdH;he 
isi^8> are pkeed' iieco»Inig to ' thar 4M^der ft^ 

Niiieteen days forethe number for Pisces, 
Tw^tpifor^nitim^ and AquariuAy - 

Tnbilil; Oefiinii Oawcr and Ams ... 

And.Cfpiicorn^Sf em^ b«va tMrnfifitwo; 
And to the others twenty three are due. 

l^KoaRAw Y^ TbAt •d^p%r(;«ie^b of tb& • sci^aoe ,of > Aatomosq^. wH^ teiicbe^ 
tb^,frrtngwepMf^H9?4i|^'W4^ tbo oidUienieiiaia ^M^d&.of irodciiig A^t/r^ 

WmB&. The siOija^D&lte •kdl'iir^MMlOHtt^^ 
dqp««d^ in a gsdaAiiMBffm, ofi^Ae^iiAiefSMslift^Md MiddnMliatt^tli^^ifajK 



Arid bf Ae netion «iid'pBHial absenee of the •riarhq^. »^VV3i«a'» pwrtkia of tbe^at- 

atempbere beDottes lirefied by tbe-tolar heat to as* to atvixd, i or^sJdfteed'faj oold 

'90 tat i»'dnem^i a eoimier conent take* plaoe in another part. HHifln thr ivnnd 

Mwa H is m^M^ tofiU up a partial vacancy 0tyiaiamuttiaiai.i^sAtakt port of the •at- 

ii»apkttQei<«Qd(a»i^e4liiiiis at 6i]e period of diB yaar.NoiUL o£ihe:Eqiiat(lr,»ancl at 

• aaottifir Aoalli ttf it, hetia thd immediate caase«f jthe:£eriodioal Mm^^mhixAi'mmy 

b^'tbasiiefin^t'diiibg tiie montls 6f May^ ^tee^ Jviy^ AaigRat:Biid-8e]M:embcr, 

) [titer Ster being Naettk'bfilK&Silwitoi;] the wind- hkNnra' firom^tllct ftmtb, (vfaem.tbe 

!jdtiaH*OM | > MtttiM^y coiaden8ed by tbetibaenoe^rf ; add 

dnr^B^rtfieieiMindtor of tte jreai; the Sim being! «onth/o£iherfiqttator, the Mirien- 

«ed ai^o£4be^NcM;lL^U4iiiia towaiftla/the melied atiDMphere'iaf ^tbe Scptiu s&&me 

- dajFk ^M(MPeranAal»»'lilie«baii0e> happeningr«bent :tbe[ 21tt.*«f IiiiaBcheand.2dlh^«f 

•6e|ileihberplte»v6|iftn9iiearrtbefE4a^ to.eiifaas)TldaUedNiyiMildt^ 

tapttitienBt SwOvoMk 

Vnteift^planiitienafiiMdatfily fte^^fintf^itaal'Wftvi'of ABf«8tronanMl(caanecof 
'4hflF!t«(iestBal!irifcids, anilUt i«ew )ida taWiuBB^dialriytiiMiidfedoby tke 
v«Mm'tfaift4feifiaith'isconiaQ0niidly re^ .irinis 

aroaiai'iMtaaHy«{ho.TQ«iU of^tthe raie&ctiiiia of -the ^atmdtpheie byr^tiieiacui^.hvt a 
^[iiBath^''tMbBAj^yiio& a/8eitth<^astad7 

'«Mbat tbetSanth ; )the ^ianiifilBg» &mm, Abo-fiim iMowiog his: coniaef from ^^aat to 
flMMMifed^themi]3tt:iii60&nanrin^ that dinedioni to^lfilLiap ifbe pKttial tacanoy voau- 
wL'l^ tiie difllnd saMfinttoii* 

