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Mathematics Dept 






J. M. F. WRIGHT, A. B. 


VOL. I. 




f\ SO: 














THE flattering manner in which the Glasgow Edition of Newton s Prin- 
cipia has been received, a second impression being already on the verge 
of publication, has induced the projectors and editor of that work, to 
render, as they humbly conceive, their labours still more acceptable, by 
presenting these additional volumes to the public. From amongst the 
several testimonies of the esteem in which their former endeavours have 
been held, it may suffice, to avoid the charge of self-eulogy, to select the 
following, which, coming from the high authority of French mathematical 
criticism, roust be considered at once as the more decisive and impartial. 
It has been said by one of the first geometers of France, that " L edition 
de Glasgow fait honneur aux presses de cette ville industrieuse. On peut 
affirmer que jamais 1 art typographique ne rendit un plus bel hommage 
a la memoire de Newton. Le merite de 1 impression, quoique tres-remar- 
quable, n est pas ce que les editeurs ont recherche avec le plus de soin, 
pour tant le materiel de leur travail, ils pouvaient s en rapporter a 1 habi- 
Lite de leur artistes : mais le choix des meilleures editions, la revision la 
plus scrupuleuse du texte et des epreuves, la recherche attentive des fautes 
qui pourraient echapper rneme au lecteur studieux, et passer inapercues 
ce travail consciencieux de 1 intelligence et du savoir, voila ce qui eleve 
cette edition au-dessus de toutes celles qui 1 ont precedee. 

" Les editeurs de Glasgow ne s etaient charges que d un travail de re 
vision. S ils avaient concu le projet cTamcliorer et complcter I ccuvre des 



commentators, Us auraient sans Joule employe, comme eux$ les travaux des 
successeurs de Newton sur les questions traitees dans le livre des Principes. 

" Les descendans de Newton sont nombreux, et leur genealogie est 
prouvee par des titres incontestibles; ceux qui vivent aujourd hui verraient 
sans doute avec satisfaction que Ton format un tableau de leur famille, en 
reunissant les productions les plus remarquables dont Pouvrage de Newton 
a fourni le germe : que ce livre immortel soit entoure de tout ce Ton peut 
regarder comme ses developpemens : voila son meilleur commentaire. 
L? edition de Glasgow pourrait done etre continuee, et prodigieusement 

The same philosopher takes occasion again to remark, that " Le plus 
beau monument que Von puisse clever a la glcire de Newton, c est une 
bonne edition de ses ouvrages : et il est etonnant que les Anglais en aient 
laisse ce soin aux nations etrangeres. Les presses de Glasgow viennent 
de reparer, en partie, le tort de la nation Anglaise : la nouvelle edition 
des Principes est effectivement la plus belle, la plus correcte et la plus com 
mode qui ait parujusqu tci. La collation des anciennes editions, la revi 
sion des calculs, &c. ont ete confiees a un habile mathematicien et rien 
n a ete neglige pour eviter toutes les erreurs et toutes les omissions. 

" II faut esperer que les editeurs continueront leur belle entreprise, et 
qu ih y seront assez encourages pour nous donner, non seulement tous les 
ouvrages de Newton, mais ceux des savans qui ont complete ses travaux." 

The encouragement here anticipated has not been withheld, nor has 
the idea of improving and completing the cpmments of " The Jesuits", 
contained in the Glasgow Newton, escaped us, inasmuch as long before 
these hints were promulgated, had the following work, which is composed 
principally as a succedaneum to the former, been planned, and partly writ 
ten. It is at least, however, a pleasing confirmation of the justness of our 
own conceptions, to have encountered even at a ny time with these after- 
suggestions. The plan of the work is, nevertheless, in several respects, 
a deviation from that here so forcibly recommended. 

The object of the first volume is, to make the text of the Principia, by 


supplying numerous steps in the very concise demonstrations of the pro 
positions, and illustrating them by every conceivable device, as easy as 
can be desired by students even of but moderate capacities. It is univer 
sally known, that Newton composed this wonderful work in a very hasty 
manner, merely selecting from a huge mass of papers such discoveries as 
would succeed each other as the connecting links of one vast chain, but 
without giving himself the trouble of explaining to the world the mode of 
fabricating those links. His comprehensive mind could, by the feeblest 
exertion of its powers, condense into one view many syllogisms of a pro 
position even heretofore uncontemplated. What difficulties, then, ta him 
would seem his own discoveries? Surely none; and the modesty for 
which he is proverbially remarkable, gave him in his own estimation so 
little the advantage of the rest of created beings, that he deemed these 
difficulties as easy to others as to himself: the lamentable consequence of 
which humility has been, that he himself is scarcely comprehended at this 
day a century from the birth of the Principia. 

We have had, in the first place, the Lectures of Whiston, who des 
cants not even respectably in his lectures delivered at Cambridge, upon 
the discoveries of his master. Then there follow even lower and less 
competent interpreters of this great prophet of science for such Newton 
must have been held in those dark days of knowledge whom it would be 
time mis-spent to dwell upon. But the first, it would seem, who properly 
estimated the Principia, was Clairaut. After a lapse of nearly half a cen 
tury, this distinguished geometer not only acknowledged the truths of the 
Principia, but even extended the domain of Newton and of Mathematical 
Science. But even Clairaut did not condescend to explain his views and 
perceptions to the rest of mankind, farther than by publishing his own 
discoveries. For these we owe a vast debt of gratitude, but should have 
been still more highly benefited, had he bestowed upon us a sort of run 
ning Commentary on the Principia. It is genemlly supposed, indeed, 
that the greater portion of the Commentary called Madame Chastellet s, 
was due to Clairaut. The best things, however, of that work are alto- 


gether unworthy of so great a master ; at the most, showing the perform 
ance was not one of his own seeking. At any rate, this work does not 
deserve the name of a Commentary on the Principia. The same may 
safely be affirmed of many other productions intended to facilitate New 
ton. Pemberton s View, although a bulky tome, is little more than 
a eulogy. Maclaurin s speculations also do but little, elucidate the 
dark passages of the Principia, although written more immediately for 
that purpose. This is also a heavy unreadable performance, and not 
worthy a place on the same shelf with the other works of that great 
geometer. Another great mathematician, scarcely inferior to Maclaurin, 
has also laboured unprofitably in the same field. Emerson s Comments 
is a book as small in value as it is in bulk, affording no helps worth the 
perusal to the student. Thorpe s notes to the First Book of the Princi 
pia, however, are of a higher character, and in many instances do really 
facilitate the reading of Newton. Jebb s notes upon certain sections deserve 
the same commendation ; and praise ought not to be withheld from several 
other commentators, who have more or less succeeded in making small 
portions of the Principia more accessible to the student such as the Rev. 
Mr. Newton s work, Mr. Carr s, Mr. Wilkinson s, Mr. Lardner s, &c. 
It must be confessed, however, that all these fall far short in value of the 
very learned labours, contained in the Glasgow Newton, of the Jesuits 
Le Seur and Jacquier, and their great coadjutor. Much remained, how 
ever, to be added even to this erudite production, and subsequently to its 
first appearance much has been excogitated, principally by the mathema 
ticians of Cambridge, that focus of science, and native land of the Princi 
pia, of which, in the composition of the following pages, the author has 
liberally availed himself. The most valuable matter thus afforded are the 
Tutorial MSS. in circulation at Cambridge. Of these, which are used in 
explaining Newton to the students by the Private Tutors there, the author 
confesses to have had abundance, and also to have used them so far as seem 
ed auxiliary to his own resources. But at the same time it must be remark 
ed, that little has been the assistance hence derived, or, indeed, from all 


other known sources, which from the first have been constantly at com 

The plan of the work being to make those parts of Newton easy which 
are required to be read at Cambridge and Dublin, that portion of the 
Principia which is better read in the elementary works on Mechanics, 
viz. the preliminary Definitions, Laws of Motion, and their Corollaries, 
has been disregarded. For like reasons the fourth and fifth sections have 
been but little dwelt upon. The eleventh section and third book have 
not met with the attention their importance and intricacy would seem to 
demand, partly from the circumstance of an excellent Treatise on Physics, 
by Mr. Airey, having superseded the necessity of such labours; and 
partly because in the second volume the reader will find the same subjects 
treated after the easier and more comprehensive methods of Laplace. 

The first section of the first book has been explained at great length, 
and it is presumed that, for the first time, the true principles of what has 
been so long a subject of contention in the scientific world, have there 
been fully established. It is humbly thought (for in these intricate specu 
lations it is folly to be proudly confident), that what has been considered 
in so many lights and so variously denominated Fluxions, Ultimate Ratios, 
Differential Calculus, Calculus of Derivations, &c. &c. is here laid down 
on a basis too firm to be shaken by future controversy. It is also hoped 
that the text of this section, hitherto held almost impenetrably obscure, is 
now laid open to the view of most students. The same merit it is with some 
confidence anticipated will be awarded to the illustrations of the 2nd, 3rd, 
6th, 7th, 8th, and 9th sections, which, although not so recondite, require 
much explanation, and many of the steps to be supplied in the demon 
stration of almost every proposition. Many of the things in the first 
volume are new to the author, but very probably not original in reality 
so vast and various are the results of science already accumulated. Suffice 
it to observe, that if they prove useful in unlocking the treasures of the 
Principia, the author will rest satisfied with the meed of approbation, 
which he will to that extent have earned from a discriminating and im 
partial public. 


The second volume is designed to form a sort of Appendix or Supple 
ment to the Principia. It gives the principal discoveries of Laplace, and, 
indeed, will be found of great service, as an introduction to the entire 
perusal of the immortal work of that author the Mecanique Celeste. 
This volume is prefaced by much useful matter relative to the Integra 
tion of Partial Differences and other difficult branches of Abstract Ma 
thematics, those powerful auxiliaries in the higher departments of Physical 
Astronomy, and which appear in almost every page of the Mecanique 
Celeste. These and other preparations, designed to facilitate the com 
prehension of the Newton of these days, will, it is presumed, be found 
fully acceptable to the more advanced readers, who may be prosecuting 
researches even in the remotest and most hidden receptacles of science ; 
and, indeed, the author trusts he is by no means unreasonably exorbitant 
in his expectations, when he predicates of himself that throughout the 
undertaking he has proved himself a labourer not unworthy of reward. 





1. THIS section is introductory to the succeeding part of the work. It 
comprehends the substance of the method of Exhaustions of the Ancients, 
and also of the Modern Theories, variously denominated Fluxions, Dif 
ferential Calculus, Calculus of Derivations, Functions, &c. &c. Like 
them it treats of the relations which Indefinite quantities bear to one ano 
ther, and conducts in general by a nearer route to precisely the same 

2. In what precedes this section, Jinite quantities only are considered, 
such as the spaces described by bodies moving uniformly in Jinite times 
with Jinite velocities ; or at most, those described by bodies whose mo 
tions are uniformly accelerated. But what follows relates to the motions 
of bodies accelerated according to various hypotheses, and requires the 
consideration of quantities indefinitely small or great, or of such whose 
Ratios, by their decrease or increase, continually approximate to certain 
Limiting Values, but which they cannot reach be the quantities ever so 
much diminished or augmented. These Limiting Ratios are called by 
Newton, " Prime and Ultimate Ratios," Prime Ratio meaning the Limit 
from which the Ratio of two quantities diverges, and Ultimate Ratio that 
towards which the Ratio converges. To prevent ambiguity, the term Li 
miting Ratio will subsequently be used throughout this Commentary. 



would infer the truth of the Lemma not only for quantities mensurable 
by Integers, but also for such as may be denoted by Vulgar Fractions. 
The necessity or use of the distinction is none ; there being just as much 
reason for specifying all other sorts of quantities. The truth of the LEMMA 
does not depend upon the species of quantities, but upon their confor 
mity with the following conditions, viz. 

4. That they tend continually to equality, and approach nearer to each 
other than by any given difference. They must tend continually to equa 
lity, that is, every Ratio of their successive corresponding values must be 
nearer and nearer a Ratio of Equality, the number of these convergen- 
cies being without end. By given difference is merely meant any that can 
be assigned or proposed. 

5. FINITE TIME.] Newton obviously introduces the idea of time in this 
enunciation, to show illustratively that he supposes the quantities to con 
verge continually to equality, without ever actually reaching or passing that 
state ; and since to fix such an idea, he says, " before the end of that 
time," it was moreover necessary to consider the time Finite. Hence 
our author would avoid the charge of " Fallacia Suppositionis" or of 
" shifting the hypothesis" For it is contended that if you frame certain 
relations between actual quantities, and afterwards deduce conclusions 
from such relations on the supposition of the quantities having vanished, 
such conclusions are illogically deduced, and ought no more to subsist 
than the quantities themselves. 

In the Scholium at the end of this Section he is more explicit. He 
says, The ultimate Ratios, in which quantities vanish, are not in reality the 
Ratios of Ultimate quantities ; but the Limits to which the Ratios of quan 
tities continually decreasing always approach ; which they never can pass 
beyond or arrive at, unless the quantities are continually and indejinitely 
diminished. After all, however, neither our Author himself nor any of 
his Commentators, though much has been advanced upon the subject, has 
obviated this objection. Bishop Berkeley s ingenious criticisms in the 
Analyst remain to this day unanswered. He therein facetiously denomi 
nates the results, obtained from the supposition that the quantities, before 


considered finite and real, have vanished, the " Ghosts of Departed 
Quantities / and it must be admitted there is reason as well as wit in the 
appellation. The fact is, Newton himself, if we may judge from his own 
words in the above cited Scholium, where he says, " If two quantities, 
whose DIFFERENCE is GIVEN are augmented continually, their Ultimate 
Ratio will be a Ratio of Equality," had no knowledge of the true nature 
of his Method of Prime and Ultimate Ratios. If there be meanino- in 


words, he plainly supposes in this passage, a mere Approximation to be 
the same with an Ultimate Ratio. He loses sight of the condition ex 
pressed in Lemma I. namely, that the quantities tend to equality nearer 
than by any assignable difference, by supposing the difference of the quan 
tities continually augmented to be given, or always the same. In this 
sense the whole Earth, compared with the whole Earth minus a grain of 
sand, would constitute an Ultimate Ratio of equality ; whereas so long as 
any, the minutest difference exists between two quantities, they cannot be 
said to be more than nearly equal. But it is now to be shown, that 

6. If two quantities tend continually to equality, and approach to one 
another nearer than by any assignable difference, their Ratio is ULTIMATE 
LY a Ratio of ABSOLUTE equality. This may be demonstrated as fol 
lows, even without supposing the quantities ultimately evanescent. 

It is acknowledged by all writers on Algebra, and indeed self-evident, that 
if in any equation put = 0, there be quantities absolutely different in kind, 
the aggregate of each species is separately equal to 0. For example, if 

since A + a is rational, (B + b) V~2 surd and C V 1 imaginary, 
they cannot in any way destroy one another by the opposition of signs, 
and therefore 

A + a = 0, B + b = 0, C = 0. 

In the same manner, if logarithms, exponentials, or any other quantities 
differing essentially from one another constitute an equation like the above, 
they must separately be equal to 0. This being premised, let L, L de 
note the Limits, whatever they are, towards which the quantities L + I, 
L 7 + 1 continually converge, and suppose their difference, in any state of 
the convergence, to be D. Then 

L + 1 L V = D, 
or L L + 1 1 D = 0, 

and since L, L are fixed and definite, and 1, 1", D always variable, the 
former are independent of the latter, and we have 




L L = 0, or j-> = 1, accurately. Q. e. d. 

This way of considering the question, it is presumed, will be deemed 
free from every objection. The principle upon which it rests depending 
upon the nature of the variable quantities, and not upon their evanescence, 
(as it is equally true even for constant quantities provided they be of dif 
ferent natures), it is hoped we have at length hit upon the true and lo 
gical method of expounding the doctrine of Prime and Ultimate Ratios, 
or of Fluxions, or of the Differential Calculus, &c. 

It may be here remarked, in passing, that the Method of Indeterminate 
Coefficients, which is at bottom the same as that of Prime and Ultimate 
Ratios, is treated illogically in most books of Algebra. Instead of 
" shifting the hypothesis," as is done in Wood, Bonnycastle and others, 
by making x = 0, in the equation 

a + bx + cx 2 +dx 3 + = 0, 

it is sufficient to know that each term x being indefinitely variable, is he 
terogeneous compared with the rest, and consequently that each term 
must equal 0. 

7. Having established the truth of LEMMA I. on incontestable princi 
ples, we proceed to make such applications as may produce results useful 
to our subsequent comments. As these applications relate to the Limits 
of the Ratios of the Differences of Quantities, we shall term, after Leib 
nitz, the Method of Prime and Ultimate Ratios, 


8. According to the established notation, let a, b, c, &c ., denote con 
stant quantities, and z, y, x, &c., variable ones. Also let A z, A y, A x, 
&c., represent the difference between any two values of z, y, x, &c., re 

9. Required the Limiting or Ultimate Ratio of A (a x) and A x, i. e. 
the Limit of the Difference of a Rectangle having one side (a) constant, and 
the other (x) variable, and of the Difference of the variable side. 

Let L be the Limit sought, and L + 1 any value whatever of the va 
rying Ratio. Then 

A (a x) a (x + A x) ax T 

L + = } -AIT- = - -ir- ; = a - b * No - 7 

L = a. 


In this instance the Ratio is the same for all values of x. But if in the 
Limit we change the characteristic A into d, we have 

* A ; A 

ax) = a d x^ 


d (ax) 
d (a x), d x being called the Differentials of a x and x respectively. 

A (x 2 ) 
10. Required the Limit of . 

Let L be the Limit required, and L + 1 the value of the Ratio gene 
rally. Then 

A (x 2 ) (x + A x) 2 x 2 
L + * = AX = AX 

2 X A X + A X 2 

"AIT" - = 2 x + A x. 

. . L 2 X + 1 A X =r 

and since L 2 x and 1 Ax are heterogeneous 
L 2 x = 0, 
L = x2 

and .-. 


d (x ~) = 2 x d x (c) 

A (x n ) 

1 1. Generally, required the Limit of A x . 

Let L and L + 1 be the Limit of the Ratio and the Ratio itself re 
spectively. Then 

T A ( X ) (X + AX) X n 

L + 1 = -^~ = - AX 

n. (n 1) 
= n x n - + -j -. x n ~ 2 A x + &c. 

and L n x n l being essentially different from the other terms of 
the series and from 1, we have 

d (x n ) 
d x = L = n x n ~ l or d (x ") = n x - l d x (d) 

or in words, 

A s 


The Differential of any potsoer or root of a variable quantity is equal to 
the product of the Differential of the quantity itself^ the same power or 
root MINUS one of the quantity, and the index of the power or root. 

We have here supposed the Binomial Theorem as fully established by 
Algebra. It may, however, easily be demonstrated by the general prin 
ciple explained in (7). 

12. From 9 and 1 1 we get 
d(ax n )=nax n ~ 1 dx ...... (e) 

A(a+x n + cx m + exP + &c.) 

13. Required the Limit of - A x 

Let L be the Limit sought, and L + 1 the variable Ratio of the finite 
differences; then 

A(a + bx D + cx m + &c.) 
*+!=,. AX 

+ &c. a bx n cx m &c. 


A X 

= nbx n ~ 1 + mcx m ~ l + &c. + P AX + Q(A x) 2 -f- &c. 
P, Q, &c. being the coefficients of A x, A x 2 + &c. And equating the 
homogeneous determinate quantities, we have 

d(a + bx n + cx m + &c.) 
- - - 

A(a + bx n + cx m + &c.) r 

14. Required the Limit of - ~~A~X~~ 

By 1 1 we have 

d. (a + bx n + cx m + &c.) r 

-d(a + bx + &c.) -=r(a + bxn + C x- + &c.) - 

and by 13 

d(a+bx n + cx m + &c.) = (nbx 11 " 1 -f mcx 1 *- 1 + &c.) dx 

= r(nbx n - 1 + mcx 1 "- 1 + &c.)(a + bx n + &c.) r - ! .. (g) 

the Limiting Ratio of the Finite Differences A(a + bx n -f-cx m + &c.), 
A x, that is the Ratio of the Differentials ofa + bx n + cx m + &c., 
and x. 

A + Bx u -f-Cx m + &c. 

15. Required the Ratio of the Differentials gf a .i.b x 4.Cx^-J-&c 

and x, or the Limiting Ratio of their Finite Differences. 

Let L be the Limit required, and L + 1 the varying Ratio. Then 

__ A + B (x + A x)? 1 + C (x + A x) m + &c. A + B x n + &c. 
L + a + b(x + AX) + c(x + Ax)^+ &c. ~ a + bx- + &c.~ 


which being expanded by the Binomial Theorem, and properly reduced 


L X ( a + b x + &c.) 2 + L X P. AX + Q (A x) 2 +&c. + 1 X {a+bx + &c. 
+ P. A x + Q (A x) 2 + &c.} =(a+bx + cx^+ &c.) X (nBx"" 1 
+ mCx- 1 + &c.) (A+Bx n +Cx m + &c.) X (^bx-- 1 
+ ft c x /- l + &c.) + P . A x + Q (A x) 2 + &c. 

P, Q, P , Q &c. being coefficients of A x, (A x) 2 &c. and independent of 


Now equating those homogeneous terms which are independent of the 

powers of A x, we get 

(A + Bx n + Cx m + &c.) (vbx - l + / ucx^- + &c.) 

A+Bx n + Cx m + &c. 
and putting u = a ^b ^TVx^^&cT we have finall y 

du du 

- = L, and therefore - = 

(a + b x + c x <" + &c.) * 
the Ratio required. 

16. Hence and from 1 1 we have the Ratio of the Differentials of 

(A + Bx+Cx + & c .) * 
(a + b x + cx^ + &c.) i and x and ln S rt 

ready been delivered it is easy to obtain the Ratio of the Differentials of 
any Algebraic Function whatever of one variable and of that variable. 

N. B. By Function of a variable is meant a quantity anyhow involving 
that variable. The term was first used to denote the Powers of a quan 
tity, as x 2 , x 3 , &c. But it is now used in the general sense. 

The quantities next to Algebraical ones, in point of simplicity, are Ex 
ponential Functions; and we therefore proceed to the investigation of 
their Differentials. 

17. Required the Ratio of the Differentials of a x and x ; or the Limit 
ing Ratio of their Differences. 

Let L be the required Limit and L + 1 the varying Ratio ; then 
A(a x ) a * + Ai a x 

L + l = 

= a x X 


a ** 1 

A X 


But since 

ay = (1 + a l)y 

2.3 -(a l) 3 + &c., 

it is easily seen that the coefficient of y in the expansion is 

(a I) 2 (a I) 3 
-g-- + v__ -- __ &c< 


a* (a I) 2 (a _ I) 3 

L + ] = Z1Z Ha 1 2 + V - 3 ~ &c.) A x + P (AX) 2 + &c.J 

and equating homogeneous quantities, we have 

d - (a *) (a I) 2 (a I) 3 

~d^~= L = fc 1 -- g -- + L_J__ &c> j a* 

= A a* ........ (h) 

or the Ratio of the Differentials of any Exponential and its exponent is 
equal to the product of the Exponential and a constant Quantity. 

Hence and from the preceding articles, the Eatio of the Differentials of 
any Algebraic Function of Exponentials having the same -variable index, 
may be found. The Student may find abundance of practice in the Col 
lection of Examples of the Differential and Integral Calculus, by Messrs. 
Peacock, Herschel and Babbage. 

Before we proceed farther in Differentiation of quantities, let us inves 
tigate the nature of the constant A which enters the equation (h). 

For that purpose, let (the two first terms have been already found) 

a x = l+Ax+Px 2 +Qx 
Then, by 13, 
d (a x ) 


But by equation (h) 

d (a*) 

~ also = A 

and equating homogeneous quantities, we get 

2 P = A 2 , 3 Q = A P, 4 R = A Q, &c. = &c. 



P _A_! o-^- il n AQ A4 

2 y - 3 - 2. 3 K = 4 = 2. 3.4 < 


A_ 2 A 3 A 4 

Again, put A x = 1, then 

A 1 l - 

a = 1+1 + 2+ + 27374 + &c. 

= 2.718281828459 as is easily calculated 
= e 

by supposition. Hence 
loff. a 

(a 1) 2 (a 1) 3 log. a 

a " ~2~ ~ + " ~3~" - &c = To^Te = L a 

for the system whose base is e, 1 being the characteristic of that system. 
This system being that which gives 

(e I) 2 (e I) 3 
e 1 s 2 - + - 3 - &c. = 1 

is called Natural from being the most simple. 
Hence the equation (h) becomes 

d(a x ) 

-^rrlaXa* ........ (1) 

17 a. Required the Ratio of the Differentials of 1 (x) and x. 

Let 1 x = u. Then e u = x 
.-. d x = d (e u ) = 1 e X e u d u = e u d u, by 16 

d (1 x) _1_ 1 
~~d!T = e u = x ........ ( m ) 


In any other system whose base is a, we have log. (x) = y^. 

d lo, x 1 1 

n x x 

We are now prepared to differentiate any Algebraicj or Exponential 
Functions of Logarithmic Functions, provided there be involved but 
one variable. 

Before we differentiate circular functions, viz. the sines, cosines, tan 
gents, &c., of circular arcs, we shall proceed with our comments on the 
text as far as LEMMA VIII. 



18. In No. 6, calling L and L Limits of the circumscribed and inscribed 
rectilinear figures, and L + 1, L + 1 any other values of them, whose 
variable difference is D, the absolute equality of L and L is clearly de 
monstrated, without the supposition of the bases A B, B C, C D, D E, 
being infinitely diminished in number and augmented in magnitude. In 
the view there taken of the subject, it is necessary merely to suppose them 


19. This LEMMA is also demonstrable by the same process in No. 6, 

Cor. 1. The rectilinear figures cannot possibly coincide with the curvi 
linear figure, because the rectilinear boundaries albmcndoE, 
aKbLcMdDE cut the curve a b E in the points a, b, c, d, E in 
finite angles. The learned Jesuits, Jacquier and Le Setir, in endeavour 
ing to remove this difficulty, suppose the four points a, 1, b, K to coincide, 
and thus to form a small element of the curve. But this is the language 
of Indivisibles, and quite inadmissible. It is plain that no straight line, 
or combination of straight lines, can form a curve line, so long as we un 
derstand by a straight line " that which lies evenly between its extreme 
points," and by a curve line, " that which does not lie evenly between its 
extreme points ;" for otherwise it would be possible for a line to be 
straight and not straight at the same time. The truth is manifestly this. 
The Limiting Ratio of the inscribed and circumscribed figures is that of 
equality, because they continually tend to a fixed area, viz, that of the 
given intermediate curve. But although this intermediate curvilinear 
area, is the Limit towards which the rectilinear areas continually tend and 
approach nearer than by any difference ; yet it does not fallow that the 
rectilinear boundaries also tend to the curvilinear one as a limit. The 
rectilinear boundaries are, in fact, entirely heterogeneous with the interme 
diate one, and consequently cannot be equal to it, nor coincide therewith. 
We will now clear up the above, and at the same time introduce a strik 
ing illustration of the necessity there exists, of taking into consideration 
the nature of quantities, rather than their evanescence or infinitesimality. 







Take the simplest example of LEMMA II., in the case of the right- 
angled triangle a E A, having its two legs A a, A E equal. 

The figure being constructed as in the text of LEMMA II, it fol 
lows from that Lemma, that the Ultimate Ratio of the inscribed and cir 
cumscribed figures is a ratio of equality ; and moreover it would also 
follow from Cor. 1. that either of these 
coincided ultimately with the triangle a 1 
a E A. Hence then the exterior boundary 
albmcndoE coincides exactly with _, 
a E ultimately, and they are consequently 
equal in the Limit. As we have only 
straight lines to deal with in this example, 
let us try to ascertain the exact ratio of 
a E to the exterior boundary. 

If n be the indefinite number of equal 
bases A B, B C, &c., it is evident, since 
A a ~ A E, that the whole length of 
a * b "i c n d o E = 2 n X A B. Also since a b = b c = &c. 
= V~al r ~+ b 1 * = V 2. A B, we have a E = n V 2. A B. 


albmcndoE:aE::2: V 2 : : V~2 : 1. 

Hence it is plain the exterior boundary cannot possibly coincide with 
a E. Other examples might be adduced, but it must now be sufficiently 
clear, that Newton confounded the ultimate equality of the inscribed and 
circumscribed figin es, to the intermediate one, with their actual coinci 
dence, merely from deducing their Ratios on principles of approximation 
or rather of Exhaustion, instead of those, as explained in No. 6 ; which 
relate to the homogeneity of the quantities. In the above example the 
boundaries being heterogeneous inasmuch as they are incommensurable, 
cannot be compared as to magnitude, and unless lines are absolutely equal, 
it is not easy to believe in their coincidence. 

Profound as our veneration is, and ought to be, for the Great Father 
of Mathematical Science, we must occasionally perhaps find fault with 
his obscurities. But it shall be done with great caution, and only with 
the view of removing them, in order to render accessible to students in 
general, the comprehension of " This greatest monument of human ge 

20. Cor. 2. 3. and 4. will be explained under LEMMA VII, which re 
lates to the Limits of the Ratios of the chord, tangent and the arc. 



[SECT. I. 


21. Let the areas of the parallelograms inscribed in the two figures be 
denoted by 

P, Q, R, &c. 
p, q, r, &c. 
respectively ; and let them be such that 

P : p : : Q : q : : R : r, &c. : : m : n. 
Then by compounding these equal ratios, we get 

P+Q+R + : p + q + r + ; ; m:n 

But P + Q + R . . . . and p + q + r + . . . . have with the curvili 
near areas an ultimate ratio of equality. Consequently these curvilinear 
areas are in the given ratio of m : n. 

Hence may be found the areas of certain curves, by comparing their 
incremental rectangles with those of a known area. 

Ex. 1. Required the area of the common Apollonian parabola comprised 
between its vertex and a given ordinate. 

Let a c E be the parabola, 
whose vertex is E, axis E A and 
Latus-Rectum = a. Then A A 
being its circumscribing rectan 
gle, let any number of rectan 
gles vertically opposite to one 
another be inscribed in the areas 
a E A, a E A , viz. A b, b A ; 
B c, c B , &c. 

And since 

A b = A K. A B 

A b = A 1. A B = ^-. A B 


from the equation to the parabola. 
A b a. A B 


A b ~ A K. A B 


(A a) 2 Bb 2 = axAE a 
(A a + B b) X A B = a X A B 

a X A 



= Aa -f Bb 

A B 

A b Aa + B b 2 Bb + K a Ka. 

AMb = ~ETb~~ B b + B b 

A b 
Hence, since in the Limit -Trr becomes fixed or of the same nature with 

the first term, we have 

A b 

A b 

= 2 


And the same may be shown of all other corresponding pairs of rec 
tangles ; consequently by LEMMA IV. 

a E A : a E A : : 2 : 1 
.. a E A : rectangle A A : : 2 : 3. 

or the area of a parabola is equal to two thirds of its circumscribing rec 

Ex. 2. To compare the area of a, semiellipse with that of a semicircle 
described on the same diameter. 


Taking any two corresponding inscribed rectangles P N, P N ; we 

P N : F N : : P M : P M : : a : b 

a and b being the semiaxes major and minor of the ellipse ; and all other 
corresponding pairs of inscribed rectangles have the same constant ratio ; 
consequently by LEMMA IV, the semicircle has to the semiellipse the ratio 
of the major to the minor axis. 

As another example, the student may compare the area of a cycloid 
with that of its circumscribing rectangle, in a manner very similar to 
Ex. 1. 

This method of squaring curves is very limited in its application. In 
the progress of our remarks upon this section, we shall have to exhibit a 
general way of attaining that object. 



22. For the definition of similar rectilinear figures, and the truth of this 
LEMMA as it applies to them, see Euclid s Elements B. VI, Prop. 4, 19 
and 20. 

The farther consideration of this LEMMA must be deferred to the ex 
planation of LEMMA VII. 


23. In the demonstration of this LEMMA, " Continued Curvature" at 
any point, is tacitly defined to be such, that the arc does not make with the 
tangent at that point, an angle equal to ajinite rectilinear angle. 

In a Commentary on this LEMMA if the demonstration be admitted, 
any other definition than this is plainly inadmissible, and yet several of 
the Annotators have stretched their ingenuity to substitute notions of 
continued curvature, wholly inconsistent with the above. The fact is, 
this LEMMA is so exceedingly obscure, that it is difficult to make any 
thing of it. In the enunciation, Newton speaks of the angle between the 
chord and tangent ultimately vanishing, and in the demonstration, it is 
the angle between the arc and tangent that must vanish ultimately. So 
that in the Limit, it would seem, the arc and chord actually coincide. 
This has not yet been established. In LEMMA III, Cor. 2, the coinci 
dence ultimately of a chord and its arc is implied ; but this conclusion by 
no means follows from the LEMMA itself, as may easily be gathered from 
No. 19. The very thing to be proved by aid of this LEMMA is, that the 
Ultimate Ratio of the chord to the arc is a ratio of equality, it being 
merely subsidiary to LEMMA VII. But if it be already considered that 
they coincide, of course they are equal, and LEMMA VII becomes nothing 
less than " argumentum in circulo" 

Newton introduces the idea of curves of " continued curvature" or 
such as make no angle with the tangent, to intimate that this LEMMA does 
not apply to curves of non-continued curvature, or to such as do make a 
Jinite angle with the tangent. At least this is the plain meaning of his 
words. But it may be asked, are there any curves whose tangents are 
inclined to them ? The question can only be resolved, by again admitting 




the arc to be ultimately coincident with the chord ; and by then showing, 
that curves may be imagined whose chord and tangent ultimately shall be 
inclined at a finite angle. The Ellipse, for instance, whose minor axis 
is indefinitely less than its major axis, is a curve of that kind ; for taking 
the tangent at the vertex, and putting a, b, for the semiaxes, and y, x, for 
the ordinate and abscissa, we have 

b 2 

, X (2ax-x 2 ) 


y 2 = 

2 a 

X 1 = 

= V 2 a x 

.-. since b is indefinitely smaller than a V x, x is indefinitely greater than 
y, and supposing y to be the tangent cut off by the secant x parallel to 
the axis, x and y are sides of a right angled A, whose hypothenuse is the 
chord. Hence it is plain the z_ opposite x is ultimately indefinitely 
greater than the L. opposite to y. But they are together equal to a right 
angle. Consequently the angle opposite x, or that between the chord and 
tangent, is ultimately finite. Other cases might be adduced, but enough 
has been said upon what it appears impossible to explain and establish as 
logical and direct demonstration. We confess our inability to do this, 
an(J feel pretty confident the critics will not accomplish it. 

24. Having exposed the fallacy of Newton s reasoning in the proof of 
this LEMMA, we shall now attempt something by way of substitute. 

Let A D be the tangent to the curve at the 
point A, and A B its chord. Then if B be 
supposed to move indefinitely near to A, the 
angle BAD shall indejinitely decrease,, pro 
vided the curvature be not indefinitely great. 

Draw R D passing through B at right an 
gles to AB, and meeting the tangent AD and 
normal A R in the points D and R respective 
ly. Then since the angle BAD equals the 
angle A R B, if A R B decrease indefinitely 
when B approaches A ; that is, if A R be 
come indefinitely greater than A B ; or 

which is the same thing, if the curvature at A, be not indefinitely great ; 
the angle BAD also decreases indefinitely. Q. e. d. 

We have already explained, by an example in the last article, what is 


meant by curvature indefinitely great. It is the same with Newton s ex 
pression " continued curvature." The subject will be discussed at length 
under LEMMA XI. 

As vanishing quantities are objectionable on account of their nothing 
ness as it has already been hinted, and it being sufficient to consider va 
riable quantities, to get their limiting ratios, as capable of indefinite diminu 
tion, the above enunciation has been somewhat modified to suit those 


25. This LEMMA, supposing the two preceding ones to have been fully esta 
blished, would have been a masterpiece of ingenuity and elegance. By 
the aid of the proportionality of the homologous sides of similar curves, 
our author has exhibited quantities evanescent by others of any finite 
magnitude whatever, apparently a most ingenious device, and calculated 
to obviate all objections. But in the course of our remarks, it will be 
shown that LEMMA V cannot be demonstrated without the aid of this 

First, by supposing A d, A b always finite, the angles at d and b and 
therefore those at D and B which are equal to the former are virtually 
considered finite, or R D cuts the chord and tangent at finite angles. 

Hence the elaborate note upon this subject of Le Seur and Jacquier is 
rendered valueless as a direct comment. 

Secondly. In the construction of the figure in this LEMMA, the de 
scription of a figure similar to any given one, is taken for granted. But 
the student would perhaps like to know how this can be effected. 

LEMMA V, which is only enunciated, from being supposed to be a mere 
corollary to LEMMA III and LEMMA IV, would afford the means immedi 
ately, were it thence legitimately deduced. But we have clearly shown 
(Art. 19.) that rectilinear boundaries, consisting of lines cutting the inter 
mediate curve ultimately atjinite angles, cannot be equal ultimately to the 
curvilinear one, and thence we show that the boundaries formed by the 
chords or tangents, as stated in LEMMA III, Cor. 2 and 3, are not ulti 
mately equal, by consequence of that LEMMA, to the curvilinear one. 

Newton in Cor. 1, LEMMA III, asserts the ultimate coincidence, and 
therefore equality of the rectilinear boundary whose component lines cut 
the curve at finite angles, and thence would establish the succeeding cor- 


ollaries a fortiori. But the truth is that the curvilinear boundary is the 
limit, as to magnitude, or length, of the tangential and chordal bounda 
ries ; although in the other case, it is a limit merely in respect of area. 
Yet, we repeat it, that LEMMA V cannot be made to follow from the 
LEMMAS preceding it. According to Newton s implied definition of simi 
lar curves, as explained in the note of Le Seur and Jacquier, they are the 
curvilinear limits of similar rectilinear Jigures. So they might be consi 
dered, if it were already demonstrated that the limiting ratio of the chord 
and arc is a ratio of equality ; but this belongs to LEMMA VII. Newton 
himself and all the commentators whom we have perused, have thus 
committed a solecism. Even the best Cambridge MSS. and we have 
seen many belonging to the most celebrated private as well as college tu 
tors in that learned university, have the same error. Nay most of them 
are still more inconsistent. They give definitions of similar curves wholly 
different from Newton s notion of them, and yet endeavour to prove 
LEMMA V, by aid of LEMMA VII. For the verification of these asser 
tions, which may else appear presumptuously gratuitous, let the Cantabs 
peruse their MSS. The origin of all this may be traced to the falsely 
deduced ultimate coincidence of the curvilinear and rectilinear boundaries, 
in the corollaries of LEMMA III. See Art. 19. 

We now give a demonstration of the LEMMA without the assistance of 
similar curves, and yet independently of quantities actually evanescent. 

By hypothesis the secant R D cuts the chord and tangent at finite an 
gles. Hence, since 

A + B + D = 180 
.-. B + D - 180 A 

orL + l-fL +l = 180 A 

L and L being the limits of B and D and 1, V their variable parts as in 
Art. 6 ; and since by LEMMA VI, or rather by Art. 24, A is indefinitely 
diminutive, we have, by collecting homogeneous quantities 
L + L = 180 

But A B, A D being ultimately not indefinitely great, it might easily 
be shown from Euclid that L = -L , and .-. A B = A D ultimately, (see 
Art. 6 ) and the intermediate arc is equal to either of them. 



[SECT. 1. 


If we refer the curve to its axis, 
A a, B b being ordinates, &c. as 
in the annexed diagram. Then, 
by Euclid, we have 

$ ... AD; I , + B + D . Bt>t 

. Bd 


Now, since by Art. 24 or LEMMA VI, the L. B A D is indefinitely less 
than either of the angles B or D, .-. B D is indefinite compared with A B 

A D 
or A D. Hence L being the limit of . - and 1 its variable part, if we 

extract the root of both sides of the equation and compare homogeneous 
terms, we get, 

L = 1 or &c. &c. 

26. Having thus demonstrated that the limiting Ratio of the chord, arc 
and tangent, is a ratio of equality, when the secant cuts the chord and tangent 
at FINITE angles, we must again digress from the main object of this work, 
to take up the subject of Article 17. By thus deriving the limits of the rati 
os of the finite differences of functions and their variables, directly from the 
LEMMAS of this Section, and giving to such limits a convenient algorithm 
or notation, we shall not only clear up the doctrine of limits by nume 
rous examples, but also prepare the way for understanding the abstruser 
parts of the Principia. This has been before observed. 

Required to find the Limit of the Finite Differences of the sine of a cir 
cular arc and of the arc itself, or the Ratio of their Differentials. 

Let x be the arc, and A x its finite variable increment. Then L being 
the limit required and L + 1 the variable ratio, we have 
L + 1 = A s *" x _ sm - (x + A x) sin, x 

A X A~X 

_ sin, x. cos. (A x) + cos, x. sin. (A x) sin, x 

A X 

sin. (A x) sin.x. cos. AX sin. x 

COS. X. 

A :c 



Now by LEMMA VII, as demonstrated in the preceding Article, the li- 

, cos. (A x) sin. x , 
l, and -- 5- - t -- 7-^7- have no definite limits. 

. ,. sm. A x . 
nut or is 

A X 

A X 

A X 


Consequently putting 

sin. (A x) 
cos. x. 3 = cos. x + 1 , 

A X 

we have 

L + 1 = cos. x + 1 + - 


and equating homogeneous terms 

L = cos. x 

or adopting the differential symbols 
d. sin. x 

d sin. 

27. Hence and from the rules for the differentiation of algebraic, expo 
nential, &c. functions, we can differentiate all other circular functions of 
one variable, viz. cosines, tangents, cotangents, secants, &c. 

d sin. ( - x^ 

\8 / f^ \ - 

= cos. ( x ) = sin. x 



d. cos. x 

sin. x ~\ 

.. -_^_. pnQ v M 

lx f 

>in. x = d x. cos. x J 



d. cos. x 

= sin. x 



1. COS. X . ^V 

j = sin. x J 

d x 

. cos. x = d x. sin. x J 


Again, since for radius 1, which is generally used as being the most simple, 
1 + tan. 2 x = sec. 2 x = 


1 2 cos. x. d. cos. x 

.*. 2 tan. x. d. tan. x = d. = 1 

cos. 2 x cos. x 

See 12 (d). Hence and from (b) immediately above, we have 

d x. sin. x 
tan. x. d. tan. x = 

cos. 3 x 

. . d. tan. x = d x. - (c) 

cos. - x 


cot. x = 

tan. x 

B 2 



, 1 d. tan. x 

cot x = d ta,,. X - -5S?nr- 

tan. 2 x. cos. 2 x sin. 2 x 



sec. x = 

.-. d. sec. x = d. 



d cos. x 

/]9 A} 


d x. sin. x 

COS. 2 X 

(* u ) 


cos. 2 x 

v c / 

we have 

and lastly since cosec. x = sec. (- 

d. (- 


d. cosec. x = d. sec. ( x) = 
d x. cos. x 



sin. x 

Any function of sines, cosines, &c. may hence be differentiated. 

28. In articles 8, 9, 10, 11, 12, 13, 14, 15, 16, 17, 26 and 27, are to 
be found forms for the differentiation of any function of one variable, 
whether it be algebraic, exponential, logarithmic, or circular. 

In those Articles we have found in short, the limit of the ratio of the 
first difference of a function, and of the first difference of its variable. 
Now suppose in this first difference of the function, the variable x should 
be increased again by A x, then taking the difference between the first 
difference and what it becomes when x is thus increased, we have the dif 
ference of the first difference of a function, or the second difference of a 
function, and so on through all the orders of differences, making A x al 
ways the same, merely for the sake of simplicity. Thus, 
A (x 3 ) = (x + Ax) 3 x 3 

= 3X 2 AX + 3XAX 2 + AX 3 

and A 4 (x) 3 = 3 (x + AX) ~ A x +<8 (x + AX) Ax 2 + A x 3 3 x 2 AX 

3XAX 2 AX 3 

= 3. 2xAX 2 3Ax 3 


denoting by A 2 the second difference. 

~A~x~ 2 = 3 - 2 - x + 3 A x 

and if the limiting ratio of A 2 (x 3 ) and Ax 2 , or the ratio of the second 
differential of x 3 , and the square of the differential of its variable x, be 
required, we should have 

L + 1 = 3. 2. x + 3 A x 

and equating homogeneous terms 

d 2 (x 3 ) 
j , = L = 3. 2. x 

d x 2 

In a word, without considering the difference, we may obtain the se 
cond, third, &c. differentials d 2 u, d 3 u, &c. of any function u of x im 
mediately, if we observe that -r is always a function itself of x, and 

(I X 

make d x constant. For example, let 

u = ax n + bx m + &c. 
Then, from Art. 13. we have 

-j = nax n-I + m b x m ~ + &c. 


, /d u\ 

VcTx/ d (d u) d 2 u 

j = ~r 9- = j o (by notation) 

d x d x 2 d x 2 v J 

= n. (n l)ax n - 2 + m(m 1) b x m ~ 2 + &c. 

d 3 u 

-j 5 = n. (n 1). (n 2) a x " - 3 + &c. 

&c. = &c. 

Having thus explained the method of ascertaining the limits of the ra 
tios of all orders of finite differences of a function, and the corresponding 
powers of the invariable first difference of the variable, or the ratios of the 
differentials of all orders of a function, and of the corresponding power 
of the first differential of its variable, we proceed to explain the use of 
these limiting ratios, or ratios of differentials, by the following 




[SECT. I. 


29. Let it be required to draw a tangent to a given curve at any given 
point of it. 

Let P be the given point, and A M 
being the axis of the curve, let P M 
= y, A M = x be the ordinate and 
abscissa. Also let P be any other 
point; draw P N meeting the ordi 
nate P M in N, and join P P . Now 
let T P R meeting M P and M A in 
R and T be the tangent required. 

Then since by similar triangles 

P N : P N : : P M : M T 

.-. M T = M T + T T = y. 

A X 

Now y being supposed, as it always is in curves, a function of x, we have 
seen that whether that function be algebraic, exponential, &c. 

- in the limit, or -^- is always a definite function of x. Hence putting 

J * 



d x 


we have 

M T + T T = y (~ + l) 

and equating homogeneous terms, 

which being found from the equation to the curve, the point T will be 
known, and therefore the position of the tangent P T. M T is called 

the subtangent. 

Ex. 1. In the common parabola, 

y 2 = a x 



d x 2 y 

d y ~~ a 

2 v 2 
MT = -^- = 2x 

or the subtangent M T is equal to twice the abscissa. 
Ex. 2. In the ellipse, 

b 2 

y 2 = ^(a 2 -x*) 

and it will be found by differentiating, &o. that 

/A 2 v Z\ 

MT = ~ 



Ex. 3. In the logarithmic curve, 

y = a* 


* cfx - * a x y ( see 17 -) 
MT = r a "v^C ^, ^ r, ^"^i ",i 

which is therefore the same for all points. 

The above method of deducing the expression for the subtangent is 
strictly logical, and obviates at once the objections of Bishop Berkeley 
relative to the compensation of errors in the denominator. The fact is, 
these supposed errors being different in their very essence or nature from 
the other quantities with which they are connected, must in their aggre 
gate be equal to nothing, as it has been shown in Art. G! This ingenious 
critic calls F R = z ; then, says he, (see fig. above) 

y. d x 
M T = d y + z accurately ; 

whereas it ought to have been 

y A x y 

MT = 

A y -f z Ay 



the finite differences being here considered. Now in the limit, - becomes a 

A X 


definite function of x represented by g-^r Consequently if 1 be put for 

A y 

the variable part of ~ -, we have 


_ __ 

dx + * + A X 

and it is evident from LEMMA VII and Art. 25, that z is indefinite com- 

z d y 

pared with A x. .-. ^-^ is indefinite compared with M T, -5 , and y ; 

and 1 is also so ; hence 

" .. M T. | + (l + ^j) M T = y 

y. d x z 

M T = ^y, and 1 + = 

which proves generally for all curves, what Berkeley established in the 
case of the common parabola ; and at the same time demonstrates, as had 
been already done by using T T instead of P R, incontestably the ac 
curacy of the equation for the subtangent. 

30. If it were required to draw a tangent to any point of a curve, re 
ferred to a center by a radius-vector and the L. 6 which describes by 
revolving round the fixed point, instead of the rectangular coordinates 
x, y ; then the mode of getting the subtangent will be somewhat different. 

Supposing x to originate in this center, it is plain that 
x g cos. 6 1 
y = g sin. 6 ) 

and substituting for x, y, d x, d y, hence derived in the expression (29. 
e.) we have 

d P cos. 6 P d 6 sin. 6 
MT = g sin.Jx d ; 8in ., + ; d , cog ., ..... (f) 

Ex. In the parabola 


"" 1 cos. 6 

where a is the distance between the focus and vertex, or the value of g at 
the vertex. Then substituting we get, after proper reductions 

and the distance from the focus to the extremity of the subtangent is 

cos. 6 cos. 6 

- cos . 6 = 2 a 


2 a 

= 1 cos. a ~ Si 

as is well known. 

30. a. The expression (f ) being too complicated in practice, the following 
one may be substituted for it. 

Let P T be a tangent to the 
curve, refei red to the center S, 
at the point P, meeting S T 
drawn at right angles to S P, 

ill T ; and let P be any other 
point. Join P P and produce 
it to T , and let T P be pro 
duced to meet S P produced in 
R, &c. Then drawing P N parallel to S T, we have 


x SF 


P N = g tan. A 6, S P = f + A g 

Therefore, substituting and equating homogeneous terms, after having 
applied LEMMA VII to ascertain their limits, we get 

Ex. 1. In the spiral of Archimedes we have 

S = ad; 

.-. S T = S - 

Ex. 2. In the hyperbolic spiral 


g = y; 

.-. S T = a 

31. It is sometimes useful to know the angle between the tangent and 

P M dy 
Tan. T = 5rT = d ^ (h) 

See fig. to Art 29. 


Again, in fig. Art. 30 a. 

SP dg 
Tan. T = ^ = ^ d , (k) 

32. It is frequently of great use, in the theory of curves and in many 
other collateral subjects, to be able to expand or develope any given func 
tion of a variable into an infinite series, proceeding according to the 
powers of that variable. We have already seen one use of such develop 
ments in Art. 17. This may be effected in a general manner by aid of 
successive differentiations, as follows. 

If u = f (x) where f (x) means any function of x, or any expression 
involving x and constants ; then, as it has been seen, 

d u = u d x 

(u being a new function of x) 

d u = u" d x 
d u" - u " d x 

&c. = &c. 

. /d u\ d 2 u X d x d 2 x X d u 

d u = d (tt = ~ d^~ ( 6 k ) 

. &c. = &c. 

denoting d. (d u), d. (d x) by d ~ u, d 2 x, and (d x) 2 by d x 2 , 
according to the received notation ; 

Or, (to abridge these expressions) supposing dx constant, and .-. d 2 x = 0, 


which give the various orders of fluxions required. 

Ex. 1. Let u = x n 


-5 n ~x a i 

d X ~ 


3--, = n. (n l)x"- z 


d 3 u 

j^- 3 = n. (n 1). (n 2)x n ~ 

&c. = &c. 

d n u 

J-^TE = n. (n 1). (n 2) ..... 3. 2. 1. 

Ex. 2. Let u = A + B x + C x 2 + D x 3 + E x 4 + &c. 



^ = B + 2Cx + 3Dx 2 + 4Ex 3 + &c. 

d 2 u 

j^, = 2C + 2. 3Dx + 3. 4 E x 2 + &c. 

d 3 u 

d^~ 3 = 2. 3 D + 2, 3. 4 E x + &c. 

&c. = &c. 

Hence, if u be known, and the coefficients A, B, C, D, &c. be un 
known, the latter may be found ; for if U, U , U", U" , &c. denote the 
d u d 2 u d 3 u 

when x = 0, then 

A = U, B = 17, C = jg- U", D = ~ U ", E = ~- U"", 
&c. = &c. 
and by substitution, 

u = U + U x + U" |l + U " ^ + &c. . ^ ^ ; . . (b) 
This method of discovering the coefficients is named (after its inventor), 


The uses of this Theorem in the expansion of functions into series are 
many and obvious. 

For instance, let it be required to develope sin. x, or cos. x, or tan. x, 
or 1. (1 -f x ) into series according to the powers of x. Here 
u = sin. x, or = cos. x, or = tan. x, or = 1. (1 + x ), 

. d- x = cos. x, or = - sin. x, or = ~g or = f j x 

llH 2 sin. x 1 

dx2 - - sin. x, or = _ cos. x, or = ,--, or = - -- , 


d 3 u 2 + 4 sin. 2 x 2 

H 3 = COSt x or = sm * x O1 = 4 ~> or = /V" i x \s 

&c. = &c. 

.-. U =0, or = 1, or = 0, or = 
U = 1, or = 0, or = 1, or = 1 
U" =0, or = 1, or = 0, or = 1 
U" = 1, or = 0, or = 2, or = 2 
&c. = &c. 


x 3 x 5 

sin. x = x 273 + 2 . 3. 4. 5 ~ &c - 

x 2 x 4 
cos. x = 1 -g- + 2 3 4, & c - 

x 3 2x 5 17x 7 
tan. x = x + -g- + g-y + 3 z 57 + &c. 

X 2 X 3 

1. (1 + X) = X -g- + -g &C. 

Hence may also be derived 


For let 

f (x) = A + Bx + Cx 2 + Dx 3 + Ex 4 + &c. 
f (x + h) = A + B. (x + h) + C. (x + h) 2 + D . (x + h) 3 + &c. 

+ (B + 2Cx + 3Dx 2 )h 
+ (C + 3Dx + 6Ex 2 )h 2 
+ (D + 4 Ex + 10 Fx 2 ) h 3 
+ &c. 

d. f (x) d^XW !l! 

d 3 f(x) h 3 

the theorem in question, which is also of use in the expansion of series. 

For the extension of these theorems to functions of two or more varia 
bles, and for the still more effective theorems of Lagrange and Laplace, 
the reader is referred to the elaborate work of Lacroix. 4to. 

Having shown the method of finding the differentials of any quanti- 


ties, and moreover, entered in a small degree upon the practical applica 
tion of such differentials, we shall continue for a short space to explain 
their farther utility. 

33. To find the MAXIMA and MINIMA of quantities. 

If a quantity increase to a certain magnitude and then decrease, the 
state between its increase and decrease is its maximum. If it decrease 
to a certain limit, and then increase, the intermediate state is its mi 
nimum. Now it is evident that in the change from increasing to decreas 
ing, or vice versa, which the quantity undergoes, its differential must have 
changed signs from positive to negative, or vice versa, and therefore (since 
moreover this change is continued) have passed through zero. Hence 
When a quantity is a MAXIMUM or MINIMUM, its differential = 0. . . (a) 

Since a quantity may have several different maxima and minima, (as for 
instance the ordinate of an undulating kind of curve) it is useful to have 
some means of distinguishing between them. 

34. To distinguish between MAXIMA and MINIMA. 

LEMMA. To show that in Taylor s Theorem (32. c.) any one term can 
be rendered greater than the sum of the succeeding ones, supposing the 
coefficients of the powers of h to be finite. 

Let Q h n - l be any term of the theorem, and P the greatest coefficient 
of the succeeding terms. Then, supposing h less than unity, 

P h n (1 + h + h 2 + . . . . in infin.) = P h n X * 

is greater than the sum ( S) of the succeeding terms. But supposing h to 
decrease in infin. 


P n> " l h = P h n ultimately. Hence ultimately 

P h > 8 


Q h " - . ; p h n ; : Q : p h, 

and since Q and P are finite, and h infinitely small ; therefore Q is > P h, 
Hence Q h n ~ l is > P h n , and a fortiori > S. 

Having established this point, let 

u = f(x) 

be the function whose maxima and minima are to be determined ; also 
when u = max. or min. let x = a. Then by Taylor s Theorem 

fl du. du h 2 d 3 u h 3 

f.-b = f._ - h . -. &c. 



and since by the LEMMA, the sign of each term is the sign of the sum of 
that and the subsequent terms, 

.-. f (a h) = f (a) ^-?. M 
d a 

f(a + h) = f(a) + ^-?. N 
d a 

Now since f (a) = max. or min. f (a) is > or < than both f (a h) 
and f (a + h), which cannot be unless 

d - u -o 

da - 

d 2 u 

f(a-h) =f(a) 
f(a + h) = f(a) 

da 2 

and f (a) is max. or min. or neither, according as f (a) is >, < or = to 
both f (a h) and f (a + h), or according as 

d 2 u . 

-T - is negative, positive, or zero 

If it be zero as well as -, , we have 
d a 

f(a + h) =f(a) + 

O. i I 

and f (a) cannot = max. or min. unless 

d 3 u 

d^~ : 
which being the case we have 

d 4 u 

f(a h) = fa + M" ) 
da f 

f(a + h)=fa + ^l?. N-) 

d a 
and as before, 


d T" " *"" """ *- 

1 4 

f (a) is max . or min. or neither, according as -, " is negative, positive, or 

zero, and so on continually. 

Hence the following criterion. 

If in u f (x), = 0, the resulting value of x shall give u MAX. 

or MIN. or NEITHER, according as -j 2 w negative, positive, or aero. 

r -d u d 2 u d^ u 

J ~dx = dTx~ 2 ~ dlT 3 = tlien the Tesultin S value of u 

shall be a MAX., MIN. or NEITHER according as - " is NEGATIVE, PO- 

11 X. 

SITIVE, or ZERO ; and so on continually. 

Ex. 1. To find the MAX. and MIN. of the ordinate of a common para 

y = V a x 
d y _ J^ V~SL 
d x 2 y~^ 
which cannot = 0, unless x = oc . 

Hence the parabola has no maxima or minima ordinates. 
Ex. 2. To Jind the MAXIMA and MINIMA of y in the equation 

y 2 2axy + x 2 = b 2 . 

d y /d y 

d_y _ ay x d 2 y __ * ^jJ^ 

dx y_ax dx 2 ~ y_ ax 

d V 
and putting ^- = 0, we get 

- _____ _ 

V (l_a 2 ) " V (1 a 2 ) dx 2 ~ b~Vjl a 8 ) 

which indicate and determine both a maximum and a minimum. 

Ex. 3. 7b rfiw/Wc a in such a manner that the product of the m lh power 
of the one part, and the power of the other shall be a maximum. 
Let x be one part, then a x = the other, and by the question 

u = x m . (a _ x )n - max . 

du _ 

* a^ ~ ~ ( a x ) " ~ X (m a x. m + n) 



d x 

_ x m - 2 ( a _ x ) n - 2 x ( m + n 1. m + n. x 2 &c.) 

Put -r- = ; then 
d x 

m a 
x 0, or x = a, or x 

in + n 
the two former of which when m and n are even numbers give minima, 

and the last the required maximum. 


Ex. 4. Let u = x x . 

d u 1 1.x 7 7 u 

j = u. i = 0, . . 1. x = 1, and x e the hyperbolic base 

Cl A. A. 

= 2.71828, &c. 

Innumerable other examples occur in researches in the doctrine of 
curves, optics, astronomy, and in short, every branch of both abstract and 
applied mathematics. Enough has been said, however, fully to demon 
strate the general principle, when applied to functions of one independent 
variable only. 

For the MAXIMA and MINIMA of functions of two or more variables, see 
Lacroix, 4to. 

35. If in the expression (30 a. g) S T should be finite when s is infinite, 
then the corresponding tangent is called an Asymptote to the curve, and 
since g and this Asymptote are both infinite they are parallel. Hence 
To Jind the Asymptotes to a curve, 

d 6 
In S T = f 2 -j , make g = oc , then each finite value of S T gives an 

Asymptote ; which may be drawn, by finding from the equation to the 
curve the values of 6 for g = a, (which will determine the positions of g), 
then by drawing through S at right angles to g, S T, S T , S T", &c. the 
several values of the subtangent of the asymptotes, and finally through 
T, T , 1", &c. perpendiculars to S T, S T , S T", &c. These perpen 
diculars will be the asymptotes required. 
Ex. In the hyperbola 

_ _ _ _ 
^ ~~ a (1 e cos. 6) 


Here g = a , gives 1 e cos. 6 = 0, .. cos. 6 = 

/. + 6 = L. whose cos. is -- 

Also S T = 



b 2 b 2 

\T~A T^o -7 = b > whence it will be seen that 

a e sin. 6 a V e z 1 

the asymptotes are equally inclined (viz. by L. 6) to the axis, and pass 
through the center. 

The expression (29. e) will also lead to the discovery and construction 
of asymptotes. 

Since the tangent is the nearest straight line that can be drawn to the 
curve at the point of contact, it affords the means of ascertaining the in 
clination of the curve to any line given in position ; also whether at any 
point the curve be inflected, or from concave become convex and vice ver 
sa ; also whether at any point two or more branches of the curve meet, 
i. e. whether that point be double, triple, &c. 

36. To Jind the inclination of a curve at any point of it to a given line , 
Jmd that of the tangent at that given point, which will be the inclination 

Hence if the inclination of the tangent to the axis of a curve be zero, 
the ordinate will then be a maximum or minimum ; for then 

tan. T = = 

(31. h) 

37. To Jind the points of Inflexion of a curve. 

A B A B 

Let y = f (x) be the equation to the curve a b ; then A a, B b being 
any two ordinates, and ana tangent at the point a, if we put A a = y, 
and A B = h, we get 

A a = f x 


i> r h 4. lly 

But B n = 

mn = y. -f. . 


dT* 172 + &c & 2 c] 

Consequently B b is < or > B n 

d 2 y. 
according as -r is negative or positive, i. e. the curve is 

concave or con- 


d 2 y . 
vex towards its axis according as -^ - z is negative or positive. 

Hence also, since a quantity in passing from positive to negative, and 
vice vwsa, must become zero or infinity, at a point of inflexion 

d 2 y 

i or a 

d x 2 

Ex. In the Conchoid of Nicomedes 

x y = (a + y ) V (b 2 y 2 ) 
which gives, by making d y constant, 

d 2 x _ 2 b 4 a b 2 y 3 3 b 2 a y * 

and putting this = 0, and reducing, there results 

which will give y and then x. 

These points of inflexion are those which the Theory of (34) indicates 
as belonging to neither maxima nor minima , and pursuing this subject 
still farther, it will be found, in like manner, that in some curves 

d 4 v d 6 v 

^ 4 = or a , -, 4 = or a , &c. = &c. 

d x 4 d x 6 

also determine Points of Inflexion. 

38. Tojind DOUBLE, TRIPLE, Sfc. points of a curve. 

If the branches of the curve cut one another, there will evidently be as 
many tangents as branches, and consequently either of the expressions, 

Tan. T = ^ (31. h) 

d x 

M T = 2-j-i (29. e) 

as derived from the equation of the curve, will have as many values as 
there are branches, and thus the nature and position of the point will be 

If the branches of the curve touch, then the tangents coincide, and the 
method of discovering such multiple points becomes too intricate to be in 
troduced in a brief sketch like the present. For the entire Theory of 
Curves the reader is referred to Cramer s express treatise on that subject, 
or to Lacroix s Different, and Integ. Calculus, 4to. edit. 

39. We once more return to the text, and resume our comments. We 
pass by LEMMA VIII as containing no difficulty which has not been al 
ready explained. 

As similar figures and their properties are required for the demonstra- 


tion of LEMMA IX, we shall now use LEMMA VII in establishing LEMMA 
V, and shall thence proceed to show what figures are similar and how to 
construct them. 

According to Newton s notion of similar curvilinear figures, we may 
define two curvilinear figures to be similar when any rectilinear polygon 
being inscribed in one of them, a rectilinear polygon similar to the former, 
may always be inscribed in the other. 

Hence, increasing the number of the sides of the polygons, and dimi 
nishing their lengths indefinitely, the lengths and areas of the curvilinear 
figures will be the limits by LEMMAS VII and III, of those of the recti 
linear polygons, and we shall, therefore, have by Euclid these lengths 
and areas in direct and duplicate proportions of the homologous sides 

40. To construct curves similar to given ones. 

If y, x be the ordinate and abscissa, and x the corresponding abscissa 
of the required curve, we have 

x:y: :x :Z x x = y \ .* . . . < a j ^ 

the ordinate of the required curve, which gives that point in it which 
corresponds to the point in the given curve whose coordinates are x, y; 
and in the same manner may as many other points as we please be de 

In such curves, however, as admit a practical or mechanical construc 
tion, it will frequently be sufficient to determine but one or two values of y . 

Ex. 1. In the circle let x, measured along the diameter from its extre 
mity, be r (the radius) ; then y r, and we have 

y = 2- x x = x 


where x may be of any magnitude whatever. Hence, all semicircles, and 
therefore circles, are similar Jfgures. 

Ex. 2. In a circular arc (2 a) let x be measured along the chord (2 b), 
and suppose x = r sin. a ; then y = r . vers. a 

, vers. a 

y = HI x x 

sin. a 

which gives the greatest ordinate to any semichord as an abscissa, of the 
required arc, and thence since 

y = r V r 2 x * 

it will be easy to find the radius r and centre, and to describe the arc 


But since 

y r vers. a! vers. vers. a 
x r sin. a! sin. a sin. a 


a a 

2 sin. * ,2 sin. ~ 

1 cos. a 21 cos. a 

sin. a a . a sin. a a . a 

2 cos. sin. 2 cos. sin. 

& 22 


a a 

tan. - = tan. ^ 


. .a = a 

which accords with Euclid, and shows that similar arcs of circles subtend 
equal angles. 

Ex. 3. Given an arc of a parabola, "whose latus-rectiim is p, to Jind a 
similar one, whose latus-rectum shall be p . 

In the first place, since the arc is given, the coordinates at its extremi 
ties are ; whence may be determined its axis and vertex ; and by the usual 
mode of describing the parabola it may be completed to the vertex. 
Now, since 

y 2 = p x 

x, x being measured along the axis, and when 

v P 

/. v = . x = . x = 2 x 

x y 

which shows that all semi-parabolas, and therefore parabolas, are similar 
figures. Hence, having described upon the axis of the given parabola, 
any other having the same vertex, the arc of this latter intercepted be 
tween the points whose coordinates correspond to those of the extremi 
ties of the given arc will be the arc required. 

Ex. 4. In the ellipse whose semi-diameters are a, b, if x be measured 
along the axis, when x = a, y = b. Hence 

y = -_. x 

and x or the semi-axis major being assumed any whatever, this value of 
y will give the semi-axis minor, whence the ellipse may be described. 
This being accomplished, let (a, (3) (a , 8 } be the coordinates at the 


extremities of any given arc of the given ellipse, then the similar one of 
the ellipse described will be that intercepted between the points whose 
coordinates, (x , y ) (x", y") are given by 

y = V (2 a x x 2 ) 
: |3 : : x : y l J a 

a : /3 : : x : y"J an b" , /2 , 

y z V (2 a x x 2 ) 


In like manner it may be found, that 

All cycloids are similar. 

Epicycloids are so, when the radii of their wheels a radii of the spheres. 

Catenaries are similar when the bases <x tensions, Sfc. Sfc. 

40. If it were required to describe the curve A c b (fig. to LEMMA 
VII) not only similar to A C B, but also such that its chord should be of 
the given length (c) ; then having found, as in the last example, the co 
ordinates (x , y ) (x", y") in terms of the assumed value of the abscissa 
(as a in Ex. 4), and (, /3), (a , /3 ) the coordinates at the extremities of 
the given arc, we have 

a function of a : whence a may be found. 

Ex. In the case of a parabola whose equation is y 2 = a x, it will be 
found that (y 2 = a x being the equation of the required parabola) 

whence (a ) is known, or the latus-rectum of the required parabola is so 
determined, that the arc similar to the given one shall have a chord = c. 

41. It is also assumed in the construction both to LEMMA VII and 
LEMMA IX, that, If in similar Jigures, originating in the same point., the 
chords or axes coincide, the tangents at that origin will coincide also. 

Since the chords A B, A b (fig. to LEMMA VII), the parallel secants 
B D, b d, and the tangents A D, A d are corresponding sides, each to 
each, to the similar figures, we have (by LEMMA V) 

A B : B D : : A b : b d 

and L B = L. b. Consequently, by Euclid the L. B A D = L b A d, 
or the tangents coincide. 


To make this still clearer. Let 
M B, M B be two similar curves, 
and A B, A B similar parts of them. 
Let fall from A, B, A , B , the or- 
dinates A a, B b, A a , B b cut 
ting off the corresponding abscissas 
M a, M b, M a , M b , and draw 
the chords A B, A B ; also draw 
A C, A C at right angles to B b, B C . 

Then, since (by LEMMA V) 


a : 

Mb : : 

A a 





: Mb : 

: A 


: B b 


a : 

ab : : 

Aa : 

B C 



: a b : 

: A a 

: B 


AC : 

B C : : 



A a 



: B C : 

: M 


: A 



M a : A a : : M a : A a 
.-. A C : B C : : A C : B C 

and the L. C = L. C 

.-. the triangles A B C, A B C are similar, and the L. B A C = 
^ B A C , i. e. A B is parallel to A B . 

Hence if B, B move up to A, the chords A B, A B shall ultimately 
be parallel, i. e. the tangents (see LEMMA III, Cor. 2 and 3, or LEMMA 
VI,) at A, A are parallel. 

Hence, if the chords coincide, as in fig. to LEMMA VII, the tangents 
coincide also. 

The student is now prepared for the demonstration of the LEMMA. 
He will perceive that as B approaches A, new curves, or parts of curves, 
A c b similar to the parts A C B are supposed continually to be described, 
the point b also approaching d, which may not only be at ajinite distance 
from A, but absolutely fixed. It is also apparent, that as the ratio be 
tween A B and A b decreases, the curve A c b approachas to the straight 
line A b as its limit. 

42. LEMMA XL The construction will be better understood when 
thus effected. 

Take A e of any given magnitude and draw the ordinate e c meeting 
A C product-d in c, and upon A c describe the curve Abe (see 39) 


A D 

similar to A B C. Take A d = A e X -r ^ and erect the ordinate d b 

A & 

meeting A b c in b. Then, since A d, A e are the abscissae corre- 

O * 

spending to A D, A E, the ordinates d b, e c also correspond to the 
ordinates D B, E C, and by LEMMA V we have 

d b : D B : : e c : E C : : A e : A E 

: : A d : A C (by construction) 
and the /- D = L. d. Hence 
b is in the straight line A B produced, &c. &c. 

43. This LEMMA may be proved, without the aid of similar curves, as 
follows : 

A B D = ^-^ . (D F + F B) 

-AD 2 tan> " -i A D B F 
~ 2 2 


where a = /L D A F. 

A BD _ AD 2 , tan, a + A D . B F 
" A C E " A E 2 . tan. a + A E . C G 

Now by LEMMA VII, since L. B A F is indefinite compared with F or B ; 
therefore B F, C G are indefinite compared with A D or A E. Hence 

if L be the limit of . ., , and L + 1 its varying value, we have 
A C Jti 

AD 2 , tan, a + A D . B F 
= A E 8 . tan. a + A E . C G 

and multiplying by the denominator and equating homogeneous terms 
we get 

L . A E 2 . tan. a = AD", tan. 

- f A BD _ AD 2 
)! AlTE ~ A~E~ 2 

44. LEMMA X. " Continually increased or diminished." The word 
" continually" is here introduced for the same reason as continued 
curvature" in LEMMA VI. 

If the force, moreover, be not "Jinite" neither will its effects be ; or 
the velocity, space described, and time will not admit of comparison. 


45. Let the time A D be divided into several portions, such as D d, 
A b B being the locus of the extremities of the ordinates which D repre 
sent, the velocities acquired D B, d b, B 
&c. Then upon these lines D d, &c. 


as bases, there being inscribed rect- 
angles in the figure A D B, and when 
their number is increased and bases 
diminished indefinitely, their ultimate 
sum shall = the curvilinear area D d D A 

A B D (LEMMA III.) But each of these rectangles represents the space 
described in the time denoted by its base ; for during an instant the ve 
locity may be considered constant, and by mechanics we have for constant 
velocities S = T X V. Hence the area A B D represents the whole 
space described in the time A D. 

In the same manner, ACE (see fig. LEMMA X) represents the tune 
A E. But by LEMMA IX these areas are " ipso motus initio," as A D * 
and A E 2 Hence, in the very beginning of the motion, the spaces de 
scribed are also in the duplicate ratio of the times. 

46. Hence may be derived the differential expressions for the space 
described^ velocity acquired, &c. 

Let the velocity B D acquired in the time t (A D) be denoted by v, 
and the space described, by s. 

Then, ultimately >, we have 

Dd = dt,Bn = dv, 

Dnbd = ds = Ddxdb = dtXv. 

d s . d s 
v = ,ds = vdt, d t = (a) 

Again, if D d =r d D , the spaces described in these successive instants, 
are D b, D m, and therefore ultimately the fluxion of the space repre 
sented by the ultimate state of D m is b n r m or 2 b m B . Hence 

d (d s) = 2 X b m B ultimately, 

and supposing B to move up to A, since in the limit at A, B coincides 
with A, arid B m with A D, and therefore b m B or d (d s) represents 
the space described " in the very beginning of the motion." 
Hence by the LEMMA, 

d (ds) a 2 d t 2 a d t 2 
or with the same accelerating force 

d 2 s a d t 2 (b) 


With different accelerating forces d 2 s must be proportionably increased 
or diminished, and .*. (see Wood s Mechanics) 

d 2 s a Fdt 2 
Hence we have, after properly adjusting the units of force, &c. 

d 2 s = Fdt 2 . 
and . . I 

d 2 s f - .*v-tfv.-. f - ( c ) 
F:= dT 2 3 

Hence also and by means of (a) considering d t constant, 

F = , v d v = F d s (d) 

all of which expressions will be of the utmost use in our subsequent 

47. LEMMA X. COR. I. To make this corollary intelligible it will be 
useful to prove the general principle, that 

If a body, moving in a curve, be acted upon by any new accelerating 
force, the distance between the points at which it would arrive WITHOUT 
and WITH the new force in the same time, or " error," is equal to the space 
that the new force, acting solely, would cause it to describe in that same 

Let a body move in the curve ABC, and when at B, let an additional 
force act in the direction B b. Also let B D, D E, E C ; 
B F, F G, G b be spaces that would be described in equal times by the 
body moving in the curve, and when moved by the sole action of the new 
force. Then draw tangents at the points B, D, E meeting D d, E e, C c, 
each parallel to B b, in P, Q, R. Also draw F M, G R, b d parallel to 
B P; M S, R N, d e parallel to D Qj and S V, N T, e c parallel to 


Now since the body at B is acted upon by forces which separately 
would cause it to move through B D, B F, or, when the number of 
the spaces is increased and their magnitude diminished in infinitum, 
through B P, B F in same time, therefore by LAW III, Cor. 1, when 
these forces act together, the body will move in that time through the 
diagonal up to M. In the same manner it may be shown to move from 
M to N, and from N to C in the succeeding times. Hence, if the num 
ber of the times be increased and their duration indefinitely diminished, 
the body will have moved through an indefinite number of points M, N, 
&c. up to C, describing a curve B C. Also since b d, d e, e c are each 
parallel to the tangents at B, D, E, or ultimately to the curve B D E C ; 
.. b d e c ultimately assimilates itself to a curve equal and parallel to 
B D E C ; moreover C c is parallel to B b. Hence C c is also equal 
to Bb. 

Hence, then, The Error caused by any disturbing force acting upon a 
body moving in a curve, is equal to the space that would be described by 
means of the sole action of that force, and moreover it is parallel to the 
direction of that force. Wherefore, if the disturbing force be constant, it is 
easily inferred from LEMMAS X and IX, and indeed is shown in all books 
on Mechanics, that the errors are as the squares of the times in which they 
are generated. Also, if the disturbing forces be nearly constant, then the 
errors areas the squares of the times quamproxime. But these conclusions, 
the same as those which Note 118 of the Jesuits, Le Seur and Jacquier, 
(see Glasgow edit. 1822.) leads to, do not prove the assertion of Newton 
in the corollary under consideration, inasmuch as they are general for all 
curves, and apply not to similar curves in particular. 

48. Now let a curve similar to the above be constructed, and completing 
the figure, let the points corresponding to A, B, &c. be denoted by 
A , B , &c. and let the times in which the similar parts of these curves, 
viz. B D, B D ; D E, D E ; E C, E C are described, be in the ratio 
t : t . Then the times in which, by the same disturbing force, the spaces 
B F, B F ; F G, F G ; G b, G b are described, are in the ratio of 
t : t . Hence, " in ipso motus initio" (by LEMMA X) we have 
B F : B F : : t 2 : t 2 
F G : FG : : t 2 : t 2 

&c. &c. 
and therefore, 

B F + F G + &c. : B F + F 7 G + &c. : : t 2 : t 2 


But, (by 15,) 

B F + F G + &c. = the error C c, 

B F + F G + &c. = the error C c , 

and the times in which B C, B 7 C are described, are in the ratio t : t . 
Hence then 

C c : a c : : t 2 : t 

or The ERRORS arising from equal forces, applied at corresponding points, 
disturbing the motions of bodies in similar curves, which describe similar 
parts of those curves in proportional times, are as the squares of the times 
in which they are generated EXACTLY, and not " quam proxime" 

Hence Newton appears to have neglected to investigate this corollary. 
The corollary indeed did not merit any great attention, being limited by 
several restrictions to very particular cases. 

It would seem from this and the last No. that Newton s meaning in 
the forces being " similarly applied," is merely that they are to be applied 
at corresponding points, and do not necessarily act in directions similarly 
situated with respect to the curves. 

For explanation with regard to the other corollaries, see 46. 

49. LEMMA XI. " Finite Curvature" Before we can form any precise 
notion as to the curvature at any point of a curve s being Finite, Infinite or 
Infinitesimal, some method of measuring curvature in general must be de 
vised. This measure evidently depends on the ultimate angle contained by 
the chord and tangent ( A B, A D) or on the angle of contact. Now, although 
this angle can have no finite value when singly considered, yet when two 
such angles are compared, their ratio may be finite, and if any known 
curvature be assumed of a standard magnitude, we shall have, by the 
equality between the ratios of the angles of contact and the curvatures, the 
curvature at any point in any curve whatever. In practice, however, it 
is more commodious to compare the subtenses of the angles of contact 
(which may be considered circular arcs, see LEM.MA VII, having; radii in 


a ratio of equality, and therefore are accurate measures of them), than the 
angles themselves. 

50. Ex. 1. Let the circumference of a circle be divided into any num 
ber of equal parts and the points of division being joined, let there be ? 
tangent drawn at every such point meeting a perpendicular let fall from 
the next point ; then it may easily be shown that these perpendiculars or 
subtenses are all equal, and if the number of parts be increased, and their 


[SECT. I. 

magnitude diminished, in infinitum, they will have a ratio of equality. 
Hence, the CIRCLE has the same curvature at every point, or it is a curve 
of uniform curvature. 

51. Ex. 2. Let two circles touch one 
another in the point A, having the 
common tangent A D. Also let B D 
be perpendicular to A D and cut the 
circle A D in B . Join A B, A B . 
Then since A "B, A B are ultimately 
equal to A D (LEMMA VII) they are 
equal to one another, and consequently 
the limiting ratio of B D and B D, is 
that of the curvatures of the respective 
circles A C, A D (by 17.) 

But, by the nature of the circle, 

A D 2 = 2 R X D B D B 2 = 2 r X 
R and r being the radii of the circles. 


D B 2 R D B 
L+ DB ~2r -DB 

and equating homogeneous terms we have 

D B D B 

i. e. The curvatures of circles are inversely as their radii. 

52. Hence, if the curvature of the circle whose radius is 1, (inch, foot, 
or any other measure,) be denoted by C, that of any other circle whose 

radius is r, is 


53. Hence, if the radius r of a circle compared with 1, definite, its 
curvature compared with C, is finite ; if r be infinite the curvature is 
infinitesimal ,- if r be infinitesimal the curvature is infinite, and so 011 through 
all the higher orders of infinites and infinitesimals. By infinites and in 
finitesimals are understood quantities indefinitely great or small. 

The above sufficiently explains why curvature, compared with a given 
standard (as C), can be said to definite or indefinite. We are yet to show 
the reason of the restriction to curves of finite curvature, in the enuncia 
tion of the LEMMA. 

54. The circles which pass through A, B, G ; a, b, g, (fig. LEMMA XI) 


have the same tangent A D with the curve and the same subtenses. Hence 
(49. and 52.) these circles ultimately have the same curvature as the curve, 
i. e. A I is the diameter of that circle which has the same curvature as the 
curve at A. Hence, according as A I is finite or indefinite, the curvature 
at A is so likewise, compared with that of circles of finite radius. 
Now A G ultimately, or 

: ^~D 
whether A I be finite or not. If finite, B D a A B 2 , as we also learn 

from the text. 

A B - 
55. If the curvature be infinitesimal or A I infinite ; then since -g-jj 

is infinite, B D must be infinitely less than A B ~, or, A B being 
always considered in its ultimate state an infinitesimal of the first order, 
B D is that of the third order, i. e. B D oc A B 3 . The converse is 
also true. 

Ex. In the cubical parabola, the abscissa tx as the cube of the or- 
dinate ; hence at its vertex the curvature is infinitely small. At other 
points, however, of this curve, as we shall see hereafter, the curvature is 


To show at once the different proportions between the subtenses of the 
angles of contact and the conterminous arcs, corresponding to the differ 
ent orders of infinitesimal or infinite curvatures, and to make intelligible 
this intricate subject, let A B ultimately considered be indefinitely small 

A B 2 

compared with 1 ; then since -^-^- = A B, A B 2 is infinitesimal com- 

A B n 
pared with A B ; and generally . p n-I = A B, shows that A B n is 

infinitely small compared with A B n - * so that the different orders of in- 
Jinitesimals may be correctly denoted by 

AB, AB 2 , AB 3 , A B*, &c. 

Also since 1 is infinite compared with the infinitesimal A B, and A B 
compared with A B \ &c. the different orders of infinites may be repre 
sented by 

1 * 1 1 &c 

A~B A~B~ 2 AB 3 AB 4 

56. Hence if the curvature at any point of a curve be infinitesimal in 
the second degree 


A B 2 1 

v> TV Qt . , and B D oc A B 4 , and conversely. 
-D L) A 15 

And generally, if the curvature be infinitesimal in the n th degree, 

A B 2 1 
JVfT a A R n? an( ^ ^^ a A B n + 2 , and conversely. 

Again, if the curvature be infinite in the n th degree, 

A B 2 

--^ cc A B n , and B D oc A B 2 - n , and conversely. 

The parabolas of the different orders will afford examples to the above 

57. The above is sufficient to explain the first case of the LEMMA. 
Case 2. presents no difficulty ; for b d, B D being inclined at any equal 

angles to A D, they will be parallel and form, with the perpendiculars let 
fall from b, B upon A D, similar triangles, whose sides being propor 
tional, the ratio between B D, b d will be the same as in Case 1. 

Case 3. If B D converge, i. e. pass through when produced to a given 
point, b d will also, and ultimately when d and D move up to A, the 
difference between the angles A d b, A D B will be less than any 
that can be assigned, i. e. B D and b d will be ultimately parallel; 
which reduces this case to Case 2. (See Note 125. of PP. Le Seur and 

Instead of passing through a given point, B D, b d may be supposed 
to touch perpetually any given curve, as a circle for instance, and B D 
will still a AD 2 ; for the angles D, d are ultimately equal, inasmuch as 
from the same point A there can evidently be but one line drawn touch 
ing the circle or curve. 

Many other laws determining B D might be devised, but the above 
will be sufficient to illustrate Newton s expression, " or let B D be deter 
mined by any other law whatever." It may, however, be farther observed 
that this law must be definite or such as will^-r B D. For instance, the 
LEMMA would not be true if this law were that B D should cut instead of 
touch the given circle. 

58. LEMMA XL Cou. II. It may be thus explained. Let P be 
the given point towards which the sagittae S G, s g, bisecting the chords 
A B, A b, converge. S G, s g shall ultimately be as the squares of 
A B, A b, &c. 




For join P B, P b and produce 
them, as also P G, P g, to meet the 
tangent in D, d, T. t. Then if B 
and b move up to A, the angles 
T P D, t P d, or the differences be 
tween the angles ATP and A D P, 
and between A t P and. A d P, may 
be diminished without limit; that is, 
(LEMMA I), the angles at T, D and 
at t, d are ultimately equal. Hence 
the triangles ATS, A D B are 
similar, as likewise are A t s, A d b. 


ST : D B 

s t : d b 

.-. S T : s t : 
Also by LEMMA VII, 

S T : st : 

and by LEMMA XI, Case 3, 
D B : d b 
.-. S G : s s : 

S G : 

AB 2 
AB 2 

A S : A B 


D B : db 

S S 

Ab 2 
Ab 2 

Q. e. d. 

Moreover, it hence appears, that the sagittte which cut the chords, in 
ANY GIVEN RATIO WHATEVER., and tend to a given point, have ultimately 
the same ratio as the subtenses of the angles of contact, and are as the squares 
of the corresponding arcs, chords, or tangents. 

59. LEMMA XL COR. III. If the velocity of a body be constant or 
"given," the space described is proportional to the time t. Hence 
A B a t, and .-. S G a A B 2 a t 2 . 

60. LEMMA XL COR. IV. Supposing B D, b d at right angles to 
A D (and they have the same proportion when inclined at a given angle 
to A D, and also when tending to a given point, &c.) we have 


AADB: AAdb::^-^-?- A d x db 

2 2 

:: ?T XAD: Ad 

A D 2 
r^-* AD: Ad 

: : A D 3 : A d 3 . 


A d 

: : (D B) ^ : (d b) * 

It may be observed here, that the tyro, on reverting to LEMMA IX, 
usually infers from it that 

A A D B a A D 2 and does not a. AD 3 , 

but then he does not consider that A D, in LEMMA IX, cuts or makes a 
Jinite angle with the curve, whereas in LEMMA XI it touches the curve. 

61. LEMMA XI. COR. V. Since in the common parabola the ab 
scissa a square of the ordinate, and likewise B D or A C a A D 2 or 
C D 2 , it is evident that the curve may ultimately be considered a 

This being admitted, we learn from Ex. 1, No. 4, that the curvilinear 
area A C B = -f of the rectangle C D. Whence the curvilinear area 
A B D = | of C D = f of the triangle A B D, or the area A B D a 
triangle A B D a A D 3 , &c. (by Cor. 4.) So far B D, b d have been 
considered at right angles to A D. Let them now be inclined to it at a 
given angle, or let them tend to a given point, or " be determined by any 
other law;" then (LEMMA, Case 3, and No. 25) B D, b d will ultimately 
be parallel. Hence, B D , b d (fig. No. 26) being the corresponding 
subtenses perpendicular to A D, it is plain enough that the ultimate dif 
ferences between the curvilinear areas A B D, A B D and between 
A b d, A b d are the similar triangles B D D , b d d , which 
differences are therefore as B D 2 , b d 2 , or as A B 4 , A b 4 , i. e. 
BDD a A B 4 . 

But we have shown that A B D a A B 3 . 



ABD = ABD+BDD / = axAB 3 + bxAB 4 =AB 3 (a + bxAB) 
and b X A B being indefinite compared with a, (see Art. 6,) 
ABD = axAB 3 a A B 3 . 

Q. e. d. 


62. What Newton asserts in the Scholium, and his commentators Le 
Seur and Jacquier endeavour (unsuccessfully) to elucidate, with regard to 
the different orders of the angles of contact or curvatures, may be briefly 
explained, thus. 

Let D B ex A D m . Then the diameter of curvature, which equals 

A D 2 

-jjg- (see No. 22 and 24), a AD 2 -" 1 . Similarly if D B ot AD", the 

diameter of curvature <x A D 2 ~ n . Hence D and D represents these 
diameters, we have 

D a X A D 2 ~ m a 

D 7 = a X AD 2 - n = "a 7 D m ( a and a bein S finite ) 

and if n = 2 or D definite, then D will bejinite, infinitesimal, or infinite, 
according as m = 2, or is any number, (whole, fractional, or even transcen 
dental) less than 2, or any number greater than 2. Again, if m = n 
then D compared with D is finite, since D : D : : a : a . If m be less 
than n in any finite degree, then n m is positive, and D is always in 
finitely less than D . If m be greater than n, then 

D a 1 

= -7 X 

D "- a AD 

and m n being positive, D is always infinite compared with D . 

Hence then, there is no limit to the orders of diameters of curvature, 
with regard to infinite and infinitesimal, and consequently not to the 

63. In this Scholium Newton says, that " Those things which have 
been demonstrated of curve lines and the surfaces which they comprehend 
are easily applied to the curve surfaces and contents of solids." Let us 
attempt this application, or rather to show, 

1st, That if any number of parallelepipeds of equal bases be inscribed in 
any solid, and the same number having the same bases be also circumscribed 

VOL. I. D 



[SECT. I. 

about it ; then the number of these parallelepipeds being increased and their 
magnitude diminished IN INFINITUM, the ultimate ratios which the aggre 
gates of the inscribed and circumscribed parallelopipeds have to one another 
and to the solid, are ratios of equality. 


Let A S T U V Z Y X W A be any portion of a solid cut off by three 
planes A A V, A A Z and Z A V, passing through the same point A , 
and perpendicular to one another. Also let the intersections of these 
planes with one another be A A , A V, A Z, arid with the surface of the 
solid be A U V, A Y Z and Z 1 V. Moreover let A V, A Z be each 
divided into any number of equal parts in the points B , T , U ; D , X , Y , 
and through them let planes, parallel to A A" Z and A A V respectively, 
be supposed to pass, whose intersections with the planes A A V, A A Z 


shall be S B 7 , T T, U U ; W D 7 , X X , Y Y 7 , and with the plane 
A 7 Z V, 1 W, m T 7 , n U ; t D 7 , s X , o Y , respectively. Again, let the 
intersections of these planes with the curve surface be S P 1, T Q m, 
U R n ; WPt, XQs, YRo respectively. Also suppose their several 
mutual intersections to be P C 7 , P E 7 , P" x, P " G 7 , Q F 7 , Q H 7 , Q" K 7 , 
&c. ; those of these planes taken in pairs and of the plane A Z V, being 
the points C 7 , E 7 , x, G 7 , F 7 , H 7 , K , F, &c. and those of these pairs of 
planes and of the curve surface, the points P, P , P", P" , Q, Q , Q", R, &c. 

Now the planes, passing through B 7 , T 7 , U 7 , being all parallel to 
A A Z, are parallel to one another and perpendicular to A A V. Also 
because the planes passing through D 7 , X 7 , Y are parallel to A A 7 V, 
they are parallel to one another, and perpendicular to A A? Z. Hence 
(Euc. B. XL) S B , T T 7 , U U 7 , W D , X X 7 , Y Y 7 , as also P C 7 , P 7 E 7 , 
P 77 x, P 777 G 7 , Q F 7 , Q 7 H 7 , Q 77 K 7 , &c. &c. are parallel to A A 7 and to 
one another. It is also evident, for the same reasons, that B 7 1, T 7 m, U 7 n, 
are parallel to A 7 Z and to one another, as also are D 7 1, X 7 s, Y 7 o to 
A 7 V and to one another. Hence also it follows that A 7 B 7 C 7 D 7 , 
B 7 C 7 E 7 T , &c. are rectangles, which rectangles, having their sides equal, 
are themselves equal. 

Again, from the points A, P, Q, R in the curve surface, draw A B, 
A D; P E, P G; Q H, Q K; R L, R N parallel to A 7 B 7 , A 7 D 7 ; 
C 7 E 7 , C 7 G 7 ; F 7 H 7 , T 7 K 7 , I 7 o, I 7 n and meeting B 7 S, D 7 W; E 7 P , 
G 7 P 777 ; H 7 Q 7 , K 7 Q 77 produced in the points B, D; E, G; H, K, re 
spectively. Then complete the rectangles A C, P F, Q I which, being 
equal and parallel to A 7 C 7 , C 7 F 7 , F 7 I 7 , will evidently, when C 7 P, F 7 Q, 
I 7 R are produced to C, F, I, complete the rectangular parallelepipeds 
A C 7 , P F 7 , Q I 7 . Moreover, supposing F 7 I 7 the last rectangle wholly 
within the curve Z V produce K 7 I 7 , H 7 I 7 and make I 7 L 7 , I 7 N 7 equal 
K I 7 , H 7 I 7 , and complete the rectangle I M 7 . Also complete the 
parallelepiped R M 7 . 

Again, produce E P, G P, H Q, K Q; L R, N R to the points d, b ; 
g, e; k, h, and complete the rectangles Pa, Q p, R q thereby dividing 
the parallelepipeds A C 7 , P F 7 , Q I 7 , each into two others, viz. A P, 
aC 7 ; PQ, pF 7 ; Q R, q I . 

Now the difference between the sum of the inscribed parallelepipeds 
a C 7 , p F 7 , q P, and that of the circumscribed ones A C 7 , P F 7 , Q P, R M 7 , 
is evidently the sum of the parallelepipeds A P, P Q, Q R, R M 7 ; that 
is, since their bases are equal and the altitudes P R 7 , R I, Q F, PC 
are together equal to A A 7 , this difference is equal to the parallelepiped 
A C 7 . In the same manner if a series of inscribed and circumscribed 



rectangular parallelepipeds, having the bases B E , E H , H L , be 
constructed, the difference between their aggregates will equal the paral 
lelepiped whose base is B E and altitude S B , and so on with every 
series that can be constructed on bases succeeding each other diagonally. 
Hence then the difference between the sums of all the parallelepipeds 
that can be inscribed in the curve surface A Z V and circumscribed about 
it, is the sum of the parallelepipeds whose bases are each equal to A C 
and altitudes are A A , S B , T T ; , U U , W D , X X , Y Y . Let 
now the number of the parts A B , B T , T U , U V, and of the parts 
A D , D X , X? Y , Y 7 Z be increased, and their magnitude diminished 
in infinitum, and it is evident the aforesaid sum of the parallelepipeds, 
which are comprised between the planes A A Z, S B 1 and between the 
planes A A! V, W D t, will also be diminished without limit ; that is, the 
difference between the inscribed and circumscribed whole solid is ulti 
mately less than any that can be assigned, and these solids are ultimately 
equal, and a fortiori is the intermediate curve-surfaced solid equal to either 
of them (see LEMMA I and Art. 6.) Q. e. d. 

Hitherto only such portions of solids as are bounded by three planes 
perpendicular to one another, and passing through the same point, have 
been considered. But since a complete curve- surfaced solid will consist of 
four such portions, it is evident that what has been demonstrated of any 
one portion must hold with regard to the whole. Moreover, if the solid 
should not be curve-surfaced throughout, but have one, two, or three plane 
faces, there will be no difficulty in modifying the above to suit any parti 
cular case. 

2dly, If in two curve-surfaced solids there be inscribed two series of paral 
lelepipeds, each of the same number ,- and ultimately these parattelopipeds 
have to each other a given ratio., the solids themselves have to one another 
that same ratio. 

This follows at once from the above and the composition of ratios. 

3dly, All the corresponding edges or sides, rectilinear or curvilinear, of 
similar solids are proportionals ; also the corresponding surfaces, plane or 
curved, are in the duplicate ratio of the sides ; and the volumes or contents 
are in the triplicate ratio of the sides. 

When the solids have plane surfaces only, the above is shown to be 
true by Euclid. 

When, however, the solids are curve-surfaced, wholly or in part, we 
must define them to be similar when any plane- surf aced solid whatever 
being inscribed in any one of them, similar ones may also be inscribed in the 


others. Hence it is evident that the corresponding plane surfaces are 
similar, and consequently, by LEMMA V, the corresponding edges are 
proportional, and the corresponding plane surfaces are in the duplicate 
ratio of these edges or sides. Moreover, if the same number of similar 
parallelepipeds be inscribed in the solids, and that number be indefinitely 
increased, it follows from 63. 1 and the composition of ratios, that the 
curved surfaces are proportional to the corresponding plane surfaces, and 
therefore in the duplicate ratio of the corresponding edges ; and also that 
the contents are proportional to the corresponding inscribed parallelepi 
peds, or (by Euclid) in the triplicate ratio of the edges. 

These three cases will enable the student of himself to pursue the ana 
logy as far as he may wish. We shall " leave him to his own devices," 
after cautioning him against supposing that a curved-surface, at any point 
of it, has a certain fixed degree of curvature or deflection from the tangent- 
plane, and therefore that there is a sphere, touching the tangent-plane at 
that point, whose diameter shall be the limit of the diameters of all the 
spheres that can be made to touch the tangent-plane or curved-surface 
analogously to A I in LEMMA XI. Every curvilinear section of a curved- 
surface, made by a plane passing through a given point, has at that point 
a different curvature, the curved-surface being taken in the general sense; 
and it is a problem of Maxima and Minima To determine those sections 
which present the greatest and least degrees of curvature. 

The other points of this Scholium require no particular remarks. If 
the student be desirous of knowing in what consists the distinction be 
tween the obsolete methods of Exhaustions, Indivisibles, &c. and that of 
PRIME AND ULTIMATE RATIOS, let him go to the original sources to the 
works of Archimedes, Cavalerius, &c. 

64. Before we close our comments upon this very important part of the 
Principia, we may be excused, perhaps, if we enter into the detail of the 
Principle delivered in Art. 6, which has already afforded us so much 
illustration of the text, and, as we shall see hereafter, so many valuable 
results. We have thence obtained a number of the ordinary rules for 
deducing indefinite forms from given definite functions of one variable ; 
and it will be confessed, by competent and candid judges, that these ap 
plications of the principle strongly confirm it. Enough has indeed been 
already developed of the principle, to prove it clearly divested of all the 
metaphysical obscurities and inconsistencies, which render the methods of 
Fluxions, Differential Calculus, &c. &c. so objectionable as to their logic, 
and which have given rise to so many theories, all tending to establish 

n 3 


the same rules. It is incredible that the great men, who successively in 
troduced their several theories, should have been satisfied with the 
reasonings by which they attempted to establish them. So many con 
flicting opinions, as to the principles of the science, go only to show that 
all were founded in error. Although it is generally difficult, and often 
impossible, for even the most sharp-sighted of men, to discern truth 
through the clouds of error in which she is usually enveloped, yet, when 
she does break through, it is with such distinct beauty and simplicity that 
she is instantly recognized by all. In the murkiness around her there are 
indeed false lights innumerable, and each passing meteor is in turn, by 
many observers, mistaken for the real presence ; but these instantly vanish 
when exposed to the refulgent brightness of truth herself. Thus we have 
seen the various systems of the world, as devised by Ptolemy, Tycho 
Brahe, and Descartes, give way, by the unanimous consent of philoso 
phers, to the demonstrative one of Newton. It is true, the principle of 
gravitation was received at first with caution, from its non-accordance 
with astronomical observations ; but the moment the cause of this discre 
pancy, viz. the erroneous admeasurement of an arc of the meridian, was 
removed, it was hailed universally as truth, and will doubtless be coeval 
with time itself. The Theories relative to quantities indefinitely variable, 
present an argument from which may be drawn conclusions directly op 
posite to the above. Newton himself, dissatisfied with his Fluxions, pro 
duces PRIME AND ULTIMATE RATIOS, and again, dissatisfied with these, he 
introduces the idea of Moments in the second volume of the Principia. 
He is every where constrained to apologize for his obscurities, first in his 
Fluxions for the use of time and velocities, and then again in the Scholium, 
at the end of Sect. I of the Principia, (and in this instance we have shown 
how little it avails him) for reasoning upon nothings. After Newton comes 
Leibnitz, his great though dishonest rival, (we may so designate him, such 
being evidently the sentiments of Newton himself), who, bent upon oblite 
rating all traces of his spoil, melts it down into another form, but yet falls 
into greater errors, as to the true nature of the thing, than the discoverer 
himself. From his Infinitesimals, considered as absolute nothings of the dif 
ferent orders, nothing can be logically deduced, unless by Him (we speak 
with reverence) who made all things from nothing. Suchjiats we mortals 
cannot issue with the same effect, nor do we therefore admit in science, finite 
and tangible consequences deduced from the arithmetic of absolute no 
things, be they ever so many. Then we have a number of theories pro 
mulgated by D Alembert, Euler, Simpson, Marquise L Hopital, &c. &c. 


all more or less modifications of the others all struggling to establish 
and illustrate what the great inventor, with all his almost supernatural 
genius, failed to accomplish. All these diversities in the views of philo 
sophers make, as it has been already observed, a strong argument that 
truth had not then unveiled herself to any of them. Newton strove most 
of any to have a full view, but he caught only a glimpse, as we may per 
ceive by his remaining dissatisfied with it. Hence then it appears, to us 
at least, that the true metaphysics of the doctrine of quantities indefinitely 
variable, remain to this day undiscovered. But it may be asked, after 
this sweeping conclusion, how comes it that the results and rules thence 
obtained all agree in form, and in their application to physics produce 
consequences exactly in conformity with experience and observation ? 
The answer is easy. These forms and results are accurately true, al 
though illogically deduced, from a mere compensation of errors. This has 
been clearly shown in the general expression for the subtangent (Art. 29), 
and all the methods, not even Lagrange s Calcul des Fonctions excepted, 
are liable to the paralogism. Innumerable other instances might be 
adduced, but this one we deem amply sufficient to warrant the above 

After these preliminary observations upon the state of darkness and 
error, which prevails to this day over the scientific horizon, it may per 
haps be expected of us to shine forth to dispel the fog. But we arrogate 
to ourselves no such extraordinary powers. All we pretend to is self- 
satisfaction as to the removal of the difficulties of the science. Having 
engaged to write a Commentary upon the Principia, we naturally sought 
to be satisfied as to the correctness of the method of Prime and Ultimate 
Ratios. The more we endeavoured to remove objections, the more they 
continually presented themselves ; so that after spending many months in 
the fruitless attempt, we had nearly abandoned the work altogether ; 
when suddenly, in examining the method of Indeterminate Coefficients in 
Dr. Wood s Algebra, it occurred that the aggregates of the coefficients of 
the like powers of the indefinite variable, must be separately equal to zero, 
not because the variable might be assumed equal to zero, (which it never 
is, although it is capable of indefinite diminution,) but because of the 
different powers being essentially different from, and forming no part of 
one another. 

From this a train of reflections followed, relative to the treatment of 
homogeneous definite quantities in other branches of Algebra. It was 
soon perceptible that any equation put = 0, consisting of an aggregate of 

D 4 


different quantities incapable of amalgamation by the opposition of plus 
and minus, must give each of these quantities equal to zero. Reverting to 
indefinites, it then appeared that their whole theory might be developed 
on the same principles, and making trial as in Art. 6, and the subsequent 
parts of the preceding commentary, we have satisfied ourselves most fully 
of having thus hit upon a method of clearing up all the difficulties of 
what we shall henceforth, contrary to the intention expressed in Art. 7, 



65. A constant quantity is such, that from its very nature it cannot be 
made less or greater. 

Constants, as such quantities may briefly be called, are denoted generally 
by the first letters of the alphabet, 

a, b, c, d, &c. 

A definite quantity is a GIVEN VALUE of a quantity essentially variable. 

Definite quantities are denoted by the last letters of the alphabet, as 

z, y, x, w, &c. 

An INDEFINITE quantity is a quantity essentially variable through all 
degrees of diminution or of augmentation short of absolute NOTHINGNESS or 

Thus the ordinate of a curve, considered generally, is an indefinite, 
being capable of every degree of diminution. But if any particular value, 
as that which to a given abscissa, for instance, be fixed upon, this value is 
definite. All abstract numbers, as 1, 2, 3, &c. and quantities absolutely 
fixed, are constants. 

66. The difference between two definite values of the same quantity (y) is 
a definite quantity, and may be represented by 

adopting the notation of the Calculus of Finite (or definite} Differences. 

In the same manner the difference between two definite values of A y is 
a definite quantity, and is denoted by 

A (A y) 


or more simply by 

and so on to 



67. The difference between a Definite value and the Indefinite value of 
any quantity y is Indefinite, and we call it the Indefinite Difference of y, and 
denote it, agreeably to the received algorithm, by 

dy (c) 

In the same manner 


the Indefinite Difference of the Indefinite Difference of y, or the second in 
definite difference of y. 

Proceeding thus we arrive at 

d n y (d) 

which means the n th indefinite difference of y. 

68. Definite and Indejinite Differences admit of being also represented 
by lines, as follows : 


Let P P = y be any fixed or definite ordinate of the curve A U, and 
taking P Q = Q R = R S = &c. let ordinates be erected meeting 
the curve in Q, R, S, T, &c. Join P Q, Q R, R S, &c. and produce 
them to meet the ordinates produced in r, s, t, &c. Also draw r s , s t , 


&c. parallel to R S, S T, &c. and draw s t", &c. parallel to s t , &c. ; and 
finally draw P m, Q n, R o, &c. perpendicular to the ordinates. 

Now supposing not only P P but also Q Q , R R , &c. fixed or defi 
nite ; then 

Q m = Q Q PP = APP = Ay 
Rr = n r n R r: Q m R n = A Q m 

= A(AP P) = A 2 PF = A 2 y 
ss =Ss Ss / = Ss Rr = A R r 
= A 3 y 

t t" = t t t t" = t t S S = A S S 

= A(A 3 y) = A 4 y. 
and so on to any extent. 

But if the equal parts P Q , Q R , &c. be arbitrary or indefinite, then 
Q m, R r, s s , 1 1", &c. become so, and they represent the several Inde- 
Jinite Differences of y, viz. 

dy, d 2 y, d 3 y, d 4 y, c. 

69. The reader will henceforth know the distinction between Definite 
and Indefinite Differences. We now proceed to establish, of Indefinite 
Differences., the 


It is evidently a truth perfectly axiomatic, that No aggregate of INDEFI 
NITE quantities can be a definite quantity, or aggregate of definite quanti 
ties^ unless these aggregates are equal to zero. 

It may be said that (a x) + ( a + x ) = 2 a, in which (x) is indefinite, 
and (a) constant or definite, is an instance to the contrary ; but then the 
reply is, a x and a + x are not indefinites in the sense of Art. 65. 

70. Hence if in any equation 

A + B x + C x 2 + D x 3 + &c. = 

A, B, C, &c. be definite quantities and x an indefinite quantity ; then we 

A = 0, B = 0, C = 0, &c. 