•rShe «^<Benoe'ofiiaf%8toQ»ian8tniil»9B».thAttheifr^^ 
(■JBiir0niine'a|p|ttoach the Sqnatfnr,^ and/moie 'lalaaUeras tiveirc^dedeliQm^ tonaards 
die Foka. In certain parts of the gloteaaiConstentaoe<th0rtiBdsi;^hAtvth€^are 
i/m»edLibf^^per»Mnent or trade .winds from Uowiog. always ^)early,iii'.the,^an^ direc- 
rtion In tl|.e Atlantic and Padfic oqean?, ^^^^er a region extending to 28° on each 
side the ^q uator^ the wind is' almost always easterly. Farther to the northward the 
wi^dapnncipally vaiy between the North and East, and farther to the southward 
the winds.gradually become more soatherly as we ascend towards the South Pole. 

In the ten^perateaoiies, where the Sun, has, not such an imn^ediate influence as at 

ibejl^natonal ^r^ons, tho'iwds are so Tariable and capricious as to render expla- 

oiMaoyi totally, iijcipoasible^. and the connee^on between the solar influence and the at- 

yaoapheie fBijpp^rs'iO:he lost* 'Connected with the subject of the* winds may be in- 

>t90^iiQad the theory ovt which' that TslaaUef instrument the barometer is constructed. 

vAi>biionlflir^a' laaehinetfcr testing Ae density and elasticity [or rarefaction] of 
lAMi4tDi08phMi^ 'In other' words* it is/ainadune by which we measure the prepare 
Mofdveair^onHie 'Earth. ^Uteiair.wn^hnHithe, like water or any other fluid, is of a 
<>4ertilin.spedfic;gia?it7»or'Weig^9»and it ^ia found that a column of it, an inch 
square and reacktog'ftodi tIterEarthivp tothe highest donceivable point of the sky, 
^,atmo9pber^ haB^ictuaQ^a specifiq gnmty of fiteeuipoMnd^ saad a pressure to 
,ihat extent v^ themefor^, .contmually exerted on-evaiy aqnare inch of the .Esrthfs 
. 4B«rfiiQe. This ^ped^ gravity is equal to that of a coUmui of water an inch square 
and 33 feet high» or of a oolunm of mercury, of the save diameter, 29i inches .in 
heigjit* A tube, therefore, to contpdn.a quantity of water which would be svpport^ 
by the atmospi^ere pressing on its lower extremity 'would have, to lie.neair4Gft. h^, 
4Hid a tabe for the common barometer oontainhig mercury is- 34 inches inJMjgfat, 

In cafan weather the^atmosphereia denser, >or heavier, tlian at any othaF.tiia^.b&- 
canse Ae particles eomposmg the air, being thenin annDdistArbed states lie ^j^r 




and are in a greater quantity in any given space, than in wet and etormy weadier, 
when the air being a^tated is spread over a larger space than that it otherwise 
occupies, and the pressure on the Barth's surface is consequently not so great. In 
cahn weather, then, the atmosphere is capable of counterpoising or supporting the 
greatest quantity of mercury, or other fluid, placed in a machine so as to twAvb the 
atmospheric pressure, and when there is rain or wind it will support the least quaa* 
tity ; it is upon these £EUSts the utility of the barometer is founded, as a weather 
guageii As the atmospheric pressure increases the mercury is forced upwards in the 
tube, and as the pressure decreases the mercury falls. But a plainer explanation 
may be afforded by the common ghssfountatM, used for bird-cages, in which we 
see a quantity of water supported in a vessel by the pressure of the air on the app- 
erture at its base precisely in the same manner as the support of the mercury is eff- 
ected in the barometric tub^. The range of the barometer, in England, is from 28 
to 31 inches ; in other words, the atmosphere is sometimes so dense or heavy that 
it will balance or support a colmnn of mercury 31 inches high, and at other times 
it is so expanded or hght as to be only capable of supportii^ 28 inches : the mean 
of this variation, namely 29i inches, is marked "^^dumgeable" on the barometric 
scale. The range is least at the Equator, where the marks on the scale ''stormy" 
nnd ''very dif' are of no utility, because the mercury never fiiUs so low as to reach 
the first of these terms and never rises so high as to point to the second. For those 
climates where the utility of the mercurial barometer is affected, and indeed in all 
situations (such as on ship-board) in which a great nicety in testing the state of 
the atmosphere is advantageous, an oleagmous (oily) instrument called the sympie* 
someter is preferred, the most modem and improved form of the instrument being 
that invented by Mr. Cummins of London, 