For Bx+ Cx 2 + Dx 3 + &c. cannot equal A unless A = 0. 
But by transposing A to the other side of the equation, it does = A. 
Therefore A = and consequently 

B x + C x 2 + D x 3 + &c. = 

x(B + Cx + Dx 2 + &c.) = 


But x being indefinite cannot be equal to ; .. 

B + Cx + Dx 2 + &c. = 
Hence, as before, it may be shown that B =: 0, and therefore 

x (C + D x + &c.) = 
Hence C = 0, and so on throughout. 
71. Again, if in the equation 

A, B, B , C, C , C", D, &c. be definite quantities, and x, y INDEFINITES ; 

A = 0-\ 

B x + B y = \-ivhen y is a function ofx. 
C x 2 + C xy + C"y 2 = Oj 

&c. = 
For, let y = z x, then substituting 

A + x (B + B z) + x 2 (C + C z + C" z 2 ) 

+ x 3 (D + D z + D" z 2 + D " z 3 ) + &c. = 
Hence by 70, 

A = 0, B + B z = 0, C + C z + C" z 2 = 0, &c. 


and substituting for z and reducing we get 


A = 0, B x + B y = 0, &c. 

In the same manner, if we have an equation involving three or more 
indefinites, it may be shown that the aggregates of the homogeneous terms 
must each equal zero. 

This general principle, which is that of Indeterminate Coefficients 
legitimately established and generalized, (the ordinary proofs divide 

B x + C x 2 + &c. = by x, which gives B + Cx+Dx 2 + &c. = 


and not ; x is then put = 0, and thence truly results B = , which 

instead of being 0, may be any quantity whatever, as we know from alge 
bra ; whereas in 70, by considering the nature of x, and the absurdity of 
making it = we avoid the paralogism) conducts us by a near route to 
the Indefinite Differences of functions of one or MORE variables. 

72. To fold the Indefinite Difference of any function ofx. 

Let u = f x denote the function. 

Then d u and d x being the indefinite differences of the function and 

of x itself, v;e have 

u + d u = f (x + d x) 

f (x + d x) = A + B d x + C d x " + &c. 


A, 13, &c. being independent of d x or definite quantities involving x and 
constants ; then 

u + du=A + B d x + C d x 2 -j- &c. 
and by 71, we have 

u = A, d u = B . d x 
Hence then this general rule, 

The INDEFINITE DIFFERENCE of any function of x, f x, is the second 
term in the devclopcmcnt off (x + d x) according to the increasing powers 

Ex. Let u = x n . Then it may easily be shown independently of the 
Binomial Theorem that 

(x + dx) n = x n + n . x n - d x + Pdx 2 

.-. d (x n ) = n . x "- 1 d x 

The student may deduce the results also of Art. 9, 1 0, &c. from this general 

73. To find the indefinite difference of the product of two variables. 
Let u = x y. Then 

u + du=(x + dx).(y + cly) = xy+x dy + y dx + dx dy 
.. d u = x dy+y dx + dx dy 

and by 71, or directly from the homogeneity of the quantities, we have- 
d u = x d y + y d x ........ (a) 


d (x y z) = x d (y z) + y z d x 

= xzdy + xydz + yzdx . . . (b) 
and so on for any number of variables. 

Again, required d . . 


Let = u. Then 


x = y u, and d x u dy + y d u 

x d x u 

. . d d u = --- d y 

y y y 

_y dx x dy } 

y 2 u 

Hence, and from rules already delivered, may be found the Indefinite 
Differences of any functions whatever of two or more variables. We 
refer the student to Peacock s Examples of the Differential Calculus for 

The result (a) may be deduced geometrically from the fig. in Art. 21. 
The sum of the indefinite rectangles A b, b A makes the Indefinite 




We might, in this place, investigate the second, third, &c. Indefinite 
Differences, and give rules for the maxima and minima of functions of two 
or more variables, and extend the Theorems of Maclaurin and Taylor to 
such cases. Much might also be said upon various other applications, 
but the complete discussion of the science we reserve for an express 
Treatise on the subject. We shall hasten to deduce such results as we 
shall obviously want in the course of our subsequent remarks ; beginning 
with the research of a general expression for the radius of curvature of a 
given curve, or for the radius of that circle whose deflection from the 
tangent is the same as that of the curve at the point of contact. 

74. Required the radius of curvature for any point of a given curve. 

Let A P Q R be the given 
curve, referred to the axis A O 
by the ordinate and abscissa 
P M, A M or y and x. P M 
being fixed let Q N, O R be 
any other ordinates taken at 
equal indefinite intervals M N, 
N O. Join P Q and produce 
it to meet O R in r ; and let 
P t be the tangent at P drawn 
by Art. 29, meeting Q N, O R 
in q and t respectively. Again 
draw a circle (as in construc 
tion of LEMMA XI, or other 
wise) passing through P and Q and touching the tangent P t, and there 
fore touching the curve ; and let B D be its diameter parallel to A O. 


Q n = d y, P 11 = d x, P q = P Q (LEMMA VII) = 
V (d x 2 -f- d y 2 ) or d s, if s = arc A P. 

Moreover let 

P M = y ; 

then it readily appears (see Art. 27) that d s = , R being the ra- 

dius of the circle. 

Pq 2 = Qq X (Qq + 2 Q N ) 

= Q q (Q q + 2 d y + 2 /) 



But since 

R t : Q q : : P r 2 : P Q 2 : : 4 : i (LEMMA XI) 

Q q : t r : : 1 : 2 
.-. R t = 2 t r, or R r = t r = 2 Q q 

- Q q = ^ = ^ (by Art. 68.) 

(d 2 y) 2 , R dx d 2 y 

- --- 

and equating Homogeneous Indefinites 
R dx d 2 

d s z = 

d s 

R - ds3 _ (dx 2 + dy 
= dxd 2 y = dx d 2 y 

dx 2 

the general expression for the radius of curvatui e. 
Ex. 1. In the parabola y 2 = a x. 

d y a 
die ~~ !2y 
and since when the curve is concave to the axis d 2 y is negative, 

d y a dy a 2 

~ die 2 = ~ 2~ 2 oTx = ~ 4~ = 


Hence at the vertex R = , and at the extremity of the latus rectum, 

R = a = a V 2. 


Ex. 2. If p be the parameter or the double ordinate passing through 
the focus and 2 a the axis-major of any conic section, its equation is 


2 y d y = pdxHh-^xdx 

2 d y 2 + 2yd 2 y = +. d x s 

d_y _ 

" d X " ~2 


d X s 4 y 

.-. R = 
which reduces to 

R = 

2p 2 

Ex. 3. In the cycloid it is easy to show that 

Aj_ _ j 2r y 
dx *v y 

r being the radius of the generating circle, and x, y referred to the base 
or path of the circle. 

d g y _ _r_ 
* cTx" 2 = " y~* 

. . R = 2v 2ry=2 the normal. 

Hence it is an easy problem iojind the equation to the locus of the centres 
of curvature for the several points of a given curve. 

If y and x be the coordinates of the given curve, and Y and X those of 
the required locus, all referred to the same origin and axis, then the stu 
dent will easily prove that 


^d x 


Y = v 

dx 2 

which will give the equation required, by substituting by means of the 
equation to the given curve. 
In the cycloid for instance 

X = x + V (2 r y y *) 
Y = --y 

whence it easily appears that the locus required is the same cycloid, only 
differing in position from the given one. 

75. Required to express the radius of curvature in terms of the polar co 
ordinates of a curve, viz. in terms of the radius vector g and traced- 
angle 6. 

x = g cos. 6 -\ 

and > 

y = g sin. 6 J 
.-. taking the indefinite differences, and substituting in equation (d) of Art. 

74, we get 

2 dr d_ 

which by means of the equation to the curve will give the radius of curva 
ture required. 

Ex. 1. In the logarithmic spiral 

d = la Xa 

. R _ (g 2 + (la) 2 ^) g 3 (^j! a) 2) 




Ex. 2. In the spiral of Archimedes 

f = a ^ 

Ex. 3. /w the hyperbolic spiral 


Ex. 4. In the Lituus 

. R _ _ 

4a 4 P 4 
Ex. 5. / Me 1 Epicycloid 

g = (r + r ) " 2 r (r + r ) cos. d 

r and r being the radius of the wheel and globe respectively. 

R -- ( r + r ) (3 r 2 2 r r r * + 2 g)* 

2 (3 r 2 r r r 2 ) -f 3 g 

Having already given those results of the Calculus of Indefinite Differ 
ences which are most useful, we proceed to the reverse of the calculus, 
which consists in the investigation of the Indefinites themselves from their 
indefinite differences. In the direct method we seek the Indefinite Differ 
ence of a given function. In the inverse method we have given the Inde 
finite Difference to find the function whose Indefinite Difference it is. This 
inverse method we call 




76. The integral of d x is evidently x + C, since the indefinite differ 
ence of x + C is d x. 

77. Required the integral of a. d x ? 
By Art. 9, we have 

d (a x) = a d x. 
Vor. I. E 


Hence reversely the integral of a d x is a x. This is only one of the in- 
numerable integrals which there are of a d x. We have not only d (a x) 
= a d x but also 

d(ax+C) = adx 
in which C is any constant whatever. 

.-. ax + C =/adx = a/d x . . . (a) (see 76) 
generally, /being the characteristic of an integral. 
78. Required the integral of 

a x P d x. 
By Art. 12 

d(ax n -fC)= n a x " - * d x" -f C =/n a x^ d x 

= n X/ax n ~ 1 dx (77) 

/(i ** X V 
a x n ~ l d x = 1 . 
n n 


But since C is any constant whatever may be written C. 

. ./ax- 1 dx = + C 

Hence it is plain that 

ft Y P + 

Or To find the integral of the product of a constant the p th power of the 
variable and the Indefinite Difference of that variable, let the index of the 
power be increased by \, suppress the Indefinite Difference, multiply by the 
constant, divide by the increased index, and add an arbitrary constant. 

79. Hence 

/(a x P d x + b x * d x + &c.) = 
a XP+ 1 bx"-*- 1 

F+T + q -+-r + &c - + c 

80. Hence also 

/ax- n dx = - - + C. 

(n 1) x n ~ l n 

81. Required the integral of 

ax m ~ 1 dx(b + ex m )P. 

u = b + e x m 

. . d u = mex m ~ l dx 

. . a x m ~ d x = . d u 

m e 

../ax m ~ 1 dx(b+ ex m )P = /* u^du 

v / m ft 

m e 


= /* T-TV u + + C (78) 

m e . (p + 1) 

= , a , .. . (b X e x m ) P+ 1 + C. 

m e (p + 1) 

d x 

82. Required the integral of . 

By 80 it would seem that 

f ci x i r~ 

and if when 

x p /d x 110 

^ ~J~T ~o~~"o~ : : 

But by Art. 17 a. we know that 

d x 

d . 1 x = 


J x 

Here it may be convenient to make the arbitrary constant of the form 1 C 
Therefore % 

/* = 1 x + 1 C = 1 C x 

Hence the integral of a fraction whose numerator is the Indefinite Differ 
ence of the denominator, is the hyperbolic logarithm of the denominator PLUS 
an arbitrary constant. 

83. Hence 

/ax m ~ 1 dx a /" mx m "~ 1 dx 

bx m + e bm , xra 


= JL.l.( x m + - 

b m \ b 

s- .i.v^iA -f- -r- I , 

b m ^ , b/ 

and so on for more complicated forms. 
84. Required the integral of&* d x. 
By Art. 17 

d.a x = la.a x dx 

E 2 


85. If y, x, t, s denote the sine, cosine, tangent, and secant of an angle 
6 ; then we have, Art. 26, 27. 

d y d x d t __ ds 

: =: ~ " 

= tan.- t+C 

/" ds _. = + C = se^- s + C 
J s V2s s 2 

sin. ~~ l y, cos. ~ l x, &c. being symbols for the arc whose sine is y, cosine is 
x, &c. respectively. 

86. Hence, more generally, 

du _ _i_ f v T du 

-bu ).- Vb/ vfl _b u 

< a > 

or = TT X angle whose sine is u ^J to rad. 1 + C. 


/ du 1 / b /i\ 

l-m - r-^v = -TT cos. - 1 u / + C . . (b) 
J V (a bu 2 ) V b V a 



, . f V d 11 

/d u __ 1 / a 

a + b u 2 " V ab J b 


. da _ J_ f V^ u 

/u V(bu 2 a) " V a / " /b, //b . 

UX U - 1 


Moreover, if u be the versed sine of an angb 6, then the sine 
= V (2 u u s ) and 

d u = d (1 cos. 6) = d 6 . sin. 6 (Art. 27.) 
= cU. V (2u u 2 ) 

. dtf- du 

" V(2u u 2 ) 


/_ du - 6 , r 

./V(2u u 2 )" 

= vers. ~ J u + C 
and generally 

2b j 

du T du 

a \ a 


87. Required the integrals of 

dx dx d x 

a + bx a bx a bx 2 

f dx = 2. /d- ( a + 
^a + bx b -/ a + bx 


_ ___ L /*d(a--bx) 
x~ b- a bx 

see Art. 17 a. 



a + bx^a bxj ~-/a s b 2 x 

}_ a-f 

-c (f) 





Hence we easily get by analogy 

/ d x 1 , V a + V b . x 

J a bx 2 ~ vTb V a b x 1 ^ 

1 i ^ a + ^ b . x 
2V r aT>* " V a v b. x 
88. Required the integral of 


ax 2 + bx + c" 
In the first place 

ax2 , f b V (b 2 4 a c) \ 

a t 5 h 2a 2a ~J X 

f , _b_ V (b 2 4 ac)\ f/ J)_x 2 _ b 2 4ac| 

1 2a~ 2a ) & \\** + 2a/ 2a } 

Hence, putting 

we have 

^ i f\ ~~ ^ 
2 a 

d x = d u 

d x d u 

ax* + bx + c -a(u._ b J=ii-<) 

which presents the following cases. 

Case 1. Let a be negative and c be positive ; then 

d x d u " 

f d x _ \7~2 / 2 a p, 

* ^ ^x"Tb^" _ / 2 tan " b 2 4ac" f 

+4ac) V b 2 +4ac 

(see Art. 86) = - / ^ tan.-Yx + ^-) ^/ r ^~ +C . . . (i) 

V ab 2 4ac V 2a/A b* 4ac 

a(b 2 +4ac) 
Case 2. Let c fo negative and a positive ; then 

r d x _ / d u 

4 a c 


2a(b 2 +4ac) 

b 2 + 4 ac 
^ U 


b 2 +4jic b 




2 a 2a 

see Art. 87. 


Case 3. Let b 2 be > 4 a c and a, c be both positive , then 

d_x r d u 

ax 2 + bx + c~ ~~ b 2 4 a 


a / b 2 4 a c 

/ T5 u 

I x I - 


A* 2a(b 2 4ac) b 2 4ac b 

v / x 

-V 2 a 2a 

Case 4. Let b 2 be < 4 a c and a, c be both positive ; 

d x 1 r d u 

a/ 4ac b 2 2 


Case 5. 7^b 2 ^>4ac a;rf a, c both negative ; 

/d x _ 1 /" d u 

ax 2 +bx c~^a / b 2 4ac 8 

Case 6. Ifb 2 be < 4 a c awrf a awrf c both negative ; 

d x 1 f d u 

-c a/ 4ac b 2 2 

/ 4ac b 2 h_ 

~ V 2a(4ac b 2 ) 1 , 4ac-^b^ IZ +C "" ^ 
N " 2 a 2 a 

89. Required the integral of any rational function whatever of one 
variable, multiplied by. the indefinite difference of that variable. 

Every rational function of x is comprised under the general form 

AY ro _ i TJ v ni l ^i C^ V* m ~~ 2 i ft*-/^ T^" -v ^L 
A "y* J_> A. y ~ \_^ A p <Xi- IV A. "^ J_j 

a x n + b x n ~ + c x n ~ 2 + &c. k x +1 
E 1 

a v m + 1 m 

Cx m ~ 


in which A, B, C, &c. a, b, c, &c. and m, n are any constants whatever. 

n = 0, 
then we have (Art. 77) 

/(A x m + B x m - -f c.) 

^ f- &c.) f- constant. 

/ a 

Again, if m be > n the above can always be reduced by actual division 
to the form 

A x m ~ n + B x m - n -f. &c. 4- = - * 

a x " + bx"" 1 + &c. 

and if the whole be multiplied by d x its integral will consist of two parts, 
one of which is found to be (by 77) 

A B . x m ~ n 

m n + 1 X m + ln~^n~ + &C> 

and the other 

r A"x- 1 + B // x n ~ 2 + &c. 



9 a x n + b x " ~ + c. 
Hence then it is necessary to consider only functions of the general 

x"- 1 + A x p - 2 + Bx u ~ 3 + &c. U 
x"+ ax"~ J + bx u ~ 2 + &c. " V 

in order to integrate an indefinite difference, whose definite part is any 
rational function whatever. 

Case 1. Let the denominator V consist ofn unequal real factors, x a, 
x (S, c. according to the theory of algebraic equations. Assume 
U _ P Q R 

V ~ X a + x /3 + x ; 
and reducing to a common denominator we shall have 


U = P.x /3 . x 7 ... to (n 1) terms 

+ Q.X a.x 7 

+ R.X a.x f3 

- (P + Q + R 4. fcc^x"- 1 

P.(S a) + Q. (S |8) + &C.} X n - 

+ P.(S a.S a) + Q.(S /3.S 

1. S 3 1.2 1 


where S, S &c. denote the sum of a, /3, y &c. the sum of the products of 

1 1.2 

every two of them and so on. 


But by the theory of equations 

S= a 

S= b 

&c. = &c. 

... u = (P + Q + R + &c.)x n - 

+ {a(P + Q + R + &c.) + P a +Q/3 + Ry + &c.} X x B ~ 2 
+ {b (P + Q + R + &c.) + a(P a + Q|8 + &c.) + 
(P 2 + Q/3 2 + Ry 2 + &c.)} x n - 3 + &c. 
Hence equating like quantities (6) 

P + Q 4. R + & c . = 1 
a + Pa + Q/3+R 7 + &c. = A 
b + a (A a) + P a 2 + Q /3 2 + R 7 2 + &c. = B 

&c. = &c. 

giving n independent equations to determine P, Q, R, &c. 
F T U x 2 + 6 x + 3 

1 - 


P+ Q + R = 1-j 
6+P+2Q+3R=6 Vwhence 
11 + P + 4Q + 9R = 3J 

P = 1, Q = 5andR = 3 

U d x r d x r 5 dx / 3 d x 


= C 1. (x + 1) + 5 1. (x + 2) 3 1. (x + 3). 
P, Q, R, &c. may be more easily found as follows : 

x"- 1 + Ax n ~ 2 &c. = P (x /3). (x 7). &c. 
+ Q ( X ). (x 7). &c. 
+ R (x a), (x |8). &c. 
+ &c. 
let x = a, j8, 7, &c. successively ; we shall then have 

a n ~ 1 + Aa tt ~ 2 + &C. = P . (a /3) . (a 7) &C. -\ 

(8 n - l + A j8 n - 2 + &c. = Q . ( ) . (p 7) &c. V. . . ( A) 

&c. = &c. 
In the above example we have 

a = 1, J3 = 2, 7 = 3 and n = 3 
A = 6 and B = 3. 

. . P = 


6 + 3 * 

1. 2. 

O 4 6. 2 + 3 

y = = r = 5 

as before. 

Hence then the factors of V being supposed all unequal, either of the 
above methods will give the coefficients P, Q, R, &c. and therefore 

enable us to analyze the general expression -^ into the partial fractions 

as expressed by 

"- P + Q +& , 

V ~~ x a ^ x 
and we then have 


= F . 1 (x 

dx a 4- b / d x a + bydx 

/iLp = P.l(x-a) + Ql. (x-/3) + 8cc. + C. 

b / d x a + D /_c 

f~/ a^TlE 2 -/a 

~ J x 2 ^ a x 2 J a+ x 

+^l(a_x)_ a +- b l.( a + x) + C 

= a 1 x (a + b) 1 V a 2 x 2 + C 
by the nature of logarithms. 

TT. /3x 5 /*d 

Ex - 9 - dx = ~ 

= I . 1 ( X _ 4) i 1. (x 2) + C. 

Ex 4 f xdx /* pt1 ^- rQ dx 

+ Q 1 . (x + j8) + C 


p - _J*_ - 2 a + V (4 a 2 + b 2 ) 

j8 \/(4a 2 + b 2 ) 2a 

= P 1 (x + ) 

a j8 ~~2 V (4 a 2 + b 2 ) 

Case 2. irf a// #7^ factors of V be real and equal, or suppose a = (3 
= y = &c. 

U ._ x n ~ + A_x_ - 2 + &Q. 
V = ~ X "a" n 


and since 

a /3 = 0, a 7 = &c. 

the forms marked (A) will not give us P, Q, R, &c. In this case we 
must assume 

U P Q R 

V " (x a) n "*" (x a) n - l + (x a) n ~ 2 "* 

to n 1 terms, and reducing to a common denominator, we get 

U = P + Q . (x ) + R (x a) 2 + &c. 
now let x = a, and we have 

a n - 1 + A a n - 2 + &c. = P. 

^ = Q + 2 R . (x a) + 3 S . (x a) ~ + &c. 

1 1 X. 

d2J =2R+3.2.S.(x a)+4.3.T(x ) 2 +&c. 

dx 2 
d 3 U 

= 2 . 3 . S + 4 . 3 . 2 T (x a) + &c. 


&c. = &c. 

and if in each of these x be put = a, we have by Maclaurin s theorem 
the values of Q, R, S, &c. 

TT 1 T , U X 2 3X+ 2 

Ex.1. Let = 

(x _ 4)3 


U = x 8 3x + 2 





.-. P = 6 

Q = 8 3 = 5 
R = i. 2 = 1 

/U d x * 6 d x / 5 d x /- d x 

~V~ ~ J (x 4) 3 + J (x 4) 2 + y x^T 

Let U - 
.Let - 

(x _ 3)6 



U = x s + x 3 

i5 = 5x+Sx 


d x 

.-. P = 3 5 + 3 3 = 27 X 10 = 270 
Q = 27 X 16 = 432 
R = 20 X 27 + 6 X 3 = 


9X_60 + 6 

_ 360 _ 

W- 12 -1 
" ~ 


-l8.(^-93. F ! 5p -|.^-i gr8 - 1 5. x -i 5 + I.(x_3) 

which admits of farther reduction. 

x 2 + x U 
Ex. 3. Let - _ yy = -y . 


U = x 2 +x 




X 2 


(x I) 2 

2(x I) 4 

// appears from this example, and indeed is otherwise evident, that the 
number of partial fractions into which it is necessary to split the function 
exceeds the dimension of-x. in U, by unity. 

This is the first time, unless we mistake, that Maclaurin s Theorem 
has been used to analyze rational fractions into partial rational fractions. 
It produces them with less labour than any other method that has fallen 
under our notice. 

Case 3. Let the factors of the denominator V be all imaginary and un 

We know then if in V, which is real, there is an imaginary factor of 
the form x + h + kV 1, then there is also another of the form 
x + h k V ]. Hence V must be of an even number of dimensions, 
and must consist of quadratic real factors of the form arising from 
(x + h + k V 1) ( X + h k V 1) 

or of the form 

(x + h) 2 + k 2 . 
Hence, assuming 

U P + Qx P + Q x 

V ir H 7^ or~l T & c - 

and reducing to a common denominator, we have 

U = (P + Qx) J(x + a ) 2 + I 8 8 } H x + a// ) 2 + I 3 " 2 } x &c - 
-}. (P _f- Q x ) ( x + a) 2 + (3 2 ] {(x + a") 2 + 13" *} X &c. 

+ (P" + Q" x) J(x + a) 2 + |8 2 } J( x + " ) 2 + ^ 2 J X &C 
+ &C. 

Now for x substitute successively 

a + |3 V 1, + fy / ], a! + j3" V 1, &C. 
then U will become for each partly real and partly imaginary, and we 
have as many equations containing respectively P, Q ; P , Q ; P", Q", &c. 
as there are pairs of these coefficients ; whence by equating homogeneous 
quantities, viz. real and imaginary ones, we shall obtain P, Q ; P , Q , &c. 


Ex. 1 . Required the integral of 

x 3 d x 

x 4 + 3x 2 + 2 
Here the quadratic factors of V are x 2 + 1> x 2 + 2 

.-. a = 0, = 0, /3 = 1, and /3 = V~2 . 

x = (P + Qx)(x 2 + 2) 

+ (P + Q x)(x 2 + l) 

Let x = \/^n. Then 

V 1 = (P + Q V 1) . ( 1 + 2) 

_.-. P=0, Q = - 1 

Again, let x = V 2. V 1, and we have 


_2? V 1 = (P + Q V 2. V l) (2+ 1) 

= P Qf V~2 . V~^l 
.-. P = 0, and Q = 2 

* x s dx / x d x /*2 x d x 

X y O X "y f *^ X ^^ A X "^ ^ 

^ /""i j I /. 2 i 1 \ | 1 /xr 2 t O\ 

Ex. 2. Required the integral of 


To find the quadratic factors of 

1 +x 2n 
we assume 

x 2 n + 1 = 0, 
and then we have 

X 2n = 1 = cos. (2p+ 1) *r+ V 1 sin. (2 p + ])T 
T being 180 of the circle whose diameter is 1, and p any integer what- 


Hence by Demoivre s Theorem 

2p+l . - - . 2p+l 

x = cos. - it + v 1 . sin. j - w 
2 n 2 n 

But since imaginary roots of an equation enter it by pairs of the form 
A. + V 1 . B, we have also 

2 p + 1 - - . 2 p + 1 

x = cos. -\. ff V 1 . sin. -*s - v 
2 n 2 n 



2 n 

which is the general quadratic factor of x 2 n + 1. Hence putting 
p = 0, 1, 2 ...... n 1 successively, 

x 2 +l = (x 2 2xcos. ^ + l) . (x 2 2xcos. ~ + 1 ) X 

Hence to get the values of P and Q corresponding to the general factor, 


P+Qx N 



_ 2xcos. - 

TV/T l+X 2n 

M = - ?- 

x 2 2 x cos. - TT -f 1 
2 n 

and becomes of the form when for x we put cos. P it + V lx 

2 p+ 1 
sin. ^ ; its value however may thus be found 

*w XI 

T , 2 p + 1 . 2 p + 1 

Let cos. -2 ic + V 1 sin. ^ ^ ff = r 
2 n 2 n 


2 p + 1 . 2 p + 1 1 

cos. T V 1 . sin. ^ r = 

2 n 2 n r 


M= 1+x " . 

Again let x r = y ; then 
M = l + y 2n + 2n y 



r 2 n = cos. 2 p + 1 . * + V 1 sin. 2p+l.w 
M - y* n ~ + 2n y 2n - 2 .r+ . . . . 2n r 2 "" 1 



Hence when for x we put r, y = 0, and 

and from the above equation we have 

O n v 2 n 1 



_ , . 2 p+ 1 -D 2 p + 1 . 2 n 1 . 

2V 1 sin. -~r v = 2 n P . cos. ^ . it + 2 n P V IX 

2 n 2 n 

2p+1.2ii 1 _ ^ i 2n ,\ 

sin. r - <r 2 n Q (since r 2n =: 1) 

.. equating homogeneous quantities we get 

. 2p+l 
sin. *1 ff=n. sin. 

. . 
2 n 2 n 


2p+1.2n 1 

P . cos. it Q. 

fw n 


2 n 
Hence the above equations become 

. 2 p + 1 r, 2 p +1 

.. sin. ^r- T = n P sin. T - 
2n 2 n 

2 p+ 1 ^ 


1 iri 1 2p+ 1 

.-. P = -, andQ= -- . cos. ^ - 
n n 2 n 

Hence the general partial integral of 



. r (\ x cos. -- tt\ d x 

1 / \ 2 n / 


. n / x - 

2 x cos. ~ v l l * + 1 

cos. v. TT / 2 x d x 2 cos. ^~ it . d x 
2 n / 2 n 

2n ( 

/ v*- 

2 n 4- 1 

2 x cos. + 1 


2 p 4- 1 

2 X COS. ^~ r + 1 

2 n 

2p+ 1 

S> 2n ,/ , 2p+ 1 . 
_ . 1 f x 2 g x cos< _ri T + 1 ) 

2 n V 2 n / 

2p+ 1 , 

sin. ^ v / x cos. 


see Art 88. Case 4. 

d x 

Hence then the integral of y - - , which is the aggregate of the results 

l -j- x 

obtained from the above general form by substituting for p = 0, 1, 2 . . . 
n 1, may readily be ascertained. 

r d x 

As a particular instance let J ^ - 6 be required. 


n = 3 
and the general term is 

2p+ 1 
cos. - ft * _ 

1 2 x cos. 

. 2p + 1 2 

sin. r x cos. 

/% * ^~ v-v/o. ff 

.tan.- 1 - 6 

sin ?JL_i 


Letp = 0, 1, 2, collect the terms, and reduce them ; and it will appear that 
dx _l|j^3 , x 2 +xV3 + l _,8x(l x 

By proceeding according to the above method it will be found, that the 
general partial fractions to be integrated in the integrals of 

VOL. I. F 


[SECT. I. 

dx , x r d x 

~ r and - 

are respectively 

v " 


cos. 2 p it 1 

* _ n , v _, 

JW - X 

x 2 2 x cos. 

Q -r\ fjf 



2 cos 



2pw 2 r p * 
E x cos. 

2 p it 
x 2 2 cos. x + 1 


and when these partial integrals are obtained, the entire ones will be 

found by putting p = 0, 1 .... or according as p is even or 


Ex. 3. Required the integral of 

x r dx 

x sn 2ax n + 1 
"where a is < 1. 

First let us find the quadratic factors ofx 211 2ax n + 1. For that 
purpose put 

x 2n 2ax n = 1 

= a + V 1. V 1 a 2 
since a is <1 1. 

Novr put a = cos. d , then 

x n = cos. d + V 1 sin. 5 

= cos. (2 p * + 5) + V^l sin. (2 p T + a) 

2 p 9 + ^ , , ; . 2 p r + 3 

. . x = cos. *- ^ + V 1 sin. : 

and the general quadratic factor of 


2 x cos. 

2 p <r -f d 

where p may be any number from 0, 1, &c. to n 1. 

Hence to find the general partial integral of the given indefinite differ 
ence, we assume 

x P + Qx u N 

x iTZ 2 a x " +-1 - 2.+ - M 


and proceeding as in the last example, we get 

. (r 1 + 1) (2pcr + 3) 1 

Q = sin. ^ - - v v -L 

n n sin. 5 


. (n r) . (2 p r -f 6) 1 

P = sin. - - - v " x _ - _____ 

n n sin. 3 

whence the remainder of the process is easy. 

Case 4. Let the factors of the denominator be all imaginary and equal in 

In this Case, we have the form 

u_ _ y 

V" {(x+)+0 f a ~ 
and assuming as in Case 2. 

u P + Qx P + Q x 

, &c 

u - 1 H 

K + Lx K + L x 

and reducing to a common denominator, 

U = P + Qx + (F + Q x) (x~+~^ 2 + /3 2 ) + &c. 

and substituting for x one of its imaginary values, and equating homoge 
neous terms, in the result we get P and Q. Deriving from hence the 

values of -: , -= - , &c. and in each of these values substituting for x 
d x d x 2 

one of the quantities which makes x + a] 2 + /S 2 = 0, and equating ho 
mogeneous terms we shall successively obtain 

P , Q ; P", Q", &c. 

This method, however, not being very commodious in practice, for the 
present case, we shall recommend either the actual developement of the 
above expression according to the powers of x, and the comparison of the 
coefficients of the like powers (by art. 6), or the following method. 

Having determined P and Q as above, make 
U - U -- (P + Q x) 

x~+^r- + /3< 

_ U - (F + Q! x) 

2 T+^p + /3* 
_. U" - (P" + Q! 1 x) 

&c. = &c. 

Then since U , U", U" , &c. have the same form as U, or have an 



integer form, if we put for x that value which makes (x + a) 2 -f- /3 2 = 
0, and afterwards in the several results, equate homogeneous quantities 
we shall obtain the several coefficients. 

P , Q ; P", Q",&c. 

Case 5. If the denominator V consist of one set of Factors simple and 
unequal of the form 

x ax a , &c. ; 
of several sets of equal simple Factors, as 

(x e) P, (x e ) % &c. 

and of equal and unequal sets of quadratic factors of the forms 
x 2 + a x + b, x s + a x + b , See. 
(x 2 + 1 x + r) ^, (x 2 + I x + r ) , &c. 

then the general assumption for obtaining the partial fractions must be 
U M M 

V == x^=~^ + xTZT H 

I E A F i a 


1 F/ 1 

1 (x-e)p- 1 (x-e)P- -> 
P + Q x F + Q 

-(x_e )< 

1 (x-er- 
x G 4- H x x 

L x 2 + ax + b + x 2 + a x 
R + Sx R + S x 

+ b 4 
G + H 

and the several coefficients may be found by applying the foregoing rules 
for each corresponding set. They may also be had at once by reducing 
to a common denominator both sides of the equation, and arranging the 
numerators according to the powers of x, and then equating homogeneous 

We have thus shown that every rational fraction, whose denominator 
can be decomposed into simple or quadratic factors, may be itself analyzed 
into as many partial fractions as there are factors, and hence it is clear 
that the integral of the general function 

&c. Kx + L 

ax n + bx u - l + &c. kx + 1 

may, under these restrictions, always be obtained. It is always reducible, 
in short, to one or other or a combination of the forms 
r / d x f d x 

/x-dx,/^-^, /^r+T 

Having disposed of rational forms we next consider irrational ones. 
Already (see Art. 86, &c.) 

/+dx ,* d x /* d x _ 

V(a bx 2 ) -/xV(bx 2 a) -/ V (ax bx 2 ) 


have been found in terms of circular arcs. We now proceed to treat of 
Irrationals generally ; and the most natural and obvious way of so doing 
is to investigate such forms as admit of being rationalized. 
90. Required the integral of 

I 1 1 J. 1 7 

dx X F Jx, x m , x n , x*, x S &c. S 

where F denotes any rational function of the quantities between the brackets. 

x _ u m n p q f &c> 


x m = u npqr .... 

X n =U mpqr .... 


( x p _ u mnq r> t m % 
&C. = &C. 

d x = mnpq . ... x u mnp< * - 1 xdu 

and substituting for these quantities in the above expression, it becomes 
rational, and consequently integrable by the preceding article. 


b + cx* 

x = u 69 
3 180 


dx = 6u 59 du. 
Hence the expression is transformed to 

n "9^ u l60 +2au 4 +l 
60 u 9 d u - 1* 1S 
b + c u 15 

whose integral may be found by Art. 89, Case 3, Ex. 2. 
91. Required the integral of 

d x X F x, (a + b x) ", (a + b x) s , &c.^ 
where F, as before, means any rational function. 

Put a-j-bx = u ntnp then substitute, and we get 

nmp . /u nm a \ 

-^ - . u nmp ---- 1 duXF( -- ^ -- , u m P--- ,u n r----,& c .) 

which is rational. 


Examples to this general result are 
x 4 dx 

[SECT. I. 


c x 5 + (a + b x) * x + c (a + b x) ^ 
which are easily resolved. 
92. Required the integral of 

f /a 4- b x\ - /a 4- b x\ 1 

dx F Sx, ( ) u>(-f )q, Sec. >- 

Vf + gx/ vf + gx/ 


a + bx 

and then by substituting, the expression becomes rational and integrable. 
93. Required the integral of 

d x F fx, V (a + b x + c x 2 )} 
Case 1. When c is positive, let 

a + b x + c x 2 = c (x + u) 2 . 

a cu" 

2cu b 

(2cu b) 


and substituting, the expression becomes rational. 

Case 2. When c is negative, if r, r be the roots of the equation 

a + bx cx 2 = 
Then assume 

V c (x r) (r x) (x r) c u 
and we have 

cru 2 4-r , (r r )2cudu 

V . _ r\ -v v _ 

~~ o T J u A / a i l \ I 

cu 2 + 1 (cu 2 + I) 2 

and by substitution, the expression becomes rational. 
94. Required the integral of 

d x F Jx, (a + b x) S (a? + b x) *} 

a + b x = (at + b x) u " ; 


a a u 

b x = 

(a b b a) 2u d u 
, - a b) _V(ab -a b) 


Hence, substituting, the above expression becomes of the form 

duF fu, V(b u 2 b)J 

F denoting a rational function different from that represented by F. 
But this form may be rationalized by 93 ; whence the expression becomes 

95. Required the integral of 


x m i dx(a + b x n )T~. 

. . m m p . 
This form may be rationalized when either , or -- 1- is an integer. 

Case 1. Leta+bx B =u q ; then(a+bx n )T = UP, x^^-"-, x m = 

u q 

Hence the expression becomes 

which is rational and integrable when is an integer. 

Case 2. Let a + bx n = x n u q ; then substituting as before, we get the 
transformed expression 


whicli is rational and integrable when + is an integer. 

Examples are 

x g dx x 2m dx 

(a a + x 2 )^ (a 2 + x 2 )^ 

2m + * X 6 d X 


96. Required the integral of 

x ra - d x (a + b x n ) q X F (x n ). 

This expression becomes rational in the same cases, and by the same sub 
stitutions, as that of 95. To this form belongs 

x m+ n -i dx(a + bx n )? 
and the more general one 




Q = A + B x n + C x 2n + &c. 

97. Required the integral of 

x m 1 dx X F{x m , x n , (a + bx n )^ 
Make a + bx n =u q ; then 

x m - l d x = S . ( U u a )" ~ l d u 

n b V. b / 

and in the cases where is an integer, the whole expression becomes ra 
tional and inte^rable. 

tegral of 



98. Required the integral of 

X + X" + V(a + bx + cx 2 ) 
where X, X , X" denote any rational functions 0/*x. 
Multiply and divide by 

X + X" V(a + bx + x 2 ) 
and the result is, after reduction, 

XX dx XX"dx Va 

_ __ 

X /2 X" 2 (a + bx-f ex 2 ) X /2 X //2 (a +bx + cx 2 ) 
consisting of a rational and an irrational part. The irrational part, in 
many cases, may also be rationalized, and thus the whole made integrable. 
99. Required the integral of 

x m dxF x n , V (a + bx n -f ex 2 ")} 
Let x n = u ; then the expression may be transformed into 

1 m + 1 , 
u n " diiF u, V (a + bu + cu 2 )] 


which may be rationalized by Art. 93, when is an integer. 

100. Required the integral of 

x m dxFx n , V (a + b 2 x 2 "), bx n + V (a + b 2 x 2n )}. 

bx u + V (a + b 2 x 2n ) = u; 

and the whole expression evidently becomes rational when - is an 

Many other general expressions may be rationalized, and much might 


be said further upon the subject ; but the foregoing cases will exhibit the 
general method of such reductions. If the reader be not satisfied let him 
consult a paper in the Philosophical Transactions for 1816, by E. Ffrench 
Bromhead, Esq. which is decidedly the best production upon the Integrals 
of Irrational Functions, which has ever appeared. 

Perfect as is the theory of Rational Functions, yet the like has not been 
attained with regard to Irrational Functions. The above and similar arti 
fices will lead to the integration of a vast number of forms, and to that of 
many which really occur in the resolution of philosophical and other 
problems ; but a method universally applicable has not yet been discover 
ed, and probably never will be. 

Hitherto the integrals of algebraic forms have been investigated. We 
now proceed to Transcendental Functions. 

101. Required the integral of 

a x dx. 
By Art. 17, 

d.a x = l.a X a x dx 

1 x 


/a m x d x = i- a m x + C (b) 

102. Required the integral of 

Xa x dx 
where X is an algebraic Junction of*. 

By the form (see 73) 

d (u v) = u d v + v d u 

we have 

f u d v = u v f\ d u. 

11 ^ /*l ^ - -.7- 

"* "" 1 a J 1 a 

/dX a*dx _ dX a* f- a* d 2 X 

J dx la = dx (la) 2 -/(la) 2 dx 

a x dx d X a* f a x d 3 X 

> ax_ 

dx 2 la 2 "" 

(la) 2 "" dx 2 (la) 

&c. = &c. 
the law of continuation being manifest. 


Hence, by substitution, 

/v x i _ v a * dX * x d 2 X a x 

*n~~dx (la) 2 + dx 2 (la) 3 ~ 
which will terminate when X is of the form 
A + Bx 

Ex /*x 3 a x dx- aXx3 3aX * 2 3.2a x x 3.2a x 
X ** * 1 a " (1 a) 2 (la) 3 "(la) 4 " 


/a x Xdx = a x /Xdx /la.a x dx/Xdx 

= a x X / la/a x X / dx 

X =/Xdx. 

/a x X dx = a x X" la/a x X"dx 

&c. = &c. 
and substituting, we get 

/a x Xdx= a x X la.a x X" + (la) 2 a x X " &c. 
X , X", X ", &c. being equal to /X d x, /X d x, /X" d x, &c. re 

T? r x dx vi , xla x 2 (la) 2 x 3 (la) 3 

&/. - = a l* + _ + -L.2- .+ _A_L + 4,, + C . 

which does not terminate. 

By this last example we see how an Indefinite Difference may be in 
tegrated in an infinite series. If in that example x be supposed less 
than 1, the terms of the integral become less and less or the series is con 
vergent. Hence then by taking a few of the first terms we get an ap 
proximate value of the integral, which in the absence of an exact one, will 
frequently suffice in practice. 

The general formula for obtaining the integral in an infinite or finite 
series, corresponding to that of Taylor in the Calculus of Indefinite 
Differences, is the following one, ascribed to John Bernoulli, and usually 


/Xdx = Xx /xdX 
rdX _ dX x 2 r x 2 dx d 2 X 

J dx ~-^ ~2~-J~^- dlF 

x 3 dx d 3 X 
2.3 dx 3 
&c. = &c. 

/d^X x g dx _ d 2 X x 3 f 
J dx 2 2 - "31* !""/ 


Hence . 

f-*r i -XT X - Cl A. X -~, 

/Xdx = X*--^. -5 + ^ . g-j-Sc. + C 

the theorem in question. 

Ex.l.x m dx = x m + 1 x m + 1 + ^ n ! 1 x m + 1 &c. + C 

But since 


as in Art. 78. 

1 02. Required the integral of 


where X is any Algebraic Function ofx, \ x the Hyperbolic logarithm of x, 
and n a positive integer. 
By the formula 

f u d v = u v f v d u 
we have 

x n /Yl x) B - /"X d x 

x " 

= (lx)"X -n/(lx)- ^ X X 

J x " v x 

&c. = &c. 

where X , X", X ", &c. are put for/Xdx, /"^- dx, / d x, &c. re- 

- / X ^ X 


/Xdx(lx)" = X (lx)" 

] 93. Required the integral of 

inhere U w any function of I x. 



Let u = 1 x. 


A dx 

d u = -. 

and substituting, the expression becomes algebraic, and therefore integra- 
ble in many cases. 

104. Required the integral of 

Xdx (lx) n 
"where n is negative. 

Integrating by Parts, as it is termed, or by the formula 

/u d v = u v f\ d u 
we get, since 

X d x d x . 

/-Xdx __ Xx 1 rdx_ dJXxj 

^(lx) n (n 1) (lx)"- 1+ n lV(l x )n-i- dx 
and pursuing the method, and writing 

y, _ d (X x) 

we have 
X Xx 

x// _ d (X x) 
&c. = &c. 

(n 1) . . . 2/1(5) 

Xx - x^ 1 / dx 

__ __ _ - _ x __ 

(n 1 ) (1 x) ~ ~ J (n 1) . (n 2) . . . . (n m) (Uj^^ 

according as n is or is not an integer, m being in the latter case the 
greatest integer in n. 

/-x"dx__ x + f 1 m+1 

X V (1 X )" n __ ! t(lx)"- 1 + (n SH rxp^ 4 C 

(m + I)"- 1 /*x m d x 

__ (m + I)"- 1 /* 

n 1) n 2 ____ I/ 

(n 1) (n 2) ____ I Ix 

when m is an integer. 

105. Required tlie integrals of 

i A i * d I . d f . . d I 

d . cos. 0, d d . sin. <L d 6 . tan. 0. d 6 . sec. 0, - - , -= A , - 

cos. I sin. ^ tan. 

By Art. 26, &c. 

d sin. 6 = d 6 . cos. 0, and d cos. 6 = d 6 sin. 6 
/./d 6 cos. r= sin. 6 + >C ......... (a) 


sin. = C cos. 6 ........ (b) 


Again let tan. 6 = t ; then 


d 6 = 

1 + t 2 

t d t 

t 2 ) 

= C 1. cos. 6 . ;i (c) 



1 + t 2 = sec. 2 6 = 
d 6 sec. 6 = 

cos. z 6 

d 6 d 6 cos. 6 

cos. 6 ~ 1 sin. 2 1 
d (sin. 6} 

"1 sin. 2 6 

l d (sin. d) d sin. 

1 sin. 6 * 1 + sin. 

/.yd 6 sec. 4 = l.(l-f-sin.0) % 1 (1 sin.0)-f-C 
rrl.tan. (45+^-) + C. . . (d) 

which is the same as f - - . 
* cos. 6 


C-. - - = fd d cosec. 6 
J sin. 6 

= /d * sec. (!-*)= -/d . ( - tf sec. - 

= 1. (tan. I) + C . . . . ...... (e) 


f ~ 

= Icos. 0) + C(byc) 

= 1 . sin. 6 + C . . . . ........ (f) 

106. Required the integral of 

sin. m cos. n 6 . d 0. 
m and n fomg- positive or negative integers. 


Let sin. 6 = u ; then d 6 cos. d = d u and the above expression becomes 

u m du(l u 2 ) ^ 
which is integrable when either or J f- n ~ = m "*"-" 

is an integer (see 95.) If n be odd, the radical disappears ; if n be even 

and m even also, then ^ = an integer ; if n be even and m odd, then 

m + I . ,. T _ T , 

^ is an integer. Whence 

u m d u (1 u ! ) n "a 
is integrable by 95. 

Integrating by Parts, we have 

ClTl HI ~ 1 A -vy-i 

/d 6 sin. m 6 cos. n 6= cos." + 1 6+- */cos. n + 2 6. sin. m - 2 Q X d 6 

n + 1 m -j- 1 

sin." 1 - 1 6 m 1 , 

= cos. n + 1 ^ H / dx sin. m ~ 2 ^ cos. "tf 

m 4- n m + n j 

and continuing the process m is diminished by 2 each time. 
In the same way we find 

and so on. 

107. Required the integrals of 

d u = d 6 sin, (a 6 + b) cos. (a 6 + b ) 

dv = d*sin.(af + b) sin. (a 6 + b ) 

dw = d 6 cos. (a 6 + b) cos. (a 6 + b ) 
By the known forms of Trigonometry we have 

du = d 6 [sin. (a + a . 0+b + b x ) + sin. (a a . + b b )} 

i d v = dd {cos. (a~+T .0+b + b ) cos. (a a .<J+b b )} 

d w = d d {cos. (a + a". 0+b + b ) + cos. (a^a 7 . 6+b b )} 
Hence by 105 we have 

r t / cos. (a^Fa 7 . ^ + b + bQ , cos, (a a 7 . + b b ) \ 
~*t~ a + a a a ~J 

sin. (a+ a . + b + b ) sin. (a a 7 ".* + b b 7 ) 
- ~ " 

- p i i/ sin - (a + a - + b + bQ . sin, (a^^a 7 . tf + b I/) 
rt | a + a a a 

These integrals are very useful. 




108. Required the integrals of 

6 n d 6 sin. 0, and d n d 6 cos. d. 
Integrating by Parts we get 

/ <) n xd0sin. 0=C n cos. 0-f-n d"- 1 sin. 0+n . (n 1) n - 8 cos.0 &c. 
/tJ"xd0cos.d:=:C + n sin. 6 + nd ll ~ l cos.d n. (n 1) n - 2 sinJ +&c. 

109. Required the integrals of 

X d x sin. l x 
X d x tan. l x 
X d x sec. ~ x 

Integrating by Parts we have 

/Xdxsin.->x = sin.-ix/Xdx- 

/ V 1 i r v 1 / d X /" X d X 

J X d x tan. - l x = tan. - l x/ X d x / r^ - j 

. ~^ 

x V(x 2 1) 

/X d x sec. - l x = sec. - l xA X d x /* r5. 

^ x x 2 

&c. = &c. 
see Art. 86. 

110. Required the integral of 

d u - ( f + g cos, tf) d 6 
(a + b cos. 6) n 

Integrating by Parts and reducing, we have 
(ag bf)sin. 6 _ _ 

(n l)(a 2 b 2 )(a 
/(n 1) (at* bg) + (n-^-2) (a g 

(n I)(a 2 

(a + b cos. 6) n ~ 

which repeated, will finally produce, when n is an integer, the integral 

(a b) tan. 

Ex./- d " 2 

r a 

+ b cos. d V (a z b 2 ) 

=r . tan. 

V (a 2 b 2 ) 

1 , b+acos. 6+ sin. 6 V (b 2 a ) _ 

V(b z a 2 ) a + b cos. 6 

Notwithstanding the numerous forms which are integrable by the pre 
ceding methods, there are innumerable others which have hitherto resisted 
all the ingenuity that has been employed to resolve them. If any such 
appear in the resolution of problems, they must be expanded into con- 


verging series, by some such method as that already delivered in Art. 101 j 
or with greater certainty of attaining the requisite degree of convergency, 
by the following 


111. Required to integrate between x = b, x = a, any given Indefinite 
Difference,, in a convergent series. 

Let f (x) denote the exact integral of f X d x; then by Taylor s 

and making 

h = b a 

f (x + b-a)-fx = X. (b-a) + d d |. 1^1!+ &c. 

Again, make 

x = a 

dX d 2 X 
dT "d^ 2 &C< 
become constants 

A, A , &c. 
and we obtain 

f(b)-f(a) = A(b-a) + . (b-a) + ^ (b-a) 3 

which, when b a is small compared with unity, is sufficiently conver 
gent for all practical purposes. 
If b a be not small, assume 

b a = p./3 

p being the number of equal parts |3, into which the interval b a is sup 
posed to be divided, in order to make /3 small compared with unity. Then 
taking the integral between the several limits 
a, a + /3 
a, a + 2 18 

a, a + p /3 


we get 

f. ( a + /3) f( a ) = A/3+ ^-. 0* + ^. . 0s + &c. 


f (a + 2jg) f (a + flrrBjS+S . /3 2 + l/3 3 + &c. 

/i <c. o 

&c. = &c. 

f (a + pj8) f (a+J=I./8) = P/3 + /3 2 + 

A, A 7 , &c. B, B , &c ....... P, P , & c . 

being the values of 

v dx 

Xj dT &c " 

when for x we put 

a, a + ft a + 2 ft &c. 

f(b)-f(a) =(A + B + ..;.. 

+ (A + B + . . . . F) 

+ (A" + B" + . . . . F ) 1^3 

+ &c. 

the integral required, the convergency of the series being of any degree 
that may be demanded. 

If j3 be taken very small, then 

f (b) f (a) = (A + B + ---- P) nearly. 
Ex. Required the approximate value of 

/X^-^dx X (1 x n )f 

between the limits of x = and x = 1, when neither 9 n r -- f- 
is an integer. 

X = x 1 "- 1 (l_x n )T 

d X p JL n p 

jY rr (m + n l)x n - 2 (] ^x) _ -^-x n - 2 (l X 

b^-a - ] - 1. 

Assume ] = 10 X ft and we have for limits 
1 2 

Tb ; To ; &c - 

YOI-. I. G 


Hence m being > 1, 

A = 


&c. = &c. 

Hence, between the limits x = 1 and x = 

1 f -P- -H- 

/Xdx = - X |(10 n l)q + (10 n 2 n )q 

_j_ (10 " 3 n ) "? + &c. + (10 n 9 n )"!r | nearly. 

W T e shall meet with more particular instances in the course of our 
comments upon the text. 

Hitherto the use of the Integral Calculus of Indefinite Differences has 
not been very apparent. We have contented ourselves so far with 
making as rapid a sketch as possible of the leading principles on which 
the Inverse Method depends ; but we now come to its 


112. Required to Jind the area of any curve, comprised between two 
given values of its ordinate. 

Let E c C (fig. to LEMMA II of the text) be a given or definite area 
comprised between and C c, or and y. Then C c being fixed or De 
finite, let B b be considered Indefinite, or let L b = d y. Hence the 
Indefinite Difference of the area E c C is the Indefinite area 

B Ccb. 

Hence if E C = x, and S denote the area E c C ; then 
d S = B Ccb = CL + Lcb 

y d x + L c b. 

But L c b is heterogeneous (see Art. 60) compared with C L or y d x. 
... d S = y d x 



the area required. 

Ex. 1. Required the area of the common parabola. 

y 2 = a x. 

2y dy 
.-. d x = *- J 



s _ " 


a -3a 

and between the limits of y = r and y = r becomes 

If m and m be the corresponding values of x, we have 

S = (r m r m ) 

= of the circumscribing rectangle. 

Let r = 0, then 


S = r m (see Art. 21.) 

Ex. 2. Take the general Parabola whose equation is 

y m __ <! x n 

Here it will be found in like manner that 


m + n* " 
between the limits of n = y = 0, and x = a, y = /3. 

Hence all PARABOLAS may be squared, as it is termed ; or a square may 
be found whose area shall be equal to that of any Parabola. 

Ex. 3. Required the area of an HYPERBOLA comprised by its asymptote, 
and one infinite branch. 

If x, y be parallel to the asymptotes, and originate in the center 

x y = a b 

is the equation to the curve. 

d x = abd y 

y 8 




Q f abdy 

s =/ IT* = C a b 1 y. 

Let at the vertex y = /3, and x == ; then the area is and 

C = a b . 1 8. 

S = a b . 1 . P- . 


1 13. If the curve be referred to a fixed center by the radius-vector and 
traced-angle 6; then 

ds = l ^- "{. . : . !; . : : ,,, ? ;. 

For d S the Indefinite Area contained by f , and f + d = (g-fdg) ^5 


d 6 . g d e d 

+ s | (Art. 26) and equating homogeneous quantities we 


d S = 

Ex. 1. In the Spiral of Archimedes 

= a 

n 2 _ 2 

. Q f AZ A A 43 I p 

. . 5 _ j e a. d - . + \^. 

Ex. 2. In the Trisectrix 

S = 2 cos. d + 1 

.-. d S = i/(2cos. tf l) 2 d^ 
which may easily be integrated. 

Hence then the area of every curve could be found, if all integrations 
were possible. By such as are possible, and the general method of ap 
proximation (Art. Ill) the quadrature of a curve may be effected either 
exactly or to any required degree of accuracy. In Section VII and many 
other parts of the Principia our author integrates Functions by means of 
curves ; that is, he reduces them to areas, and takes it for granted that 
such areas can be investigated. 

114. To find the length of any curve comprised within given values of the 
ordinate ; or To RECTIFY any curve. 

Let s be the length required. Then d s = its Indefinite Chord, by 
Art. 25 and LEMMA VII. 

.. d s = V (d x 2 + d y 2 ) 

s =fV (dx* + dy 2 ) (a) 


Ex. 1. In the general parabola 

y m = ax". 



dx 2 = 

2 2 m 


n a n 

n a 

which is integrable by Art. 95 when either 

1_ 1 1_ 

O TV* O ryi "* O 

that is, when either 





2 m n 2 m n 
is an integer ; that is -when either m or n is even. 

The common parabola is Rectifiable, because then m = 2. In this case 

ds= dy V(l + -y 2 ) 
Hence assuming according to Case 2 of Art. 95, 


we get the Rational Form 

ds = 

Hence by Art. 89, Case 2, 

- + V u 

l 4- 8 

Butu = +/ * zy . 

cessary reductions 

Hence by substituting and making the ne 


** ^ * * 


s = 



a 1 . 

[SECT. I. 

Let y = ; then s = and we get C = 
and .-. between the Limits of y = and y = /3 

+ a 1 . 

In the Second Cubical Parabola 

y 3 = ax 2 

d s = d y 
which gives at once (Art. 91) 

Ex. 2. In the circle (Art. 26) 

ds = 





which admits of Integration in a series only. Expanding (1 v z )~"i 
by the Binomial Theorem, we have 



and between the limits of y = and y = - or for an arc of 30 we have 

s - j ___ _ 4. . 

2 h 2. 3. 2 3 + 5 


1 4. _L_ 4, 3 , 5 5. 7 

2 + 3. 2 4 "*" 5. 2 8 + 7. 2 11 + 9. 2 16 

! .0208333333 

+ &c. 

= <! .0023437500 
I .0003487720 


= .5235851943 nearly. 


Hence 180 of the circle whose radius is 1 or the whole circumference 
it of the circle whose diameter is 1 is 

cr = . 5235851943 ... X 6 nearly 
= 3.1415111658 

which is true to the fourth decimal place ; or the defect is less than . 

By taking more terms any required approximation to the value of T may 
be obtained. 

Ex. 3. In the Ellipse 

a 2 e 2 x 2 
s = /dx. N / a2 _ x2 

where x is the abscissa referred to the center, a the semi-axis major and 
ae the eccentricity (see Solutions to Cambridge Problems, Vol. II. p. 144.) 
115. If the curve be referred to polar coordinates, and 8; then 

s =fV fe*d* +dg 2 ) (b) 


y = g sin. 6 
x = m + cos. d 

and if d x 2 , d y 2 be thence found and substituted in the expression 
(114. a) the result will be as above. 
Ex. 1. In the Spiral of Archimedes 
P a $ 

. 8 a ! t+ * (s + O - c 

2 a 

see the value for s in the common parabola, Art. 1 14. 
Ex. 2. In the logarithmic Spiral 

S - e 


and we find 

s = V~2fd g = g V 2 + C. 

116. Required the Volume or solid Content of any solid formed by the 
revolution of a curve round its axis. 

Let V be the volume between the values and y of the ordinate of the 
generating curve. Then d V = a cylinder whose base is T y 2 and alti 
tude d x + a quantity Indefinite or heterogeneous compared with either 
d V or the cylinder. 



But the cylinder = v y ~ d x. Hence equating homogeneous terms, we 

d V = cry 2 dx 

V = cr/y*dx (c) 

Ex. 1. In the sphere (rad. = r) 

y 2 = r 2 x 2 

.-. V = ff/r 2 d x w/x 2 d x 
/ x 3 

and between the limits x = and r 

which gives the Hemisphere. 
Hence for the whole sphere 

Ex. 2. In the Paraboloid. 

y z = ax 
.-. V = ,r/a x d x 

<x a 2 

: ~2~ : C; 
and between the limits x = and a 

Ex. 3. In the Ellipsoid. 

,.V: -^./(a 2 dx~x 2 dx) 


and between the limits x = and a 


Hence for the whole Ellipsoid 
V = jUab 2 . 


The formula (c) may be transformed to 

y (d) 




where S = f y d x or the area of the generating curve, which is a singular 
expression, f S d y being also an area. 

In philosophical inquiries solids of revolution are the only ones almost 
that we meet with. Thus the Sun, Planets and Secondaries are Ellip 
soids of different eccentricities, or approximately such. Hence then in 
preparation for such inquiry it would not be of great use to investigate 
the Volumes of Bodies in general. 

If x, y, z, denote the rectangular coordinates, or the perpendiculars let 
fall from any point of a curved surface upon three planes passing through 
a point given in position at right angles to one another, then it may easily 
be shown by the principles upon which we have all along proceeded, 

d V = d y/z d x"l 

= d z/y d x \ . ..... (e) 


= dx/zdyj 

according as we take the base of d V in the planes to which z, y, or x is 
respectively perpendicular 

For let the Volume V be cut off by a plane passing through the point 
in the surface and parallel to any of the coordinate planes ; then the area 
of the plane section thus made will be 

/z d 


fy d x 

/ z d y 

see Art. 112. 

Then another section, parallel to^z d x, orfy d x, or J z d y and at 
the Indefinite distance d y, or d z, or d x from the former being made, 
ic Indefinite Difference of the Volume will be the portion comprised by 
icse two sections ; and the only thing then to be proved is that this por 
tion is = d yyz d x or d zy*y d x, or d x JT* d y. But this is easily to 
proved by LEMMA VII. 

This, which is an easier and more comprehensible method of deducing 
V than the one usually given by means of Taylor s Theorem, we have 
lerely sketched ; it being incompatible with our limits to enter into de- 
1. To conclude we may remark that in Integrating both y z d x, and 
d y y z d x must be taken within the prescribed limits, first considering 
Definite and then .r. 


117. To find the curved surface of a Solid of Revolution. 
Let the curved surface taken as far as the value y of the ordinate re 
ferred to the axis of revolution be a, and s the length of the generating 
curve to that point; then d a = the surface of a cylinder the radius of 
whose base is y and circumference 2 <r y, and altitude d s, by LEMMA VII. 
and like considerations. Hence 

d * = 9 *r y d a 

. = 2<r/yds . . . . -. .- . .: . . (a) 


= 2vrys 2cr/sdy ...... (b) 

which latter form may be used when s is known in terms of y ; this will 
not often be the case however. 
Ex. In the common Paraboloid. 

y 2 = a x 

Let y = and |S, then a between these limits is expressed by 

If the surface of any solid whatever were required, by considerations 
similar to those by which (116. e) is established, we shall have 

d a = V (dy 2 + dz 2 )/ V (d x 2 + d z 2 ) . . . . (c) 
and substituting for dzin V d x 2 + dz 2 its value deduced from z = f . 
(x, y) on the supposition that y is Definite ; and in V (d y 2 + d z 2 ) its 
value supposing x Definite. Integrate first V (d x 2 + d z 2 ) between the 
prescribed limits supposing y Definite and then Integrate V (d y 2 + d z 2 ) 
f V (d x 2 + d z 2 ) between its limits making x Definite. This last result 
will be the surface required. 

We must now close our Introduction as it relates to the Integration of 
Functions of one Independent variable. 

It remains for us to give a brief notice of the artifices by which Func 
tions of two Independent Variables may be Integrated. 

118. Required the Integral of 

Xdx + Ydy = 0, 
where X is any function o/ x, and Y a function ofy the same or different. 


When each of the terms can be Integrated separately by the preceding- 
methods for functions of one variable, the above form may be Integrated, 
and we have 

/Xdx+/Ydy = C. 

This is so plain as to need no illustration from examples. We shah 1 , 
nowever, give some to show how Integrals apparently Transcendental 
may in particular cases, be rendered algebraic. 

Ex. 1. + ^- = 0. 

.-. 1 x + 1 y - C - 1 . C 


.-. x y - C or = C. 

d x d y _ 

ii(X. . i TJ 3V ~f~ ~i" i -, _. o\ " 


sin. - l x + sin. ~ y C = sin. - C 
.-. C = sin. sin. - 1 x sin. - 1 y} 

=. sin. (sin. ~ x) . cos. (sin. l y ) + cos. (sin. ~ l x) sin. (sin. "~ l y) 
- x . V (1 y 2 ) + y V (1 x 2 ) 
which is algebraic. 

Generally if the Integral be of the form 
f- (x) + f.- (y) = C 
Then assume 

C = f.- (C) 
and take the inverse function off" 1 (C) and we have 

which when expanded will be algebraic. 
119. Required the Integral of 

Ydx + Xdy = 0. 
Dividing by X Y we get 

which is Integrable by art. 118. 
120. Required the Integral of 

inhere P and Q are each such Junctions of\ and y that the sum of the expo 
nents of-x. and y in every term of the equation is the same. 


Let x = u y. Then if m be the constant sum of the exponents, P and 
Q will be of the forms 

U X y m U y m 
U and U being functions of w. 

Hence, since dx = udy + ydu, we have 

U.(udy + ydu) + U dy = 

(Uu-fU )dy + Uydu = 
d y , U d u - 

y y + tnr+U = ..... ^ 

which is Integrable by art. 118. 

Ex. 1. (a x + b y) d y + (f x 4- g y) d x = 0. 

P = f x + g y, Q = a x + b y 
U= fu+ g, U = a u + b 
. ( ll 4. (fu + g) du _ 

y h fu 2 + (g + a)u + b - 

which being rational is Integrable by art. (88, 89) 
Ex. 2. x d y y d x d x V (x 2 + y 2 ) 


Q = x, P = y V (x 2 +y z ) 

U = u, U = 1 V (1 + u 2 ) 
d_y 2 

u V (1 + u 2 ) 

ll - 1^ 4. du 

y u r U V (1 + U 2 ) " 

which is Integrable by art. (82, 85.) 
These Forms are called Homogeneous. 
121. To Integrate 

(ax4-by4-c)dy + (mx+ny4-p)dx = 0. 

By assuming 

= vj 


m x + n y + P 
we get 

m d u adv bdv ndu 

d y = -- 1 , and d x - T ---- 
J mb na mb ria 

and therefore 

(m u n v) d u + (b v a u) d u = 
which being Homogeneous is Integrable by Art. 120. 




We now come to that class of Integrals which is of the greatest use in 
Natural Philosophy to 


122. Required to Integrate 

dy + yXdx^X dx, 
where X, X are functions of X. 

y = u v. 

udv+vdu+Xuvdx= X dx 
Hence assuming 

d v + v X d x = (a) 

we have also 

v d u = X d x (b) 


.-. Iv +/Xdx = C 


v = e c-/xdx 
= e c X e~ 
= C X e- xdx . 
Substituting for v in (b) we therefore get 

1 /Xdx 

du = -p,.e X dx 

which may be Integrated in many cases by Art. 118. 
Ex. dy + ydx = ax 3 dx. 

X = 1, X = a x 3 

/X d x = x 

/X d x e Xdx = a/x 3 e * d x 

= a e x (x 3 3 x 2 + 
see Art. (102) 

y = Ce~* + a (x 3 3x 2 + 6x 6) 

6 x 6) 


122. Required to Integrate the LINEAR Equation of the second order 

dx 2 .dap-T- 

"where X, X are functions o/*x. 

Let y = e-/" 11 ^; then -y-^ = ue /udx 
d x 

d x 2 ~ MX / 

and .*. by substitution, 

d~x "* 

which is an equation of the first order and in certain cases may be Integ- 
rable by some one of the preceding methods. When for instance X and 
X are constants and a, b roots of the equation 

u 2 + Xu+ X = 
then it will be found that 

y = C e a x + C e b x . 

123. Required the Integral of 

d x 2 d x 

where X" is a new function ofx. 

Let y = t z ; then Differencing, and substituting, we may assume the 

^+X^+X Z = .... ... . (a) 


d z\ , X /x ,. 

E) dx:= ir ( b > 

Hence (by 122) deriving z from (a) and substituting in (b) we have a 
Linear Equation of the first order in terms of fjrrJJ whence (g 
be found ; and we shall thus finally obtain 



X v ~\ ft 

, ov j , vv 


Equat. (a) becomes 

d 2 z dji 1 z 
dx~ 2 + dx x " x 2 

wherein z = e /udx ; which becomes homogeneous when for u we put v~ \ 
Next the variables are separated by putting (see 120) 

X = V S 


we have 


1 S2 + 

s 1 


s(s 2 

- 1) 



/s + 1 

s Vs 1 

x 2 + 1 , , x 2 1 

-TTi fx/ udx = ! - 


x 2 1 



f> /Xd x Ix v 

^ C A 


/X" e/ Xdx z d x =/a d x = a x + C 

x 2 1 r (a x + C) xd x 

r _\ _ !___ 

y x J (x 2 I) 2 

which being Rational may be farther integrated, and it is found that 

A v 4- C v 2 1 ,, x _ 

C* A. J \*J A. Jl -I / f~^i " 

2 x 4 x \ x + 

Here we shall terminate our long digression. We have exposed both 
the Direct and Inverse Calculus sufficiently to make it easy for the 
reader to comprehend the uses we may hereafter make of them, which 
was the main object we had in view. Without the Integral Calculus, in 
some shape or other, it is impossible to prosecute researches in the higher 
branches of philosophy with any chance of success ; and we accordingly 
see Newton, partial as he seems to have been of Geometrical Synthesis, 
frequently have recourse to its assistance. His Commentators, especially 


the Jesuits Le Seur and Jacquier, and Madame Chastellet (or rather 
Clairaut), have availed themselves on all occasions of its powers. The 
reader may anticipate, from the trouble we have given ourselves in establish 
ing its rules and formulae, that we also shall not be very scrupulous in that 
respect. Our design is, however, not perhaps exactly as he may suspect. 
As far as the Geometrical Methods will suffice for the comments we may 
have to offer, so far shall we use them. But if by the use of the Algo 
rithmic Formulae any additional truths can be elicited, or any illustrations 
given to the text, we shall adopt them without hesitation. 


124. This Proposition is a generalization of the Law discovered by Kepler 
from the observations of Tycho Brahe upon the motions of the planets 
and the satellites. 

" When the body has arrived at B," says Newton, " let a centripetal 
force act at once with a strong impulse, #c."] But were the force acting 
incessantly the body will arrive in the next instant at the same point C. 

For supposing the centripetal force 
incessant, the path of the body will 
evidently be a curve such as A B C. 
Again, if the body move in the chord 
A B, and A B, B C be chords de 
scribed in equal times, the deflection 
from A B, produced by an impulsive 
force acting only at B and communi- -^ 
eating a velocity which wouldhavebeen 
generated by the incessant force in the time through A B, is C c. But 
if the force had been incessant instead of impulsive, the body would have 
been moving in the tangent B T at B, and in this case the deflection at the 
end of the time through B C would have been half the space describ 
ed with the whole velocity generated through B C (Wood s Mech.) 

C T = i C c 
.. the body would still be at C. 



Let F denote the central force tending constantly to S (see Newton s 
figure), which take as the origin of the rectangular coordinates (x, y) 
which determine the place the body is in at the end of the time t. Also 
let g be the distance of the body at that time from S, and 6 the angular 
distance of g from the axis of x. Then F being resolved parallel to the 
axis of x, y, its components are 

F.- and F. 3L 

S S 

and (see Art. 46) we .. have 

d 2 x _ F x ^ d 2 y _ F JT 


yd 2 x _ p,xy__xd 2 y 
d t 2 ~J~ ~dT 2 

< y d 2 x x d g y 

d t 

yd 2 x xd 2 y = dydx + yd 2 x dxdy xd 2 y 

= d . (y d x x d y) 
.. integrating 

y d x x d v 

j = constant = c. 

d t 


x = g cos. d, y = g sin <?, x 2 + y 2 = g 2 
. . d x = g d 6 sin. + d g cos. 6 
d y = g d 6 cos. 6 + d g sin. S; 
whence by substitution we get 

ydx xdy = f 2 d 

But (see Art. 1 13) 

g 2 = d . (Area of the curve) = d . A 

.-. d t = s - r = . d A. 

c c 

Vor.. I. H 


Now since the time and area commence together in the integration 
there is no constant to be added. 


.-. t = X A oc A. 

Q. e. d. 

J25. COR. 1. PROP. II. By the comment upon LEMMA X, it appears 
that generally 


v = d-t 

and here, since the times of describing A B, B C, &c. are the same by 
hypothesis, d t is given. Consequently 

v oc d s 

that is the velocities at the points A, B, C, &c. ai*e as the elemental spaces 
described A B, B C, C D, &c. respectively. But since the area of a A 
generally = semi-base X perpendicular, we have, in symbols, 

d . A = p X d s 
d. A 

. . V OC d S CC - ; 


and since the A A B S, B C S, C D S, &c. are all equal, d A is constant, 
and we finally get 

1 c 

v a or = 

P P 

the constant being determinable, as will be shown presently, from the 

nature of the curve described and the absolute attracting force of S. 

126. COR. 2. The parallelogram C A being constructed, C V is equal and 
parallel to A B. But A B = B c by construction and they are in the 
same line. Therefore C V is equal and parallel to B c. Hence B V is 
parallel to C c. But S B is also parallel to C c by construction, and 
B V, B S have one point in common, viz. B. They therefore coincide. 
That is B V, when produced passes through S. 

127. COR. 3. The body when at B is acted on by two forces ; one in 
the direction B c, the momentum which is measured by the product of its 
mass and velocity, and the other the attracting single impulse in the di 
rection B S. These acting for an instant produce by composition the 
momentum in the direction B C measurable by the actual velocity X mass. 
Now these component and compound momentums being each propor 
tional to the product of the mass and the initial velocity of the body in 
the directions B c, B V, and B C respectively, will be also proportional 
to their initial velocities simply, and therefore by (125) to B V, B c, B C. 





Hence B V measures the force which attracts the body towards S when 
the body is at B and so on for every other position of the body. 

128. COR. 1. PROP. II. In the annexed 
figure B c = A B, C c is parallel to 
S B, and C c is parallel to S B. Now 
A S C B = S c B = S A B, and if the 
body by an impulse of S have deflected 
from its rectilinear course so as to be 
in C, by the proposition the direction 
in which the centripetal force acts is that 
of C c or S B. But if, the body having 
arrived at C , the ASBC be>SAB 
(the times of description are equal by 
hypothesis) and .-. > S B C, the vertex 
C falls without the A S B C, and the 
direction of the force along c C or B S , 
has clearly declined from the course 
B S in consequentia. 

The other case is readily understood 
from this other diagi am. 

129. To prove that a body cannot de 
scribe areas proportional to the times round 
two centers. 

If possible let 



S A B = S B C. 


A S B C ( = S A B) = S B c 
and C c is parallel to S B. But it is 
also parallel to S B by construction. 
Therefore S B and S B coincide, which 
is contrary to hypothesis. 

130. PROP. III. The demonstration of this proposition, although strictly 
rigorous, is rather puzzling to those who read it for the first time. At least 
so I have found it in instruction. It will perhaps be clearer when stated 
symbolically thus : 

Let the central body be called T and the revolving one L. Also lef 
the whole force on L be F, its centripetal force be f, and the force ac- 



celerating T be f . Then supposing a force equal to f to be applied to 
L and T in a direction opposite to that of f , by COR. 6. of the Laws, 
the force f will cause the body L to revolve as before, and we have 

f = F f 

F = f + f . 

Q. e. d. 


Suppose on the deck of a vessel in motion, you whirl a body round in a 
vertical or other plane by means of a string, it is evident the centrifugal 
force or tension of the string or the power of the hand which counteracts 
that centrifugal force i. e. the centripetal force will not be altered by the 
force which impels the vessel. Now the motion of the vessel gives an 
equal one to the hand and body and in the same direction ; therefore the 
force on the body = force on the hand + centripetal power of the hand. 

131. PROP. IV. Since the motion of the body in a circle is uniform by 
supposition, the arcs described are proportional to the times. Hence 

., , arc X radius 
t a arc described oc 5 

oc area of the sector. 

Consequently by PROP. II. the force tends to the center of the circle. 

Again the motion being equable and the body always at the same dis 
tance from the center of attraction, the centripetal force (F) will clearly 
be every where the same in the same circle (see COR. 3. PROP. I.) But 
the absolute value of the force is thus obtained. 

Let the arc A B (fig. in the Glasgow edit.) be described in the time T. 
Then by the centripetal force F, (which supposing A B indefinitely small, 
may be considered constant,), the sagitta D B (S) will be described in 
that time, and (Wood s Mechanics) comparing this force with gravity as 
the unit of force put = 1, we have 

S = fFT< 

g being = 32 feet. 
But by similar triangles A B D, A B G 



If T be given 

If T = arc second 


2S (arc A B) 
~ jfT 2 = g R T 2 


Fa (arcA^ 

_ (arcAB) 
r 7^ 

132. COR. 1. Since the motion is uniform, the velocity is 



F - oc 

* * T-J "* T> 

g R R 
133. COR. 2. The Periodic Time is 

circumference 2 it R 

p _ 


* 2 R 

gRP 2 gP 

134. COR. 3, 4, 5, 6, ^. Generally let 
P = k x R n , 

k being a constant. 


2 T R 2 if 

~P~~ = k R- 



P 2 


F = 


gk 2 R 


Conversely. If F a Rgn-1 ; P will a R 
For (133) 


135. COR. 8. A B, a b are similar 
arcs, and A B, a h contemporaneous 
ly described and indefinitely small. M 

Now ultimately 

an: am:: ah :ab* 

a m : A M : : a b : A B 
.-. an : A M : : ah 2 : ab. A B 





f : F 

ah* e A B 
a b 

a s 

A B 2 

. ,% (LEMMA V) 
A Ib v 

a s 


A B 

V 2 

_V 2 

* A S* 

And if the whole similar curves A D, a d be divided into an equal 
number of indefinitely small equal areas A B S, B C S, &c. ; a b s, b c s, 
&c. these will be similar, and, by composition of ratios, (P and p being 
the whole times) 

P : p : : time through A B : time through a b 
A B ab AS 


v V 


V 2 

a s 

A S 

rp 2 



; RB (131) 
AB 2 

136. COR. 9. Let A C be uniformly described, 
and with the force considered constant, suppose 
the body would fall to L in the same time in 
which it would revolve to C. Then A B being 
indefinitely small, the force down R B may be 
considered constant, and we have (131) 
A C 2 : A B 2 : : T 2 : 

A B 
. . TT 2 . 

A L 

: : AL 
: . AL 


AB 2 =ALxAD. 

PROP. VI. Sagitta ex F when time is given. Also sag. a (arc) 2 by 
LEMMA XI, ex t 2 when F is given 
.. when neither force nor time is given 

sag. ex F X t 2 ; 



By LEMMA X, COR. 4, 

space ipso motus initio 

* C a 7-g 



To generalize this expression, let -^ be the space described in I" at 

the surface of the Earth by Gravity. Also let the unit of force be Gravi 
ty. Then 

1 : : 1^" : 2X I 772 
2_sag. _2_ ^ } 

gt 2 g t 2 

by hypothesis. 

137. COR. 1. F oc 5J 1 a Q ^ 

t 2 (area S P Q) 2 


S P 2 x Q T 2 

To generalize this, let a be the area described in I . Then the area 

described in t" a X t = . 


SP x QT 

and substituting in (a) we get 

8 a 2 _QR b) 

~Y < SP 2 x QT 2 

Again, if the Trajectories turn into themselves, there must be 
a : I" : : A (whole Area) : T (Period. Time) 

a = A 

Hence by (b) we have 

8A 2 QR ,^ 

r = _.- X 

gT 2 S P 2 x QT 2 

which, in practice, is the most convenient expression. 

8 A 2 Q R 

138. COR. 2. F = g-^- 2 X g-y^x Q P 2 ^ 

139. Cor. 3. F = |A| X SY x PV (e) 


Hence is got a differential expression for the force. Since 
P v - ~P d * 

A. T i 


__.8 A 2 i 

.". -T lFf\H X 

gT 2 2p 2 pdg 

- 1A! x dp m 

-gT 2 Vdg 

Another is the following in terms of the reciprocal of the Radius Vector 
o and the traced-angle 6. 

1 .- dg 2 + g 2 d 
p" 2 = g 4 d d z 
d 2 1 


, du 

d g = 5- 

u 2 


1 du 


dp 2dud 2 u 


dp d 2 u 2 3 

p^d~g == "d^ L 
and substituting in f we have 

F - 1AI v ( u M- u 
- ^F 2 \d ^ 2 

140. COR. 4. F a _- x V 2 X 

* FV* 
This is generalized thus. Since 

v _ space __ P Q 

Time "" t 





aXt(=7~Xt) = area described 
P Qx S Y 


and by COR. 3. 

.v PQ - 2A 
* t T 



S Y 

4 A 

v 2 V 
I = - X 


g" PV 
From this formula we get 

V 2 =- X F X P V 


- 2 F 

But by Mechanics, if s denote the space moved through by a body 
urged by a constant force F 

V 2 = 2gF x s 

P V 

s = -4- 

that is, the space through which a body must fall when acted on by the force 
continued constant to acquire the velocity it has at any point of the Trajec 
tory, is % of the chord of curvature at that point. 

dp dp 

The next four propositions are merely examples to the preceding formulae. 
141. PROP. VII. 

R P 2 (= Q R x R L) : Q T 2 : : A V 2 : P V* 

. QR * RL x PV 2 _, n T 

A ir 9 V^ 1 

A V 


W |J 

and multiplying both sides by ^-^ and putting P V for R L, we have 

Also by (137 c.) 

S P 2 x P V 3 _ SP* x QT S 

AV 2 QR 

A V 2 1 

C SP 2 x P V 3<X S P" 2 x P V 3 

_ 8 A 2 

: x 

A V 


P V 

S P 2 X P V 3 * 



From similar triangles we get 

A V : P V : : S P : S Y 
SP x PV 

.-. SY = 


S P 2 x P V 2 

S Y - X P V = A yf X P V 

S P 2 x PV 3 

^A V 2 

Foe 1 

SY* X PV SP 2 x PV 

as before. 


r 2 a 2 + e 2 
P ~- -2~ 
is the equation to the circle ; whence 

_dp _ j_ 
df ~" r 

_ 4A 2 dp _ 4 A 8 
= gT~ 2X p T dl~gT 2 
4?rr 8 r 3 

3 2crr 4 


The polar equation to the circle is 

2 a cos. 
~ 1 + cos. 2 6 


. /_ U 1 

\ p / 2 a cos. 

d_u 1 / sin. ^ 

" d 6 2 a \cos. 2 ^ 

I 2 a 


1 sin. 
~ ~ X 

2a cos. 2 
d u _ J_ /3 sin. 2 tf 2 sin 4 tf \ 
d 6 "" 2~a \ cos. 6 cos7 3 1/ 

= 0^ X^V^X(3-sin 
2 a cos. 3 6 v 




d 2 u 

sin. z 6 . 2 _J cos. I 

2 a cos. 3 <T (A ~ 6) + 2 a cos.^ * ~2~a~ 


2 a cos. 3 d 

2 a cos. 3 6 

X (3 sin * 6 sin. 4 6 + cos. 2 6 + cos. 4 

X (2 sin. 2 sin. 4 0+ 1 + 12 sin. 

a cos. 3 6 
which by (139) gives 

4A 2 u 

a cos. d 6 

4 A 2 ( 1 + cos. 2 6) z 
v \ * __ 

g T 2 4 a 3 cos. 5 ^ 

cos. 5 6 

142. COR. 1. F oc - 
But in this case 

.-. Foe 

S P = P V. 

1 _32gr 4 

or ^ m X 

SP 5 gT 2 ^ SP S 

COR. 2. F: F:: RP 2 x PT 3 : SP 2 x PV S 

: : S P x R P 

SP 3 x PV 

PT 3 
:: S P x R P 2 : SG 3 , 

by similar triangles. 

This is true when the periodic times are the same. When they are 
different we have 

F: F::SPxRP 2 -4-xSG 3 , 

S K 1 


where the notation explains itself. 
143. PROP. VIII. 

C P 2 : PM 2 :: PR 2 : QT 2 

PR 2 = QRx(RN + QN)=QR X 2PM 
.-. C P 2 : P M 2 : : Q R x 2 P M : Q T* 

Q T " _ 2PM 3 
* Q R : C P 2 



QT Z X SP 2 2PM 3 X SP 2 

QR CP 2 

CP 2 


2PM 3 x SP 2 PM 3 
Also by 137, 

CP 2 

g SP 2 x PM 3 


_ S P X velocity __ S P X V 

V 2 CP 2 
.-. F = X 

g PM 3 



F oc 

SP 2 X P V 3 

But S P is infinite and P V = 2 P M. 


.-. F 

P M 3 


The equation to the circle from any point without it is 

c 2 - r 2 g 2 
P ~ " 2r 
where c is the distance of the point from the center, and r the radius, 

Moreover in this case 

g = c + PM = c + y 

c 2 r 2 c 2 2cy y 8 
.-. P = - -jj- 

c y 

. dp _ c + y x 


r c y 


Hence (139) 

_ 4a*r 2 1 ._ V 2 r 2 1 

* "^ ~* " o ^> ~^ ^\ q 

c 2 g y 3 g y 3 


144. Generally we have 

P R 2 : QT 2 : : P C 2 : P M* 

PR 2 O T 
J 1V ^ J 

. . p p 2 . p TV/I 2 

- Q~R J 


PR 2 

P V 



P C : P M : : 2 R (R = rad. of curvature) : P V 

QT 2 _ PM 2 _2RxPM 

QR : PC 2 : P C 

2 R X P M 3 

PC 3 

QT 2 _2AC 2 
QR B C 4 * 


From the expression (g. 139) we get 

,-, 4a 2 d 2 u 

F = X -j r X u 2 . 

& U a 


a dd dx 

4a 2 V 

a X t = 5-g- = a X -^ 

d d 2 " d x 2 

j UP 

.. d u = ~ 






= r ( see 69 ) 

V 2 ? 4 d 2 e 1 

T| _ V/ VX 

g ax^ 
This is moreover to be obtained at once from (see 48) 


F = - x 


d t = 

.-. F = 

g dt" 



V 2 

g d x : 

145. PROP. IX. Another demonstration is the following: 


gdx 2 

V 2 

f 2 
, d 2 f 



V 2 

dx 2 

d 2 y 



S T P 

Let Z-PSQ = /-pSq. Then from the nature of the spiral the 
angles at P, Q, p, q being all equal, the triangles S P Q, S p q are simi 
lar. Also we have the triangles R P Q> r p q similar, as likewise Q P T, 

QT 2 



S P : S p 

and by LEMMA IX. 

q r : q r : : p r 2 : p r 2 : : q t /2 : q t 4 




q r 


q t 2 _ q_t_ 8 

q r 



,, . c p 

a S P 


.-. F 

S P 



The equation to the logarithmic spiral is 


p = - X S 

d_p _ b 
d a a 
and by (f. 139) we have 

F = 


Using the polar equation, viz. 


4 a " 


4 a 2 



a 3 

4 a 2 .a 2 






/ / 2 2\ 

v (a 2 b 2 ) a 

the force may also be found by the formula (g). 
146. PROP. X. 

P v x v G : Q v 2 : : P C 2 : C D 2 


Q v 2 : QT 2 : : P C 2 : P F 
.-. P v x v G : QT 2 : : PC 4 : CD 2 x P F 2 

.-. v G : 

P v 

CD 2 X P F 
PC 2 


P V = Q R, and C D x P F = (by Conies) B C X C A 

ult. v G = 2 P C. 

B C 2 X C A 2 

.-.2 PC : 

PC 8 


Q R PC p r 

*QT 2 X CP 2BC 2 x C A 2 
Also by expression (c. 137) we get 

_ 8A 2 PC 

r = Fi=n; X 

gT 2 2B C 2 X C A 2 

A= * X BC X C A 

The additional figure represents an Hyberbola. The same reasoning 
shows that the force, being in the center and repulsive, also in this curve, 
a C P. 



Tu = TV 


u V : v G : : D C 2 : P C* 

Then since 

Q v 2 : Pv x vG : : D C 2 : P C 2 

.-. u V : v G : : Q v 2 : P v x v G 
.-. Q v 2 = P v x u V 

.-.Qv 2 + uPxPv= PvX (uV + uP) 
= P v x V P. 


Qv J = QT 2 + Tv 2 = QT 2 + Tu 2 

= p Q 2 P T 2 + T u 2 

= p Q2_ (PT- Tu 2 ) 
= PQ2_P U X Pv 
(chord PQ) 2 = Pv x VP. 

Now suppose a circle touching P R in P and passing through Q to 
cut P G in some point V . Then if Q V be joined we have 

z.PQv=z-QPR = ^-QV P 
and in the A Q P v, Q V P the L. Q P V is common. They are there 

fore similar, and we have 

P v : P Q : : P Q : P V 
.-. P Q 2 = P v x V P = PvxVP 

.-. V P = V P 
or the circle in question passes through V ; 

.. P V is the chord of curvature passing through C. 


Again, since 

DC 2 

u V = v G x p ^ a = C x v G 


p V P u = C (P G P v) 

P V, PG 

being homogeneous 

2 D^C 2 2CD* 

PC 2 PC 

.-. (Cor. 3, PHOP. VI.) 


2 PF a x CD 2 

But since by Conies the parallelogram described about an Ellipse is 
equal to the rectangle under its principal axes, it is constant. .. P F x 
CD is. 


F p C. 


By (f. 139) we have 

g T 
But in the ellipse referred to its center 

- a * + b 8 ~- 

._ a 2 + b 2 

and differentiating, and dividing by 2, there results 

dp _ g 
p s dg a 2 b i! 
which gives 

4A 2 P 4^r 2 

TT _ _ v _ - \( a. 

~gT 2 a 2 b 2 ~ g T* 

In like manner may the force be found from the polar equation to die 
ellipse, viz. 


" 1 _ e 2 cos. 2 6 
by means of substituting in equat. (g. 131). ) 


147. COR. 1. For a geometrical proof of this converse, see the Jesuits 
notes, or Thorpe s Commentary. An analytical one is the following. 

Let the body at the distance R from the center be projected with the 
velocity Vin a direction whose distance from the center of attraction is P. 
Also let 

F = *< 

IL being the force at the distance 1. Then (by f ) 
4 A 2 ^ dp 

= ^r**P*-*l = ^ 

which gives by integration, and reduction 
1 _^gT 2 
p" 2 -"^^ h 

R and P being corresponding values of g and p. 
But in the ellipse referred to its center we have 
_!_ _ a 2 +b 2 g 2 
p 2 ~ a 2 b 2 a 2 b 2 

which shows that the orbit is also an ellipse with the force tending to its 
center, and equating homogeneous quantities, we get 


a 2 b 2 4 A 2 P 


a 2 b 2 4 A 2 

A = cr a b 

... T = 2 * (1) 


which gives the value of the periodic time, and also shows it to be con 
stant. (See Cor. 2 to this Proposition.) 

Having discovered that the orbit is an ellipse with the force tending to 
tne center, from the data, we can find the actual orbit by determining its 
semiaxes a and b. 

By 140, we have 

v - L 

V T 1 P 

a 2 + b g _ R 2 l_ 

* ~~ a^b 2 " -^g x V 2 P 2 "*~P 2 

1 _L 

aTp-^S x V 2 P 2 


V 2 

l 2 -i-h 2 R 2 _L 
. . cl -]- U IV -}- 


2 VP 

2 a b = =-r 

. . a + b = ^ 

g v>g 

which, by addition and subtraction, give a and b. 


By formula (g. 139,) we have 

...4. u _ 

d tf 2 ^ TT 2" x u~ 3 ~ ( 

and multiplying by 2 d u, integrating and putting 8 * T 2 _ ^ 

4< A 

d u 2 M 

dT* + u2 + ^2 + ^ = 

To determine C, we have 

d u 2 _ J_ dj 8 

d0 2 ~ f * dl" 8 
and in all curves it is easily found that 

. I 1 ," 2 _ e 2 p 8 _ _i 
d^- g p s = p~" 
Hence, when ^ = R, and p = P, 

which gives the constant C. 
Again from (2) we get 

_ _ 
- V ( M Cu u 4 ) 

which being integrated (see Hersch s Tables, p. ItiO.-^Englished edit 
published by Baynes & Son, Paternoster Row) and the constants properly 
determined will finally give g in terms of *- whence from the equation to 
the ellipse will be recognised the orbit and its dimensions. 

I 2 



148. COR. 2. This Cor. has already been demonstrated see (1). 
Newton s Proof may thus be rendered a little easier. 
By Cor. 3 and 8 of Prop. IV, in similar ellipses 

T is constant. 
Again for Ellipses having the same axis-major, we have 


cr a b b 
oc a 

But since the forces are the same at the principal vertexes, the sagittae 
are equal, and ultimately the arcs, which measure the velocities, are equal 
to the ordinates, and these are as the axes-minores. Hence, a (which 

v X S Yx , 
- ) oc b. 

.*. T oc -T- <x ] or is constant. 

Again, generally if A and B be any two ellipses whatever, and C a third 
one similar to A, and having the same axis-major as B ; then, by what 
has just been shown, 

T in B = T in C 

T in C = T in A 
.-. T in B = T in A. 

149. SCHOL. See the Jesuits Notes. Also take this proof of, " If one 
curve be related to another on the same axis by having its ordinates in a 
given ratio, and inclined at a given angle, the forces by which bodies are 
made to describe these curves in the same time about the same center in 
the axis are, in corresponding points, as the distances from the center." 

The construction being intelligible from the figure, we have 

P N : Q N : : p O : q O 
.-. P N : p O : : Q N q O 

: : N T : O T ultimately. 




.-. Tangents meet in T, 

the triangles C P T, C Q T are in the ratio of P N : Q h or of parallelo 
grams PNOp, QNOq ultimately, i. e. in the given ratio, and 
C p P : C P T : : p P : P T ultimately. 
: : NO: NT 
: : qQ:QT 
: :CQq: CQT 
.. C p P : C q Q in a given ratio. 

. bodies describing equal areas in equal times, are in corresponding 
points at the same times. 

.-. P p, Q q are described in the same time, and m p and k q are as the 

Draw C R, C S parallel to P T, Q T; then 

p O : q O : : P N : Q N : : n O : 1 O 
.-. n O : p O : : 1 O : q O 

1 O : O S) 


n p 

: n O 

: Iq 

1 Q-) 




: n R 

: IQ 

1 S j 

(since n O 

: O R 


O C: 

* P 

: n R 

1 q 

1 S 

.-. n p 

: p R 

1 q 



n p 

1 q 

: p R 

: q S 

m p 
k q 

q C) 

.-. mp 

: P C 

k q 




: F at q 

P C 


Q. e. d. 


150. PROP. XI. This proposition we shall simplify by arranging the pro 
portions one under another as follows : 



( = Px) : L xPv : 

: PE 

P C 

A C 

P C 


: G v x P v 


G v 

G v x P v 

: Q v 2 

PC 2 


Qv 2 




Qx 2 

:QT = 

PE 2 

P F 2 


CA 2 

P F- 

CD 2 

C B 


.-.Lx QR: QT 2 : : A CxLx P C 2 xCD 2 : PC xGvxCD 2 xCB 2 



QT 2 ~ G v x C B* -" 2 PC X C B 2 2 C B 2 

T? QR (_ AC x 1 

* * a Q T 2 x S P A- 2 C B 2 x S P 2 ) SP 2 

Q. e. d. 

Hence, by expression (c) Art. 137, we have 
8 A 2 AC 

T? v 

-- rr* o ^ 

gT 2 2 CB 2 x S P 2 

" 2 b 2 x e 2 
X^ (a] 

where the elements a and T are determinable by observation. 


A general expression for the force (g. 139) is 
4 A 2 9 /d 2 u , x 
F = g-T 2 x u (dT 2 + u ) 
But the equation to the Ellipse gives 
_ 1 _ 1 -f e cos. 6 
= - = -^(T^^eY 
where a is the semi-axis major and a e the eccentricity. 

d u e sin. 6 

dT : ~a(l e 2 ) 

d 2 u e cos. 8 

d 2 u 
dT 2 + u = 


F = 

T 2 X a(l e 2 ) 


A s = w 2 a 2 b 2 = * 2 a 2 (a 2 a 2 e 2 ) 

. F _ ill^ 3 x u , 
gT 2 

the same as before. 



Another expression is (k. 140) 

_ 4A 2 dp 
F = -77^ X -,-f- . 
g 1 p a g 

Another equation to the Ellipse is also 

j. _ 2 a g _ 2 a J_ 

dp a 

P 5 ^! "" ^V 

T? _ 

- b 2 g 

u a v 

X i o 5 - rfi ij ^N " o * 

b 2 P^ G -L ~ 

^ b O 

151. PROP. XII. The same order of the proportions, which are also let 
tered in the same manner, as in the case of the ellipse is preserved here. 

Moreover the equations to the Hyperbola are 
a (e 2 I) 
1 + e cos. 6 

P 2 = -^i- 

which will give the same values of F as before excepting that it becomes 
negative and thereby indicates the force to be repulsive. 

152. PROP. XIII. By Conies 

4SP.Pv = Qv 2 = Qx 2 ultimately. 

.-. 4 SP. Q R : Qx 2 : : 1 : 1 

Qx 2 : QT 2 : : SP 2 : S N 2 

:: S P : S A 
.-. 4SP.QR : QT 2 :: S P : S A 

QR 1 . !_ 

" Q T 8 ~ 4 S A " L 
L being the latus rectum. 

.-. F 

Q~T 2 X S P 2 S P 2 

F = ! X g^QHj T , (b. 


8a 2 1 2 P 2 V 2 1 

X ] X 

~ g L S P 2 gL 

a being the area described by the radius-vector in a second, or P the per 
pendicular upon the tangent and V the corresponding velocity. 


In the parabola we have 


which give 

12 22 

u = - = -j- (1 + cos. 0) = -J- + T cos. 

1^ 4 1 

P~ 2 ~ L X J 

d 2 u 2 

d7^ + u = X 


d p _2 _1 

and these give, when substituted in 

F - ?2 V2 u 2 ( 
g \p~} 


P V a dp 

o; p a d P 

O Jt 9 

the same result, viz. 



Newton observes that the two latter propositions may easily be deduced 
from PROP. XL 

In that we have found (Art. 150) 

4 A 2 a 

= JTT 5 x 

P 2 V 2 

g r 

Now when the section becomes an Hyperbola the force must be repul 
sive the trajectory being convex towards the force, and the expression re 
mains the same. 


Again by the property of the ellipse 

b : : ax a: -g a - 

4 4 \ 

which gives 

a_ _2 _ JL 

b 2 ~ L ~~4 a 
and if c be the eccentricity 

b 2 = a 2 c 2 = (a + c) X (a c) 
" _ a _ _ 2 1 
(a + c) X (a c) "" L ~ 4 a 
Now when the ellipse becomes a parabola a and c are infinite, a c is 

finite, and a + c is of the same order of infinites as a. Consequently r 9 


\sjinite, and equating like quantities, we have 

_a _J2 

b~ 2 ~"L 
which being substituted above gives 

2P 2 V 2 1 

the same as before. 

Again, let the Ellipse merge into a circle; then b = a and 

v P 2 V 2 a 
TV _ _ v 

A A 

K 2 2 

5 D S 

a V 2 ^ 

g X ? 2 
V s 


g X 

153. PROP. XIII. COR. 1. For the focus , point of contact, and position of 
the tangent being given, a conic section can be described having at that point 
a given curvature. ] 

For a geometrical construction see Jesuits note, No. 268. 

The elements of the Conic Section may also be thus found. 

The expression for R in Art. 75 may easily be transformed to 

R = 

p 2 d 6* * d <T- 

p z ~dl~ ~7~ a ** - 


Now the general equation to conic sections being 

b 2 1 
s = x 

a 1 + e cos. 6 
the denominator of the value of R is easily found to be 

which gives 

R - *- 
a p 3 


b 2 p 3 
- = - x R 

a f J 

is known. 

Again, by the equation to conic sections we have 

b 2 g 

P = 2 a ipe 

which, by aid of the above, gives 

a = 2g 2 ~p R 

p 8 R 
~ 2 g 2 p R* 

Whence the construction is easy. 

154. The Curvature is given from the Centripetal Force and Velocity being 


If the circle of curvature be described passing through P, Q, V, and O 
(P V being the chord of curvature passing through the center of force, 
and P O the diameter of curvature) ; then from the similar triangles 
P Q R, P V Q, we get 

P Q 2 

QR - . 

iv - P V 

Also from the triangles P Q T and P S Y (S Y being the perpendicu 
lar upon the tangent) we have 

^^~ SY 
and from P S Y, P V O, 



whence by substitution, &c. 


QT 2 xSP*~2Rx SY 2 

_ 2P 2 V 2 QR V 2 x SP 

g * QT 2 x SP 2 " Rx SY 
which gives 

SP_ V 2 

- > ~- 

Hence, S P, S Y and g being given quantities, R is also given if V and 
F are. 

155. Two orbits which touch one another and have the same centripetal 
force and velocity cannot be described. ] 

This is clear from the " Principle of sufficient Reason." For it is a 
truth axiomatic that any number of causes acting simultaneously under 
given circumstances, viz. the absolute force, law of force, velocity, direc 
tion, and distance, can produce but one effect. In the present case that 
one effect is the motion of the body in some one of the Conic Sections. 


Let the given law of force be denoted generally by f g, where f g means 
any function; then (139) 

F _ P 2 V 2 dp 

g *p a de 

and since P and V are given 

pv _ . ^ P . 

g p 3 d P 

But if A be the value of F at the given distance (r) from the center to 
the point of contact ; then 

F : A : :fg :fr 

F: A: :f :fr 


~ f r S 



1Z! jL.p_ A r 

3 d ~ fr X 



g P 

P 2 V 2 dp A 

r Via 

/ Q i / r* ^. * C 

s p 3 d / f r 

and integrating, we have 
P 2 V 2 f r 


Po TT o n i i 

2 V 2 f r /!_ JL \ _ /- i e 

Nowyd g f g and yd g f g are evidently the same functions of g and g t 
which therefore assume 

a P and P 5 

and adding the constant by referring to the point of contact of the two 
orbits, and putting 

p? v*fr 
2 g A = M, 

we get 

M X (p-^ r,) = <p g <f> r 

MX (1 -L)=^ -?r. 

. J_ - L _L 
" p =: "M "" P*~ 

p 7 " 2 =: 31 + F 2 ~ 

in which equations the constants being the same, and those with which 
g and f are also involved, the curves which are thence descriptible are 
identical. Q. e. d. 

These explanations are sufficient to clear up the converse proposition 
contained in this corollary. 

156. It may be demonstrated generally and at once as follows : 
By the question 




/d g ^ 

and substituting in (d) we have 

1 1 1 1 

p 8 = r M + P 2 H " M g 
But the general equation to Conic Sections is 

_L 2a _L 

p 2 ~ b 3 g b 2 " 

Whence the orbit is a Conic Section whose axes are determinable from 
2a. 1 2 g A r 2 
b"2- M = pa V 2 


- _L 1 1 

+ b 2 ~ ~ r M. " P 2 

1 2 g A r 
^0^2 " p 2 "y 2" 

and the section is an Ellipse, Parabola or Hyperbola according as 

V 2 is >, or = or < 2 g Ar. 

Before this subject is quitted it may not be amiss by these forms also to 
demonstrate the converse of PROP. X, or Cor. 1, PROP. X. 

ff = < 

f r = r 

VV hence 

1 r 2 J_ g 2 

p 2 ~ 2 M H " P 2 2 M 

But in the Conic Sections referred to the center, we have 

which shows the orbit to be an Ellipse or Hyperbola and its axes may be 
found as before. 




In the case of the Ellipse take the following geometrical solution and 

C, the center of force and distance C P are given. The body is projected 
at P with the given velocity V. Hence P V is given, (for V 2 = -|. F . P V.) 

Also the position of the tangent is given, .-. position of D C is given, and 

SCO 2 

P V = .p, n . Hence C D is given in magnitude. Draw P F per- 
P C 

pendicular to C D. Produce and take P f = CD. Join C f and bisect 
in g. Join P g, and take g C, g f, g p, g q, all equal. Draw C p, C q. 
These are the positions of the major and minor axis. Also \ major axis 
= P q, \ minor axis = P p. 

For from g describe a circle through C, f, p, q, and since C F f is a 
right Z-j it will pass through F. 

.-.Pp.Pq= PF.Pf= PF.CD 

PC 2 +Pf 2 = Pg 2 -f g C 2 + Pg 2 + gf 2 , (since base of A bisected in g) 

= Pq 2 2 + 
= Pq 2 + Pp 2 

... Pp. Pq PF.CD \ But a and b are determined by the same 
Pp 2 + Pq 2 = PC 2 + CD 2 / equations. . . P q = a, P p = b. 

Also since p and F are right angles, the circle on x y will pass through p 
and F, and APpx = Cpq=CFq = xFp, because ^xFC = pFq. 
.-. L. Pp x = /-in alternate segment. .-. P p is tangent. 

Pp = PF.Px .-. P F. Px = b 2 . 

But if in the Ellipse C x be the major axis, P F . P x = b 2 . 


.. C x is the major axis, and . . C q is the minor axis. 
. . the Ellipse is constructed. 

PROP. XIII, COR. 2. See Jesuits note. The case of the body s 
descent in a straight line to the center is here omitted by Newton, be 
cause it is possible in most laws of force, and is moreover reserved for a 
full discussion in Section VII. 

The value of the force is however easily obtained from 140. 

O T 2 O T 2 

157. PROP. XIV. L = ^jL ^5 

W tt 

a Q T 2 X S P 2 by hypoth. 


By Art. 150, 

F - 4 A a 8 A 2 \ 

- g T* X b V " LgT 2 * p 
for the circle, ellipse, and hyperbola, and by 152. 

O P 2 V2 1 

F= r x 

T ^ *> 

Lg e 2 

for the parabola. 

Now if /& be the value of F at distance 1, we have 

Whence in the former case 

8 A 2 2 P 2 x V 2 

T T 2 P r 

and in the latter 

2 P 2 x V 2 


~-8 * : 1 2 : A 2 : T 2 


Aj; S P 2 x QT 2 P^x V 2 

" * T 2 ~ 4 ~ "4 ~ 

158. PROP. XIV. COR. I. By the form (a) we have 
A(= crab) = JtJl X V L X 1. 
T V L. 


159. PROP. XV. From the preceding Art. 

T= / X -. 
~ V AC, g V L 

But in the ellipse 

L = 


T X a 2 ... (e) 

V /*g 

160. PROP. XVI. For explanations of the text see Jesuits notes. 


By Art. 157 we get 

for the circle, ellipse, hyperbola, and parabola. 
But in the circle, L = 2 P. 

.-. V = V^X^p - A/Y^x ^ . . . (g) 

r being its radius. 

In the ellipse and hyperbola 

L - 2b2 

161. PROP. XVI, COR. I. By 157, 

L = X P 2 X V 2 . 

162. COR. 2. V = / X -, 

D being the max. or min. distance. 

163. COR. 3. By Art. 160, and the preceding one, 

* X : X 

: : V L : V 2 D. 
164. COR. 4. By Art. 160, 



2 b 2 
L = , P = b, and r = a 


.*. v : v : : 

b V a Va* 

165. COR. 6. By the equations to the parabola, ellipse, and hyper 
bola, viz. 

n * . O 

the Cor. is manifest. 