Zenith. That point of the celestial sphere immediately ovet-head at any place. 

The Nadir is that point of the sphere immedi- 
ately opposite the Zenith. Zenith distance is 
the apparent distance of a celestial body from 
the zenith of an observer, and is measured on 
an arc of his meridian from the zenith to the 
horizon. When the zenith is North of the bo- 
dy the zenith distance is called North, and 
when the zenith is South the zenith distance is 
called South. The * |, in the diagram, is 45^ 
South of the zenith, yet its zenith distance is 
called 45^North, the zenith being to the North 
of the star. The * 2 is 22^" North of the xe- 
nith, yet its zenith distance is 22i^°.Soath, the 
zenith being South of the ^tar. 

Zodiac. A broad belt, or space, in the heavens, 8° on each side of the Edipdc^ 
and, consequently, 16° in breadth. There are 12 constellations of Fixed Stars in 
this belt which give their names to the 12 divisions or Signs of the Zodiac, the first 
6 of which, r Aries, Taurus, n Gemini, S5 Cancer, iXLeo and ig? Virgo are termed 
boreal or northern, because the Sun when in those signs is at the North of the 
Equinoctial, and the last 6, £i Libra, in.Scorpio, ^Sagittarius, YfCapricomus, rr 
Aquarius and K Pisces, the austral or southern signs, as they are South ef the 
Equinoctial. All the Planets (with the exception of the Asteroides, or telescopic 
Planets^^ make their excursions within the Zodiac. " 




39 South Castle Street^ LiverpooL 

E8TABLI8HBD 1770. 






have constantly in store^ for wholesale and retail demand^ 
every article connected with the ahove branches of trade. 
Chronometers Repaired and Rated by a Transit Instnunent. 
Second-hand Chronometers, with good rates. 




M ^ P are now prepared to execute orders for the above, 
and warrant iheir accuracy in compensating the magnetic in- 
fluence of Iron craft on the compass needle. 

The appearance of this Binnacle is octagonal, sormounted 
by a handsome brass skylight containing a himp. The size in 
diameter is 2 ft., and in height 2^ ft. Price, complete in ev- 
ery respect. Twenty Guineas. 

Agent for the Binnacle, in London, Mr. J, C. Dennis, Opti- 
cian, 118 Bishopsgate St. 



The Patent Mineral Sympiesometer has now been in use 
in all climates, for a considerable tirne^ and in no single 
instance has it been known to fail. It gives to the Mariner 
perfect indications of the slightest change taking place in 
wind or weather : not like the old sympiesometer, continually 
causing^ doubts in the mind of the observer by false rising 
and falling without causey it will* in all temperatures, give the 
true barometric state of the atmosphere with the great adviin- 
tage of showing the variations much sooner, while the instru. 
ment is not above one third the siie, does not require to swing 
in gimbals, is not the least affected by the motion of the ship, 
requires neither cork nor stopper to prevent the fluid from 
coming out when carried^ will keep in repair a length of tune 
and the fluid will not evaporate or congeal. 

Made and Sold by Charles Cummins, Chronometer Maker, . 
148 Leadenhall St. London. 

Agents for Liverpool, Mellmg ^ Payne, South Castle ^t. 




2B, King Street^ ClerkenweUf London. 

¥tma CAPTAIN BEAUFORT, Hydrosimhtf to the AmiralU.— 1831. 