166. COR. 7. By Art. 160 we have 
/2 1 L 1 

v 2 . y 2 . . . 

2 P 2 r 

which by aid of the above equations to the curves proves the Cor. 


By Art. 140 generally for all curves 

pv - 

JL. T - 



P V = 2 g (racl. = e) 

But generally 

and in the circle 

An analogy which will give the comparison between v and v ; for any 
curve whose equation is given. 
167. COR. 9. By Cor. 8, 


.: ex equo 

v : v : : =- : p 


VOL. ]. 



1GB. PROP. XVII. The " absolute quantity of the force" must be 
known, viz. the value of ^ or else the actual value of V in the assumed 
orbit -will not be determinable ; i. e. 

L : L : : P 2 V 2 : P /2 V /2 
will not give L . 

It must be observed that it has already been shown (Cor. 1, Prop. 
XIII) that the orbit is a conic section. 

See Jesuits notes, and also Art. 153 of this Commentary. 

169. PROP. XVII, COR. 3. The two motions being compounded, the 
position of the tangent to the new orbit will thence be given and therefore 
the perpendicular upon it from the center. Also the new velocity. 
Whence, as in Prop. XVII, the new orbit may be constructed. 


Let the velocity be augmented by the impulse m times. 

Now, if /* be the force at the distance 1, and P and V the perpendicu 
lar and velocity at distance (R) of projection, by 156 the general equation 
to the new orbit is such that its semi-axes are 

R R 

or = 

- 2 m 2 " rn 2 2 



2 m 2 

according as the orbit is an ellipse or hyperbola. Moreover it also 
thence appears that when m 2 = 2, the orbit is a parabola, and that the 
equations corresponding to these cases are 



2 m 


m 2 P 


= P X 







170. In the parabola theforce acting in lines parallel to the axis, required F, 

4SP.QR:QT 2 ::Qv 2 :QT 2 ::YE 2 :YA 2 ::SE:SA::SP:SA 
Q R 1 

" QT 2 ~~ 4 S A a ^ ^ * s constant * F i g constant. 


Let u be the velocity icsolved parallel to P M then since the force acts 
perpendicular to P M, u at any point must be same as at A. .. if P Q be 

the velocity in the curve, Q T = u = constant quantity, and a = S/ P Q T 

S P.u 

. F _ 8a*.QR 2u 2 

" gS P .QT* ~ g~L" ^ S 
which avoids the consideration of S P being infinite ; and 

. . body must fall through - to acquire the velocity at vertex, which agrees 

with Mechanics. (At any point V = u / . 

^/ S A 
171. In the cycloid required the force when acting parallel to the axis. 




RP 2 : QT 2 :: Z P 2 : ZT 2 :: VF 2 : E F* : : VB: BE 

and since the chord of curvature (C. c) = 4 P M, R P 2 = 4 P M. R Q, 
/. 4 P M. R Q : Q T 2 : : V B : (B E =) P M 

" QT 2 ~~ 4 
p M 

F = 

S P constant ) 

* a = Yelocit > parallel to A B - 

/* / B V 

(At any point v = u . ^/ p-^ 

172. In the cycloid the force is parallel to the base 

R P 2 : QT 2 : : Z P e : ZT 8 : : V E 2 : V M 2 : : VB: VM 

and since C . c = 4 E M 

R P 2 = 4 E M.RQ, 
.-. 4EM.RQ:QT :: VB: V M, 
QR V B 1 

[f V M = y, F = 


4 E M. V M a E M. V M 
u g r / VBx 

2 r y v " V - 2 >/ 

u = velocity parallel to V B. 


8a 2 QR 2u 2 .QJR __""JL V ^__ \ 

= ^TS P^Q T 2 = g . Q T 2 ~ 2 g . E M . V M V 


(At any point v = u 

B V 


173. Find F in a parabola tending to the vertex. 


T P : P N : : T A : A E 


V 4 x 2 + y 2 : y : : x : 


V 4 x 2 + y 
4 x 2 + ax 4 x + a 

cl X 

= p, (A E), 

p ax 

2 dp __ g 2axdx(4x 
~ a 2 x 4 


dp _ 2 x + a 
p 3 ax 3 

2 a x , 2 2x + a ,, v 

. d x = . 5 d x, 

a x 3 


= V x* + y 2 , 
- x d x + y d y 

d x 

V x 

dp _ 2 x + a 2 V x 2 + 
* p *~d~p a x 3 2 x + a 

A P 

A N 

y 2 V X 2 + tl X 

^~x 2 V x a + ax 

a x 



174. Geometrically. Let P Q O be the circle of curvature, 



P v (C. c through the vertex of the parabola) = 
PQ 2 PO.Az 

PP. Az 

PQ 2 

A P 2 

QT 2 ~ 

Az 2 
A P 3 

QT 2 * 

. T? 

PO.Az 3 
8a 2 .Q R 

8a 8 . A P 

g. A P 2 .QT 2 ~ g.PO. A z s 

P O.Az 3 = 2 A S. 
.-. F = 

S P 3 SY 3 AT 


4a l . A P 

SP ; 

= 2 A S.A N 3 

g.A S.AN 3 

175. If the centripetal be changed into a repelling force, and the body 
revolve in the opposite hyperbola, F ot p g . 




The body is projected in direction P 11 ; R Q is the deflection from the 
Tangent due to repelling force H P, find the force. 

L . S P 
176. In any Conic Section the chord of curvature = ^-^r 


pv QP 2 QT 2 .S P 2 L.SP 2 
QR " Q RS Y 2 v* 

L.SP 3 

S Y 

177. Radius of curvature = ~ o~ 


P W = 


S"V SY 3 

o .. 2 

178. Hence in any curve F = s~Y*~p\r 

_8ji*_ 4a a .SP 

~g.SY .2RTSY~ 

K 4 

see Art. 



[SECT. Ill 

179. Hence in Conic Sections 

8a 2 8a 2 

F = 

g.SY 2 .PV~g.SY 2 .L.SP 2 

S Y 2 " 

8 a 2 1 


gTL.S P 2 SP~ 2 

L S P 2 

180. If the chord of curvature be proved = vs - independently of 

f~\ T 1 

he proof that ~ = L, this general proof of the variation of force in 

tonic sections might supersede Newton s; otherwise not. 

181. A body attached to a string, whose length = b, is whirled round so as 
to describe a circle whose center is the Jixed extremity of the string parallel 
to the horizon in T" ; required the ratio of the tension to the weight. 

Gravity = 1, .*. v of the revolving body = V g F b, if b be the length of 
the string ; t 

V 2 
.. F (= centripetal force = tension) = -T- (131) 


_ circumference 2 v b V b 

i =?^ ===== __ 2 T . , 


V g F b 

- gT 2 

4 T 2 b 
.. F : Gravity : : ^ ,, : 1, or Tension : weight : : 4 


If Tension = 3 weight; required T. 

4* 2 b:gT 2 : :3: 1, 

b : g T z . 

T 2 = - - - 

If T be given, and the tension = 3 weight, required the length of the string. 

"jp 2 __ _ ff 

.-. b = 

- - 

4 cr 

1 82. If a body suspended by a string from 
any point describe a circle, the string describes 
a cone , required the time of one revolution or 
of one oscillation. 

Let A C = 1, B C = b, 

The body is kept at rest by 3 forces, gra 
vity in the direction of A B, tension in the 
direction C A, and the centripetal force in 
the direction C B. 


As before, centripetal force = 


z b 


2 > 

and centripetal force : gravity : b : V 1 s b 2 , (from A) 
4 vr 2 V 1 - b 2 

. rPZ _ ^ 

= 2 if = a constant quantity if V 1 

2 n 2 

c n 

2 n ; 

be given. 

.-. the time of oscillation is the same for all conical pendulums having a 
common altitude. 

183. v in the Ellipse at the perihelion : v in the circle e. d. : : n : 1, Jind 
the major axis, eccentricity, and compare its T with that in the circle, and 
Jind the limits ofn. 

Let S A = c, 

v in the Ellipse : that in the circle e. d. : : V H P : V A C 

: : V H A : VAC in this case 
: : n : 1 by supposition, 

.-.2 AC AS = n 2 AC, 

... A C = C 

Excentricity =AC A S = 5- 


T : T in the circle : : A C^ : A S * : : 

(2-n 2 ) 

Also n must be <C V 2, 
for if n = V 2, the orbit is a parabola 
if n > V 2, the orbit is an hyperbola. 

184. Suppose of the quantity of 
matter ofto be taken away. How 
much would T of D be increased, and 
what the eccentricity of her new orbit ? 
the D s present orbit being considered 

At any point A her direction is 
perpendicular to S A, 

.. if the forcer be altered at any 
point A, her v in the new orbit will 

c 2 : : 1 : (2 n s ) 


= her v in the circle, since v = y > an d S Y = S A, and a is the 
same at A. 

Let A S = c, P V at A = L, and F = * ^ oc _. 

in this case, 

2 b z 
/. 3:4::2c(=Lin the circle) : ( = L in the ellipse) 

3b 2 3(a 2 a c) 3(2ac c 2 ) _ 3c 2 
. . 4 c ~~ - _ N 7 * ft f 

a a a 

3c 2 
.-. = 2c, 


And T in the circle : T 7 in the ellipse : : -^-7 : (~~] 

V 4 v 2 / 

V 3 
V~3 f 3 \ ^ 1 3 

V4 V2/ V 2 2 

: : V 2 : 3. 

And the excentricity = a 



185. What quantity must be destroyed that D s T may be doubled, and 
what the excentricity of her new orbit ? 
Let F of : f (new force) : : n : 1 

.*. v = / s. F . P V, and v is given, 


P V 

2b 2 n a 2 a c 2ac c 2 

.. n : 1 : : : 2 c : : : c : : - : c : : 2 a c : a 

a a a 

.*. n a =r 2 a c, 

2 n 
Also T in the circle : T in the ellipse : : 1 : 2 


: : (2 n) * : n * 
/. 1 : 4 : : (2 n) 3 : n .-. n =r 4 (2 n) 3 , whence n. 


And the excentricity 


c = 

c c (2 c nc) __ c (n 1) 

2 n~ 2 -n 2 n 

186. What quantity must be destroyed that D s orbit may become a 

parabola ? 

L = 4 c, 

.-. F : / : : 4 c : 2 c : : 2 : 1, 
.. \ the force must be destroyed. 

187. F a =T-J, a body is projected at \ given D, v = v in the circle, 

L. with S B = 45,yrcc7 axis major, excentricity, and T. 
Since v = v in the circle, .*. the body is projected from B, 

and L. S B Y= 45 ; 
.-. L. S B C, or B S C = 45, 

S B 

.-. S C = S B. cos. 45 = 


V 2 

S B = D 

axis major 

.. axis major and excentricity are found. 
And T may be found from Art. 159. 



188. Prove that the angular v round H : that round S : : S P : H P. 
This is called Seth Ward s Hypothesis. 

In the ellipse. Let P m, p n, be perpendicular to S p, H P, 
.-. p in = Increment of S P = Decrement of H P = P n 
.-. triangles P m p, P n p, are equal, 

.. P m = p n, and angular v -p 


189. Similarly in the hyperbola. 

Angular v of S P : angular vofSY::PV:2SP:: $.* S P 

C D 2 

: : HP : A C. 


190. Compare the times of fatting to the center of the logarithmic spiral 
from different points. 

The times are as the areas. 


c s 

, 2 

d . area = ( 6 - ^_ C S P), ford, area = - . 

fit fit 

f~\ r r* i A 

Also Tp^p = -- , = tan. L. Y P T = tan. , (a being constant) = a 

a p 
.-. area = s - g 2 , (for when P, = 0, area = 0, /, Cor. = 0) 

.*. if P, p, be points given, 

T from P to center : t from p to center : : S P 2 : S p 2 . 
191. Compare v in a logarithmic spiral with that in a circle, e. d. 

2 V 2 

F = 

.-. if F be given, V oc 
.-. v in spiral : v in the circle : : V P V in spiral : V 2 S P ::!:!. 
192. Compare T in a logarithmic spiral with that in a circle., e. d. 

rr . ! whole area a e 2 a P 2 

J in spiral = - 5 ? 

- : - - X7 - - _ - 
area in 1 4 . v . S Y 2 v . . sin. a 

T in cirrlp - whole area - g g* _ 2 or g 2 _ 2 cr 

A ill Clinic - ; - _ - . __ - - - 

area in 1" v . ib Y v . v 

ap* 2^p a 

- ^_ - . - i . . - : 2 T : : a : 4 * . sin. a. 
v . g . sin. a v 2 sin. a 

: : tan. a : 4 T . sin. a : : 1 : 4 T cos. . 




192. In the Ellipse compare the time from the mean distance to the Aphe- 
lion, with the time from the mean distance to the Perihelion. Also given the 
Excentricity, tojind the difference of the times, and conversely. 

A D V is - - described on A V. 


T of passing through Aphelion : t through Perihelion 
: : S B V : S B A 
: : S D V : S D A 

Let Q = quadrant C D V, 

. rp (-^ a . a e 

^ " 2 : ^ " 2 
.-. (T + t =) P : T t : : 2 Q : a . a e 

.-. T t = 

2 Q 

whence T t, or, if T t be given, a e may be found. 

193. If the perihelion distance of a comet in a parabola = 64, s mean 
distance = 100, compare its velocity at the extremity of It with s velocity 
at mean distance. 

Since moves in an ellipse, v at the mean distance = that in the circle 
e . d . and v in the parabola at the extremity of L 

: v in the circle rad. 2 S A : : V 2 : 1 
v in the circle rad. 2 S A 

: v in the circle rad. AC 
. v in the parabola at L 

: v in the ellipse at B 

V A C : V S A 

V 2 . AC : V S~A.~ 2 
: : 10 V 2 : 8 V 2 
: : 5 : 4 

194. What is the difference between L of a parabola and ellipse, having 
the same < st distance = 1, and axis major of the ellipse = 300? Compare 
the \ at the extremity ofL> and <" distances. 
In the parabola L = 4 A S = 4. 




In the ellipse L = 

2B C 
A C 




(A C 2 A C SA") 
(2 AC. AS AS 2 ) = 

600 J 

V 2 : 1 


\/50 : V299 

V 300 : V 299. 

v in the parabola at A : v in the circle rad. S A 
v in the circle rad. S A : v in the ellipse e. d. 
: : V AC : V 2AC SA 
/. v in the parabola at A : v in the ellipse e. d. : 
Similarly compare v s . at the extremity of Lat. R. 
1 95. Suppose a body to oscillate in a 
whole cycloidal arc, compare the tension 
of the string at the lowest point with 
the weight of the body. 

The tension of the string arises 
from two causes, the weight of the 
body, and the centrifugal force. At 
V we may consider the body revolving 
in the circular arc rad. D V, . . the 
centrifugal = centripetal force. Now 
the velocity at V = that down C V by the force of grav. 

= that with which the body revolves in the circle rad. 

2 C V. 

.. grav. : centrifugal force 
.-. tension : grav. 

196. Suppose the body to oscillate 
through the quadrant A B, compare the 
tension at B with the weight. 

At B the string will be in the direction of 
gravity; . . the whole weight will stretch 
the string; /.the tension will = centrifugal \ 
force + weight. Now the centrifugal 
force = centripetal force with which the 
body would revolve in the circle e. d. 

2 : 1 

And v in the circle = V 2 g . F . 




/. F = 


in this case, 

also v at B from grav. = V 2 g . C B, grav. = 1 . 

/. grav. = 1 = 
.*. F : grav. : : 

2g C B 

v 2 v 

2gCB g C B 
since v = v . 

/. tension : grav. : : 3 : 1. 
197. A body vibrates in a circular arc 
from the center C ; through what arc must 
it vibrate so that at the lowest point the 
tension of the string = 2 X weight? 

v from grav. = v d . N V, (if P 
be the point required) v of revo- 

, CV 
lution m the circle = v d . -^r . 

2: 1, 


/QV _ 

.-. centrifugal force : grav. : : v : v : : / : V N V 

.. centrifugal force + grav. (= tension) : grav. 

_ _ 
1- V N V : V N V 

2 : 1 by supposition. 

C V 

C V 

.-. N V = 

= V N V, 
C V 

198. There is a hollow vessel in form 
of an inverted paraboloid down which 
a body descends,, the pressure at lowest 
point = n . weight, find from what point 
it must descend. 

At any point P, the body is in the 
same situation as if suspended from G, 
P G being normal, and revolving in the 
circle whose rad. G P. Now P G = 

V 4 A S . S P, .*. at A, P G = 


V 4 A S 2 = 2 A S. Also.,* 2 at A with which the body revolves = 

.. centrifugal force = 

2g A S 


and grav. = - p , if h = height fallen from. 

But the whole pressure arises from grav. + centrifugal force, and = n . grav. 

. . centrifugal force + grav. : grav. : : n : 1 

1 1 1 

AS+ h : ::n:1 

1 1 

A~S : h ::n ~ l : J 

... h -- n 1 . A S. 

199. Compare the time (T ; ) in which a body de 
scribes 90 of anomaly in a parabola with T in the 
circle rad. = S A. 

Time through A L : 1 : : area A S L : a in 1" 

| A S. SL 4 A S 2 

a 3 a 

T in the circle rad. S A : 1 : : whole circle : a in 1" 

w A Q 2 

a A ij 

A S a 

.-. T = 


. T 1 T 



a: a :: VL: V2AS:: V4AS: V2AS:: 



.-. T : T : : 

: r : : 2 V 2 : 3 r. 

3 V 2 

Compare the time of describing 90 in the parabola A L voith that hi the 
parabola A 1, (fig. same.) 

t : T in the circle rad. S A : : 4 : 3 V 2 . T 

T in the circle S A : T in the circle rad. o A : : S A.% : a A* 
(since T 2 R 3 ) 

T : t through 1 A : : 3 V 2 . v : 4 

~ e .. ~~ z . k % i. VU g.i v ;.*. . . ^ i* : <7 A ff . 

See Sect. VI. Prop. XXX. 




200. Draw the diameter P p such that the time through P V p : time 
through p A P : : n : 1, force oc g-p-^ 
Describe the circle on A V. 

Let t = time through P V p, and T the periodic time 

n _ PVpS _ QVq S circle + A Q q S 
n + 1 ellipse " circle ;i* 


circle S R. 2 C Q 
2 2 


j- a e . sm. u . a 

_ , (u = excentric anomaly) 

= + e . sin. u 

.-. n it n + 1 . {= + e sin. u) 

sn. u 

sin. u = 

n 1 


2 e 

which determines u, &c. 

201. The Moon revolves round the Earth in 30 days, the mean distance 
from the Earth = 240,000 miles. Jupiter s Moon revolves in day, the 
mean distance from Jupiter = 240,000 miles. Compare the absolute Jorces 

of Jupiter and the Earth. 

VOL. I. L 



T oc - , A being the major axis of the ellipse, 

. . If A be given, ^ ^ > 

Mass of Jupiter _ T 2 of the Earth s Moon _ 30j _ 14,400 
* Mass of the Earth ~~ T 7 2 of Jupiter s Moon 1 1 

4 2 

202. A Comet at perihelion is 400 times as near to the Sun as the Earth 
at its mean distance. Compare their velocities at those points. 

Velocity 2 of the Comet F . 4 A S F 4 _ _L 

Velocity 2 of the Earth " F. 2 B S = F 2~." 400 F 200 

400" 2 1 

1 2 200 

= 800 

V V 2 . 20 30 , 
=r nearly. 


203. Compare the Masses of the Sun and Earth, having the mean distance 
of the Earth from the Sun = 400, the distance of the Moon from the Earth, 
and Earth s P d . = 13. the Moon s P d . 

T 2 oc , 

" i" 1 a -T^Z 

Mass of the Sun 400 3 J^ _ 64,000,000 _ 40Q Q0 
* Mass of the Earth = I 3 13 2 " 169 

204. If the force - 2 z , where x is the distance from the center 
of force, it will be centripetal whilst 2 > ~ , or x > a ; there will be 

-\. A 

a jKMTtf o/ 7 contrary flexure in the orbit when - = ^ , or x = a, and 

afterwards when x < a, the force will be repulsive, and the curve change 
its direction. 




205. The body revolving in an ellipse, at 
B the force becomes n times as great. Find 
the new orbit, and under what values ofn it 
will be a parabola, ellipse, or hyperbola. 

S being one focus since the force 

the other focus must lie 


in B H produced both ways, since 
S B, H B, make equal angles with 

the tangent. V 2 = - F.PV = -^F.2ACin the original ellipse, or 

* & 

= - n F . P V in the new orbit. 

2AC = n.PV = n. 

2 SB. h B 
S B"+"h B* 

.-. (S B + h B) A C = 2 n . S B . h B, 
.-. A C 2 + h B . A C = 2 n A C . h B, 

hB -f=r 

If 2 n 1 = 0, or n = $, the orbit is a parabola ; if n > , the orbit 
is an ellipse; if n < , the orbit is an hyperbola. 
Let S C in the original ellipse be given B C, 

.-. S B H = right angle, and S B or A C = B h . cot. B S h 
whence the direction of a a , the new major axis ; also 


a a = S B + B h, and S c = 

VBh 2 SB 2 

If the orbit in the parabola a a be parallel to B h, and L . R = 2 S B, 
since S B h = right angle. 

206. Suppose a Comet in its or 
bit to impel the Earth from a cir 
cular orbit in a direction making 
an acute angle with the Earth s 
distance from the Sun, the velo 
city after impact being to the velo 
city before : : V~B : V~2. Find 
the alteration in the length of the 

Since V 3 : V 2 < ratio than V 2 : 1, .*. the new orbit will be an 




V 2 


2 S P. H P HP 


p y 
2 SP 

A C. 2 S P " A C 

C S P 

A C 

.-. 3AC=4AC 2SP 

.-. 2 S P = A C 

T in ellipse _ 2^ S P? 8 
T r in circle = gp f : ~3 l 

207. A body revolves in an ellipse, at any given point the force becomes 
diminished by ^ th part. Find the new orbit. 

\~ F. P V 

in this case P V -=- , 

P V in ellipse 1 n n 1 
pv in new orbit ~ I n 



in conic section pv n 1 PV 

- _* _ . _ _ of M 

2 in circle e. d. " 2 S P " 2 S P 

n HP 
" n 1" A C 

. H P = AC, the new orbit is a Circle 
= 2 A C, Parabola }> 

n 1 

< 2 A C, 
> 2 A C, 

Hyperbola J 

If - ^- = 2, or n = 2, then when the orbit is a circle or an ellipse, P 

11 J. 

must be between a, B ; when the orbit is a parabola, P must be at B ; 
when the orbit is an hyperbola, Pmust be between B, A. 


208. If the curvature and inclination of tlie tangent to the radius be the 
same at two points in the curve, the forces at those points are inversely as the 
radii z . 

8 a 2 __ 8 a 2 _ 8 a 2 1 

g.SY 2 .PV~g.SY.S P.R~g.sin.0SP 2 .R SP 2 

This applies to the extremities of major axis in an ellipse (or circle) in 
the center offeree in the axis. 

209. Required the angular velocity of %. 
By 46, 6 being the traced-angle, 


W rr -r; - 

d t 
But by Prop. I. or Art. 124, 

d t : T : : d A : A 

d 6 _ 2 A 1 

dl - T~ x ~ 


P x V 


210. Required the Centrifugal Force (<p) in any orbit. 

When the revolving body is at any distance g from the center of force, 
the Centrifugal Force, which arises from its inertia or tendency to persevere 
in the direction of the tangent (most authors erroneously attribute this force 
to the angular motion, see Vince s Flux. p. 283) is clearly the same as it 
would be were the body with the same Centripetal Force revolving in a 
circle whose radius is g. Moreover, since in a circle the body is always 
at the same distance from the center, the Centrifugal Force must always 
be equal to the Centripetal Force. 

But in tlie circle 


g e 3 

P and V belonging to the orbit. 



P 2 V 2 1 

Hence also and by 209, 

And 139, 

F : <* IE If 


P S 3 

211. Required the angular velocity of the perpendicular upon the 

If two consecutive points in the curve be taken ; tangents, perpendiculars 
and the circle of curvature be described as in Art 74, it will readily ap 
pear that the incremental angle (d -^} described by p = that described 
by the radius of curvature. It will also be seen that 

But from similar triangles 

P V : 2 R : : p : g. 
.-. d 6 : d 4> : : P V : 2 g 
P V being the chord of curvature. 

d ^\ d 6 2 



Ex. 1. In the circle P V = 2 ; whence 


~ ^ " 

Ex. 2. In the other Conic Sections, we have 

w X 


; PV 
2P X V 


g X P V 
P X V dp 


p = 


which gives by taking the logarithms 

2 lp = lb 2 + lg l(2a + g) 
and (17 a.) 

2 d p _ dj , d g _ 2 a d g 

P "T~2aqp^~ f (2a + g) 

aP X V 


212. Required the Paracentric Velocity in an orbit. 
It readily appears from the fig. that 

d s : d g : : g : V g 2 p 2 . 
.. If u denote the velocity towards the center, we have 

/ d g\ ds V e p 

u ( = i ! ) = -3~i X - 

\ d t/ d t g 

x e-P (125) 


2 A //I IN ,. 

~T~ X V \p~ 2 ~~ g z ) * 
Also since 

p 2 

= PV 

213. Tojind where in an orbit the Paracentric Velocity is a maximum. 

From the equation to the curve substitute in the expression (212. g) 
for p*, then put d u = 0, and the resulting value off will give the posi 
tion required. 

Thus in the ellipse 

- 2a g 


v- s - = ) = max. 

2 a 1 1 


" b = 


8ad g , 2 d g _ 

"" ~~ 


b s Latus-Rectum 

e = T = - -g- 

or the point required is the extremity of the Latus-Rectum. 


Generally, It neither increases nor decreases when F = p. Hence 
when u = max. (see 210) 

d p _ d g 

? :: 7 

which is also got from putting 

d (u 2 ) = 
in the expression 212. h. 

214. Tojlnd where the angular velocity increases fastest. 

By Art. 209 and 125, 

---- , 

"l - - < JT V J\ - ; 7\ o 1 . - 4 <" 1 f, > 

d t 3 f 2 d 6 f 4 g d 

But from similar triangles 

t / r> 9\ f~\ T 1 ~D T* . - ^1 A . A 

p: V (g 2 p } : y 1 : " l ::gae:ag 

j ,. o pa V 2 
... "I = l-^j X V ( f 2 - p 2 ) = max. 

,.!*-?*= I i^-max (b) 

either of which equations, by aid of that to the curve, will give the point 

Ex. In the ellipse 

_ - = TO ax. = m 

i d m _ . 
and -, = gives 

4 . 


which gives 

P = a + V (49 a 2 48 b 2 ) 
6 6 

for the maxima or minima positions. 
If the equation 

_ b_ 8 1 

a 1 + e cos. d 

and the first form be used, we have 

d e a e . 

T-* = T-T * s sln - 
d d b 2 


sin. 6 
- 3 - = max. = m. 

Whence and from d m = 0, we get finally 

215. To fold where the Linear Velocity increases fastest. 

d v 

-p- = max. 

d t 

But (125) 

P x V 


g 2 d 6 p d g 

: p^v~ P x v ): v s z p l 

d v py V(g 8 p 8 ) d_p_ 
Tt = ~~i~ < p^dl 

V ^ 2 D 2 ^ 

- g F X ". 


, V (?* P 2 ) v d P 

or ? max. = m. 



d m = 
will give the point required. 


Thus in the ellipse 

p 2 1 b 2 

= 4 H j = max. 

which gives 

d m _ _4_ 10 a b 8 g 4 6 b 2 g 5 

d s " g 5 " (2 a g)V 

whence the maxima and minima positions. 

In the case of the parabola, a is indefinitely great and the equation 

4 a 2 1 4 a b 2 = 


5 b 2 5 

f = o x T^ * Latus- Rectum. 
o a ID 

Many other problems respecting velocities, &c. might be here added. 
But instead of dwelling longer upon such matters, which are rather 
curious than useful, and at best only calculated to exercise the student, 
I shall refer him to my Solutions of the Cambridge Problems, where -he 
will find a great number of them as well as of problems of great and 
essential importance. 


216. PROP. XVIII. If the two points P, p, be given, then circles whose 
centers are P, p, and radii AB+SP, AB+Sp, might be described 
intersecting in H. 

If the positions of two tangents T R, t r be given, then perpendiculars 
S T, S t must be let fall and doubled, and from V and v with radii each 
= A B, circles must be described intersecting in H. 

Having thus in either of the three cases determined the other focus H, 
the ellipse may be described mechanically, by taking a thread = A B in 
length, fixing its ends in S and H, and running the pen all round so as to 
stretch the string. 


This proposition may thus be demonstrated analytically. 

1st. Let the focus S, the tangent T R, and the point P be given in 
position ; and the axis-major be given in length, viz. 2 a. Then the per 
pendicular S T ( = p), and the radius- vector S P ( = f) are known. 

But the equation to Conic Sections is 

whence b is found. 

Also the distance (2 c) between the foci is got by making p = g, thence 
finding and therefore c = a Ijl . 

This gives the other focus ; and the two foci being known, and the axis- 
major, the curve is easily constructed. 

217. 2d. Let two tangents T R, t r, and the focus S be given in position. 

Then making S the origin of coordinates, the equations to the trajectory 


b 2 g b 2 1 

P " 3 : 

a being the inclination of the axis-major to that of the abscissae. 

Now calling the angles which the tangents make with the axis of the ab 
scissae T and T , by 31 we have 

tan * T = dV 

x = cos. 6, y = g sin. 6 

tan. T = d g sm - 6 + g d 6 cos. 6 
d cos. d 6 sin. 6 

-Vl tan. 6 + I 

= ^ - (b) 

g d 6 
Also from equations (a) we easily get 



V 2 

COS. (d a) = g (2) 

ae g 

sin. (d a) = ^X V (2ag g b) . . (3) 

_ Sap* 


and putting 

R = V (2ae e b 2 ) ... (5) 
we have 

R , tan. 6 tan. a 

{- = tan. (6 a) = . (6) 

b 2 ag 1 + tan. . tan. 6 

which gives tan. 6 in terms of a, b, , and tan. a. 

Hence by successive substitutions by means of these several expres 
sions tan. T may be found in terms of a, b, p, tan. a, all of which are given 
except b and tan. . Let, therefore, 

tan. T = f (a, p, b, tan. a). 
In like manner we also get 

tan. T = f (a, p , b, tan. a) 
p belonging to the tangent whose inclination to the axis is T. 

From these two equations b and tan. a may be found, which give 
c = V a 2 b 2 and a, or the distance between the foci and the position 
of the axis-major; which being known the Trajectory is easily con 

218. 3d. Let the focus and two points in the curve be given in posi 
tion, &c. 

Then the corresponding radii g, f , and traced angles 6, tf, in the 

+ a (1 e 2 ) 

1 + e cos. (6 a) 


1 + e cos. (& a) 
are given ; and by the formula 

cos. (d a) = cos. 6 . cos. a -f- sin. & sin. a 

2 a e and a or the distance between the foci and the position of the axis- 
major may hence be found. 

This is much less concise than Newton s geometrical method. But it 
may still be useful to students to know both of them. 

219. PROP. XIX. To make this clearer we will state the three cases 

Case 1. Let a point P and tangent T R be given. 

Then the figure in the text being taken, we double the perpendicular 
S T, describe the circle F G, and draw F I touching the circle in F and 
passing through V. But this last step. is thus effected. Join V P, sup 
pose it to cut the circle in M (not shown in the fig.), and take 
V F 2 = V M x (V P + P M). 

The rest is easy. 




Case- 2. Let two tangents be given. Then V and v being determined 
the locus of them is the directrix. Whence the rest is plain. 

Case 3. Let two points (P, p) be given. Describe from P and p the 
circles F G, f g intersecting in the focus S. Then draw F f a common 
tangent to them, &c. 

But this is done by describing from P with a radius = S P S p, a 
circle F G , by drawing from p the tangent p F as in the other case (or 
by describing a semicircle upon P p, so as to intersect F G in F ) by 
producing P F to F, and drawing F f parallel to F p. 

See my Solutions of the Cambridge Problems, vol. I. Geometry, where 
tangencies are fully treated. 


These three cases may easily be deduced analytically from the general 
solution above ; or in the same way may more simply be done at once, 
from the equations 

L L 1 

P 2 = T ft S = -Z X 

2 1 + cos. (6 a) 

220. PROP. XX. Case 1. Given in species] means the same as " simi 
lar" in the 5th LEMMA. 

Since the Trajectory is given in species, &c.] From p. 36 it seems that 
the ratio of the axes 2 a, 2 b is given in similar ellipses, and thence the 
same is easily shown of hyperbolas. Hence, since 
c 2 = a 

2 c being the distance between the foci, if = m, a given quantity, we 



V a 

which is also given. 

With the centers B, C, &c.] 

The common tangent L K is drawn as in 219. 

Cases 2. 3. See Jesuits Notes. 


221. Case 1. Let the two points B, C and the focus S be given. 

+ a (1 e 2 ) 
1 + e cos. (6 a) 
- a(l e 2 ) f 
S I + e cos. (d f a)) 

a being the inclination of the axis of abscissas to the axis major. 
But since the trajectory is given in species 

e = is known, 

and in equations (1), g, 6; g , tf, are given. 
Hence, therefore, by the form 

cos. (6 a) = cos. 6 . cos. a + sin. 6 sin. a, 
a and , or the semi- axis-major and its position are found; 

also c = a e is known ; 
which gives the construction. 


Case 2. By proceeding as in 220, in which expressions (e) will be 
known, both a, a e, and a may be found. 
Case 3. In this case 

will give a. Hence c a e is known and 

+ a(l e 2 ) 
S ~ I + e cos. (0 a) 
gives a. 

Case 4. Since the trajectory to be described must be similar to a given 
one whose a and c are given, 

c c 

G = a = 17 
is known (217). 

Also g and 6 belonging to the given point are known. 
Hence we have 

1 + e cos. (d a) 

And by means of the condition of touching the given line, another 
equation involving a, a may be found (see 217) which with the former 
will give a and a. 


Given three points in the Trajectory and the focus to construct it. 


Let the coordinates to the three points be g, 6 ; g, Of ; g", 6", and a the 
angle between the major axis and that of the abscissae. Then 

+ a.(l-e 2 ) "I 
1 + e cos. (d a) 

4- a H P 2 ^ 

/ ~ H J. I , i x 

~ 1 + e cos. (<f a) 
/= + a (l e 2 ) 

1 + e cos. (d" ) ^ 

and eliminating + a (1 e 2 ) we get 

g g = e . cos. (& a) e cos. (6 a) 
g = e . cos. (d" a) e cos. (6 ) J 


from which eliminating e, there results 

__ g-g __ g-g" 

__ _ _ 

g . COS. (^ a) g COS. (0 a) g" COS. (0" a) COS. (<J a) 

Hence by the formula 

cos. (P Q) = cos. P . cos. Q + sin. P . sin. Q 

g-fV cos. J" (g - g") g cos. f + s (f - g Qcos.d 


(S gO f" sin. <?" (g e" ) /sin. + ^ f <")sinJ 
which gives a. 

Hence by means of equations (B) e will be known ; and then by substi 
tution in eq. (A), a is known. 


The preliminary LEMMAS of this section are rendered sufficiently intel 
ligible by the Commentary of the Jesuits P.P. Le Seur, &c. 

Moreover we shall be brief in our comments upon it (as we have been 
upon the former section) for the reason that at Cambridge, the focus of 
mathematical learning, the students scarcely even touch upon these sub 
jects, but pass at once from the third to the sixth section. 

223. PROP. XXII. 

This proposition may be analytically resolved as follows : 
The general equation to a conic section is that of two dimensions (see 
Wood s Alg. Part IV.) viz. 

y 2 + Axy+Bx 2 + Cy + Dx + E = 

in which if A, B, C, D, E were given the curve could be constructed. 
Now since five points are given by the question, let their coordinates be 
a, j3 ; a, j3 ; a, j3 ; a, (3 ; a, /3 . 

11 22 33 44 

These being substituted for x, y, in the above equation will give us five 
simple equations, involving the five unknown quantities A, B, C, D, E, 
which may therefore be easily determined: and then the trajectory is 
easily constructed by the ordinary rules (see Wood s Alg. Lacroix s Diff. 
Cal. &c.) 

224. PROP. XXIII. The analytical determination of the trajectory 
from these conditions is also easy. 


a, /3 ; a, ; a, ; a, /3 

11 22 33 


be the coordinates of the given point. Also let the tangent given in posi 
tion be determinable from the equation 

y = m x + n ......... (a) 

in which m, n are given. 

Then first substituting the above given values of the coordinates in 

y 2 + Axy + Bx 2 + Cy+Dx+ E = . . . (b) 
we get four simple equations involving the five unknown quantities 
A, B, C, D, E ; and secondly since the inclination of the curve to the axis 
of abscissas is the same at the point of contact as that of the tangent, 
d y _ d y 
cfx dx 

y = y 

x = x 

. Ay+ 2Bx + D 
2y+ Ax + C 

and substituting in this and the general equation for y its value 

y = m x + n 
we have 

A(mx + n)+2Bx + 

2(mx + n) + Ax+C 

from the former of which 

, _ n A + m C + D 

2(m 2 
and from the latter 

2(m 2 +nA+B) 

and equating these and reducing the result we get 

4,m 2 n 2 = (nA + mC + D+ 2 m n) 2 (n 2 + n C + E) (m 2 +m A+B) 

and this again reduces to 

+ 2mCD nBCmAE BE+ 3mn 2 A 
+ 3nm 2 C + 4mnD n B m 2 E n a m 2 = 
which is a fifth equation involving A, B, C, D, E. 

From these five equations let the five unknown quantities be determined, 
and then construct eq. (b) by the customary methods. 



225. PROP. XXIV. 



,<3; a , /3 ; a", 0" 
be the coordinates of the three given points, and 

y = m x + n 

y"= m x" + n 

the equations to the two tangents. Then substituting in the general 
equation for Conic Sections these pairs of values of x, y, we get three 
simple equations involving the unknown coefficients A, B, C, D, E ; and 
from the conditions of contact, viz. 

dy _ dy _ 

dx ~~ dx 

x = x 

We also have two other equations (see 224) involving the same five un 
knowns, whence by the usual methods they may be found, and then the 
trajectory constructed. 

226. PROP. XXV. 

Proceeding as in the last two articles, we shall get two simple equations 
and three quadratics involving A, B, C, D, E, from whence to find them 
and construct the trajectory. 

227. PROP. XXVI. 

In this case we shall have one simple equation and four quadratics to 
find A, B, C, D, E, with, and wherewith to describe the orbit. 

228. PROP. XXVII. 

In the last case of the five tangents we shall have five quadratics, 
wherewith to determine the coefficients of the general equation, and to 


229. PROP. XXX. 


After a body has moved t" from the vertex of the parabola, let it be re 
quired to find its position. 

If A be the area described in that time by the radius vector, and P, V 
the perpendicular or the tangent and velocity at any point, by 124 and 
125 we have 

c P V 

A = ~2 * * = -3- X t 

and by 157, 

L being the latus-rectum. 

* A = 1 vV x L 



= ixy_ Mx __ r)y 
where r = A S, &c. (see 21) and 

y 2 = 4rx 

. .y 3 + 12r z y = 12 rt V g^r 
by the resolution of which y may be found and therefore the position of P. 

230. By 46 and 125, 

V " C 


i ?d o 

U S = r-2 

M 9 



which is an expression of general use in determining the time in terms of 
the radius vector, &c. 
In the parabola 

P 2 = re, 

c V(g r) 
and integrating by parts 

2 V r . . 2 V r ,, .. . 
t = -rj* S V (S ~ r) fd g^ (g 

2 V r 


c= PV= VlT^r (229) 

which gives 

whence we have g and the point required. 

liy the last Article the value of M in Newton s Assumption is easily 
obtained, and is 

1VA ~~ ___ ~* /\ / _ * 

4 r 4 -V 2r 

231. COR. 1. This readily appears upon drawing S Q the semi-latus- 
rectura and by drawing through its point of bisection a perpendicular to 

232. COR. 2. This proportion can easily be obtained as in the note of 
the Jesuits, by taking the ratio of the increments of G H and of the curve 
at the vertex ; or the absolute value of the velocity of H is directly got 

d.GH3dM * / 

dt dt 4^ 2r 

Also the velocity in the curve is given by (see 140) 


and at the vertex = r, 

.-. v : v : : 3 : 8. 

233. COR. 3. Either A P, or S P being bisected, &c. will determine 
the point H and therefore 

4 2 r 

X GH. 

234. LEMMA XXVIII. That an oval cannot be squared is differently 
demonstrated by several authors. See Vince s Fluxions, p. 356; also 

235. PROP. XXXI. This is rendered somewhat easier by the follow 
ing arrangement of the proportions : 

If G is taken so that 




GK: 2*OG:: t: T 


n v 2^x OA 2 t 

Then, &c. &c. For 


= ~ X(OQA OQS) 

= 27 (OQx AQ OQx SR) 

= ^-(AQ SR). 

S R : sin. A Q : : S O : O A 
: : O A : O G : : A Q : F G 
S R A Q sin. A Q 




= |x(FG-sin.AQ) 

(FG _ sin<AQ) 

(see the Jesuits note q.) which is identical with (a), since 

_1 A S _^ 

T ~~ Ellipse 

_ ASP 

v ab 


236. By 230 we have 

But in the ellipse 


r\ t 

. . U I - . . , j j% 

and putting 

g a zz u 
it becomes 

. b . (a + u) d u 

2 a e being the excentricity. 


b a p du _b / udu 

T^ V(a 2 e 2 u 2 ) + ~IJ V(a 8 e 8 u 

L? s in.- .- U - V(a 2 e 2 u 2 ) + C. 
c a e c 

Let t zz 0, when u zz a e ; then 
and we get 

_ba * 
~ V X 2 


which is the known form of the equation to the Trochoid, t being the ab 
scissa, &e. 

Hence by approximation or by construction u and therefore may be 
found, which will give the place of the body in the trajectory. 

It need hardly be observed that (157) 


237. dt = 

but in the ellipse 

b 2 1 

= x 

a 1 -j- e cos. 6 

.-. d t = -- x 

a 2 c ( 1 + e cos. 6} 2 
and (see Hirsch s Tables, or art. 110) 

a 2 (l e 2 ) f 1 . e + cos. 6 e sin. d 

t = x < cos. ~ . 

c I M* e ) l+ecos.0 1 + ecos. 

which also indicates the Trochoid. 
To simplify this expression let 
. e 4- cos. d 


1 + e cos. i 

1 ~ 


e + cos. d 

*^~ /*OC 11 

1 + e cos. 6 

CUp* II 


rr\<i A 

e < 

e cos. u 1 

A/ { 1 2\ 

sin. 6 = 

1 e cos. u 

e sin, d e sin. u 

1 + ecos. d ~ V (1 e 2 ) 

a 2 V (I e 2 ) 
.. t = * X ^u esm. u} 

But (157) 



a 2 
.*. t = ==- x (u e sin. u) 

V cr/jb 

a* 1 

Let = _ . 

V g(* n 

nt=.u esin. u (1) 

Again, 6 may be better expressed in terms of u, thus 

2 _0 1 cos. 6 _ 1+e 1 cos. u _ 1 + e 2 u 

2 ~ 1 + cos. 6 ~ T^Ti X 1 + cos. u ~ T^> tan> "2~ 


Moreover g is expressible in terms of u, for 

g= I a i 1 ~ e2) , = a(l ecos.u) ..... (3) 
1 + e cos. 6 

In these three equations, n t is called the Mean Anomaly ,- u the 
Excentric Anomaly, (because it = the angle at the center of the ellipse 
subtended by the orduiate of the circle described upon the axis-major 
corresponding to that of the ellipse) ; and 6 the True Anomaly. 


Newton says that " the approximation is founded on the Theorem that 
The area APSocAQ SF, SF being the perpendicular let fall from 
S upon O Q."] 

First we have 


S P R = S Q R x 


.-.ASP = ASQx 





= i AO x (AQ SF). 

.-. A S P = ~ x (A Q S F) 

= X (a u a e sin. u ) ..... (1) 


u being the L A O Q. 


(Hence is suggested this easy determination of eq. 1. 237. 4 . 

For 5 (a - > 

t = T x A Sp 2 * flg v- 2 

Ellipse V ^ g 
= X (u e sin. u). ) 

V i 

* - 

Again, supposing u an approximate value of u, let 

u = u H 


Then, by the Theorem, we have 

2 A b Sp = A q S O X sin. A q 

= AQ + Qq + SOx sin. (A Q + Q q) 
to radius 1. 

But A Q being an approximate value of A q, Q q is small compared 
with A O, and we have 

sin. ( A Q + Q q) = sin. A Q cos. Q q + cos. A Q sin. Q q 
= sin. A Q + Q q cos. A Q nearly. 


.*. Q q = ( ^ ? A Q + SO sin. A Q) x -= nearly 

^=r + cos. A Q 

which points out the use of these assumptions 

XT/ 2 A Sp 2 t , , 

N = 1 ^ = r-?f, X area of the Ellipse 


D = S O. sin. A Q = B sin. A Q 

I/ a -I 

- so 


Q q = (N A Q + D ) X , , _ 

, , _ . 
\J + cos. A Q 

in which it is easily seen B , N x , D , I/ 
are identical with B, N, D, L. 


E = Qq= (N-AQ + D) T _ L _. 

L + cos. A Q 




Having augmented or diminished the assumed arc A Q by E, then re 
peat the process, and thus find successively 
G, I, &c. 

For a developement of the other mode of approximation in this 
Scholium, see the Jesuits note 386. Also see Woodhouse s Plane Astro 
nomy for other methods. 


1 A 

239. PROP. XXXII. F -^ 2 Determine the spaces which a 


body descending from A in a straight line towards the center of 
force describes in a given time. P 

If the body did not fall in a straight line to the center, it would 
describe some conic section round the center of force, as focus 

C ellipse ~\ 

(which would be < parabola > if the velocity at any point were to S 
(_ hyperbola j 

the velocity in the circle, the same distance and force, in R.-J = V 

V 2 : 1.) 

(I) Let the Conic Section be an Ellipse A R P B. 

Describe a circle on Major Axis A B, draw 
C P D through the place of the body perpendi 
cular to A B. 

The time of describing A P a area A S P a 
area A S D, whatever may be the excentricity 
of the ellipse. 

Let the Axis Minor of the ellipse be diminish 
ed sine limite and the ellipse becomes a straight 
line ultimately, A B being constant, and since 
A S . S B = (Minor Axis) 2 = 0, and A S finite 
/.SB = 0, or B ultimately comes to S, and 

time d . A C a area A D B. .. if A D B be taken proportional to time, 
C is found by the ordinate D C. 

(T . A C a area ADBaADO + ODBaarcAD + CD 

/. take 6 + sin. & proportional to time, and D and C are determined.) 



the time down A O 
T.O B 





N. B. The time in this case is the time 
from the beginning of the fall, or the time 
from A. 

(II) Let the conic section be the hyperbola 
B F P. Describe a rectangular hyperbola on 
Major Axis A B. 

T a area S B F P or area SEED. 

Let the Minor Axis be diminished sine 
limite, and the hyperbola becomes a straight 
line, and T or area B D E. 

N. The time in this case is the time from 
the end of motion or time to S. 

Let the conic section be the parabola B F P. 
Describe any fixed parabola BED. 

T or area S B F P a area SEED. 

Let L . R. of B F P be diminished sine 
limite the parabola becomes a straight line, 
and T a area B D E. 

N. The time in this case is the time from 
the end of motion, or time to S. 

Objection to Newton s method. If a 
straight line be considered as an evanescent 
conic section, when the body comes to peri 
helion i. e. to the center it ought to return to aphelion i. e. to the original 
point, whereas it will go through the center to the distance below the 
center r= the original point. 

240. We shall find by Prop. XXXIX, that the distance from a center from 
which the body must fall, acted on by a blc force, to acquire the velocity such 
as to make it describe an ellipse = A B (finite distance), for the hyperbola 
= A B, for the parabola = a . 

241. Case 1. v d v = g ^ d x, f = force distance 1, 

x 2 

v = 

if a be the original point 

a ~ x \ 

dx Va 

Ut = -- = 
v V 2 

dx . 

V ax x 



r(|_x)dx -fdx | 

Vax x 

. . t = / -^ .. / 
V 2g/z \ 

/ a 

^ . / rt 

Va. x x ! 

+ C, when t = 0, x = a, 
V ax x 2 + /circumference 
V 2~ 


rs. ~ l x ~) 

1 1 

vers. ~ x, 
rad. = - 

^ (C D + A D) 

if the circle be described on B A = a, 

/"~a~ 4 /CD.OB AD.ODx 
"~ -S 2fir/ct aA 2 2 ~/ 


Case 2. v 2 = 2 g ^ . 

a x 

, if a be an original point, 


tf/V V 


x + 


for t in this case is the time to the center, not the time from the original 

, . d x d x 

.*. d t = , or d t = . 

v v 

Now if with the Major Axis A B = a, we describe the rectangular 


we have 





d.BED=d.BEDC d.ABDC=ydx 


Vax + x 

a x d x 

i / 

.*. t from B = / .BED, for they begin or end together at 15. 




Case 3. v 2 = 2 g p , if a be a , 

, . dx Vxdx 

.*. a t = = _ 

v V 2 2 u 

. . . T, 

, t being time to B, 

+ C, when t = 0, x = 0, .-. C = 0. 

V" 2 g /A 3 

Describe a parabola on the line of fall, vertex B, L . R. = any fixed 
distance a, 


. -v/ x . x = 

2 V 2 

- 2 V 2 T> ^ T. 

a x . x = ===== .BED. 

2 V 2 
Hence in general, in Newton Prop. XXXII, t = _. . curvili- 

V a g ft 
near area, a being L . R. of the figure described. 

T a, T -D 2 (Ax. Min.) 2 . f A 

In the evanescent conic sections, L . R. = \ -^ , . . if Ax, 

Min. be indefinitely small, L. R. will be indefinitely small with respect to the 
Ax. Min. The chord of curvature at the finite distance from A to B is ulti 

mately finite, for P V = LL*_^L?j but at A or B, P V = L, = in- 

finitesimal of the second order. Hence S B is also ultimately of the second 

order, for at B, S B = L. -4^ 

2 AS 

PROP. XXXIII. Force a 
Vat C 


(distance) * 


-r = i JT-T ?T7s = in the ellipse and hyperbola. 

v in the circle distance S C V SA 




~Ajr "" ~T^T whentheconiGsectlonbecomesa straight line 1 ) 

2 V 2 


V 2 SY 2 L SP 

v 2 ~" 2SP " 2 S Y 2 

A C.CB AO 2 2 AO 2AO 

C P 2 /Min. AX.N 8 - 2/Min.Ax.x * ~ L 
V 2 / V 2 / 


. L _ AO.CP 
2 : A C.C B 

* v 2 = ATCTC~BTS Y 2 

B O "" TO 

C O __ C B comp. in the ellipse 
B O ~~ B T div. in the hyperbola, 
. A C _ C_T div. in the ellipse C P 

B O " B T comp. in the hyperbola ~~ BQ 
A C 2 _ C P 2 
* AO 2 ~ BQ 1 
. BQ 2 .A C _ AQ.CP 2 

V 2 _ BQ 2 . A C.S P 
*v 2 ~AO.BC.SY 2 
but ultimately 

B/~k__C!\7 Q"D T> C* 
v^ o l,Oirr o *~/f 

, . A , V 2 in a straight line A C 

.-. ultimately ^-. r 5-^ = -T-TS;* 

v 2 in the circle A O 


Y - / 
v ~ V 

COR, 1. It appeared in the proof that 


A O 




.-. ultimately -^-^ = ^-^ . 

(This will be used to prove next Prop.) 
COR. 2. Let C come to O, then A C = A O and V = v, 
.. the velocity in the circle = the velocity acquired by falling externally 

through distance = rad. towards the center of the force a 

ILL 11 Ul3lt.ll.ld ~- 1 till* i,\J W til Ho Lilt/ V.,^11 lv>i W* H.1W J-WJ. WV> A- o 

distance z 
242. I Vwrf actual Velocity at C. 

V 2 atC = AC 

v 2 in the circle distance B C B A* 

. vz _. ^ " ^ T7 2 _ 2A C g /* R p 

"FA" 1 "BT Fc 5 

if At- = the force at distance 1, 

. V2 AC 

~ g ^B A.B C 

V a x 

.-. V = V 2 g y, . r " , if B A = a, B C = x. 
V a x 

Tr . 1,. V space described 

If a is given, V a r 

V space to be described 

In descents from different points, 

, T V space described 

V a * -. 

V space to be described X initial height ; 

In descents from different points to different centers, 

V space described X absolute force 
V or . 

V space to be described X initial height 

243. Otherwise. vdv = ^dx, 

ft T X 

.\v 2 = 2 g (A. ^-^- > wn en a is positive, as in the ellipse 

o ^L Y 

= 2 g ^ . when a is negative as in the hyperbola 

= 2 g fi . , when a is a , as in parabola 

(when x = 0, v is infinite) 
V 2 in the circle radius x (in the ellipse and hyperbola) 

v 2 2 a x . , a 

. . y-j = in the ellipse, = 




v 2 2 a + x . , , a + x 

^^ = in the hyperbola, = 

V a (|) 

f /* X 

- z . = 


2 ff fJ> 

V 2 in the circle radius = (in the parabola) = 


V 2 1 

.*. ^2 = in the parabola. 

244. In the hyperbola not evanescent 
Velocity at the infinite distance _ S A 
velocity at A " S Y 

finite R., but when the hyperbola van 
ishes, S Y ultimately = Min. Ax. for 

S Y S C 

-r-r- = -r-p 5 and ultimately S C = 

A C, and b C = A C, .-. ultimately S Y = A b = C B, .-. ultimately 
S Y _ infinitesimal of the first order 
S A " of the 2d order 

velocity at A 
velocity at cc distance 


245. PROP. XXXIV. 

Velocity at C - _L f 

velocity in the circle, distance S C ~~ T ( 


S P 


the parabola. 

For the velocity in the parabola at P = velocity in the circle 

ever be L . R . of the parabola. 

246. PROP. XXXV. Force oc rr -^ . 

(distance) 2 

The same things being assumed, the area swept out by the indefinite 

T T? 
radius S D in fig. D E S = area of a circular sector (rad. = 

of fig.) uniformly described about the center S in the same time. 
Whilst the falling body describes C c indefinitely small, let K k be the 
arc described by the body uniformly revolving in the circle. 

Case ] . If D E S be an ellipse or rectangular hyperbola, - = -^ , 





S Y 


T S 



D~~A c~v ~ Tf*~S ~r~r\ ultimately. 
ti.oY IS AO J 

(Cor. Prop. XXXIII.) 


velocity at C VAC 

v in the circle rad. S C "" v^L^ 
v in the circle rad. S C S K / A~O 

v in the circle rad. S K ~~ ** S C = +*> ~S~C 


velocity at C x __ Cc _ A^C _ A C 
in the circle rad. S K/ ~" K k ~ V ~S~C ~ (Tl) 
.-. Cc.CD = Kk.AC 
. Kk. A C _ A C 
D d . S Y r A~O 
.-. A O. Kk = Dd. S Y, 
. . the area S K k = the area S D d, 
.-. the nascent areas traced out by S D and S K are equal 
.*. the sums of these areas are equal. 

Case 2. If D E S be a parabola S K = L ; R . 


As above 

Cc. CD _ CT 2- 
D d . S Y ~ T~S = T 

also ^ p 

Cc = _ velocity at C _ ^locity in the circle -^ 

Kk "" velocity in the circle L . R ~~ velocity in the circle L . R 
_ 2 2" 

_ VS K SK 


v~$Tc CD 

2 2 


.-. K k . S K = D d . S Y. 

247. PROP. XXXVI. Force a _ L_ 


To determine the times of descent of a body falling from the given (and 
. .finite] altitude A S 

On A S describe a circle and an equal circle round the center S. 

From any point of descent C erect the ordinate C D, join S D. Make 
the sector O S K = the area A D S (O K = A D + D C) the body 
will fall from A to C in the time of describing O K about the center S 

Vet. J. N 


uniformly, the force oc _ -. Also S K being given, the period 

in the circle may be found, (P =^/ . r . S K *), and the time through 


O K = P . - ? . the time through O K is known. .-. the time 


through A C is known. 

248. Find the time in which a Planet would fall from any point in its 
orbit to the Sun. 


circle S P 

Time of fall = time of describing ^ O K H, S O = g- , 


period in the circle O K H _ period in the circle rad. S O _ S O g 
period in the ellipse " period in the circle rad. AC A C ^ 

.-. the time of fall = i . P . 
be considered a circle 

, P = period of the planet. If the orbit 


and the time of fall 

4 V 2 



= P. nearly. 

= nearly. 




249. The time down A C a (arc 
= A D + C D), a C L, if the cy 
cloid be described on A S. Hence, 
having given the place of a body at a 
given time, we can determine the 
place at another given time. 

time d. A C 

Draw the ordinate m 1 ; 1 c will deter 
mine c the place of the body. 

250. PROP. XXXVII. To determine the times of ascent and descent of a 

body projected upwards or downwards from a given point, F a . 


Let the body move off from the point G with a given velocity. Let 

V 2 at G m 2 

=-= TV i i = -7-, (V and v known, . . m known), 
v 2 m the circle e. d. 1 v 

To determine the point A, take 

G A 


G A 

m z 

G A + G S 
G A 


m ~ 

" G S 

2 m 2 

.. if m 2 = 2, G A is + and 00 , /. the parabola -\ must be des- 

if m 2 < 2, G A is + and fin. .. the circle Vended on the 

if m s > 2, G A is andfin. .-. the rectangular hyperbola-/ axis S A. 

With the center S and rad. = - - of the conic section, describe the 


circle k K H, and erecting the ordinates G I, C D, c d, from any places 
of the body, the body will describe G C, G c, in times of describing the 
areas S K k, S K k , which are respectively = S I D, S I d. 

251. PROP. XXXVIII. Force ex distance. 

Let a body fall from A to any point C, 
by a force tending to S, and a g . as the 
distance. Time a arc A D, and V acquir 
ed a C D. Conceive a body to fall in an 
evanescent ellipse about S as the center. 
.*. the time down A P or A C 



a A D for the same descent, i. e. when 

A is given. 

NT 2 




The velocity at any point P 
oc V F. P V 

S P. 

a CD. 

COR. 1. T. from A to S = period in an evanescent ellipse. 

= % period in the circle A D E. 
= T. through A E. 

COR. 2. T. from different altitudes to 
S a time of describing different quadrants 
about S as the center oc 1. 

N. In the common cycloid A C S it is 
proved in Mechanics that ifSca=SCA 
and the circle be described on 2 . Sea, 
and if a c = A C, the space fallen through, 
then the time through A C a arc a d, 
and V acquired a c d, which is analogous 
to Newton s Prop. 

Newton s Prop, might be proved in the 
same way that the properties of the cycloid 
are proved. 


252. vdv = g/AX.dx, 

..v 2 = 2 g A* (a 2 x 2 ), if a = the height fallen from 
.. v = V 2o-/i . V a 2 x 2 = -v/2gAt . C D. 
d x d x 1 

v V Spy* V a 2 x 2 

.-. t = + 


COS. = 

. = *N 

.. = a/ 


a V2g/j, 

.: velocity oc sine of the arc whose versed sine = space, and the arc 
a time, (rad. = original distance.) 
253. The velocity is velocity from ajinite altitude. 
If the velocity had been that from infinity, it would have been infinite 


cl x x 

and constant. .. d t = , and t = ., ._ -j- C, when t = 0, 

v . a. V g p. 

a, a = a . 

x = a, .*. c is finite, . . t = C = 

v g (i 

Similarly if the velocity had been > velocity from infinity, it would 
have been infinite. 

254. PROP. XXXIX. Force a (distance}*, or any function of distance. 

Assuming any oc n . of the centripetal force, and also that quadratures of 
all curves can be determined (i. e. that all fluents can be taken) ; Re 
quired the velocity of a body, when ascending or descending perpendicu 
larly, at different points, and the time in which a body will arrive at any 

(The proof of the Prop, is inverse. Newton assumes the area A B F D 
to oc V 2 and A D to oc space described, whence he shows that the force 
D F the ordinate. Conversely, he concludes, if F oc D F, A B F D 
a V 2 .) 

v 2 a/v d v oc/F. ds. 

Let D E be a small given increment of space, and I a corresponding 
increment of velocity. By hypothesis 

A BFD V_ 2 _ V 2 

AB G E " v 2 =: V 2 + 2V.I+ I 2 

ABFD V 2 V 2 

* TPP~P~F = 9~V 1~ t" 2 = 9~V T u " iniate y- 


ABFDocV 2 .-. D F G E 2 V . I 

.-. D E . D F ultimately, a 2 . V . I 

2V. I I.V 
.". JJ r a ex ^ . 

But in motions where the forces are constant if I be the velocity gene 
rated in T, F oc _ , f F oc -= \ and if S be the space described with uni 
form velocity V in T, ~- = -^ , (d t = ) . Also when the force is 
fe JL v / 

I V 

a ble , the same holds for nascent spaces. .-. F , and D E re- 


presents S. . . D F represents F. 

N 3 




Let D L a ,- = , .-. D L M E ultimately = D L . D E 

V A B F D v 

D F 

-=^- <x time through D E ultimately. 

.. Increment of the area A T V M E increment of the time down A D. 
.-. A T V M E oc T. 


/d s 

(Since A B F D vanishes at A, .-. A T is an asymptote to the time 
curve. And since E M becomes indefinitely small when A B F D is in 
finite, .. A E is also an asymptote.) 

255. COR. 1. Let a body fall from P, and be acted on by a constant 
force given. If the velocity at D = the velocity of a body falling by the 
action of a ble force, then A, the point of fall, will be found by making 



= ~ by Prop. 

D R S E " D R ~ i 

if i be the increment of the velocity generated through D E by a constant 







256. COR. 2. If a body be projected up or down in a straight line 
from the center of force with a given velocity, and the law of force given ; 
Find the velocity at any other point E . Take E g / for the force at E r . 


velocity at E = velocity at D. - -^^^^~ + if pr " 

jected down, if projected up. 

y P Q R U D F g E V A Bg j/x 
( V P QRD" " V A B F D 

257. COR. 3. Find the time through D E . _ _ 
Take E m inversely proportional to V P Q R D + D F g E (or 

to the velocity at E ). 

T.PD _ V"P D _ _VTD__ = _ Vir P* ( D E small) 

T77E~ VTHE~ V(PD+DE) . 

2V PD 

T.PD _ 2 PD _ 2 P D . D L 


T.D Eby ble force _ DJL^M E 

T.DE by do7~ = D L m E /J 
but T . D E by a constant force = T . D E by a ble force since the velo- 

/ d s\ 

cities at D are equal ( d t = 1 

T. PD _ 2 PD. D L 
T.DE X " D L m E x 

d v 
258. It is taken for granted in Prop. XXXIX, that F a ^ (46), 

and that v = ^ , whence it follows that ifc.F = ^,dv = c.F.dt, 
d t 

and vdv = cF.ds. 

.-. v 2 = 2c/Fds 

Newton represents/ F d s by the area A B F D, whose ordinate D I 
always = F. 

d ds 


v " V2c./Fds ; 
d s 




Newton represents / . - by the area A B T U M E, whose or- 
J V f d s 

dinate D L always = - 

. A BTF D 


In COR. 1. If F be a constant force V 2 = 2 g F . P D, by Mechanics 

V 2 = 2c./Fds 

And F 7 . P D or P Q R D is proved =/F d s or A B F D, 
.-. c = g 


v* = 2g./Fds. 

In COR 2 velocit y at E/ _ V/Fd s when s = A E 7 
velocity at D "" VfF d s when s = A D 

V A B g E 

In COR. 3. t = time through D E X =/A? -f __ 

v V 2 gy F d s 

T = time through P D = = 


= 2 P D. D L 
P D . D L 

t D L m E 
259. The force a x n . 

.. v d v = g ^ x n d x, fjt, the force distance 1. 

if a be the original height. 

Let n be positive. 

V from a finite distance to the center is finite 1 
V from x to a finite distance is infinite. / 

Let n be negative but less than 1. 

V from a finite distance to the center is finite 1 
V from co to a finite distance is infinite. J 

Let n = 1 the above Integral fails, because x disappears, which 
cannot be. 



v d v = g p - 

.-. V from a finite distance to the center is infinite 1 
V from x to a finite distance is infinite. f 

1 x 

But the log. of an infinite quantity is x ly less than the quantity itself -- when 


x is infinite = -- . Diff, and it becomes * = = . 
x x 


Let n be negative and greater than 1. 

V from a finite distance to the center is infinite ") 
V from oo to a finite distance is finite. / 

260. If the force be constant, the velocity-curve is a straight line parallel 
to the line of fall, as Q R in Prop. XXXIX. 


261. To find under what laws of force the velocity from x to a finite 
distance will be infinite or finite, and from a finite distance to the center 
will be finite or infinite. 

If (1) F a x 2 , V a V~^ 3 ~~^ 


, v 

. */ n 2 TT 2 




/ a 



~ V x 


Va x 

X 2 




/a 2 x 2 

X 3 

V a z x 2 


n 1 x n 



x n 

V o n 1 v n I 

^ cli A 

In the former cases, or in all cases where F cc some direct power of 
distance, the velocity acquired in falling from co to a finite distance or to 
the center will be infinite, and from a finite distance to the center will be 




In the 4th case, the velocity from oo to a finite, and from a finite dis 
tance to the center will be infinite. 

In the following cases, when the force a as some inverse power of 
distance, the velocity from CD to a finite distance will be finite, for 

a"- 1 x n ~ l _ /_L_ 

V a n 1 x n 1 ^/ -^n 1 

when a is infinite. And the velocity from a finite distance to the center 
will be infinite, for 

- a n - l x n - 
when x = 0. 

262. On the Velocity and Time-Curves. 

B A B 

n D 





( 1 ) Let F a D, the area which represents V 2 becomes a A. 
For D F a D C. 

(2) Let F a V D, /. D F 2 a D C and V-curve is a parabola. 

(3) Let F a D 2 , . . D F a DC 2 , and V-curve is a parabola the 
axis parallel to A B. 

(4) Let F a yr, /. D F a yx-fo * V-curve is an hyperbola referred 

to the asymptotes A C, C H. 

(5) If F a D, and be repulsive, V 2 aDC.DFDC 2 j 

/. V a D C, . . the ordinate of the time curve a -^- a T-\ n > 
.. T-curve is an hyperbola between asymptotes. 

(6) If a body fall from co distance, and F a =p, V a -^-, 

.-. the ordinate of the time-curve D, . . T-curve is a straight line. 

(7) If a body fall from , and F <x jp , V a - , 

.-. the ordinate of T-curve V D C, . . T-curve is a parabola. 

(8) If a body fall from x, and F a 

V a , 

.-. the ordinate of T-curve a D C 2 , .-. T-curve is a parabola as in case 3. 





263. Find the external fall in the ellipse, the force in the focus. 

Let x P be the space required to acquire the velocity in the curve at P. 
V 2 downPx Px 

V 2 in the circle distance S P 

S x 

V * in the circle distance S P A a 

V 2 in the ellipse at P " 2. H P 

, V 2 down Px A a . P x 

V 3 in the ellipse at P ~~ S x. H P 

Sx " A a 

P x _ HP 

S P " S P 

.-. P x = H P 

.-. S x = SP-f-Px = Aa, and the locus of x is the circle on 2 A a, 
the center S. 

264. Find the internal fall in the ellipse, the force in the focus. 

V z down P x 
V * in the circle S x 

V 8 in the circle S x 



_SP I 

V 2 in the circle S P ~ S x tOrCe a distance 1 



V 2 in the circle S P A a 


V 2 in the ellipseatfP 

V 2 down P x 
V z in the ellipse at P 

S x 

2 H P 

Px. Aa 
S x . H P 


A a 

H P 

SP~Aa + HP 

Describe a circle from H with the radius A a. Produce P H to the 
circumference in F. Join F S. Draw H x parallel to F S. 
265. Generally. 

For external falls. 

V 2 down P x Sg.areaAB FD Newton s fig. 

V 2 in the circle distance S P ~ g F . S P F = force at distance S P 

V 2 in the circle S P 2 S P 

V 2 in the curve at P 
V 2 down P x 

P V 
4. A B FD 

* V 2 in the curve " F. P V 
.-. 4 . A B F D = F . P V 

. , , . , fordinate = F I 

K md the area in general < , > 

t abscissa = space J 

In the general expression make the distance from the center = S P, 
and a the original height, S x will be found. 

266. For internal falls. 

V 2 down P x 2g. AB F D Newton s fig. 

"2 g F . ST F = force at P 

2 SP 

V 2 in the circle S P 
V 2 in the circle S P 

V 2 in the curve at P 

V 2 down P x _ 

"V 2 in the curve at P ~ F. P V 

.. if the velocities are equal, 4 A B F D = 


267. Ex. For internal and external falls. 


In the ellipse the force tending to the center. 

In this case, D F a D S. Take A B for the force at A. Join B S. 

A D 

.-. D F is the force at D, and the area A B F D = - (A B + D F) 

= AS _ S D A B + D F. Let /^ equal the absolute force at the dis 
tance 1. Let S A = a, S D = x, .-. A B = a p. 

D F = 

.-. A B F D = ft . 

x. a -f x 



4ABFD = F.PV, 

CD 2 

x 2 = C P . 

- in the ellipse, 


a 2 x 2 = C D 2 . 
For the external fall, make x = C P, then a = C x, and C x 2 C P 2 = C D 2 , 
or Cx 2 = C P 2 + CD 2 

= A C 2 + B C 2 
= AB 2 
.-. C x = A B. 
For the internal fall, make a = C P, then x = C x , and 

C P 2 Cx /2 = CD 2 , 

Cx 2 = CP 2 CD 2 , 

.-. Cx = V C P 2 CD 2 . 

268. Similarly, in all cases where the velocity in the curve is quadrable, 
without the Integral Calculus we may find internal and external falls. 
But generally the process must be by that method. 




Thus in the above Ex. 

vdv = g/u-x.dx 
gfi (a 2 x 2 ) 

.-. v 

269. And in general, 


, as above, &c. 

(a n + 1 x 1 ^ 1 ), if the force a 




-+ - x +) = ,-. P. 

And to find the external fall, make x = , and from the equation find a, 
the distance required. 

And to find the internal fall make a = r, and from the equation find x, 
the distance required. 

270. Find the external fall in the hyperbola, the force oc from the focus. 

V 2 down O P : V in the circle rad. S P : : O P : 


V * in the circle S P : V 2 in the hyperbola at P : : A C : H P 


.-. V 2 down OP: V 2 in the hyperbola : A C. O P : SQ ^ H P 

.-. 2 A C. O P = SO. HP 
.-. 2AC.SO 2AC.SP = SO. HP 


To find what this denotes, find the actual velocity in the hyperbola. 
Let the force = /3, at a distance = r, . . the force at the distance 


V 2 in the circle S P jS. r* x /3 x 

2 g x 2 2 2 x 

V 2 in the hyperbola _ (2 a + x) j3 r 2 
2 g a . 2 x 

- /3r , $Ll 

x "2 a 

V 2 B r z V - 

But -^ when the body has been projected from oo = -- 1- -$ of 
g x ^g 

V s 8. r z V 2 

projection from oo , .-. - of projection from oo = -^ = down 2 a, 

O O 


F being constant and = - 5 , or = V 2 from GO to O , when S O = 2 A C. 

.*. V in the hyperbola is such as would be acquired by the body ascend 
ing from the distance x to CD by the action of force considered as repul 
sive, and then being projected from co back to O , S O being = 2 A C. 

In the opposite hyperbola the velocity is found in the same way, the 

c , . ,, 2 H C . S P 

torce repulsive, p externally = \T\> 

A \^i - AT. L 

271. Internal fall 

V 2 down P O : V 2 in the circle rad. SO: : P O : 

V 2 in the circle S O : V 2 in the circle S P : : S P : S O 

V 2 in the circle S P : V 2 in the hyperbola at P : : A C : H P 

.-. V down P O : V 2 in the hyperbola : : A C. PO : S H P 

.-. 2 AC. PO = S O. H P 


2 A C. SP 





Hence make H E = 2 A C, join S E, and draw H O parallel to S E. 

Hence the external and internal falls are found, by making V acquired 
down a certain space p with a ble force equal that down i . P V by a 
constant force, P V being known from the curve. 

272. Find how far the body must fall externally to the cir 
cumference to acquire V in the circle, F distance towards the 
center of the circle. 

Let OC = p,OB = x,QA=ta,C being the point re 
quired from which a body falls. 

Let the force at A = 1, .*. the force at B = 

x A 

~* "I 

v d v g.F.dx, (for the velocity increases as x decreases) 

* i 

= g . d x 
fo a 

and when v = 0, x = p, 

v z = 

and when x = a, 

at A = 

(P - 


v 2 at A = 2g. -g- 
the force at A being constant, and 

= ga 

p a s = a 

p 2 = 2 a 2 , .-. p = V 2 . a. 
273. Find how far the body must fall internally from the circumference to 
acquire V in the circle, F a distance towards the center of the circle. 

Let P be the point to which the body must fall, O A = a, O P=p, 

O Q = x, F at A = 1, .. the force at Q = . 


i X 

.. v d V = ft . . d x 

... v 2 = --| .x 2 + C, 
and when v = 0, x = a, 


.-. v 2 = (a 2 x 2 ) 

and when x = p, 

v 2 = (a 2 p s )from a ble force 


v 2 = g . a, from the constant force 1 at A. 

.-.a 2 p 2 = a 2 , .-. p = 0, .-. the body falls from the circumference 
to the center. 

274. Similarly, when F oc . . 


O C, or p externally = a V~~e, (e = base of hyp. log,) 

OP, or p internally = -^ . 

275. When F a . 

distance 2 
p externally = 2 a 

2 a 

p internally = - . 

276, When F oc -r. J 

distance 3 
p externally = x . 

p internally = ~-^- 

277. When Fa 1 

distance n + l 


p externally = a ^J - 


p internally = a / ; 

V 2 + n 

If the force be repulsive, the velocity increases as the distance increases, 
. . v d v = g F . d x 

Vor.. I. O 



[.SECT. VI J. 

278. Find how far a body must fall externally to any point P in the 
parabola, to acquire v in the curve. F a =^2 towards the focus. 

P V = 4 S P = c, S Q = p, S B = x, S P = a, force at P = 1, 
a 2 


FatB = 


. yl _ s! 4. r 

o v 

when v = 0, x = p 
, r _ g a2 

= 2ga 2 (- -- ) = 2ga 2 f ) at P, 
Vx p/ \ a p/ 

= 2g.~ = 2ga, 

279. Similarly, internally, p = 

280. In the ellipse, F a 
xternally = 
p internally = 

towards a focus 

p externally = PH + P S. (. . describe a circle with the center S, rad. = 2 A C) 

(Hence V at P = V in the circle e. d.) 

281. In the hyperbola, F a ^p towards focus 

pexternally 2 A C (Hence V at P = V in the circle e. d.) 


p internally = p ^-^j . (Hence V at P= V in the circle e. d., p. 190) 

<5 A \~/ "}- Jr Jrl 

282. In the ellipse F cc D from the center 
pexternally= V A C 2 -f- B C 2 , (= A B)} (Hence construction) 

or (= V C D 2 + C P 2 ) 

(Hence also V at P = V in the circle radius C P, when C D = C P) 
p internally = V G P 2 CD 2 . 




(Hence if C P = C D s p = 0, and V at P = V in the circle e. d, as 
was deduced before) 

(If C P < C D, p impossible,. .-. the body cannot fall from any distance 
to C and thus acquire the V in the curve) 

283. In the ellipse, F a D from the center. 

External fall. 

The velocity-curve is a straight line, (since D F a C D, also 
since F = 0, when C P = 0, this straight line comes to C, as 
C d b, V a V TTO b a C O, O being the point fallen from, to acquire 
Vat P. 

.-. V from O to C : V from P to C : : O C : P C 

Also since vdv = gF.dx, and if the force at the distance 1 = 1, 
the force at x = x. .-. v d v = g x d x, and integrating and correct 
ing, v 2 = g (p * x 2 ), where p = the distance fallen from. 

.; v a V p 2 x 2 , and if a circle be described, with center C, rad. C O 
a P N (the right sine of the arc whose versed P O is the space fallen 

.-. V from O to P : V from O to C : : P N : (C M =) O C 

V from P to C : V in the circle rad. C P : : 1 : 1 
(for if P v = i P C, v d = C d P) and 

V in the circle C P : V in the ellipse : : C P : C D. 
Compounding the 4 ratios, 

V down O P : V in the ellipse : : P N : C D 
.-. Take P N = C D, and 

V down O P = V in the ellipse, 

.-. C O = C N = V C P 2 + C D . 



Internal fall. 



V in the ellipse : V in the circle rad. C P : : CD: C P 
V in the circle : V down C P : : 1 : ] 

V down C P : V down PO: : (CM=)CP: ON 
.-. V in the ellipse : V down P O : : C D : O N 
.-. Take O N = C D, and V in the curve = V down P O, and C O 
= V C P * C D 2 . 

284. Find the point in the ellipse.! the force in the center, where V = the 
velocity in the circle, e. d. 


In this case C P = C D, whence the construction. 

Join A B, describe 


on it, bisect the circumference in D , join 

B D , A D . From C with A D cut the ellipse in P. 

2AD /2 (=2PC 2 ) = AB 2 =AC 2 + BC s (=CP e + CD 2 ) 
.-. 2 C P 2 = C P 2 + CD 2 

... C P 2 = C D 2 . (C P will pass through E.) 

A simpler construction is to bisect A B in E, B M in F, then C P is 
the diameter to the ordinate A B, and from the triangles C E B, C F B, 
C F is parallel to A B, .-. C D is a conjugate to C P and = C P. 

p externally (to which body must 

285. In the hyperbola, 
force repulsive, a D, from the center 

rise from P,)= V C D 2 + C P 2 

p internally (to which body must 

rise from the center) = VCP -CD* 
(Hence if the hyperbola be rectangular p internally = 0, or the body must 
rise through C P.) 




286. In any curve, F oc --j-qri ,Jind p externally. 

where a = S P, c = P V. 
287. If the curve be a logarithmic spiral, c = 2 a, 

/a \ i 
.. p = a I 

n a 

o F a jp, ( .-. 

.-. n = 2 j 

p = a -- n = cc 

288. In any curve, F a -p. n + ][ t jind p internally. 

f a \ I . / 4a + 1 x 

p = a / -- \ V. (p * - - - - - ) 

n c v 1 4 a + n c/ 

\ a + I 
4> J 

289. If the curve be a logarithmic spiral, c = 2 a, n = 2, 

290. If the curve be a circle, F in the circumference, c = a, and n = 4, 

/a \ 

.*. p externally = a ( ) * = x 

* cl tl/ 

/ 1 \ *L 

and p internally = a ( ) * = ~ . 

\a + a/ * f 

291. In the ellipse, F a =^ from focus. External fall. 

V 2 down O P : V 2 in the circle radius S P : : O P : , Sect. VII. 


V ! in the circle S P : V 2 in the ellipse at P : : A C : II P, 



.-. V 2 down O P : V 2 in the ellipse : : A C . O P : 



.-. s o = 

.-. 2 AC.O P = SO. HP 


H P 

H P 

Internal fall. 

U - 2 A C H P - ^ A 

V 2 down P O : V 2 in the circle radius S O : : P O : - - , 


V 2 in the circle S O : V 2 in the circle S P : : S P : S O 
V * in the circle S P : V 2 in the ellipse at P : : A C : H P 

.-. V 2 down P O : V 2 in the ellipse : : P O . A C : 

.-. 2PO.AC = SO.HP 
.-. 2SP.AC 2SO.AC = SO.HP 

2 A C.S P 


.-. S O = 

F a 

2 A C + H P 

Hence, make.H E = 2 A C, join S E, and draw H O parallel to E S. 
292. External fall in the parabola, 

^ from focus. 


V 2 d . O P : V 2 in the circle radius S P 

:: OP: 

, Sect. VII. 

V 2 in the circle S P : V 2 in the parabola 
atP:: 1 : 2, 


.-. V 2 down O P : V " in the parabola : : O P : S O 

.-. O P = S O, .-. S O = a 
Internal fall. 

Vdown OP : V 2 in the circle S O : : O P : ~- 


V 2 in the circle S O : V 2 in the circle S P : : S P : S O 
V 2 in the circle S P : V 2 in the parabola at P: : 1 : 2 

.-. V 2 down OP: V 2 in the parabola : : O P : S O, 
.-. O P = S O, 

.-. S O - ~ . 
V = V down - =r V down S P = V . down E P = V of a body describ- 


ing the parabola by a constant vertical force = force at P. / x 

293. Find the external fall so that the velocity* ac 
quired = n . velocity in the curve, Fax". 

v d v = g ,a . x n . d x, (/ = force distance 1), 

.-. v 2 = ~~ (a n + l x tt + l ) a = original height, /x 

\TI .1 P d P g ., 2 p d P / 

V " in the curve = a u, . ^ = ^ - u. . c, if c = , =, / 
dp 2 dp 

* 2 ~~n + 1 ^ ~" n+1* " 

Make x = S P = g, and from the equation we get a, which = S x. 
For the internal fall, make a = S P = g, and from the equation we get 
x, which = S x . 

294. Find the external fall in a LEMNISCATA. 

(x 2 + y 2 ) 2 = a 2 (x 2 y 2 ) 

is a rectangular equation whence we must get a polar one 
Let L. N S P = 6, 

.*. y = g. sin. 6 t x = g. cos. &, g 2 = (x 2 + y 2 ) 
.. g 4 = a *" . (g 2 (cos. 8 d sin. z 6}} = a 2 g 2 . cos. 2 0, 
.. g 2 = a 2 . cos. 2 d 

r e\ 

.: 2 6 = L. (cos. = a-;), 
V av 

2gdg 2 g d g 

a 2 : Va 4 g 4 

/ 1 L! 

v "" 




but in general 

.-.p = 

r d~ 

= in this case - 

P 6 

D 8 i- 

" a 4 


_ ?J_P - _ SL 
.*. force to S a 



v d v = *f . d x, 


P V = 


* - g-^ ^l - 2 g^- JL 


^ 3 6 

Make x in the formula above = j, 

. . ^ = 0, ,*. a is infinite. 

rt D * 




295. Find the force and external fall in an EPICYCLOID 
CY 2 =CP 2 YP 2 = CP 2 CA 2 . 


CY = p, 

YB ! 

= g, CB = c, CA=b, 

C 2 p 2 

.-. c 2 p 2 = 

b 2 c 

b 2 p 

c 2 b 2 
JL c 2 b 2 

* * 2 "~ ""^ /""" 2 V\ gV 

2 dp _ c 2 b 2 ( 

p 3 "" c 2 

.. force 

b 2 ) 

oc -i-. 

(as in the Involute of the circle which is an Epicycloid, when the radius 
of the rota becomes infinite.) 

Having got <x a of force, we can easily get the external (or internal) fall. 

296. Find in what cases we can integrate for the Velocity and Time. 

Case 1. Let force a x a , 

.-. v d v = g (i . x n d x, 


... t - /*"~ dx = / n + 1 /* 

J v -> 2s //, / Vfa 


Now in general we can integrate x m dx.(a + bx n1 ) , when 

m-f-1. , . m+lp ,, 

is whole or \- whole. 

n n q 

. . in this case, we can integrate, when 




= p any whole number 

= p- 

.. n = " , (p being positive), (a) 



.*. these formulas admit only and 1 for integer positive values of n, and 
no positive fractional values. . . we can integrate when F a x, or F a 1. 

297 oc -1 

297. Case 2. Let force oc -1 , 


, d x 

.*. v d v = g . 

fo x n 

2rv n /Q n 1 ^^ ,,. n i 
... v* = ^ ^ (? : x _> 

/ dx /n l.a n-1 r dx.x 

. . t = I = *J n / ; ; , 

J V ** 2 g (Jj J -V/a n ~ 

n 1 

,n I 

in which case we can integrate, when - ^ , or ^ , whole. 

i. e. if - -\ or ^ , be whole. 

2 n 1, n 1 

Let r =: p, any whole positive No,, 

1 _ 2 p 1 

n 1 2 


2p V 

. . these formulae admit any values of n, in which the numerator ex 
ceeds the denominator by 1, or in which the numerator and denominator 
are any two successive odd numbers, the numerator being the greater. 


.. we can integrate, when F 5, -7-= , , - , &c. 

X X g" -^3" ^ X 

1 -1 J_ l * 

- ~ 5 5 <v 9 n 9 *^ 

v 3 -v*? v 7 ~v y 
X A * A -^ A -7- 


298. Case 3. The formulas ( ) (ft ), in which p is positive, cannot be 
come negative. But the formulas (a) and (/3) may. From which we can 

integrate, when F oc -___.____ & c . 

299. When the force a x. n ,Jind a n . of times from different altitudes 
to the center of force. Find the same, force a s - . 


Fa x n , .. v d v = g / u.x n dx, 


d x n+ 1 

a 7- , , , ; which is of ^ dimensions. 

^/ <j n + 1 X n ~^~ 2 

. . t will be of dimensions. 

and when x = 0, t will 

x a _ 2 - 



a 2 

n + 1 x n + i a 


! *" + ,1.3 x ! " 

+ lr r r+-au..- + a74- 8n + 3 

when t = 0, x = a, 

.-. C a I. + 1 . __ . U _?_ . &c I 

I 2 n + 8+ 2. 4" 8l , + 3 i 

. . when x zr 0, t a - -" a ^ 


1 n + l 

when n is negative t a _ n _ 1 a a 2 . 
a _ 

COR. If n be positive and greater than 1, the greater the altitude, the 
less the time to the center. 

300. A body is projected up P A with the velocity V from the given 
po nt A, force in S K^jind the height to which the body will rise. 

vdv = g ,& x n d x, 
for the velocity decreases as x increases, A 

when v = V, x = a, 


. x - /v g .n + i 


COR. Let n = 2, and V = the velocity down , force at A con- 

slant, = velocity in the circle distance S A. 

= 2 a. 



301. PROP. XLI. Resolving the centripetal force I N or D E (F) 
into the tangential one IT (F ) and the perpendicular one T N, we 
have (46) 

I N : I T : : F : F : : ^ : 

d t d t 

.-. d v : d v : : d t x I N : d t x I T. 

But since (46) 

v v 

and by hypothesis 

v v 7 

.-. d t : d t : : d s : d s : : I N : I K 
.-. d v : d v : : I N 2 : I K x I T 

: : 1 : 1 

d v = d v , 
&c. &c. 


302. By 46, we have generally 

vdv gFds 

s being the direction of the force F. Hence if s be the straight line and 
s the trajectory, &c. we have 

vdv =. gFds 

v d v = g F d & 
.-. v 2 V 2 - 2g/Fds 

v"_ V 1 = 2g/Fd s 

V and V being the given values of v and v at given distances by which 
the integrals are corrected. 

Now since the central body is the same at the same distance the central 
force must be the same in both curve and line. Therefore, resolving F 


when at the distance s into the tangential and perpendicular forces, we 

= F x 


IN - I K 

d s 

d s 

.-. F d s = F d s 

v/a _ V /2 = 2 g/F d s = v 2 V 2 

which shows that if the velocities be the same at any two equal distances, 
they are equal at all equal distances i. e. if 

V = V 

v = v . 
303. COR. 2. By Prop. XXXIX, 

v 2 A B G E. 

But in the curve 

y a Fa A n - l 
.-. y d x a A"- 1 d A 
Therefore (112) 

ABGE =/ydxa ~ + C 

P n A n 




v 2 a P n A". 

304. Generally (46) 



d v = gFds 

and if 

F = 



But when v = 0, let s = P ; then 


C = P". 


,2 _ jLfaJ 6 /pn _ 


in which s is any quantity whatever and may therefore be the radius vector 
of the Trajectory A ; that is 

v 2 = i^(pn_ A") or = ?-g-^(D n e n ) 
n n v 

in more convenient notation. 

N. B. From this formula may be found the spaces through which a 
body must fall externally to acquire the velocity in the curve (286, &c.) 

305. PROP. XLI. Given the centripetal Jbj-ce to construct the Trajec 
tory, and to find the time of describing any portion of it. 

By Prop. XXXIX, 

v = V~2~g. V A B F D = ^ (46) = ^ 


T /-i yr v , Time T _, XT Time 
d t = I C K X -T = I CxK NX 

A .m. vx ^s *** .L^ ^\ _. j 

Area 2 Area 

= p TT~ (P being the perpendicular upon the 

tangent when the velocity is V. See 125, &c.) 

Moreover, if V be the velocity at V, by Prop. XXXIX, 

V = V~2~~. V A B L V. 


V A B F D - x 



. . putting 

A V 2 g 
we have 

ABFD : Z 2 : : I K 2 : KN 2 

.-. A B FD Z 2 : Z 2 : : I K 2 K N 2 : K N 2 

V A B F D Z" 2 : Z = - : : I N : K N 


. A x K N - Q X IN 

V (AB FD Z 2 ) 

Also since similar triangles are to one another in the duplicate ratio 01 
icir homologous sides 

YXxXC = AxKNx ^- 2 


_ Q x CX a x I N 

= A 2 V (A B FD Z 2 ) 
and putting 

y = ]>b = 2 V (A B FD Z ) 

/ - n Q x CX* 

y ~ 2 A 2 V (A B FD Z 2 ) 


Area V C I =/ y d x = V D b a\ ( ^ 

AreaVC X = /y dx = V D caj 
Now (124) 

2 VCI _ 2 V_D>ji 
P X V : P X V 

2 V D b a 

" <v/2g.Px VABLV 
the time of describing V I. 

Also, if^.VC 1=6, we have 

_ _ XV X CV = <_x CV* 

_ 2VDca 
P 2 

which gives the Trajectory. 

306. To express equations (5) and (6) in terms ofg and 6, ( = A). 

V 2 


Q 2 _P 2 xV 8 

" " 

v 2 P 2 X V* 




P X Vg 


P 3 x V 

P 2 V 2 ) 


2 J V (e 2 v 2 P 2 V 2 ) 

P 3 v r de 
x / 

l = 7 v<**v 2 P 2 V 2 ) 

P 2 V 2 ) 

But by Prop. XL. 

the integral being taken from v = 0, or from f =D, D being the same as 
P in 304. 

fs d e 


P 8 V r ) 

, or =/ 

V 2 V 2_ 



Px Vdg 

P S V 

. . (7) 
ix ( 8 ) 

307. Tojtnd t awrf ^ m terms of % and p. 
Since (125) 


" -J 

P 2 V 2 p 



But previous to using these forms we must find the equation to the tra 
jectory, thus (139) 

P 2 V 2 d D 
X 4-- = F = f(j) 

f denoting the law of force. 

VOL. I. 





~~ 17 2 o . r A 4- 



308. To these different methods the following are examples : 
1st. Let F a s = p s . Then (see 304) 

and if P and V belong to an apse or when P = g ; 
V 2 = g ft (D 2 P 2 ) 

A/ , .. J 

P 2 (D 2 P 2 )} 

?_ 2 


Let g 2 = u. Then we easily get 


2 t V or u = 

pa - 1 - 7 


and making t = at an apse or when g = P, we find 

D 2 

C = sin. . ^ps-r = sin. ~ l 1 


2 V 


1)2 ) 

T r( 

D 2 "" 2 f 

"a" 3 


/dt__ 1 

J^~9 A/ 


" 2 ^/( u+ W{( p -^V-" ! } 

and assuming 

we get 

PV " 2 


2V 5 2 


and making 6 = 0, when g = P we find 

C =_ sin.-l = 1.. 


V= V gp. V (D 2 P 2 ) 

= sn. 

- sin. ( , + i 

= cos. 20=2 cos. 2 1 
which gives 

P2 /T)2 _ p2\ 

r ^ r 

Now the equation to the ellipse, g and 6 being referred to its center, is 

b 2 

o nn? - 

1 e 2 cos. 8 d 

Therefore the trajectory is an ellipse the center of force being in its 
center, and we have its semiaxes from 
b 2 = D 2 P 2 

c 2 a 2 b 2 2P Z D 


a 2 a 2 P 2 


b = V(D 2 P 2 )} 

and V (3) 

a = P J 

which latter value was already assumed. 
Tojind the Periodic time. 
From (3) it appears that when 


and substituting in (1) we have 




sm.- l ( 1) = --. 

4 " 2 V gf* 

T = 2ff , . . (4) 

V gi* 

which has already been found otherwise (see 147). 

To apply (9) and (10) of 307 to this example we must first integrate 
(11) where f $ = /tig; that is since 

~ 2 * 2 
we have 

P2 YT2 

P 2 = 

V 8 

V 2 = g^*(D 2 P 2 ) 

D 2 - g s 

which also indicates an ellipse referred to its center, the equation being 

2 _ a 2 b 2 
- a 2 + b 2 g 2 


g2 g2( D 2_g2)_p2(D2_ P 2) 

p- P 2 (D 2 P 2 ) 

. t _ i 

the same as before. 

With regard to 6 t the axes of the ellipse being known from (5) we have 
the polar equation, viz. 

,2 r . 

"1 e 2 cos. 2 6 

309. Ex. 2. Let F = -4- . Then (304) 


V 2_?J 




= 2ffA6 X ^~ S 


^ DP 


P and V belonging to an apse. 


g* DP + P 2 ) 

D 8 

which, adding and subtracting , transforms to 

t- V D r 

A i- D 
and making g = u 

t = 


(see 86). 
Let t = 0, when 

= P. Then 



J_ . r dt - 
PV-JT? - 


But assuming 

tlie above becomes rationalized, and we readily find 




[SECT. VI11. 

VP.(D P) 

X < tan. ~ l 


and making 6 = 0, when g = P, or when u = P - - , we get 

Hence, since moreover 

Dx D 


2 8 

= sm. 

= sin. (0 4. *2~] = cos 6 

P 2 

2 P . (D P) 


!+(!_-) cos.. 

. (2) 

But the equation to the ellipse referred to its focus is 

b 2 1 

S= T- x 

a 1 + e cos. 
b_ 2 P (D P) 

a " D 


e" = 



.b*_4P 4P*_4P 
a" 2 " - TJ " " ~D^ ET* - 
b 2 2 


-~a~ X D 



b= VP x (D 

To find the Periodic Time ; let 6 = *. Then g = 2 a P = JD P, 
and equation (1) gives 

tf IL ^2 2 / 

see 159, 


First find the Trajectory by fonnula (11. 307) ; then substitute for 
in 9 and 10, &c. 

310. Required the Time and Trajectory when F= ^ 

By 304, 

V 2=_g ;u ,x (D- 2 P- 2 ) 

O \ 9 * 

, 2 

~D 2 X f 2 
.. if V and P belong to an apse we have 
g tt D 2 P 2 

= JJ2 X p 2 



V L . 
and taking t = at an apse or when g = P, C = 0, 

V g/i 

6 r dt D 

X (C+ VP 8 %*) 

= 0, 

. . . . (1) 



(P 2 f 2 ) ~ +P 



11 _ , ^ (P 2 -g 2 )+P 

Tk 2 T>2\ * I 

V (D s P 2 ) 

and making ^ = at the apse or where g = P, 

C = -l. = 

- V D 


e\/(D 2 

wliich gives 


311. Required the Trajectory and circumstances of motion when 

or for any inverse law of the distance. 

The readiest method is this ; By (11) 307, if r, and P be the values of 
g and p for the given velocity V (P is no longer an apsidal distance) 

p2Af2 O,, r n 1 __ p n 1 

v _, v 2 4- ^ v g n) 

p 2 h (n l)r n - J g"- 1 

the equation to the Trajectory. 
Also since 

vdv = gFdf 





and if we put 


-(n l)r 
in which m may be > = or < 1 we easily get 

D- / m -- PeV 

~ V m 1 



m= 1 

/ ni 
-J r X 

N m 1 

n 1 

P = 

w (r=^n"~ e 

To Jind 6 on this hypothesis. 
We have (307) 

. m< 1 

n 1 

which gives by substitution 

n 5 , 
r P 2 d 

n 3 


m= 1 

= + 




a d 


the positive or negative sign being used according as the body ascends or 

Ex. If n = 2, we get 

. . . . m> 1 




P = 
P = 

m = 1 

1 m 


the equations to the ellipse, parabola and hyperbola respectively. 
Also we have correspondingly 

I m l 

= +r P. 



which are easily integrated. 

Ex. 2. Let n = 3. Then we get 

Vm _, 

5T3n>< p x 

. . m > 1 


P = T g 

. . m = 1 
. m < 1 

cH = 


mP 2 

-C V (r 2 P 2 ) 

+ / m v 

- V 1 m X 


. m> 1 

m= 1 
. m< 1 

312. In the first of these values of 6, m P 8 may be > = or < r 2 . 
(1). Let m P 2 > r 2 . Then (see 86) 

/ m / / m 1 / m 1 N 

/ -i- n I / ^S \-f t* I c**r* " I / Cfi/" "~* * 1* / , 

^V mP r zXj \ se W nTP r 2 ~ V mP rV 

at an apse or when r = P 

6 = + J m , X P X sec.- 1 4 . . . (a) 
>r m 1 i 




/ m 1 1 1 

/ , Ol* ~~* 

V m P 2 r 2 P " r 
(2) Let m P ~ r 2 . Then we have 


V (m l) f 
P = - 

/ r 

* ( + HT^l 


a= + 

V (m 1) 

1 X J 2 ~ 

= i 

V m 1 

X ( 


e r 

- V m _ 1 

which indicates the Reciprocal or Hyperbolic Spiral. 
(3) LetmP 2 be < r 2 . Then 

V i 
p = 


+ r- m *"S 
m i y 


m r 

^mP Xl V 
at an apse r = P ; and then 

6 = + . 


i^-i-r 2 mP) V(i 2 mP 2 ) 

^i- 2 P) V(r z mP : 



V (r 8 g 8 ) r 

Thus the first of the values of 6 has been split into three, and integrat 
ing the other two we also get 


tf a = + 
= + 

V (r s P 2 ) 


V(r e P ! 

s ; * (1 ~ 1 ) 
x 1.-^ 





^ 1 

* mP g V(m.r 2 ^ 2 ) V (r 8 mP 2 ) 
and if rf is measured from an apse or r = P it reduces to 

= + P /-SL-i. 

N 1 m 

313. Hence recapitulating we have these pairs of equations, viz. 



_ x sec.- l. 
m 1 P 

Jb construct the Trajectory, 
put = 0, then 

g = P= SA; 
let f = CD, then 





and taking A S B, A S B for these values of 0, 
and S B, S B for those of p and drawing B Z, 
B Z 7 at right angles we have two asymptotes ; S C being found by put 
ting 6 = it. Thus and by the rules in (35, 36, 37, 38.) the curve may 
be traced in all its ramifications. 

2. p = 

V (m 1) 

V \ S 


V (m 1) 





This equation becomes more simple when 
we make 6 originate from = oo ; for then 

it is 


V (m 

and following the above hinted method the 
curve, viz. the Reciprocal Spiral, may easily be B 

described as in the annexed diagram. 


. p = p /-i- X 
^V 1 m 


>- = +rP / 

*j f2 

2 \/"nT(F 2 P 2 ) 

and when 6 is measured from an apse or when P = r 

-^Igg+rz mP) V(r 2 mP 
V (r 2 mP 2 )~ 

Whence may easily be traced this figure.* 

A j * 


From which may be described the Logarithmic Spiral.^ 


^-=+rP / 
- Vr 2 



(m.r 8 - 2 ) V (r 2 m P -) 


= r 



i r- V(g 2 -r 2 ) 


i ^ / , 

V 1 m g 

when P = r. 

Whence this spiral. 

These several spirals are called Cotes Spirals, 
because he was the first to construct them as 

314. If n = 4. Then the Trajectory, &c. 
are had by the following equations, viz. 


d 6 = r P 

315. Ifn = 5. Then 
p = P V in 

d6 = r P 


I m 
m 1 


!(,* 5_ 

V V m 1 

V (m 1 .g 2 +r 4 ) 
m d 


m 1 m 

which as well as the former expression is not integrable by the usual 

"1 T* O O . 

m 1 

is a perfect square, or when 

m 1 

m 2 P 

m _ 1 - 4 (m 1) 

then we have 

Therefore (87) 

" 2 (m 1) 

/ m P * 


1) , N2(m 1) 




V (2.m l.g 2 m P 2 ) 

V(mP 2 2.m l. 
and these being constructed will be as subjoined. 

316. COR. 1. OTHERWISE. 
To find tlie apses of an orbit where F = -^ . 



P = f- 



n 1 

f n 3 



- ; 
m 1 

= m > 1 

, m = 1 


n-l + 

. n ] 

. . . m < 1 

1 ni l_m 

which being resolved all the possible values off will be discovered in each 
case, and thence by substituting in 6, we get the position as well as the 
number of apses. 

Ex. 1. Let n = 2. Then 

,* + .-JL- mpt -o 

r m 1* m 1 


PJ _ 4" r J^ 
r 4 

mP ! 

r 1 


which give 

r r 2 + 4m P g .(m 1) 

?- -g( m _ 1)-~ 4(m I) 2 

S = : 4 


r /r 2 4 m P 2 .(l m) 

K- 2 (1 m)- V 4.(1 m) 2 

Whence in the ellipse and hyperbola there are two apses (force in the 
focus) ; in the former lying on different sides of the focus ; in the latter 
both lying on the same side of the focus, as is seen by substituting the 
values of g in those of 6. Also there is but one in the parabola. 
Ex. 2. Let n = 3. Then eq. (A) become 
2 _ m P 2 + r 2 

which indicate two apses in the same straight line, and on different sides 
of the center, whose position will be given by hence finding 6 ; 


r o 

(2) S = = < 


because r is > P, 

whence there is no apse. 

r 2 mP 2 

(3) g = - l __ m 

which gives two apses, r 2 being > m P 2 because m is < 1 and P < r ; 
and their position is found from 6. 

317. COR. 2. This is done also by the equation 


p = g. sin. <p, or sin. <f> = ~ 

<p being the L. required. 

Ex. When n = 3, and m = 1, we have (4. 313) 

p = T e 

.. sin. <p = -y 
.-. v is constant, a known property of the logarithmic spiral. 

318. To find when the body reaches the center of force. 

Put in the equations to the Trajectory involving p, g ; or g, 6 

Ex. 1. When n = 3, in all the five cases it is found that 

p = 



6 =r x . 

Ex. 2. When n = 5 in the particular case of 315, the former value of 
6 becomes impossible, being the logarithm of a negative quantity, and the 
latter is = co . 

319. Tojind when the Trajectory has an asymptotic circle. 

If at an apse for & = cc the velocity be the same as that in a circle at 
the same distance (166), or if when 

6 co 

P = f 
we also have 

p dp 

then it is clear there is an asymptotic circle. 
Examples are in hypothesis of 315. 

320. Tojind the number of revolutions from an apse to = co . 

Let & be the value of d a when g = p or at an apse, and (/ when 
f = co . Then 

= the number of revolutions required. 

2 >, 
Ex. By 313, we have 



= P sec. 

>r m 

m ft 

.*. v = 

- . 
m 1 

321. COR. 3. First let V R S be an hyperbola whose equation, x being 
measured from C, is 


VCR = y-^ X 

/ydx = -^/dx V 

a a J V (x * a 2 ) 

VOL. I. Q, 


b ,/o ox b ,, , ,, ,x b /* a 2 dx 
=-xWx 2 a 8 ) - /dxWx 2 a 2 ) -/- r - ^ 
a a 17 a* 7 V(x 2 a 2 ) 

.*. 2/y d x = -xV(x 2 a ^) abl. X +V ( x2 ~ a *) 
a a 


VCR=^l. X+ *( *> .... (1) 


g=CP=CT=x subtangent 

= x 


x 2 a 2 _ a^ 
x " x 

and substituting for x in (1) we have 

VCR = ~.l. 

2 a 

+ V ^~ e} .... (2) 

N being a constant quantity. 
322. Hence conversely 

and differentiating (17) we get 

x ^2. _L\ 
N 2 V u aV 

dd 2 ~ a 2 b 2 
and again differentiating (d 6 being constant) 

dT 2 = a 2 b 2 N 8 X ] 

Hence (139) 

P*V 2 / 4 


322. By the text it would appear that the body must proceed from V 
in a direction perpendicular to C V i. e. that V is an apse. 
From (1) 322, we easily get 


and since generally 

de 2 


a b N - - 

P 2 = - -- - .... (i) 

which is another equation to the trajectory involving the perpendicular 
upon the tangent. 
Now at an apse 

P = g 
and substituting in equation (1) we get easily 

g = a 
which shows V to be an apse. 



Put d g = 0, for g is then = max. or min. 

324. With a proper velocity. ~] 

The velocity with which the body must be projected from V is found 

vdvrr gFdf. 

325. Descend to the center}. When 

s = 0, p = (1. 323) and = oo (2. 321). 

326. Secondly, let V R S be an ellipse, whose equation referred to the 
center C is 


and as above, integrating by parts, 

x v (ti z -v ^ a z A v 

/dxV(a-x)=i-*Jl J4-i " 

^ V (a 2 x 2 ) 


x y ( a a _x 2 ) a]_ / . , x r 
o o 



a 8 x ; 
~~ X "*" x 

rr Sin.~* 

a / w 2 \ 20 

- =. sin ( r-xf] = cos. , XT 

j \2 ablN/ abJN 


2 tf ..... (2) 

Conversely by the expression for F in 139, we have 

Foe 1 

327. Tojind when the body is at an apse, either proceed as in 323, 
or put 

d x . sin. x 

By (27) d . sec. x = 
sin. 6 

cos. 2 6 


that is the point V is an apse. 

328. The proper velocity of projection is easily found as indicated 

in 324. 

329. Will ascend perpetually and go ojfto infinity. } 

From (2) 327, we learn that when 

2 6 * 

a~FN " 2 

g is ce>; 
also that g can never = 0. 