^ Ton bare done me the nonour oi aaking my opinion orvDor Patent Loff j I Iibtotio hadtation in xvpljing 
tihat it is a ntoat Talnable iniitnmiflnt, and if lued along with Irofeaeor Barloirs correction for the local attraction 
of tkkB CompaaBy a ihip's reckoning would approach yerf nearly to the troth ; a large proporlion of the rappoeed 
ennenta in the ocean wonld diaappear, and thoee that do exist wonld be deteinuned with predaion.'* 


**D«ep as the water is to the northward of this dangerous reef, (Green Idaad ReeO^here ii no other guide, ina 
thickfoff, wban the light cannot be seen, but the ■oondingi; yet it wUl nerer do-to loae command of the TeaMl 
by ronndiBff to, in the ramd ebb tide, (which lefai np<m the rea at the rate of five knote) for the pmpoae of getting 
bottom in tlio Usual way by the common Deep Sea Lead. Here, then, it is that MA86ET'S Patent SODNDINO 
Machink becomes ofinraluable service to the seaman, enaUinghmi to obtain correct soundings despite of the 
rapid tide« and without interfering wUh the course and rate of the Teaael,— ^unwy qfthe Biwr St. Lawmen,' 

Printed fbr the H^drographer'a Offict. 

Copy of a letter from CAPT. BASIL HALL. R.N., Extracted from the Tunes, March 23, 1S41. 

To THE Editor of the Times.— &, I feel very desirous of calling the attention of shipowners, shipmastersL 
nnderwritera. and all other persons interested in the seeurxty of navigation to an instrument of long-tried and 
well-eiitablisbed utility, but which, in the merchant senrice at least, ii Tery rarely used, and searoely at all 
known, exeept to the most educated and intelligent comnumdeis. 

I aUode to Maiaey'a Patent Sounditt: Machine, which I do not hesitate to say ii one of the most usefial instra- 
menta ever cmtployed on board ship. jNothing, indeed, seems more unaccountable than the feet that any ship 
shonld be allowea to proceed to sea widiout bdng fnnuahed with so cheap, so ample, and so infallible a means 
of aaocntaanini^ one of^the most important elements in the practice of nsyigatlon, an element, too, which by any 
other method it is generally difficult, and often quite impossible, to obtain with the required degree of accuracy. 

Ev^ery one can understand that the depth of water on such dangerous coasts as Uiose of Great Britain and Ire* 
land is of much value in the navigation of a ship, especially in dark winter nights, or foggy weather. But it 
may not bave occurred to persons who have not ccmsidered the sntject praeticalfy, wat the ** aoundinjgs," as they 
are technically called, owe the whole of their value to two material dreumstaaces, only one of which is taken into 
aceonnt. Tae first is, a oorfeet knowledge, from actual survey, of the depUi of water on all the different parts 
of the eoasts; and seomdly, to the fiMuity and accuracy with which the navigator can measure the deptti of 
water firom on board his ship. 

It is qnita obvions, that unless we possess charti on whidi the soundings are correctly laid down, it is of no use 
to detennine the depth of water when making a voyage ; but it surely is as obvious, or ought to be so, that the 
best charts in the world are uselesi, unless the navigator has the means of measuring at any moment dT the day 
ixt night, and in all weathen, the true depth of water in which his ship is sailing, ft may be said that ineocrect 
soundinn with correct charts are worse than ussIms, inasmuch as tney must tend to mislead, and thus nmch 
of the rtaentific labour and expense which are bestowed on our great national surveys are wasted. 

It is perfectly well known to every practical Maman, that when a ship is going through the water even at a 
moderate rate, particularly if the nignt be dark and rainy, and the water not very shallow, it is the most difficult 
thing possible to get a thoroughly correct ** cast of the lead;" and if tfie depta of water be considerable, and 
the wind blowing hard, with a high sweU, it is always a mattOT of great uncertainty, even when the ship is hove 
to, and her way as much deadened as is p<Msible. But there arise continually cases in which, thoush it be highly 
important to ascertain the true depth of water, it is so inconvenient or dsngerous, or both, to heave the sh^> to, that 
eitaer no soundings are taken at ul, or a most incorrect, and therefore a mischievous, determinatioa is come to. 