330. When the force is changed from centripetal to centrifugal, the 
sign of its expression (139) must be changed. 

331. PROP. XLII. The preceding comments together with the Jesuits 
notes will render this proposition easily intelligible. 

The expression (139) 

F _P 2 V* dp 

-L XN q 1 

g P d 

or rather (307) 

pz y 2 

in which P and V are given, will lead to a more direct and convenient 
resolution of the problem. 

It must, however, be remarked, that the difference between the first 
part of Prop. XLI. and this, is that the force itself is given in the former 
and only the law of force in the latter. That is, if for instance F = p n - *, 
in the former /^ is given, in the latter not. But since V is given in the 
latter, we have //. from 304. 


332. PROP. XLIII. To mafce a body move in an oibit revolving about 
the center of force, in the same way as in the same orbit quiescenf] 
that is, To adjust the angular velocity of the orbit, and centripetal force 
so that the body may be at any time at the same point in the revolving 
orbit as in the orbit at rest, and tend to the same center. 

That it may tend to the same center (see Prop. II), the area of the new 
orbit in a fixed plane (V C p) must a time a area in the given orbit 
(V C P); and since these areas begin together their increments must also 
be proportional, that is (see fig. next Prop.) 

KR = CK x ^KCP 
and C P = C p, and C K = C k 

.-. L K C P a k C p 

and the angles V C P, V C p begin together 
/.^.VCP a /LVCp. 


Hence in order that the centripetal force in the new orbit may tend to 
C, it is necessary that 

. V C p a ,L V C P. 
Again, taking always 

CP= Cp 

VCp: VCP:: G: F 

G : F being an invariable ratio, the equation to the locus of p or the orbit 
in fixed space can be determined; and thence (by 137, 139, or by Cor. 
1, 2, 3 of Prop. VI) may be found the centripetal force in that locus. 
333. Tojind the orbit infixed space or the locus of p. 
Let the equation to the given orbit V C P be 

where = C P, and 6 = V C P, and f means any function; then that of 
the locus is 

which will give the orbit required. 


Let p be the perpendicular upon the tangent in the given orbit, and p 
that in the locus ; then it is easily got by drawing the incremental figures 
and similar triangles (see fig. Prop. XLIV) that 
K R : k r : : F : G 
k r : pr :: p : V (f 2 p 2 ) 
pr :PR:: 1 : 1 
PR :KR:: V ( z p 2 ) : p 

1 : 1 : : F . p V (^ p 2 ) : G p V ( s 9 p s ) 

" F 2 g 2 + (G 2 F 2 )p /2 

334. Ex. 1. Lei the given Trajectory be the ellipse with the force in 
its focus; then 

K2 a M P 2 1 

p> 2 = JLi-, and g = * ^ ecos , 

and therefore 

b 2 G 2 (2a-g)g 2 
/ " b 2 (G 8 F 2 ) -H F 2 (2ag g 2 ) 



- a.(I-e 2 ) 

/ F 
1 + e co 

Hence since the force is ( 139) 

and here we have 

a(l e *) u r= 1 -J- e cos. 

2F 2 F 2 


and again differentiating, &c. we have 

d 2 u F 2 G 2 F 2 

d~^ H = Ga(l e*) H ~G^~ 
But if 2 R = latus-rectum we have 

/. the force in the new orbit is 

p V 2 ( F 2 R G R F 2 

X 1 ~T2 T ~5 

gRG 2 ^ s g j 

335, Ex. 2. Generally let the equations to the given trajectory be 

g = f (0 )~) 

Then since 

d e u F 2 d u 

d fl 2 H = G 2 d^ J H 

F 8 v /d 2 u . N F 2 

= G~ 2 X VdT 2 + u ) + u ~ G^ u 

and if the centripetal forces in the given trajectory and locus be named 
X, X , by 139 we have 

gX . FJ gX G 2 -F v 1 
p? yi - G t A p ,j y /t 1 ^ x yy 



_ p*y* , F 2 X G 2 F 2 _1 

/4 X 

Also from (2. 333) we have 

JL - L s _I_ G 8 F _i 

p 2 G 2 X p 2 ~ G 2 X ? 2 

dp Fj- dp / G 2 F * 1 
p 3 d f ~G 2X p 3 d f 4 ~^ X "p" 

.-. by 139 

gX .._F gX GF 1 

p 2 y 2 ~ p/ 2 y/ 2 "t (j 2 "P 

the same as before. 

This second general example includes the first, as well as Prop. XLIV, 
&c. of the text. 

836. Another determination of the force tending to C and which shall 
make the body describe the locus of p. 

First, as before, we must show that in order to make the force X tend 
to C, the ratio L. V C P : L. V C p must be constant or = F : G. 

Next, since they begin together the corresponding angular velocities 
u, u f of C P, C p are in th^t same ratio ; i. e. 

: : : F : G. 

Now in order to exactly counteract the centrifugal force which arises 
from the angular motion of the orbit, we must add the same quantity to 
the centripetal force. Hence if p, p denote the centrifugal forces in the 
given orbit and the locus, we have 

X = X +. p p 

X being the force in the given orbit. 
But (210) 

P 2 V 1 

P = - x -3 

g ? 


a w 2 
when o is given. 

a/ ! G 2 P 2 V G 2 1 

<?/ 0; v _ ffi V - __ V V 

a 2 ~ * F 1 ~ g X F f j 8 

p*Y 2 G 2 F 2 1 





pz y 2 


P 2 V 2 / dp , G 2 F 2 X ._. 

= T~~ * V dl + FV ) (8) 

O ib b 

337. PROP. XLIV. Take u p, u k similar and equal to V P and V K ; 

m r : k r : : . V C p : V C P. 

Then since always C P = p c, we have 

p r = P R. 
Resolve the motions P K, p k into P R, R K and p r, r k. Then 

and therefore when the centripetal forces PR, p r are equal, the body 
would be at m. But if 

P Cn:pCk::VCp:VCP 

C n = C k 

the body will really be in n. 

Hence the difference of the forces is 

m k X m s (m r k r) . (m r + k r) 

m n = = * * ~ . 

m t m t 

But since the triangles p C k, p C n are given, 


K r a m r a 


1 1 

.. m n cc -= , X - . 
C p 2 m t 

Again since 

p C k : p C n : : P C K : p C n : : V C P : V C p 
: : k r : m r by construction 
: : p C k : p C m ultimately 
. . p C n = p C m 
and m n ultimately passes through the center. Consequently 

m t = 2 C p ultimately 


in n a -^ 3 



338. By 336, 

X X = / p 

p 2 y 2 G 2 F 2 1 
v v 

g F 2 3 

ex - . 

S 3 

339. To trace the variations of sign qfmn. . 

If the orbit move in consequentia, that is in the same direction as C P, 
the new centrifugal force would throw the body farther from the center, 
that is 

or m n is positive. 

Again, when the orbit is projected in antecedentia with a velocity < 
than twice that of C P, the velocity of C p is less than that of C P. 

C m is < C n 
or m n is negative. 

Again, when the orbit is projected in antecedentia with a velocity = 
twice that of C P, the angular velocity of the orbit just counteracts the 
velocity of C P, and 

mn = 0. 

And finally, when the orbit is projected in antecedentia with a velocity 
> 2 vel. of C P, the velocity of C p is > vel. of C P or C m is > C n, or 
m n is positive. 


By 338, 

m n oc <p p 

oc u * 2 

= 01 + W 

W being the angular velocity of the orbit. 
.-. m n oc + 2 uW+ W 2 

+ 2 + W 
j- or being used according as W is in consequentia or antecedentia. 




Hence m n is positive or negative according as W is positive, and nega 
tive and > 2 ; or negative and < 2 u. That is, &c. &c. 

Also when W is negative and = 2 <w, m = 0. Therefore, &c. 

340. COR. 1. Let D be the difference of the forces in the orbit and in 
the locus, and f the force in the circle K R, we have 

D: f : : m n : z r 

.ink X m s . r k 2 
m t 2~k~c 

(m r + r k) (m r r k) r k * 
2 k c 2kc 

::mr 2 rk 2 :rk 2 
:: G 2 F 2 : F 2 . 

341. COR. 2. In the ellipse with the force in the focus, we have 

F 2 R G 2 R F 2 

x/a i- 2 + - -^ - 

For (C V being put = T) 

v 2 y 2 

Force at V in Ellipse : Do. in circle : : -= j-wrr TV-TT/ 

chord P V : P V 

1 1 

Also F in Circle : m n at V 
m n at V : m n at p : 

.*. F at V in ellipse : m n at p ; 

2 R 2 T 

T: R 

F 2 : G 2 F 2 

J_ JL 

T 3 A * 

TF 2 RG 2 RF 2 

we have 

x- F2 

x - 

F in ellipse at V = ~^ 


RG 2 

m n = 


X = X + m n 

F 2 RG 2 RF 

see 834. 



342. By 336, 

P 2 v 2 n 2 


X - ^ 



P 2 V 2 L 

- = -^ ft = R p (157) 
g 2 

p r F 2 G 2 F 2 1 

= F 2 x i 7^ + ~p J 

343. COR. 3. /w the ellipse with the force in the center. 

X FZ A . R G 2 R F 2 

T 3 A 3 

v 2 
For here X a A and the force generally oc ^--^ (140) 

/-Force in ellipse at V : Force in circle at V : : T : R 
J F in circle : m n at V : : F 2 : G z F 2 

(.m n at V : m n at p : : 7 ^r 3 : -r- 3 

1 A 

T? I.- /W F 2 ^ RG 2 RF Z 

.-. F in ellipse at V : m n at p : : 7^3 . T : 

7^3 . - T- 
1 A 

F 2 A 
assuming F in ellipse at P = .3- , we have 


F 2 

F in ellipse at V = =r- 3 x T 

RG 2 R F 2 

.-. m n = - A3 

.-. X 7 a X + m n a , &c. 


. P 2 V 2 4 (Area of Ellipse) 

344. X = p P, and = T^ . i - 

g g( Period) 2 

_ 4?r 8 a 2 b 2 _ 2 , 
g( Period) 2 


Therefore by 886 

ft2 p 2 1 

X ^ + ^a b X-^i- X- 

^a 3 fF 2 g , b 2 x (G 2 F 2 )) 
F 2 \ a 3 ag 3 / 

RG 2 --RF*1 
S * J 

845. COR. 4. Generally let X &? /Ac >rce <tf P, V ~ at V, R the 

radius of curvature in V, C V = T, &c. 

V R ft 2 V R F 2 

X a X 4 AS 

A 3 


f F in orbit at V : F in circle at V : : T : R 
jl* : m n at V ::F 2 :G 2 F 2 

Im n at V : m n : : A 3 : T 3 

V TT 2 ft 2 TT * 

.-. F in orbit at V : m n : : 8 : V R . !2-^l- 

. . since by the assumption 

F in orbit at V = 

T 2 
VR(G 2 F 8 ) 

A 3 


This may better be done after 336, where it must be observed V is not 
the same as the indeterminate quantity V in this corollary. 
346. COR. 5. The equation to the new orbit is (333) 

2 _ 

G*p /2 g 2 

g 2 + (G" 2 " F 2 )p /8 
p belonging to the given orbit. 

Ex. 1. Let the given orbit be a common parabola. 

s _ G 2 rg s 

: F 2 g + (G 2 F 8 )r 
and the new force is obtained from 836. 


Ex. 2. Let the given orbit be any one of Cotes Spirals, whose general 
equation is 

D" - -- 
- 2 

Then the equation of 333 becomes 

G 2 

-b 2 ? 2 

which being of the same form as the former shows the locus to be similar 
in each case to the given spiral. 

This is also evident from the law of force being in each case the same 
(see 336) viz. 

/ - U 


~~ ~ " ~ /~* 

f g 

Ex. 3. If the given orbit be a circle, the new one is also. 
Ex. 4. Let the given trajectory be a straight line. 
Here p is constant. Therefore 

2 _ G 2 p /2 x g g 

P T? 2 n>2 __ T2 

the equation to the elliptic spiral, &c. &c. 

Ex. 5. Let the given orbit be a circle with the force in its circumference. 

2/^2 2\ 

P (4 1 " P ) 
P 2 = 47*- 

and we have from 333 

" 4r 2 F 2 + (G 2 F 2 )g 2 

Ex. 6. Let the given orbit be an ellipse with force in the focus. 

2a g 
and this gives 

P 8 = F * g (2 a ? ) + b s (G J Y 


347. To find the points of contrary Jlexure, in the locus put 

dp = 0; 
and this gives in the case of the ellipse 

b 2 F 2 G* 


In passing from convex to concave towards the center, the force in the 
locus must have changed signs. That is, at the point of contrary flexure, 
the force equals nothing or in this same case 

F 2 A + RG 2 RF 2 = 
.-. A = S s x (F 8 G 2 ) 

- k! F 2 G 3 

: T* F 1 

And generally by (336) we have in the case of a contrary flexure 

which will give all the points of that nature in the locus. 

348. To Jind the points where the locus and given Trajectory intersect 
one another. 

It is clear that at such points 

g = g , and tf = 2 W + 6 
W being any integer whatever. But 

f = ~ 6 = m 6 

2 W* 
= "nT+T 

This is independent of either the Trajectory or Locus. 

349. Tojtnd the number of such intersections during an entire revolution 

Since 6 cannot be > 2 * 
W is < m + 1 and also < m 1 
.-. 2 W is < 2 m. 

Or the number required is the greatest integer in 2 m or - . 

This is also independent of either Trajectory or Locus. 




350. Tojlnd the number and position of the double points of the Locus, 
i. e. of those points where it cuts or touches itself. 

Having obtained the equation to the Locus find its singular points 
whether double, triple, &c. by the usual methods ; or more simply, 
consider the double points which are owing to apses and pairs of equal 
values of C P, one on one side of C V and the other on the other, thus : 

The given Trajectory V W being V 

symmetrical on either side of V W, let 
W 7 be the point in the locus correspond 
ing to W. Join C W 7 and produce 
it indefinitely both ways. Then it is 
clear that W is an apse; also that the 
angle subtended by V v x 7 W 7 is 


= -r X it = \v r 

L. V C y , w being 

the greatest whole number in -^ 


supposes the motion to be in consequentia). Hence it appears that where- 
ever the Locus cuts the line C W 7 there is a double point or an apse, and 

also that there are w + 1 such points. 

Ex. 1. Let -T=T = 2 ; i. e. let the orbit move in conse- 

quentia with a velocity = the velocity of C P. Then L. 
V C y 7 = 0, y 7 coincides with V, and the double points 
are y 7 V, x 7 and W 7 . 

The course of the Locus is indicated by the order of 
the figures 1, 2, 3, 4. 

Ex. 2. Let -p = 3. 

Then the Locus resembles this figure, 1, 2, 3, 
4, 5, 6. showing the course of the curve in which 

V, x 7 , A, W 7 are double points and also apses. 

Ex. 3. Let ^ = 4. 

Then this figure sufficiently traces the Locus. 
Its five double points, viz. V, x 7 , A, B, W 7 are 
also apses. 


Higher integer values of -p will give the Locus 




still more complicated. If -^ be not integer, the 

figure will be as in the first of this article, the 
double points, lying out of the line C V. More- 


over if ^ be less than 1, or if the orbit move in 

antecedentia this method must be somewhat 
varied, but not greatly. These and other curio 
sities hence deducible, we leave to the student. 

351. To investigate the motion of (p) when the 
ellipse, the force being in the focus, moves in ante 
cedentia with a velocity = velocity of C P in 

Since in this case 

G = 

.-. (333) also 

p = 
ov the Locus is the straiht line C V. 

Also (342) 

/F 2 


= it x 



i Y/ i 
v d v ex X d oc 


. . V z OC 


1 a 

1 e 2 

, , axis major , , , , . 

(where -- ^ = 1 ;) and the body stops when 

or when 

g - 1 e. 

Hence then the body moves in a straight line C V, the force increasing 


to of the latus-rectum from the center, when it = max. Then it 


decreases until the distance = or R. Here the centrifugal force pre 

vails, but the velocity being then = max. the body goes forward till the 
VOL. I. R 


distance = the least distance when v = 0, and afterwards it is repelled 
and so on in infinitum. . 

352. Tojind "when the velocity in the Locus = max. or min. 
Since in either case % 

d.v 2 = 2vdv = 

v d v = X d f 
.-. X = 
.-. (336) 

pz v 2 G 2 _ F 2 1 
X+^ x UpA x = o 

Ex. In the ellipse with the force in the focus, we have (342) 
v <" f FZ j_ RG R F S 

= F^-p- + -p- -y 

F 2 R G 2 R F 2 



.-. = R x 


b 2 F 2 G 2 
: a X ~ F 2 

b 2 L 

If G = 0, v = max. when g = , or when P is at the extre- 

a & 

mity of the latus-rectum. 

If F = 2 G, v = max. when e = R . ~^ = R = - - 

4- \j ~ 4 o 

lat. rectum. 

353. To find when the force X in the Locus = max, or min. 
Put d X = 0, which gives (see 336) 

3 p 2 v* G 2 F 2 1 
d X = r X FZ X p 

Ex. In the ellipse 

~ T 2 

and (157) 

pa v 2 

r v , . R 

p" lit 


2 F 2 d g 3 R G 2 d g 3 RF 2 dg _ 

which gives 

3 R F 2 G 2 

Q , y __^ , . 

C r- / ^ 1^ O 


Hence when 

G = 

X = max. when = ~ . 


When g = R, and G = 0. Then 

Y F 2 RF 2 

X = R 2 ~ -RT = 

When F = 2 G, or the ellipse moves in consequentia with the velo 
city of C p ; then 

X = max. when 

3 J^ 4G 2 G 2 j) 
2 4, G 2 : 8 

354. COR. 6. Since the given trajectory is a straight line and the center 
offeree C not in it, this force cannot act at all upon the body, or (336) 

X = 0. 
Hence in this case 

x/ _ P 2 V 2 v G 2 -F 2 1 
~F^- 73 

where P = C V and V the given uniform velocity along V P. 
In this case the Locus is found as in 346. 

355. If the given Trajectory is a circle, it is clear that the Locus of p 
is likewise a circle, the radius-vector being in both cases invariable. 

356. PHOP. XLV. The orbits (round the same center of force) acquire 
the same form, if the centripetal forces by which they are described at equal 
altitudes be rendered proportional. ] 

Let f and f be two forces, then if at all equal altitudes 

f a f 

the orbits are of the same form. 
For (46) 

dt 2 dt 2 S P 2 x QT 

1 1 



QT* SP 2 x 


d 6 2 d V ~ 

d C a d V. 

R 2 


But they begin together and therefore 

6 a (f 

p f/. 

Hence it is clear the orbits have the same form, and hence is also sug 
gested the necessity for making the angles 0, 6 proportional. 


Hence then X , and X being given, we can find -^ such as shall ren 
der the Trajectory traced by p, very nearly a circle. This is done ap 
proximately by considering the given fixed orbit nearly a circle, and 
equating as in 336. 

357. Ex. 1. To Jind the angle between the apsides when X is constant. 
In this case (342) 

X a 1 a -^ a jt j-^ . 

Now making = T x, where x is indefinitely diminishable, and 
equating, we have 

(T x) 3 = F 2 T F 2 x + RG 2 RF 2 

= T 3 3T 2 x + 3Tx 2 x 3 
and equating homologous terms (6) 

T 3 -F 2 T+RG 2 RF 2 = F 2 x (T R) + RG 2 

F 2 = 3T 2 

G_ 2 T 3 T R 
* F 2 ~ R F 2 R 

T 3 _J_ Jl 
= 3 R T 2 R 

T T R _ 3 R 2T 
~ 3 R ~ R 3 R 

= nearly 


since R is = T nearly. 

Hence when F = 180 = it 

the angle between the apsides of the Locus in which the force is constant. 
358. Ex. 2. Let X a g n ~ 3 . Then as before 

(T x) n = F 2 (T x) + RG 2 RF 2 
and expanding and equating homologous terms 

T n = F 2 T + RG 2 RF 2 



But since T nearly = R 

T n_l = G 2 

.*-. ! 

* F 2 ~ n 
and when F = <s 


y (JT i . 
V n 

Thus when n 3 = 1, we have 


When n 3 = 1, n = 2, and y = ^ = 127. 16 . 45". 

When n 3 = ^ , n = ] , and 7 = 2 ?r = 360. 

4 4 

359. Let X oc 

l-> n m _j_ f, n 

Pg Cg 

. Then 

b.(T x) m + c(T x) n = F 2 .(T x)+ R.(G 2 F 2 ) 
and expanding and equating homologous terms we get 
bT m + cT n = F 2 (T R) + RG 2 


bm T 111 - 1 ^ en T 11 - 1 = F 2 . 

But R being nearly = T, we have 
bT m-i4. cT n-i _ G 2 

G 2 bT m - 1 + cT n ~ 1 b T m + c T n 

F 2 " bm T m - 1 + cnT n ~ 1 == mbT m + ncT n 
which is more simply expressed by putting T = 1. Then we have 
G* b+ c 
F 2 ~ mb + nc 
and when F = it 

b + c 

360. COR. 1. Given the L. between the apsides to Jind the force. 
Let n : m : : 360 : 2 7 

: : 180 -K \ y 

.*. y = r 


ButifX oc e p- 

y *~~ 



n 1 

p = t 

. . X 7 gib" 3 

Ex. 1. If n : m : : 1 : 1, 

X oc -L 

as in the ellipse about the focus. 

2. If n : m : : 363 : 360 

3. Ifn : m : : 1 : 2 



And so on. 



Again if X _ _ 


and the body having reached one apse can never reach another. 

IfX oc 

+ q 

.. the body never reaches another apse, and since the centrifugal force 
- , if the body depart from an apse and centrifugal force be > centri 
petal force, then centrifugal is always > centripetal force and the body 
will continue to ascend in infinitum. 

Again if at an apse the centrifugal be < the centripetal force, the centri 
fugal is always < centripetal force and the body will descend to the center. 

The same is true if X a and in all these cases, if 

centrifugal = centripetal 
the body describes a circle. 

361. COR. 2. First let us compare the force -^ c A, belonging to 
the moon s orbit, with 

Fo T> /"I o "D TJ^ 2 

rv \jf ri J; 

A? + A 3 
Since the moon s apse proceeds, (n m) is positive. 


.-. c A does not correspond to n m and . . -^ does not correspond 



j^ A c A 4 a b A m c A p 

A 2 ~ C "A 3 A 3 

l-*c Ft 

.-. X oc A i- a A 02 

1 _ 4 c _ F_ 2 
* l 2 = G 2 

F2 RG 2 RF 2 1 4c , 3cR 


A 3 A 3 
1 4 c , 1 


3 c R 

mn = ~A^~ 

Hence also 

y =T / _ . . &C. &C. &C. 

*V 1 4 c 

362. To determine the angle between the apsides generally. 

f (A) meaning any function whatever of A. Then for Trajectories which 
are nearly circular, put 

f(A) F 2 A + R.(G 2 F 2 ) 
IT A 3 

... f. A = F 2 A + R(G 8 F 2 ) 

f.(T x) = F 2 (T x) + R(G 2 F 2 ) 
But expanding f (T x) by Maclaurin s Theorem (32) 

u = f (T x) =U U x + U"^ 2 &c. 
t J, U &c. being the values of u, -T , -T &c. 

(1 X. Cl. X- 

when x = 0, and therefore independent of x. Hence comparing 
homologous terms (6) we have 

U = F 2 T+R(G 2 F z ) 

U = F 2 




Also since R = T nearly 
U = TG 2 

1 U 

F ~~ T . U 7 

Hence when F =r v, the angle between the apsides is 


N U 
making T = 1. 

Ex. 1. Let f (A) = b A m + c A n = u 



= mbA m - 1 +ncA n - 1 . 

Hence since A = T when x = 

U = fT = b T ra + c T n 
U = mbT" 1 - 1 + n c T 11 - 1 
G 2 b T m -f- c T n 
F 2 " mbT 

G_ 8 b+ c 

F 2 - m b + n c 


7 = 

b + c 
m b + n c 


as in 359. 

Ex. 2. Let f . (A) = b A m + c A n + e A r + &c. 

j^ = mbA m - 1 + ncA n - 1 + reA r - 1 
.-. U = bT m cTeT r &c. 


T X U = m b T m + n c T " + r e T r + &c. 

- b Tm + c T " + e Tr + &c - 
F 2 mbT 


when T = 1. 


7 = 

b + c + e 

m b -f- n c -f r e + . . 




Ex. 3. Let -*4* = a A = u. 

Here (17) 


j^ = A 2 a A x(3 + Ala) 


U = Ta T x (3 -f Tla) 
T X U = T 3 a T (3 + Tla) 
G 2 1 

F 1 =: T X (3 + T 1 a) 
and when T = 1 

G 2 1 


F 2 ~ 3 +la 

.*, <y sr r / _ 

V3 + la 

Hence if a = e the hyperbolic base, since 1 e = 1, we have 

Ex. 4. Let f (A) = e A = u. 


j~ e 
d x 

.-. U = e T 

T . U = T e T 

.*. 7 = T. 
Ex. 5. Let ti^i = sin. A. 

u = f(A) = A 3 sin. A 
.-. U = T 3 sln. T 

^ = 3A 8 sin. A + A 3 cos. A 
.-. T U = 3 T 3 sin. T + T 4 cos. T 
. G_ 2 _ _ sin. T 
F 2 ~3sin.T+ t cos. T 

sin. T 
sin.T + Tcos.T* 


" 4"- 


363. To prove that 

bA m +cA n _ 1 mb + nc_ 3 

~K~ 3 ~b~+~c 

= b + c (mb + nc)x+ &c, 

1 /, mb+nc 

= f i I 1 C-T x + &c 

b + c v b + c 

1 mb + n c 

~b + c v 

1 mb + nc 

= b + c* 

364. To Jind the apsides when the eccentricity is infinitely great. 


2 q : V (n + 1) : *. velocity in the curve : velocity in the circle of the 
same distance a. 

Then (306) it easily appears that when F g n 

n + 3 


g V (a n + 1 f n + 1 )g 2 q 2 a n + 1 (a 2 

gives the equation to the apsides, viz. 

(a + 1 g n + l )g z q a"-*- 1 (a 2 ? 2 ) = 
whose roots are 

a (and a when n is odd) and a positive and negative quantity (and when 
n is odd another negative quantity). 
Now when q = 

two of whose roots are 0, 0, and the roots above-mentioned consequently 
arise from q, which will be very small when q is. 
Again since 

when q and are both very small 



s = q- 

.. the lower apsidal distance is a q. 
A nearer approximation is 

g= + . 1SL_. 


n + 3 

g v/(^_a 2 q 2 + /3) X Q 

where /S contains q 4 &c. &c., and this must be integrated from g = b to 

g = a (b = a q). 

But since in the variation off from b to c, Q may be considered con 
stant, we get 

6 = sec. - . J- + C = sec. - . . 
aq a q 


if 3 it 5 it a , . 
7 - -Q -g- > -g- > &c - ultimately 

the apsidal distances required. 
Next let 

Then again, make 

v : v in a circle of the same distance : : q V 2 : V (n 1) 
and we get (306) 

and for the apsidal distances 

which gives (n > 1 and < 3) 





a tj f n 3n 

a q d 

2 a 3 - " + /?) x Q 

V Q J ^ */ t n 3 n r"g~3^TiT 



3 n 

g 3 

7 3 n 3 ~" 3 n 3 n 

qa 2 

Hence, the orbit being indefinitely excentric, when 

F oc g . ... we have . . . . *y = -^ 

1 T 


any number < 1 2 

Foe- . . . 7 = 

r oc y ^ 

g number between 1 and 2 2 

FpWs ?>* 

But by the principles of this 9th Section when the excentricity is inde 
finitely small, and F a n 

y = V (n + 3) 
(see 358), and when 


V (3 n) 

Wherefore when n is > 1 
7 increases as the excentricity from 

V (3 + n) t0 2 
When F oc g 

7 is the same for all excentricities. 

When F a g 1 "? 
7 decreases as the excentricity increases from 


n) 2 

which is also true for F oc . 



decreases as the excentricity increases from 


; tO 

V(3 n) 3 n 

When F oc -L 

When F oc 

2 <3 

7 increases with the excentricity from 


V(3_n) 3 n* 
If the above concise view of the method of rinding the apsides in this 
particular case, the opposite of the one in the text, should prove obscure ; 
the student is referred to the original paper from which it is drawn, viz. 
a very able one in the Cambridge Philosophical Transactions, Vol. I, 
Part I, p. 179, by Mr. Whewell. 

365. We shall terminate our remarks upon this Section by a brief dis 
cussion of the general apsidal equations, or rather a recapitulation of re 
sults the details being developed in Leybourne s Mathematical Repository, 
by Mr. Dawson of Sedburgh. 

It will have been seen that the equation of the apsides is of the form 

x n Ax m B = (1) 

the equation of Limits to which is (see Wood s Algeb.) 

nx n-i mAx m - 1 = (2) 

and gives 

/" m A \ n 
x = ( A) 
V n / 



If n and m are even and A positive, * has two values, and the number 
of real roots cannot exceed 4 in that case. 

Multiply (1) by n and (2) by x and then we have 

(m -^ n) A x m nB = 
which gives 

B -v "in" 

and this will give two other limits if A, B be positive and m even ; and if 
(1) have two real roots they must each = x. 


If m, n be even and B, A positive, there will be two pairs of equal roots. 
Make them so and we get 

n _ /nx 


n n-m 

which will give the number of real roots. 

(1). If n be even and B positive there are two real roots. 

(2). If n be even, m odd, and B negative and (M), the coefficient to 
A n , negative, there are two ; otherwise none. 

(3). If n, m, be even, A, B, negative, there are no real roots. 

(4). If m, n be even, B negative, and A positive, and (M) positive there 
are four real roots ; otherwise none. 

(5). If m, n be odd, and (M) positive there will be three or one real. 

(6). If m be even, n odd, and A, B have the same sign, there will be 
but one. 

(7). If m be even, n odd, and A, B have different signs, and M s sign 
differs from B s, there will be three or only one. 

(8). If 

x n _j_ An m B = 

is positive, and it must be > B, and the whole must be positive. 

x n Ax m + B = 
the result is negative. 


366. PROP. XLVI. The shortest line that can be drawn to a plane 
from a given point is the perpendicular let fall upon it. For since 
Q C S = right L^ any line Q S which subtends it must be > than either 
of the others in the same triangle, or S C is < than any other S C. 

A familiar application of this proposition is this : 

367. Let S Q be a sling with a body Q at the end of it, and by the hand 
S let it be whirled so as to describe a right cone whose altitude is S C, and 
base the circle whose radius is Q C; required the time of a revolution. 

Let S C = h, S Q = 1, Q C = r = VI 2 h 2 . 


Then if F denote the resolved part of the tension S Q in the direction 
Q C, or that part which would cause the body to describe the circle P Q, 
and gravity be denoted by 1, we have 
F : 1 : : r : h 

But by 134, or Prop. IV, 

p x p _ ^^ * \ A. v p 2 

J. /\ JL i S\ A 

g h 

A**.7/i (1) 

<\ or 

the time required. 

If the time of revolution (P) be observed, then h may be hence obtained. 

If a body were to revolve round a circle in a paraboloidal surface, whose 
axis is vertical, then the reaction of the surface in the direction of the 
normal will correspond to the tension of the string, and the subnormal, 
which is constant, will represent h. Consequently the times of all such 
revolutions is constant for every such circle. 

368. PROP. XLVII. When the excentricity of the ellipse is indefi 
nitely diminished it becomes a straight line in the limit, &c. &c. &c. 

369. SCHOLIUM. In these cases it is sufficient to consider the motion 
in the generating curves.] 

Since the surface is supposed perfectly smooth, whilst the body moves 
through the generating curve, the surface, always in contact with the 
body, may revolve about the axis of the curve with any velocity whatever, 
without deranging in the least the motion of the body ; and thus by ad 
justing the angular velocity of the surface, the body may be made to trace 
any proposed path on the surface. 

If the surface were not perfectly smooth the friction would give the 
body a tangential velocity, and thence a centrifugal force, which would 
cause a departure from both the curve and surface, unless opposed by 
their material ; and even then in consequence of the resolved pressure a 
rise or fall in the surface. 

Hence it is clear that the time of describing any portion of a path in a 
surface of revolution, is equal to the time of describing the corresponding 
portion of the generating curve. 

Thus when the force is in the center of a sphere, and whilst this force 
causes the body to describe a fixed great-circle, the sphere itself revolves 
with a uniform angular velocity, the path described by the body on the 
surface of the sphere will be the Spiral of Pappus. 


370. PROP. XLVIII and XLIX. In the Epicycloid and Hypocycloid, 


s : 2 vers. : : 2 (R + r) : R 

where s is any arc of the curve, s the corresponding one of the wheel, and R 
the radius of the globe and r that of the wheel, the + sign being used for 
the former and in the Hypocycloid. (See Jesuits notes.) 


If p be the perpendicular let fall from C upon the tangent V P, we 
have from similar triangles in the Epicycloid and Hypocycloid 

PY: CB:: VY: VC 


p 2 n 2 R 2 . . /T> JL 9 ,N 2 n 2 . / U _i_ O -\2 

J JL v I L I 1 * 1 j Y* * \ / 

which gives 

n 2_ / R J- O r \ 2 v S ** / 1 \ 

JJ \i\,-^TA IJ * / r> J_ Q \ 2 T> 2 \ l l 

Now from the incremental figure of a curve we have generally 
d s 



p 2 ) 



4-0 r \ 2 _ .2? 

,.ds = 


and integrating from 

s = 0, wheng = R 
we get _ 

V (R + 2r) 2 

+ 2r ) 8 R 8 V(R2 r) 8 

which is easily transformed to the proportion enunciated. 

The subsequent propositions of this section shall now be headed by a 
succinct view of the analytical method of treating the same subject. 

371. Generally, A body being constrained to move along a given curve by 
known forces, required its velocity. 

Let the body P move along the curve 
P A, referred to the coordinates x, y 
originating in A ; and let the forces be 
resolved into others which shall act 
parallel to x, y and call the respective 
aggregates X, Y. Besides these we 
have to consider the reaction (R) of the 


curve along the normal P K, which being resolved into the same direc 
tions gives (d s, being the element of the curve) 

n dx d y 

It -3 , and R -r* . 
ds ds 

Hence the whole forces along x and y are (see 46) 

d l x 

2 =X + 

LV ds 
Again, eliminating R, we get 

2dxd 2 x + 2dyd 2 y 

jji * l = 2Xdx + 2Ydy 


d x z + dy 2 


. . v*= 2/(Xdx+ Ydy) (]) 

Hence it appears that The velocity is independent of the reaction of the 

372. If the force be constant and in parallel lines, such as gravity, and 
x be vertical ; then 


Y = 
and we have 

v 2 = 2/-gdx 

= 2g(c x) 

= 2g(h x) 

h being the value of x, when v = ; and the height from which it begins to 

373. To determine the motion in a common cycloid, when the force is gravity. 
The equation to the curve A P is 


r being the radius of the generating circle. 


.-. ds = dx I- 
V x 

VOL. I. 




- / r 
-x ~ V 

. A/(h-xj ~ g V (hx-x 2 ) 

t being = 0, when x = h. 

Hence the whole time of descent to the lowest point is 
T , r 


which also gives the time of an oscillation. 

374. Required the time of an oscillation in a small circular arc. 


y = V (2rx x 2 ) 

r being the radius of the circle, and 

__ rd x 
S - V (2rx x 2 ) 

*- dt - v 2g V (h x) 


x)(2rx x 2 )} 

r dx 

X V {(hx x z )(2r x)} 

to integrate which, put 



d 9 - 2 A/Oix x*j 

and since 

= 2r(l a 2 sin. 

d * = V 

Now since the circular arc is small, h is small ; and therefore 3 is so. 
And by expanding the denominator we get 



and integrating by parts or by the formula 

fd & . sin. m = cos. 6 sin. m - J 6 A fdd sin. m -%Q 

m m J 

and taking it from 

d = to 6 = -J- 
we get 

rr -I 

f. d 6 sin. m 6 = ^ f,dd sin. m ~ 2 & 
m Jl 

the accentedy denoting the Definite Integration from 6 = 0, to 6 = . 
In like manner 

f. d 6 sin. ra - 2 = ~- /~ d sin. m - * 
m 2 <// 

and so on to 


(m 1) (m 3) 1 r 

7, d Sin. m = V -T ^rr 1 X -5- 

m (m 2) 2 2 


/. d d f = 0") 

I , , .. r? 5~; I rom I 

/ x V (1 5 2 sin. 2 6 & _ _* >- 

is the same as 

V (1 3 s sin. 2 0) from 
whence then 

CJ* | 

= oi 

and taking the first term only as an approximate value 

t = ~2"tJ ~~^ 


which equals the time down a cycloidal arc whose radius is -7- 


If we take two terms we have 

- I?-(14 
2 V g V 4 



375. To determine the velocity and time in a Hypocycloid, the force 
tending to the center of the globe and g. 

By (370) 

the equation to the Hypocycloid is 

R 2 P Z 

by hypothesis. 

Now calling the force tending to the center F, we have 

X = F x - ,Y = F 

...v 2 = C 2/Fd f 
But by the supposition 



Cl L ^ 

To integrate it, put 
2 D = u 8 


V R 2 D 2 d u 

dt = - ; 

V^a V (h 2 D 2 u 2 ) 

V (R 2 D 2 ) /^ _ D 2 

< v : pcm 1 / = 

RVp Vh 2 D 2 

Hence making = D, we have 

Oscill. cr /R 2 D 


376. Since h does not enter the above expression the descents are 

We also have it in another form, viz. 

I- /rJi J__A 

2 " A/ VR^ RV/ 



If R ^ = g or force of gravity and R be large compared with b, 


the same as in the common cycloid. 

377. Required to Jind the value of the reaction R, when a body is con 
strained to move along a given curve. 

As before (46) 

d 2 x r. d y 

_ Y R 

- i 



. Xdy Ydx , dyd 2 x dxd 8 y 
"> j~I T j * 2 J 


But if r be the radius of curvature, we have (74) 

ds 3 

~ dyd x dxd 2 y 

dt 2 ds 

B Ydx Xdy^ ds 2 
rt i r ..j i2 

d s 

rdt ! 

Another expression is 

Y d x X d y v^ 


Ydx Xdy 


+ P 

<p being the centrifugal force. 

If the body be acted on by gravity only 

ds + rdt ! 






If the body be moved by a constant force in the origin of x, y, we have 

xdy y d x 
\ d x X d y = F 

J * 

= F i d 6. 



[SECT. X. 


xdy y d x = g 2 d 

i? . , 

.-. R = 



d s r d t 



_ FjjH 
d s 

378, To Jind the tension of the string in the oscillation of a common 



dy = 

d s = 

d s ^ r d t 

;2 a x 



d_y _ 2 a x 
d s ~ V WIT 

r - 2 V 2 a V (2 a x) 
~~ = 2 g (h x) 

^R = g J*Z 

& V 2 a 

= g 

__ _ 

\/2a V(2 a x) 
2 a + h 2x 

When x =r h 

When x = 

2 ax) 

R = . 


a 2 2 a h) 

(2 a) 

2 a + h 


K rr 
J.V . 

2 a 

When moreover h = 2 a, the pressure at A the lowest point is = 2 g. 

379. To Jind the tension "when the body oscillates in a circular arc by 



dv - (C ~ x) d X 

y A/(2cx x*) 

c d x 
d s = 

V (2 ex x 2 ) 
d y _ c x 
d x c 

r = c 

= g 

When x = 

c c 

c + 2 h 3 x 

v c + 2 h 




r= 3 g or h = c. 
If it fall through the whole semicircle from the highest point 

h = 2c, 

R = 5g 

or the tension at the lowest point is five times the weight. 
When this tension = 0, 

c+2h 3x = 0, orx = ^ 

A body moving along a curve whose plane is vertical will quit it when 

R = 
that is when 

c + 2h 
x - 

and then proceed to describe a parabola. 

380. To Jind the motion of a body upon a surface of revolution, when 
acted on by forces in a plane passing through the axis. 

Referring the surface to three rectangular axes x, y, z, one of which (z) 
is the axis of revolution, another is also situated in the plane of forces, and 
the third perpendicular to the other two. 

Let the forces which act in the plane be resolved into two, one parallel 
to the axis of revolution Z, and the other E, into the direction of the 
radius-vector, projected upon the plane perpendicular to this axis. Then, 




[SECT. X. 

calling this projected radius g, and resolving the reaction R (which also 
takes place in the same plane as the forces) into the same directions, these 
components are 

R ds 

d s 

supposing ds= V / (dz 
of jf is 

F + R 

and the whole force in the direction 



and resolving this again parallel to x and y, we have 

d 2 x _ 

~ ds 

F j 
~- " 



= - 

Hence we get 

xd g y y d 2 x _ _ d xdy y dx 

dt 2 
dxd 2 x + dy d 2 y+dzd 2 z 

Which, since 

x d x+ y dy 

d s 

d s 

xdx + y dy _ d 



dz 2 _dz 2 dg 2 
dt 2 ~" d * d t 2 



and from the nature of the section of the surface made by a plane passing 
through the axis and body, ~ is known in terms of g. Let therefore 


and we have 

d_z_ 2 2 dg 2 
d t 2 ~ dt 2 * 
Also let the angle corresponding to g be 0, then 

xdy ydx = g 2 d 

dx 2 + dy 2 = dg 2 -fg 2 d0 2 , 
and substituting the equations (2) and (3) become 

Integrating the first we have 

P 2 d = h d t 

h being the arbitrary constant. 

The second can be integrated when 

2 Fdg 2Zdz 

is integrable. Now if for F, Z, z we substitute their values in terms of e, 
the expression will become a function of and its integral will be also a 
function of g. Let therefore 

/(F d g + Z d z) = Q 
and we get 

dp 2 p 2 d 6 Z dp 2 


which gives, putting for d t its value 

~o~vv\ i i jj . (6) 

Hence also 

Ol L 7 f-. c\~~s~\\ o I o^ ( ) 

V \ (c 2 Q) g 2 h *} v 

If the force be always parallel to the axis, we have 

F = 
and if also Z be a constant force, or if 

we then have 

Q = /Z d z = g z (8) 


Z being to be expressed in terms of g. 

381. Tojind under what circumstances a body will describe a circle on a 
surface of revolution. 

For this purpose it must always move in a plane perpendicular to the 
axis of revolution ; g, z will be constant; also (Prop. IV) 
cos. 6 = x 

d 2 x _ g cos. 6 d 6 z 
dT 2 " : dt 2 


dt 2 
Hence as in the last art. 

. 2 

If the force be gravity acting vertically along z, we have 
yj _ d z 

Hence may be found the time of revolution of a Conical Pendulum. 
(See also 367.) 

382. To determine the motion of a body moving so as not to describe a 
circle, when acted on by gravity. 

Q = gz 

C 2 Q = 2g. (k z) 
k being an arbitrary quantity. 

g 2 = 2 r z z 2 
z being measured from the surface. 

.. cl g = (r z) d z 

_ * r ~ 

+ P - + (r z) z ~ (r z) 


Hence (380) 



In order that 

the denominator of the above must be put = ; i. e. 

2 g (k z) (2 r z z 2 ) h 2 = 

h 2 
z 3 (k + 2r)z 2 + 2krz - = 

which has two possible roots ; because as the body moves, it will reach 

one highest and one lowest point, and therefore two places when 

Hence the equation has also a third root. Suppose these roots to be 

", ft 7 

where a is the greatest value of z, and j3 the least, which occur during the 
body s motion. 

(2g) V {(_ z ).(z j8)(y z) 

To integrate which let 



d 6 = 

_ cfrz 

= 2V {( z) (z - 

.-. z = 13 + (a jg) sin. l 6 

y z = 7 {|3 + ( /S) sin. * 

= (7 P) U a sin. ^, 


.-. d t = 

V2g. (y /3). 
which is to be integrated from z = /3, to z = a ; that is from 

6 = to 6 = ~ 

this expanded in the same way as in 374 gives 
t= va 2r _^: 

which is the time of a whole oscillation from the least to the greatest 


h d t h d t 

= 2 ~~ = 2 r z z 2 

and & is hence known in terms of z. 

383. A body acted on by gravity moves on a surface of revolution whose 
axis is vertical : when its path is nearly circular, it is required to find the 
angle between the apsides of the path projected in the plane o/ x, y. 

In this case 

and if at an apse 

o = a, z = k 
we have 
(C 2gk)a z h 2 := 

... C = ^ + 2 g k. 

Hence (380) 

d 6 = 


V(l +p)~,"* 

Let = + 

? a 



<i a 2g (k z) h 

Q U 

It is requisite to express the right-hand side of this equation in terms 
of w 

Now since at an apse we have 

w = 0, z = k, and g = a 
we have generally 

dz , d 2 z w 2 

z = k + d-. w + dV 2 -i72 + &c - 

the values of the differential coefficients being taken for 

w = (see 32) 

d z = p d f z= p 2 d w 
d 2 z = 2p^dgdw g d w d p 
or, making 

d p = q d g 

d 2 z = (2p + qg)dgdw = (2 p + q g) f 3 d 2 . 

And if p/ and q/ be the values which p and q assume when w = 0, 
=r a, we have for that case, 

^f,= (2p,+ q ,a)a> 

Z = k p 7 a 2 w + (2p + q,a) a 3 . ^ Sac. 

wV = + + w 2 
/ "a 2 a 


1 _ /I , \ 2 

e 2 " v a ; 

2g(k_z)-h 2 (-l_^) 


2 g (p, a 2 co _ (2 p, + q, a) a 3 . ^ + &c.)- h *(^ + **). 

But when a body moves in a circle of radius = a, we have 

h2 = Sf s P = ga p, 

in this case. And when the body moves nearly in a circle, h 2 will have 
nearly this value. If we put 

h 2 = (1 + a)ga 3 P/ 
we shall finally have to put 

5 = 


in order to get the ultimate angle when the orbit becomes indefinitely near 
a circle. Hence we may put 



in which the higher powers of u may be neglected in comparison of u 2 ; 
. d " 2 _ _ ga 3 (3 P/ + q/ a)q. 2 _ (3 P/ + q/ a)^_ 2 
d^ 2 " h 2 (1 + p 2 ) P/ (1 + P 2 ) 

_ (3 p,+ q/ a) a 2 

P/(l +P/ 2 ) 

again omitting powers above u z : for p = p / + A u + &c. 
Differentiate and divide by 2 d ca, and we have 

suppose ; of which the integral is taken so that 

6 = 0, when u = 

u = C sin. 6 V N. 

And 01 passes from to its greatest value, and consequently g passes 
from the value a. to another maximum or minimum, while the arc 6 V N 
passes from to <r. Hence, for the angle A between the apsides we have 

A V N v or A = r^j 
V N 


N - 3 P/ + q/ a . 

384. Let the surface be a sphere and let the path described be nearly a 
circle : to Jind the horizontal angle between the apsides. 

Supposing the origin to be at the lowest point of the surface, we have 
z = r V (r 2 e ") 
d z g 

" P - V( r _ a -J 


4 r 2 3 a 

/. N = = 

Hence the angle between the apsides is 

A - 


V(4r 2 3 a 2 ) 

The motion of a point on a spherical surface is manifestly the same as 
the motion of a simple pendulum or heavy body, suspended by an inex- 
tensible string from a fixed point ; the body being considered as a point 
and the string without weight. If the pendulum begin to move in a ver 
tical plane, it will go on oscillating in the same plane in the manner al 
ready considered. But if the pendulum have any lateral motion it will 
go on revolving about the lowest point, and generally alternately ap 
proaching to it, and receding from it. By a proper adjustment of the velocity 
and direction it may describe a circle (134) ; and if the velocity when it 
is moving parallel to the horizon be nearly equal to the velocity in a cir 
cle, it will describe a curve little differing from a circle. In this case we 
can find the angle between the greatest and least distances, by the for 
mula just deduced. 

. _ *_r 

: V (4 r a 3 a 8 ) 

if a = 0, A = 7- , the apsides are 90 from each other, which also ap- 


pears from observing that when the amplitude of the pendulum s revolu 
tion is very small, the force is nearly as the distance ; and the body de 
scribes ellipses nearly ; of which the lowest point is the center. 

If a = r, 

A = * = 180 

this is when the pendulum string is horizontal ; and requires an infinite 

If a = - ; so that the string is inclined 30 to the vertical ; 

A = J _ =99 50 . 
V 13 


If a 2 = -jr- ; so that the string is inclined 45 to the vertical ; 

A = *r J | = J13. 56 . 

3 r 2 

If a 2 _ . so th a t the string is inclined 60 to the vertical ; 


A = -^z = 136 nearly. 

385. Let the surface be an inverted cone, with its axis vertical : to find 
the horizontal angle between the apsides when the orbit is nearly a circle. 

Let r be the radius of the circle and 7 the angle which the slant side 
makes with the horizon. Then 

z = g tan. 7 
p = tan. 7 


tan. 7. sec. * 7 


A = 

cos. 7 V 3 

If 7 = 60 

A = 
386. Let the surface be an inverted paraboloid whose parameter is c. 

= c z 
d z 


6_a 2a 


If a = - , or the body revolve at the extremity of the focal ordinate, 


N = 2 


387. When a body moves on a conical surface, acted on by a force tend 
ing to the vertex ; its motion in the surface will be the same., as if the sur 
face were unwrapped, and made plane, the force remaining at the vertex. 

Measuring the radius-vector (g) from the vertex, let the force be F, 
and the angle which the slant side makes with the base = 7 : then 
z = g tan. 7 
p = tan. 7 
1 + p 2 = sec. 2 7 

Q=/(Fdg + Zdz) =/F dg . 
Hence (380) 

i A _ sec - 7 h d g 


or putting 

h cos. 7 for h 
d tf sec. 7 for d 6 

g cos. 7 for g 
we have 

h dg 

Now d (f is the differential of the angle described along the conical sur 
face, and it appears that the relation between V and / will be the same as 
in a plane, where a body is acted upon by a central force F. For in that 
case we have 

h 2 d t> 2 h 2 1 

a ? j. _ I 9 F d P 

4 d ^ 2 ^ ? 2 J " 

and integrating 

h 2 d g 2 h 2 

/ 4 J / 2 +7^ = ^ 

^which agrees with the equation just found. 

388. When a body moves on a surface of revolution, to Jind the reac 
tion R. 

Take the three original equations (380) and multiply them by x d z, 
y d 2, g d f ; and the two first become 

x d 8 x d z ^ _ F x 2 d z _ R d z 2 x 2 
dt 2 T~ " "dT 7 

y d*y dz F y 2 d z R dz 2 "y 2 

dt 2 ? l ds -y 

VOL. 1. T 


add these, observing that 

and we have 

<xd 2 x+yd 2 y)dz _ _ _ d z* 

"dT 2 " WUF 

Also the third is 

Subtract this, observing that dz 2 + d g 2 = ds 2 , and we have 
(xd 2 x + yd 2 y)dz gdgd 2 z 

dt 2 

s (Z d s F d z) R | d s. 

x 2 + y 2 = g 2 
xdx+ydy = gdg 
xd 2 x + yd 2 y + dx 2 + dy 2 = gd 2 g + dg 2 . 


(dg 2 dx 2 dy 2 ) dz gd z d 2 g gdgd 2 z 
dt 2 dt 2 

g (Z d g F d z) R g d s 

dg 2 = ds 2 dz 2 . 

R _ Z d g F d z dgd 2 z dzd 2 g 

ds dt 2 ds 

(dx 2 + dy 2 + dz 2 ds 2 )dz 

gdt 2 d s 
Now if r be the radius of curvature, we have (74) 

ds 3 

: dgd 2 z_dzd 2 g 

d x 2 + dy 2 + d z 2 = d tf 2 
a being the arc described. 

Z d g F d z d s 2 
ds h FdT 1 

dg 2 ds 2 dz 

1 gdt 2 d~s 
Here it is manifest that 

d s 2 


is the square of the velocity resolved into the generating curve, and that 

d 2 d s 2 

dt 2 

is the square of the velocity resolved perpendicular to g. The two last 
terms which involve these quantities, form that part of the resistance 
which is due to the centrifugal force ; the first term is that which arises 
from the resolved part of the forces. 

From this expression we know the value of R ; for we have, as before 


da 2 _ds 2 _ g*dd ~ __h* 

~ dt 2 TT 2 " = r* 


|j-=C--2/(F dH-Zdz) 
h 2 

389. To find the tension of a pendulum moving in a spherical surface. 

C 2/(F dg + Zdz) = 2g(k-,z) 
* - V (2rz z 2 ) 

d _ r z 

<Tz ~~ V (2rz z 2 ) 

d s r 

de r z 

d s _ r r 

d~z ~ V(2rz z 2 ) = 7 

2g(k z) -- ~ 2 

R = g( r - z ) + _: __ : __ ii 

r r 

_g(r+2k 3z) 


and hence it is the same as that of the pendulum oscillating in a vertical 
plane with the same velocity at the same distances. 