Maasey*8 sounding Machine (as I can testify from having used it in every part of the world, in all weathers, and 
at all depths) nvss an exact measure of the mpth of water, evenOuragh the ship's wa^ be considerable, the night 
as dark as pitch, and the swdl very high. With moderate care the results are not only infellible, but the treble 
of using the instrument is not one whit grMter, and vcvy often much less, than that of heaving the lead in the 
ordinaoy way. In bad weather, when, be it remembered, we are generally most anxious about our soundings, it 
takes a longer timeMUid employs a greater number of hands, to heave the ship to, in order to get a good cast of 
the deep-sea-lead. This, in fruit, is so serious a consideradon in a merchant vessel^ that soundings, which ought 
to be actually measured, are not unfrequently taken for granted, to the imminent nsk of the ship. But with Mas- 
aey's machine two or tluee hands, with a proper length of Ium, not only accomplish the work, but insure its being 
done much more expeditiously and much more oorrectly than if all hands were turned out of their hammocks 
and drenched to the skin to obtain a result which could not be depended on. 


department w , 

wilh any officer if, when on his trial for the loss of his ship, suppomng the s&pwredc to have been caused' by an 
error faibis soundings, it shonld be established that he had neglected to avail himself of fliis admirable method of 
ascertaining his depth of water. 

The Thames steamer, on her voyage from Dublin to London <m the <th of Jaauaiy last, having lost her reckoning 
in a gale of wind, was carried on the rocks of Scilly and perished, frmn having misotken St. Asnes Lighthouse for 
that of the Loncnhip, near the Land's-end, a mistake into which they could hardly have frillen had they have been 
provided with Mas8ey|s Machine, for without any difficulty they might have ascertained that no such soondings ex- 
isted near the LongsnipB lights as those which they must nave nad when near the Cribawethan rock, on which they 

The same observation might be made with no less troth Tespectin|; many of the shipwrecks on which pave our 
beadles every winter, and therefore, I anxiously appeal to tiie shippmg interests of our country (as I have repeatedly 
done before ), to disregard the petty cost of an instrument as usefiil m its way as either the sextant or the chronometer, 
and frff more easily handled. If 1 had not already occupied so much of your valuaUe space, I diould be tempted to 
recommend also the use of the patent log devised by the same ingenious and public-spinted pers<m. It is an instra- 
ment rimilar in principle, and of tiie greatest use m navigation, but perhaps, not of sndi primary importance as 
the sounding machine, which itis a positive crime in any navigator to oe witnont 

I remain, your most obedient servant, BASIL HALL, Captain, R.N. 

« North 8SA^— The quality of the bottom, was noted at every fifth cast of the lead ; 12,000 of thespedmens 
have already been preserved, and the greater part are laid out in dietr correct positions on a large chart, delineated 
on the floor of a store-house in Deptfoid dock-yard. The bottom consists of sand, fine sand ana blade specks, and 
occasftonally broken shells, yet too irregularly disposed to enable the navigator to profit by them. But the banks 
tluuBisd ves, as strikinsly illustrated in the several sections here given, from excellent points of depsrtnre. so that by 
the aid ofthischart,tne mariner in the thickest fog, may boldly cross from England to the coast of Holland, if he 
willbutattendb>hi8lead,ande8pedally ifhehave on board uiat invaluable instrument Massey's Lead, without 
whidino ship shoold navigate the North Sea." — iVaa/tcoJ Magtuin^t April, 1842. 

AgentifoT Liverpool^ MeUing and Payne, No. 39» 8auth Castle Street. 

» V