390. To find the Velocity , Reaction, and Motion of a body upon any 
surface whatever. 

Let R be the reaction of the surface, which is in the direction of a nor 
mal to it at eacli point. Also let i, s , t" be the angles which this normal 


+ _ __ __ + . . 

j 3 r 



[SECT. X. 

makes with the axes of x, y, z respectively ; we shall then have, consider 
ing the resolved parts of R among the forces which act on the point 

d 2 x 
-- = X + R cos. 

d 2 z 
dT 2 

= Z+R.cos./ 

Now the nature of the surface is expressed by an equation between 
x, y, z: and if we "suppose that we have deduced from this equation 
dz =pdx + qdy 

, dz , d z 

where p = ~j and q = -. . 
dx dy 

p and q being taken on the supposition of y and x being constants respec 
tively ; we have for the equations to the normal of the points whose co 
ordinates are 

x, y, z 
x x + p (z z) =0 

y-y + q(z f -z) = 

x , y , T! being coordinates to any point in the normal (see Lacroix, 
No. 143.) 

Hence it appears that if P K be the normal, 
P G, P H its projections on planes parallel to 
x z, y z respectively. 
The equation of P G is 

x x + p . (z z) = 0, 
and hence 


G N = p . P N. 
Similarly the equation of P H is 

y y + q( z z ) = 


HN+ q.PN = 

H N = q . P N. 
And hence, 


:. t = cos. K P h = 




NG e + HN*) 



V (\ +p + i*) 

cos. t = cos. K P g = p- 

V(PN 2 + NG 2 + HN 2 ) 


V (1 + p 2 + q 2 ) 
Whence, since 
cos. 2 -f cos. 2 E + cos. s t" = 1 

COS. 2 ?" = V ( 1 COS. 2 e COS. 2 e ) 

__ 1 

Substituting these values; multiplying by d x, d y, d z respectively, in 
the three equations ; and observing that 

dz pdx q d y = 
we have 

dxd 8 x + dyd g y + d z d * z , 
-T-ri = Xdx + Ydy + Zdz 

Cl I * 

and integrating 

dx s + dy* + dz 2 
grfi -2/(Xdx+ Ydy-f Zdz) 

L4. L * * 

and if this can be integrated, we have the velocity. 

If we take die three original equations, and multiply them respectively 
ty P, q, and 1, and then add, we obtain 

- P X- 

d z = p d x + q d y. 

^ 5 = D ^ x _L a ^J y 4. dp dx + d q d y 

d t 2 P d t " q d t 2 "*" "dT 8 "" 

Substituting this on the first side of the above equation, and takinr 
the value of II, we find 

R P^ + q Y Z ^1 p d x + d q d y 

If in the three original equations we eliminate R, we find two second 
differential equations, involving the known forces 

X,Y, Z 

T 3 


and p, q, which are also known when the surface is known, combining 
with these the equation to the surface, by which z is known in terms of 
x, y, we have equations from which we can find the relation between the 
time and the three coordinates. 

391. To find the path which a body mil describe upon a given surface, 
when acted upon by no force. 

In this case we must make 

X, Y, Z each = 0. 

Then, if we multiply the three equations of the last art. respectively by 

(qdz + dy), pdz + dx, qdx pdy 
and add them, we find, 

(qdz + dy)d 2 x + (pdz+dx) d 2 y+ (qdx pdy) d 2 z 

/- (q d z + d y) cos. s ~\ 
= R d t 2 -| + (pdz + dx) cos. t t 
v. + (qdx pdy) cos. t") 
or putting for cos. e, cos. t , cos. *" their values 
Rdt 2 

Hence, for the curve described in this case, we have 

(p d z + d x) d 2 y = (p d y q d x) d 2 z+ (q d z + d y) d 2 x. 
This equation expresses a relation between x, y, z, without any regard 
to the time. Hence, we may suppose x the independent variable, and 
d 2 x = ; whence we have 

(pdz + dx) d 2 y = (pdy qd x)d 2 z. t 
This equation, combined with 

dz=rpdx + qdy, 

gives the curve described, where the body is left to itself, and moves along 
the surface. 

The curve thus described is the shortest line which can be drawn from 
one of its points to another, upon the surface. 

The velocity is constant as appears from the equation 

v = 2/(Xdx + Ydy + Zdz). 

By methods somewhat similar we might determine the motion of a point 
upon a given curve of double curvature, or such as lies not in one plane 
when acted upon by given forces. 

392. To fold the curve of equal pressure, or that on which a body descend 
ing by the force of gravity, presses equally at all points. 



Let A M be the vertical abscissa = x, M P the hori 
zontal ordinate = y ; the arc of the curve s, the time t, 
and the radius of curvature at P = r, r being positive 
when the curve is concave to the axis ; then R being the 
reaction at P, we have by what has preceded. 

R = ~dT + r~TF (1) 

But if H M be the height due to the velocity at P, 
A H = h, we have 





= 2g(h-x). 

Also, if we suppose d s constant, we have (74) 
d s d x 

and if the constant value of R be k, equation ( 1 ) becomes 

k = S d y _ 2g(h--x)d 2 y 

d s d s d x 

k dx , , d 2 v dy 

d x 


The right-hand side is obviously the differential of 
V (h 

hence, integrating 

k d v 

g * d s 

d_y = k C 

: g - V (h x) 


If C = 0, the curve becomes a straight line inclined to the 
which obviously answers the condition. The sine of inclination 

In other cases the curve is found by equation (2), putting 

V(dx 2 + dy 2 ) for ds 
and integrating. 

If we differentiate equation (2), d s being constant, we have 
d*y_ Cdx 

d S n /!_ 


is - 

And if C be positive, r is positive, and the curve is concave to the axis. 




[SECT. X. 

We have the curve parallel to the axis, as at C, when ^ = 0, that is, 

u s 

; when 

, k C 

when = ., 

g V (h x 

x = 

When x increases beyond this, the curve approaches the axis, and -r-^ 

U -V 

is negative ; it can never become < 1 ; hence B the limit of x is 
found by making 



x =h 




If k be < g, as the curve descends towards Z, it approximates perpe- 

tually to the inclination, the sine of which is . 


If k be > g there will be a point at which the curve becomes horizontal. 

C is known from (2), (3), if we knew the pressure or the radius of cur 
vature at a given point. 

If C be negative, the curve is convex to the axis. In this case the part 
of the pressure arising from centrifugal force diminishes the part arising 
from gravity, and k must be less than g. 

393. To find the curve which cuts a given assemblage of curves, so as to 
make them Synchronous, or descriptive by the force of gravity in the same 

Let A P, A P , A P", &c. be curves of the 
same kind, referred to a common base A D, 
and differing only in their parameters, (or the 
constants in their equations, such as the radius 
of a circle, the axes of an ellipse, &c.) 

Let the vertical A M = x, M P (horizontal) 
= y ; y and x being connected by an equation 
involving a. The time down A P is 

the integral being taken between 

x = and x = A M ; 
and this must be the same for all curves, whatever (a) may be. 


Hence, we may put 


k being a constant quantity, and in differentiating, we must suppose (a) 
variable as well as x and s. 


d s = pdx 

p being a function of x, and a which will be of dimensions, because d x, 
and d s are quantities of the same dimensions. Hence 

f P dx _ k 

J V (2gx)~ 
and differentiating 

Now, since p is of dimensions in x, and a, it is easily seen that 

r p 

J V2 

is a function whose dimensions in x and a are , because the dimensions 
of an expression are increased by 1 in integrating. Hence by a known 
property of homogeneous functions, we have 

k p V x 
q ~2a~a V (2g) 
substituting this in equation (2) it becomes 

pdx k d a p d a V x __ .. 

V (2gx) H " ~2l a V (2 g) ~ 

in which, if we put for (a) its value in x and y, we have an equation to the 
curve P P P". 

If the given time (k) be that of falling down a vertical height (h), we 

* = J, 

and hence, equation (3) becomes 

p(adx xda) + da V (h x) = . . . . (4) 

Ex. Let the curves A P, A P , A P" be all cycloids of which the bases 
coincide with A D. 

Let C D be the axis of any one of these cycloids and = 2 u, : t being 
the radius of the generating circle. If C N = x , we shall have as before 

2 a 


and since 

x = 2 a x 

/ 2 a 

N 2a x 


P ~ 

and equation (4) becomes 


V (2 a x) 

Let = u 

so that 

adx xda= a 2 du 

x = au; 
and substituting 

a 2 du V2 d v h , 
V(2 u)" 1 

du V 2 da Vh 

V(2u-u 2 ) a f 

. V 2 X vers. - l u 2 J C (6) 

When a is infinite, the portion A P of the cycloid becomes a vertical 
line, and 

x = h, .-. u = 0, .-. C = 0. 

x , 2 h .. 

= vers. . / [71 

a >r a 

From this equation (a) should be eliminated by the equation to the 
cycloid, which is 

y = a vers. - V (2 a x x 2 ) . . . . (8) 

and we should have the equation to the curve required. 
Substituting in (8) from (7), we have 

y = V (2 ah) V (2 ax x 2 ) 
_dav h xda + adx x d \ 
V (2a) V (2 ax x*) 

and eliminating d a by (5) 

dy _ 2 a x / 2 a x 

dx~ ~ V (2ax x 2 ) ~ "~-**J x 


But differentiating (8) supposing (a) constant, we have in the cycloid 

2 a 

And hence (31) the curve P P P" cuts the cycloids all at right angles, 
the subnormal of the former coinciding with the subtangent of the latter, 

each being 

2 a 


The curve P P P" will meet A D in the point B, such that the given 
time is that of describing the whole cycloid A B. It will meet the vertical 
line in E, so that the body falls through A E in the given time. 

394. If instead of supposing all the cycloids 
to meet in the point A, we suppose them all to 
pass through any point C, their bases still being 
in the same line A D ; a curve P P drawn so 
that the times down P C, P C, &c. are all 
equal, will cut all the cycloids at right angles. 
This may easily be demonstrated. 

395. Tojind Tautochronous curves or those down which to a given Ji xed 
point a body descending all distances shall move in the same time. 

(1) let the force be constant and act in parallel lines. 

Let A the lowest point be the fixed point, D that 
from which the body falls, A B vertical, B D, M P 
horizontal. A M = x, A P = s, A B = h, and the 
constant force = g. 

Then the velocity at P is 

v = V (2g.h x) 


dt = = 


V 2g V (h x) 

and the whole time of descent will be found by integrating this from 
x = h, to x = 0. 

Now, since the time is to be the same, from whatever point D the body 
falls, that is whatever be h, the integral just mentioned, taken between the 
limits, must be independent of h. That is, if we take the integral so as 
to vanish when 

x = 

and then put h for x, h will disappear altogether from the result. This 
must manifestly arise from its being possible to put the result in a form 


v v 2 

involving only -r- , as r^ , &c. ; that is from its being of dimensions in 

x and h. 

d s = p dx 

where p depends only on the curve, and does not involve h. Then, we 

t - f 

1 / f p d x t 1 pxd x 1.3 pxMx 

Ws) J I *TT*T T* 271 ~vT c 

and from what has been said, it is evident, that each of the quantities 
/*p d x /-pxdx /px n dx 

y i y JT } y~~gir+T 

h ^ h 2 h T- 

must be of the form 

CX 2 

2 n + 1 

that is 

f p x " d x must = c x 2~~ ; 

. , 2 n + 1 Hi^ 1 . 
p x n d x = -^ c x a d x ; 

2n + 1 c 

P = 

or if 

2 n + 1 


which is a property of the cycloid. 

Without expanding, the thing may thus be proved. If p be a function 

of m dimensions in x, ,/ . is of m i dimensions : and as the 

V (h x) 

dimensions of an expression are increased by 1 in integrating 
f. P dx 




is of m -j- 1 dimensions in x, and when h is put for x, of m -{- ^ dimen 
sions in h. But it ought to be independent of h or of dimensions 

i = o 

p = a^ 

as before. 

396. (2) Let the force tend to a center and vary as any function of the 
distance. Required the Tautochronous Curve. 

Let S be the center of force, A the point to 
which the body must descend ; D the point from 
which it descends. Let also 

S A = e, S D = f, S P = ^ A P = s 
P being any point whatever, 

= C 2/Fdf 

Now we have 

or if 

the velocity being when f. 

Hence the time of describing D A is 

t=/-: ds 

taken from g = f, to g = e. And since the time must be the same what 
ever is D, the integral so taken must be independent of f. 

<pf <p e = h 

d s = p d z 
p depending on the nature of the curve, and not involving f. Then 

/p d z f 
r-7-j r , from z = h to z = 
V (h z) 

= /* r~i r from z = to z = h. 

J V (h z) 

And this must be independent of f, and therefore of <p f, and of h 
Hence, after taking the integral the result must be when z = 0, and 
independent of h, when h is put for z. Therefore it must be of dimen 
sions in z and h. But if p be of n dimensions in z, or if 
p = cz n 

V (h z) 

will be of n \ dimensions, 



/-. TT - r of n + s dimensions. 
V (h z) 

Hence, n + \ = 0, n = , and 


/ C C 

d s =r d z / = <f> o d g J - 7 ; 
>r z V p g <f> e 

whence the curve is known. 

If 6 be the angle A S O, we have 


g 2 
whence may be found a polar equation to the curve. 

397. Ex. 1. Let the force vary as the distance, and be attractive. 

F = Mg, 

z <p p 
dz = 2 # i 


d s 
when = e, -r- is infinite or the curve is perpendicular to S A at A. 

If S Y, perpendicular upon the tangent P Y, be called p, we have 
p2_ ds 2 dg 2 

8 " ds 2 

j _ e 2 (1 

4 C/(A 

If e = 0, or the body descend to the center, this gives the logarithmic 

In other cases let 




a 2 e 2 



a* e z 
the equation to the Hypocycloid (370) 

If 4 c p = 1, the curve becomes a straight line, to which S A is per 
pendicular at A. 

If 4 c ^ be > 1 the curve will be concave to the center and go off to 

398. Ex. 2. Let the force vary inversely as the square of the distance. 


and as before we shall find 

g 5 (g e) 

c e 

399. A body being acted upon by a force in parallel lines, in its descent 
from one point to another, to find the Brachystochron, or the curve of quick 
est descent between them. 

Let A, B be the given points, and A O P Q B 
the required curve. Since the time down 
A O P Q B is less than down any other curve, if 
we take another as A O p Q B, which coincides 
with the former, except for the arc O P Q, we 
shall have 

Time down A O : T. O P Q + T. Q B, less than 

Time down A O+T. O p Q + T. Q B 

and if the times down Q B be the same on the two suppositions, we shall 


T. O P Q less than the time down any other arc O p Q. 
The times down Q B will be the same in the two cases if the velocity 
at Q be the same. But we know that the velocity acquired at Q is the 
same, whether the body descend down 

A O P Q, or A O p Q. 

Hence it appears that if the time down A O P Q B be a minimum, the 
time down any portion O P Q is also a minimum. 


Let a vertical line of abscissas be taken in the direction of the force; 
and perpendicular ordinates, O L, P M, Q N be drawn, it being sup 
posed that 

L M = M N. 

Then, if L M, M N be taken indefinitely small, we may consider them 
as representing the differential of x : On this supposition, O P, P Q, will 
represent the differentials of the curve, and the velocity may be supposed 
constant in O P, and in P Q. Let 

AL = x, L O = y, OA = s, 

and let d x, d y, d s be the differentials of the abscissa, ordinate, and 
curve at Q, and v the velocity there ; and d x , d y , d s , v be the cor 
responding quantities at P. Hence the time of describing O P Q will 
be (46) 

d s d s 
v + V 

which is a minimum ; and consequently its differential = 0. This dif 
ferential is that which arises from supposing P to assume any position as 
p out of the curve O P Q ; and as the differentials indicated by d arise 
from supposing P to Vary its position along the curve O P Q, we shall 
use d to indicate the differentiation, on hypothesis of passing from one 
curve to another, or the variations of the quantities to which it is 

We shall also suppose p to be in the line M P, so that d x is not sup 
posed to vary. These considerations being introduced, we may pro 
ceed thus, 

d. d,, ........ 

And v, v are the same whether we take O P Q, or O p Q ; for the 
velocity at p = velocity at P. Hence 

d v = o, a v = o 


8 d s d d s _ 

" i~ 7 " 

v v 


ds 2 =dx 2 + dy 2 
.-. d s a d s = d y d d y, 
(for d d x = 0). 

d s 6 d s = d y d d y . 


Substituting the value of d d s, d d s which these equations give, 
we have 

dyddy d y _ 

vds ~v ds 

And since the points O, Q, remain fixed during the variation of P s 
position, we have 

d y + d y = const. 

d d y = d d y. 
Substituting, and omitting 8 d y, 

d y. jiy. 

vds v 7 d s - 

Or, since the two terms belong to the successive points O, P, their 
difference will be the differential indicated by d; hence, 

d -~/- = 


.*. j = const ....... . iv\ 

vds v 

Which is the property of the curve; and v being known in terms of x, 
we may determine its nature. 
Let the force be gravity ; then 

v = V(2gx); 



dy J_ 

d s V x V a 
a being a constant. 

d -? - / 

ds ~ V a 

which is a property of the cycloid, of which the axis is parallel to x, 
and of which the base passes through the point from which the body 

If the body fall from a given point to another given point, setting off 
with the velocity acquired down a given height; the curve of quickest 
descent is a cycloid, of which the base coincides with the horizontal line, 
from which the body acquires its velocity. 

400. If a body be acted on by gravity, the curve of its quickest descent 
from a given point to a given curve, cuts the latter at right angles. 

Let A be the given point, and B M the given curve; A B the curve of 
quickest descent cuts B M at right angles. 

VOL. I. 




[SECT. X. 

It is manifest the curve A B must be a cycloid, for 
otherwise a cycloid might be drawn from A to B, in A 
which the descent would be shorter. If possible, let 
A Q be the cycloid of quickest descent, the angle 
A Q B being acute. Draw another cycloid A P, and 
let P P be the curve which cuts A P, A Q so as to 
make the arcs A P, A P synchronous. Then (394) P P 
is perpendicular to A Q, and therefore manifestly P is 
between A and Q, and the time down A P is less than the time down 
A Q ; therefore, this latter is not the curve of quickest descent. Hence, 
if A Q be not perpendicular to B M, it is not the curve of quickest 

The cycloid which is perpendicular to B 
longest descent from A to B M. 

M may be the cycloid of 

401. If a body be acted on by gravity, and if A B be the 
curve of quickest descent from the curve A L to the point B ; 
A T, the tangent of A L at A, is parallel to B V, a perpen 
dicular to the curve A B at B. 

If B V be not parallel to A T, draw B X parallel to 
A T, and falling between B V and A. In the curve A L 
take a point a near to A. Let a B be the cycloid of quick 
est descent from the point a to the point B; and Bb being 
taken equal and parallel to a A, let A b be a cycloid equal 
and similar to a B. Since A B V is a right angle, the 
curve B P, which cuts off A P synchronous to A B, has B V for a tan 
gent. Also, ultimately A a coincides with A T, and therefore B b with 
B X. Hence B is between A and P. Hence, the time down A b is less 
than the time down A P, and therefore, than that down A B. And 
hence the time down a B (which is the same as that down A b) is less 
than that down A B. Hence, if B V be not parallel to A T, A B is not 
the line of quickest descent from A L to B. 

402. Supposing a body to be acted on by any forces whatever, to determinf 
the Brachystochron. 

Making the same notations and suppositions as before, A L, L O. (see 
a preceding figure) being any rectangular coordinates ; since, as before, 
the time down O P Q is a minimum, we have 


4. IfLi __ d s 3 v d s 3 v _ 

v v v 2 v 2 "~ * 

Now as before we also have 

* i d y 3 d y 

o Cl S =r 1_ - 

supposing 6 d x = 0, and 

_ dy .a.dy 


d s d s 

dv = 

for v is the velocity at O and does not vary by altering the curve. 

v = v + d v 

dv = dv + ddv = ddv. 

vds v d s v 72 = 


v ~ v+"d~v ~~ v v" 2 

for d v 2 , & c . must be omitted. Substituting this in the second term of 
the above equation, we have 

j> __ dy ady d y d v a d y d s 8 d v 

vds vds v 2 d~s ~ ~~V 2 ~ 


M! s d s) v "*" d s . v 2 v 72 " Tdy = 
Now as before 

d y d y d y 

d7 ~~d7- d dY 

And in the other terms we may, since O, P, are indefinitely near, put 

d s, d y, v for d s , d y , v : 
if we do this, and multiply by v, we have 
d dy dy.dvds adv 

which will give the nature of the curve. 

If the forces which act on the body at O, be equivalent to X in the 
direction of x, and Y in the direction of y, we have (371) 

d v = Xd *+ Ydy 


* i Yddy 

. . o d v = i. 





[SECT. X. 

because 5 v = 0, <5 d x = ; also X and Y are functions of A L, and L O, 
and therefore not affected by d. 

Substituting these values in the equation to the curve, we have 
d dy dy Xdx+Ydy ds Y = Q 
d s d s v 2 v v 


, dy dx Xdy Ydx _ _ 
a . -= -j . 

d s d s - 2 


which will give the nature of the curve. 

If r be the radius of curvature, and d s constant, we have (from 74) 

d s d x 

r =: 

d 2 y 

r being positive when the curve is convex to A M ; 
l d y _ d x 

d s r 

and hence 

v_ 2 _ Xdy Ydx 
r d s 

v 2 . 
The quantity is the centrifugal force (210), and therefore that part 

,., . e . ,Xdy Ydx.. 
of the pressure which arises from it. And ^ - is the pressure 

which arises from resolving the forces perpendicular to the axis. Hence, 
it appears then in the Brachystochron for any given forces, the parts of 
the pressure which arise from the given forces and from the centrifugal 
force must be equal. 

403. If we suppose the force to tend to a center S, 
which may be assumed to be in the line A M, and F 
to be the whole force ; also if 

then we have 

C ^ ~ = force in P S resolved parallel to 


Y S = F x -- 

v 2 = C 2/g F d 
2 g./ F d g _ F p 

r s 





2dp_ 2Fdg 

p = C- 
and integrating 

whence the relation of p and is known. 
If the body begin to descend from A 
C-2g/Fdg = 
when = a. 

404. Ex. 1. Let the force vary directly as the distance. 

p=C>(a g 2 ) 
which agrees with the equation to the Hypocycloid (370). 

405. Ex. 2. Let the force vary inversely as the square of the distance $ 

by supposition. 

S 2 _ S 3 + C *f CE 


p d g 

ci a ~ . . 

c V (a g) . d g 
~ f V (g 3 + c *g c*a) 
_ _ cdg 

When g = a, d J = ; when 

g 3 + c g c 2 a = 

d 6 is infinite, and the curve is perpendicular to the radius as at B. Tills 
equation has only one real root. 

If we have c = , S B = ~ 

B being an apse. 



If c = 

n 3 + n n 2 -f 1 

406. When a body moves on a given surface, to determine the Brachy- 
stochron. , 

Let x, y, z be rectangular coordinates, x being vertical ; and as before 
let d s, d s be two successive elements of the curve ; and let 

d x, d y, d z, 
d x , d y 7 , d z 

be the corresponding elements of x, y, z ; then since the minimum pro 
perty will be true of the indefinitely small portion of the curve, we have 
as before, supposing v, v the velocities, 
ds d s 

j- = mm. 

The variations indicated by a are those which arise, supposing d x, d x 
to be equal and constant, and d y, d z, d y , d z to vary 

d s 2 = dx 2 + dy 2 + dz 2 
.-. d s a d s = d y a d y + d z a d z. 

d s a d s = d y a d y + d z a d z. 

Also, the extremities of the arc 

d s + d s 
being fixed, we have 

d y + d y = const. 
.-. ady + ady = 

d z -f- d z const 
.-. a d z + a d z = 0. 

ads - 

rt c " ft c W 


And the surface is defined by an equation between x, y, z, which we 

may call 

L = 0. 


Let this differentiated give 

....... (3) 

Hence, since d x, p, q are not affected by 8 

3dz = q.3dy ......... (4) 

For the sake of simplicity, we will suppose the body to be acted on 
only by a force in the direction of x, so that v, v will depend on x alone, 
and will not be affected by the variation of d y, d z. Hence, we have by ( 1 ) 

6ds d d s _ 

which, by substituting from (2) becomes 

_-- ; - 

d s v d s / \ v d s v d s 

Therefore we shall have, as before 

* adz=0; 

. . 

v d s v d s 

and by equation (4), this becomes 

d.-^L + qd.4^ = ....... (5) 

v d s v d s 

whence the equation to the curve is known. 

If we suppose the body not to be acted on by any force, v will be con 
stant, and the path described will manifestly be the shortest line which 
can be drawn on the given surface, and will be determined by 

d.iZ+q.d.^ = ..... " . (6) 

d s d s v 

If we suppose d s to be constant, we have 

d 2 y + qd 2 z=:0 

which agrees with the equation there deduced for the path, when the 
body is acted on by no forces. 

Hence, it appears that when a body moves along a surface undisturbed, 
it will describe the shortest line which can be drawn on that surface, be 
tween any points of its path. 

407. Let P and Q be two bodies, of which the Jirst hangs 
from ajixedpoint and the second from the Jirst by means of 
inextensible strings A P, P Q; it is required to determine the 
small oscillations. 

A M = x, M P = y, 

AN = x / ,NQ = y / 

A P = a, P Q = a 

mass of P = p, of Q = p 

tension of A P =p,ofPQ=r p . 



Then resolving the forces p, p , we have 

y -.p g./ y_p_g 

d t 2 p a ft 

<* 2 y _ _P^g y -y 


a t 



d t 2 (j! a 

By combining these with the equations in x, x and with the two 

x 2 +y = a 2 , 

(x -x)*+(y _y) 2 :=a 2 ; 

we should, by eliminating p, p find the motion. But when the oscilla 
tions are small, we may approximate in a more simple manner. 

Let /3, j3 be the initial values of y, y . Then manifestly, p, p will de 
pend on the initial position of the bodies, and on their position at the time 
t : and hence we may suppose 

p= M + P/3 + Q/3 + R-y + Sy + &c. 
and similarly for p . 

Now, in the equations of motion above, p, p are multiplied by y, y y 
which, since the oscillations are very small are also very small quantities, 
(viz. of the order /S). Hence their products with |3 will be of the order 
B\ and may be neglected, and we may suppose p reduced to its first 
term M. 

M is the tension of A P, when /3, /3 &c. are all = 0. Hence it is the 
tension when P, Q, hang at rest from A, and consequently 

M = ^ + til. 

Similarly, the first term of p , which may be put for it is m . Substi 
tuting these values and dividing by g, equations (1) become 



v / 


gdt 2 " a " a 

Multiply the second of these equations by X and add it to the first, and 
we have 

_ _/j m x / j^x 

V a " t* a af ) y \ a! /*a ) y 


g d I 8 , V a t* a 

and manifestly this can be solved if the second member can be put in 
the form 

k.(y + xy ) 
that is, if 


k x = - 

a [A & 


/i A 6 a u, a 
a k = 1 1 

> (8) 

- = (a k 1)X 

Eliminating X we have 


(a k) 2 ^1 + )(l + -^ a k = - .... (4) 

From this equation we obtain two values of k. Let these be de 
noted by 

k, 2 k 
and let the corresponding values of X, be 

x, 2 x . 
Then, we have these equations. 

and it is easily seen that the integrals of these equations are 
y + x y = 1 C cos. t V ( k g) + D sin. t V ( l k g) 
y + 2 Xy = 2 Ccos.t V ( 2 kg) + 2 Dsin.t V ( 2 kg) 
C, 1 D, 2 C, 2 D being arbitrary constants. But we may suppose 
1 C = E cos. >e 
D = E sin. >e 

*C = 2 E cos. 2 e 
D 2 = 2 E sin. 2 e 
By introducing these values we find 

y + X y = E cos. {t V ( k g) + ej 
y + 2 X y = 2 E cos. [i V ( 2 k g) + 2 c} 
From these we easily find 

The arbitrary quantities *, e, &c. depend on the initial position and 


velocity of the points. If the velocities of P, Q = 0, when t = 0, we 
shall have 

% 2 e, each = 
as appears by taking the Differentials of y, y . 

If either of the two J E, 2 E be = 0, we shall have (supposing the latter 
case and omitting l e) 

y = 8 - j- cos. t V ( k g) 

y = 

Hence it appears that the oscillations in this case are symmetrical : that 
is, the bodies P, Q come to the vertical line at the same time, have similar 
and equal motions on the two sides of it, and reach their greatest dis 
tances from it at the same time. It is easy to see that in this case, the 
motion has the same law of time and velocity as in a cycloidal pendulum ; 
and the time of an oscillation, in this case, extends from when t = to 
when t V ( J k g) = ir. Also if /3, /3 be the greatest horizontal deviation 
of P, Q, we shall have 

y = j3 . cos. t V ( : k g) 
y = /S .cos. t V ( kg). 

In order to find the original relation of /3, |3 , (the oscillations will be 
symmetrical if the forces which urge P, Q to the vertical be as P M, Q N, 
as is easily seen. Hence the conditions for symmetrical oscillation might 
be determined by finding the position of P, Q that this might originally 
be the relation of the forces) that the oscillations may be of this kind, the 
original velocities being 0, we must have by equation (5) since 2 E = 0. 
)8 + 2 X /3 - 0. 

Similarly, if we had 

|8 + X /3 = 

we should have *E = 0, and the oscillations would be symmetrical, and 
would employ a time 

When neither of these relations obtains, the oscillations may be consi 
dered as compounded of two in the following manner : Suppose that we 

y = Hcos. t V ( kg) + Kcos. t V ( 2 kg) ... (7) 
omitting *e, 2 e, and altering the constants in equation (6) ; and suppose 
that we take 

M p = H . cos. t V ( l k g) ; 


Then p will oscillate about M according to the law of a cycloidal pen 
dulum (neglecting the vertical motion). Also 
p P will - K . cos. t V ( 2 k g). 

Hence, P oscillates about p according to a similar law, while p oscil 
lates about M. And in the same way, we may have a point q so moved, 
that Q shall oscillate about q in a time 

while q oscillates about N in a time 

V( kg) 

And hence, the motion of the pendulum A P Q is compounded of the 
motion A p q oscillating symmetrically about a vertical line, and of A P Q 
oscillating symmetrically about A p q, as if that were a fixed vertical line. 
When a pendulum oscillates in this manner it will never return exactly 
to its original position if V *k, V 2 k are incommensurable. 
If V l k, V 2 k are commensurable so that we have 

m V : k = n V 2 k 

m and ri being whole numbers, the pendulum will at certain intervals, re 
turn to its original position. For let 

t V ( k g) = 2 n r 

t V ( 2 k g) = 2 m T 
and by (7) 

y = H cos. 2 n * -|- K . cos. 2 m T 

= H + K, 
which is the same as when 

t = 0. 
And similarly, after an interval such that 

t V ( l k g) = 4 n T, 6 n T, &c. 

the pendulum will return to its original position, having described in the 
intermediate times, similar cycles of oscillations. 
408. Ex. Let (if = p, 
a = a 

to determine the oscillations. 
Here equation (4) becomes 

a 2 k 2 4 ak = 2 

a k = 2 + V 2. 


Also, by equation (3) 


a k = 3 X 
.-. x = 1 + V 2, 2 X = 1 V 2. 

Hence, in order that the oscillations may be symmetrical, we must 
either have 

/3 + ( I + V 2) j3 = 0, whence /3 = ( V 2 I) 

f3 ( V 2 1) (S = 0, whence /3 = ( V 2 + 1) 0. 
The two arrangements indicated by these equations are thus repre 

Q N Q 

The first corresponds to 

/3 = (V 2 + l)./3 


In this case, the pendulum will oscillate into the position A P Q , simi 
larly situated on the other side of the line ; and the time of this complete 
oscillation will be 

In the other case, corresponding to 

P = (V 2- l)/3 

Q is on the other side of the vertical line, and 
QN=(V2 1)PM. 

The pendulum oscillates into the position A P Q , the point O remain 
ing always in the vertical line ; and the time of an oscillation is 

<jt /a 

V (2 + V~2)+J g~ 

The lengths of simple pendulums which would oscillate respectively in 
these times would be 

2 _ V 2 and 2 + V 2 





1 .707 a and .293 a. 

If neither of these arrangements exist originally, let |8, /3 be the origi 
nal values of y, y when t is 0. Then making t = in equation (5), we 

E = |8 + ( V 2 + 1) |S 

2 E = /3 (V 2 1) /3 . 
And these being known, we have the motion by equation (6). 

409. Any number of material points P 1} P 2 , P 3 . . . Q, 

^awg &/ means of a string without weight^ from a point 
A ; it is required to determine their small oscillations in 
a vertical plane. 

Let A N be a vertical abscissa, and PJ M,, P 2 M 2 , 
&c. horizontal ordinates ; so that 

A M! = x l5 A M 2 = x 2 , &c. 

PI M! =.y,, P 2 M 2 = y 2 , &c. 

A P! = a l5 P! P 2 = a 2 , &c. 

tension of A P! = p l9 of P 1 P 2 = p 2 , &c. 

mass of P! = p lt of P 2 = /4 2 , &c. 

Hence, we have three equations, by resolving the forces parallel to the 

d2 yi _ PI g yi .PS g y a 3 

d t 2 " ~LL ~FL~ * T 

d 2 y 2 p 2 g y 2 ; 

i r-j r> 

d t * ~~ ~ ~ ~ " 7T~ 

\-i L fj^ tl^ fJ^2 

" y? - Pag ys ya , p* g 

2 "~ 


y 3 

d t 2 

^n _ P n 

y n y n _ 

. . . (1) 

And as in the last, it will appear that p,, p 2 , &c. may, for these small 
oscillations, be considered constant, and the same as in the state of rest. 
Hence if 


P! = M, p 2 = M A&I, p 3 = M ^, - /Kg, &c. 

Also, dividing by g, and arranging, the above equations may be put in 
this form : 



r SECT. X. 



;)y> + 


^2 _ 2_yi __ / p 2 



a 2 

y 2 + 

PS y 3 

lL - P2_Z* __ / Ps , P4 \ , 

i- 2 " /. Q \ "T" _ I J 3 ~i 

r^3 3 r^i a*} f^ \ **4* 


u v D v i n v 

" jn ^ h n Jn I Pn Jn 

gdt 2 /* a n /i n a n 

The first and last of these equations become symmetrical with the rest 
if we observe that 

y = o 


Pn + i = 0. 
Now if we multiply these equations respectively by 

1, X, X , X", &c. 
and add them, we have 

f\ 2 TT I % A 2 T T I \t A 2 ,, i 5irr 


a 3 

a 3 

a 4 

w-n - 1 a n /z. n a n 

and this will be integrable, if the right-hand side of the equation be redu 
cible to this form 

k (y, + X y 2 + X y 3 + &c.). 
That is, if 

k _ _Pj_ 

, _ 

kx = 

(n - 2) _ __ 

/ (n - 3) n > / (n - 2) 

_ Pn 

n a n 



If we now eliminate 

X, X , X", &c. 

from these n equations, it is easily seen that we shall have an equation of 
n dimensions in k. 

% 2 k, 3 k ...... k 

be the n values of k ; then for each of these there is a value of 

X , X", X" 
easily deducible from equations (3), which we may represent by 

X, X , >X", &c. 

2 X , 2 X", 2 X ", &C. 
Hence we have these equations by taking corresponding values X and k, 

_ t 

and so on, making n equations. 

Integrating each of these equations we get, as in the last problem 

yi + * y 2 + * y 3 + &c. = E cos. ft V (>k g ) + e $ 1 , r . 

yi + 2 *- y 2 + 2 >- J 3 + &c. = 2 E cos. {t V ( 2 k g) + 2 e] ) 
1 E, 2 E, &c. ! e, 2 e, &c. being arbitrary constants. 

From these n simple equations, we can, without difficulty, obtain the n 
quantities y l5 y g , &c. And it is manifest that the results will be of this 

yi= I H 1 cos.{t V ( kg) + 1 e}+ 2 H 1 cos.{lV( 8 kg) + 2 e} + &c.-j 

y^^cos.Jt V Ckg) + 1 e}+ 2 H 2 cos.Jt\/( 2 kg) + 2 e] + &c. V . . . (6) 
&c. = &c. ) 

where H^ Ha, &c. must be deduced from (Sj, /3 2 , &c. the original values 
of yi, y 2 , &c. 

If the points have no initial velocities (i. e. when t = 0) we shall have 
E = 0, 2 E = 0, &c. 

We may have symmetrical oscillations in the following manner. If, 
of the quantities 1 E, *E, 3 E, &c. all vanish except one, for instance n E ; we 

yi + ^ y 8 + ^ y 3 + &c. = o ^ 

yi + ^y 2 + 2 ^y3 + &c. = o 

yi + 3 ^y a + 3 x y 3 + &c. = o k - - (T) 


yi+ n ^y a + n ^y3+&c.- n Ecos.tV( n kg)J 

omitting n E. 


From the n 1 of these equations, it appears that y 2 , y 3 , &c. are in a 
given ratio to y l ; and hence 

n >- y3 + &c. 

is a given multiple of y t and = m yj suppose. Hence, we have 

m y! s= n E cos. V ( n k g) ; 
or, omitting the index n, which is now unnecessary, 

m y l = E cos. t V (k g). 
Also if y 2 = e 2 y lt 

m y 2 = E e 2 cos. t V (k g) 
and similarly for y 3 &c. 

Hence, it appears that in this case the oscillations are symmetrical. All 
the points come into the vertical line at the same time, and move similar 
ly, and contemporaneously on the two sides of it. The relation among 
the original ordinates ft, /3 2 , /3 3 , &c. which must subsist in order that the 
oscillations may be of this kind, is given by the n 1 equations (7), 
ft + 1 X& + X /3 3 +&c. = 
ft + 2 */3 2 + 2 >//3 3 + &c. = 
ft + 3 *& + 3 >//3 3 + &c. = 

&c. = &c. 

These give the proportion of ft /3 2 , &c; the arbitrary constant n E, in 
the remaining equation, gives the actual quantity of the original displace 

Also, we may take any one of the quantities L E, S E, 3 E, &c. for that 
which does not vanish ; and hence obtain, in a different way, such a sys 
tem of n 1 equations as has just been described. Hence, there are n 
different relations among ft ft, &c. or n different modes of arrangement, 
in which the points may be placed, so as to oscillate symmetrically. 

( We might here also find these positions, which give symmetrical oscil 
lations, by requiring the force in each of the ordinates Pj MI, P 2 M 2 to 
be as the distance; in which case the points P M P 2 , &c. would all come 
to the vertical at the same time. 

If the quantities V l k, V 2 k have one common measure, there will be 
a time after which the pendulum will come into its original position. And 
it will describe similar successive cycles of vibrations. If these quantities 
be not commensurable, no portion of its motion will be similar to any 
preceding portion.) 

The time of oscillation in each of these arrangements is easily known ; 
the equation 

m yi = n E cos. t V ( n k g) 


shows that an oscillation employs a time 

And hence, if all the roots : k, 2 k, 3 k, &c. be different, the time is dif 
ferent for each different arrangement. 

If the initial arrangement of the points be different from all those thus 
obtained, the oscillations of the pendulum may always be considered as 
compounded of n symmetrical oscillations. That is, if an imaginary pen 
dulum oscillate symmetrically about the vertical line in a time 


and a second imaginary pendulum oscillate about the place of the first, 
considered as a fixed line, in the time 

and a third about the second, in the same manner, in the thnc 


and so on ; the n th pendulum may always be made to coincide per 
petually with the real pendulum, by properly adjusting the amplitudes of 
the imaginary oscillations. This appears by considering the equations 
(6), viz. 

yi = Hj cos. t V ( k g) + 2 H! cos. t V ( 2 k g) + &c. 
&c. = &c. 

This principle of the coexistence of vibrations is applicable in all cases 
where the vibrations are indefinitely small. In all such cases each set of 
symmetrical vibrations takes place, and affects the system as if that were 
the only motion which it experienced. 

A familiar instance of this principle is seen in the manner in which the 
circular vibrations, produced by dropping stones into still water, spread 
from their respective centers, and cross without disfiguring each other. 

If the oscillations be not all made in one vertical plane, we may take a 
horizontal ordinate z perpendicular to y. The oscillations in the direc 
tion of y will be the same as before, and there will be similar results ob 
tained with respect to the oscillations in the direction of z. 

We have supposed that the motion in the direction of x, the vertical 
axis, may be neglected, which is true when the oscillations arc very 

410. Ex. Let there be three bodies all equal (each = /a,), and also their 
distances a 1} a. 2 , a 3 all equal (each = a). 

VOL. I. X 



p = 3 (*, p. 2 = 2 ft, p 3 = a 
and equations (3) become 

a k = 5 2 X 
a k X = 2 + 3 X X 
a k >/ = X + X . 
Eliminating k, we have 

5 X 2 X 2 = 2 + 3 X X , 
5 x 2 X X = X + X , 

X = 2X 2 2 X 2, 

4 X 2 X X = X 


.-. x = 

2 X 4 

... (2X 2 2X 2)(2X 4) = X 


X 3_3X 2 + ^-X + 2 =0, 


which may be solved by Trigonometrical Tables. We shall find three 
values of X. 

Hence, we have a value of X corresponding to each value of X ; and 
then by equations (7) 

ft -f- x ft + X X ft = \ , 7 v 

j3 + 2 x ft + 2 x ft = J 
whence we find ft, ft in terms of ft. 
We shall thus find 

ft = 2. 295 & 

ft = ]. 348 ft 

ft = .643,3, 
according as we take the different values of X. 

And the times of oscillation in each case will be found by taking tiie 
value of 

a k = 5 2 X; 

that value of X being taken which is not used in equation (7 ). For the 
time of oscillation will be given by making 

t V (k g) = cr. 
If the values of ft, ft, ft have not this initial relation, the oscillations 




will be compounded in a manner similar to that described in the example 
for two bodies only. 

411. A flexible chain, of uniform thidcness, hangs from a Jixed point : 
to find its initial form, that its small oscillations may be symmetrical. 

Let A M, the vertical abscissa x ; M P the hori 
zontal ordinate = y; A P = s, and the whole length 
A C = a; 

.-. A P = a s. 

And as before, the tension at P, when the oscillations 
are small, will be the weight of P C, and may be represent 
ed by a s. This tension will act in the direction of a 
tangent at P, and hence the part of it in the direction 
P M will be 


tension X 



(a - s) $* . 

d s 

Now, if we take any portion P Q = h, we shall find the horizontal 
force at Q in the same manner. For the point Q, supposing d s constant 

h d 3 " ^ 2 

dy . dy , d 2 

-* becomes 3-= + -= 
ds d s d s 

(see 32). 

Also, the tension will be a s -f- h. 
the direction N Q, is 

y L , 

1 ^ d s 3 

-IT2 &C - 

Hence the horizontal force in 

Subtracting from this the force in P M, we have the force on P Q 

h <P h 2 

+ Z + &c.) 
s d s 2 1 / 

and the mass of P Q being represented by h, the accelerating force 

( = -- -*j is found. But since the different points of P Q move 

* rnuss / 

with different velocities, this expression is only applicable when h is inde 
finitely small. Hence, supposing Q to approach to and coincide with P, 
we have, when h vanishes 

12 1 

accelerating force on P = (a s) , -\ ^ . 

d s 2 d s 



But since the oscillations are indefinitely small, x coincides with s and 
we have 

d 2 v d v 

accelerating force on P = (a x) -j ^. 

dx 2 dx 

Now, in order that the oscillations may be symmetrical, this force must 
be in the direction P M, and proportional to P M, in which case all the 
points of A C, will come to the vertical A B at once. Hence, we must 

(a x) -, ^ ^~ = kdy (!) 

dx 2 d x 

k being some constant quantity to be determined. 

This equation cannot be integrated in finite terms. To obtain a 
series let 

y = A + B. (a x)+ C(a x) 2 + &c. 

.-.i = B 2C(a x) 3D (a x) 2 

... <JlZ = 1. 2. C + 2. 3 D (a x) + &c. 

(I *v 


~ v " dx 2 dx * 

= 1. 2. C (a x) + 2. 3 D (a x) 2 + &c. 

+ B + 2 C (a x) + 3 D (a x) 2 + &c. 
+ kA + kB(a x) + k C (a x) 2 + &c. 
Equating coefficients ; we have 

B = _ k A, 
2 2 C= k B 
3 2 D = k C 
&c. = &c. 
.-. B = k A 
k 2 A 

C = 

D = 

2 2 
k 3 A 

2 2 .3 2 
&c. = &c. 




A is B C, the value of y when x = a. When x = 0, y = ; 

k 2 a 2 k 3 1 3 

. 1 L. r, _L I . _i_ &T O f^\ 

- 1 K a -f- g 2 ga 32 "T "~ W 

From this equation (k) may be found. The equation has an mfinite 
number of dimensions, and hence k will have an infinite number of values, 
which we may call 

l ]f 2 k n t l 

2v, Iv, ... IV . . . J , 

and these give an infinite number of initial forms, for which the chain 
may perform symmetrical oscillations. 

The time of oscillation for each of these forms will be found thus. At 
the distance y, the force is k g y : hence by what has preceded, the time 
to the vertical is 



and the time of oscillation is 

(The greatest value of k a is about 1.44 (Euler Com. Acad. Petrop. 
torn. viii. p. 43). And the time of oscillation for this value is the same as 


that of a simple pendulum, whose length is a nearly.) 


The points where the curve cuts the axis will be found by putting y = 0. 
Hence taking the value n k of k, we have 

n^a/o _ Y \ 2 n 1, 3 / _ x \ * 
0= l-n k(a _ x)+ _ (*J=2 _ + k ^ 32 X) +&C. 

which will manifestly be verified, if 

n k (a x) = k a 

n k ( a _ x ) = 2k a 


*k(a x) = 3 ka 

&c. = &c. 

because l k a, 2 k a, &c. are roots of equation (3). 
That is if 

x = a l - or = a J ~ or = &c - 

Suppose k, 2 k, 3 k, &c. to be the roots in the order of their magnitude 
k being the least. 

Then if for n k, we take k, all these values of x will be negative, and 
the curve will never cut the vertical axis below A. 




[SECT. X. 

If for n k, we take *k, all the values of x will be negative except the 
first; therefore, the curve will cut A B In one point. If we take 3 k, all 
the values will be negative except the two first, and the curve cuts A B 
in two points ; and so on. 

Hence, the forms for which the oscillations will be 
symmetrical, are of the kind thus represented. 

And there are an infinite number of them, each 
cutting the axis in a different number of points. 

If we represent equation (2) in this manner 

y = A <f> (k, x) 
it is evident that 

y = 1 A? (>k, x) 

y = 2 A p ( 2 k, x) 
&c. = &c. 
will each satisfy equation (1). Hence as before, if we put 

y = A p ( k, x) + 2 A p ( 2 k, x) + &c. 

and if A, *A, &c. can be so assumed that this shall represent a given 
initial form of the chain, its oscillations shall be compounded of as many 
coexisting symmetrical ones, as there are terms A, 2 A, &c. 

We shall now terminate this long digression upon constrained mo 
tion. The reader who wishes for more complete information may con 
sult Whewell s Dynamics, one of the most useful and elegant treatises 
ever written, the various speculations of Euler in the work above quoted, 
or rather the comprehensive methods of Lagrange in his Mecanique 

We now proceed to simplify the text of this Xth Section. 

412. PROP. L. First, S II Q is formed by an entire revolution of the 
generating circle or wheel, whose diameter is O R, upon the globe 

413. Secondly, by taking 

C A : C O : : C O : C R 
we have 


: : A O : O R 

and therefore if C S be joined and produced to meet the exterior globe 
in D, we have also 

AD : SO(:: C A: CO) :: AO: OR. 

S O = the semi-cireumference of the wheel O R = -^-^ . 


. .AD = ^ = the circumference of the wheel whose diameter is 


A O. That is S is the vertex of the Hypocycloid A S, and A S is per 
pendicular in S to C S. But O S is also perpendicular to C S. There 
fore A S touches O S in S, &c. 

414. The similar jigures A S, S R.] 

By 39 it readily appears that Hypocycloids are similar when 

R : r : : R : r 
R and r being the radii of the globe and wheel : that is when 

C A : AO ::CO : O R 
or when 

.. A S, S R are similar 

415. V B, V W are equal to O A, O R.] 

If B be not in the circumference AD let C V meet it in B . Then 
V P being a tangent at P, and since the element of the curve A P is the 
same as would be generated by the revolution of B P around B as a 
center, and .. B P is perpendicular both to the curve and its tangent 
P V, therefore P B, P B and .-. B, B coincide. That is 

V B = O A. 

Also if the wheel O R describes O V whilst A O describes A B, the 
angular velocity B P in each must be the same, although at first, viz. at 
O and A, they are at right angles to each other. Hence when they shall 
have arrived at V and B their distances from C B must be complements 
of each other. But 

.TVW = BVP=-5 PBV 


/. T V is a chord in the wheel O R, and 

.-. V W = O R. 
See also the Jesuits note. 


416. Construct the curve S P, to which the radius of curvature to every 
point of S R Q is a tangent ; or which is the same, find S A the Locus of 
the Centers of Curvature to S R Q. 

Hence is suggested the following generalization of the Problem, viz. 

417. To make a body oscillate in any given curve. 

Let S R Q (Newton s fig.) the given curve be symmetrical on both sides 



of R. Then if x, y be the rectangular coordinates referred to the vertex 
R, and a, (3 those of the centers of curvature (P) we have 

r 2 _ p T 2 _ (y /3) 2 + ( X a) 2 . 
Hence, the contact being of the second order (74) 

X- + (y -0)^ = (1) 


d v 2 d 2 v 

!+ HI + &-$<- (a) 

These two equations by means of that of the given curve, will give us 
Q in terms of , or the equation to the Locus of the centers of curvature. 

Let S A be the Locus corresponding to S R, and A Q the other half. 
Then suspending a body from A attached to a string whose length is R A, 
when this string shall be stretched into any position APT, it is evident 
that P being the point where the string quits the locus is a tangent to it, 
and that T is a point in S R Q. 

Ex. 1. Let S R Q be the common parabola. 


y 2 = 2 a x 

d y a 
d x y 

d 2 y ady a 2 a 

dx 2 = " y* d~x = ~ y" 3 ~ ~ 2 x y 
/. substituting we get 

-/S).! = 



... x a + fl + ^-} . ^ = = 3x a-fa 
V V. 2 x/ a 



y 8 = 2 a x 

8x ; 


8 (a a) 3 8 .. 

_ vx V / _ __ /~ o I 3 /Ql 

s\ ~nri ~ "fjry * \ ~~~ I \ ) 

Now when /3 = 0, a = a; which shows that A R the length of the 
string must equal a. Also making A the origin of abscissas, that is, aug 
menting a, by a, we have 

- x 

the equation to the semicubical parabola A S, A Q, which may be traced 
by the ordinary rules (35, &c.); and thereby the body be made to oscillate 
in the common parabola S Q R. 

Ex. 2. Let S R Q be an ellipse. 

Then, referring to its center, instead of the vertex, 


b 2 x 2 = a 2 b 

a y 

d y 
d x 

... a 2 y + b 2 x = 



ii y -TJ r- B j q -p - v. 

J dx d x. 2 

These give 

d y b 2 -X. 

dx. ~ ~ a 2 y 

d^y b 4 

dx 2 = a 2 y 3 

(a 2 b 2 ) x 3 

a 3 -i 

a 4 


^=- (a "" b 4 )y3 - 

Hence substituting the values of y and x in 

a 2 y 
we get 

* M r\ i^ x *-< o v .*_ 


b \f / a a \ 

the equation to the Locus of the centers of curvature. 



[SECT. X. 

In the annexed figure let 

SC = b, CR = a 
C M = x, T M = y. 

P N = ft C N = . 
And to construct A S by points, first put s 

whence by equation (a) 

j_ a 2 b * 

C6 -^ "~| 

the value of A C. Let 

a. = 

S = + =-^ 

the value of S C or C Q . 

Hence to make a body oscillate in the semi-ellipse S R Q we must 
take a pendulum of the length A R, (part = A P S flexible, and part 
= S S rigid ; because S S is horizontal, and no string however stretched 
can be horizontal see Whewell s Mechanics,) and suspend it at A. 
Then A P being in contact with the Locus AS , P T will also touch 
A S in P, &c. &c. 

Ex. 3. Let S R Q be the common cycloid ,- 

The equation to the cycloid is 

1? - / 

d x ~ V 

- /f?- r 

V V 


dx 2= 
whence it is found that 





d^ _ 2r y 

dx ~ y 




2r y 


. /^-. 3 

do" Ar y 
which is also the equation of a cycloid, of which the generating circle is 


precisely the same as the former, the only difference consisting in a change 
of sign of the ordinate, and of the origin of the abscissae. 

The rest of this section is rendered sufficiently intelligible by the 
Notes of P. P. Le Seur and Jacquier ; and by the ample supplementary 
matter we have inserted. 


417. PROP. LVII. Two bodies attracting one another, describe round 
each other and round the center of gravity similar figures. 


Since the mutual actions will not affect the center of gravity, the bodies 
will always lie in a straight line passing through C, and their distances 
from C will always be in the same proportion. 

.-. S C : T C : : P C : Q C 

z-SCT = QCP. 
.*. the figures described round each other are similar. 

Also if T t be taken = S P, the figure which P seems to describe 
round S will be t Q, and 

Tt : TQ:: S P: TQ 
: : C P : C Q 

t- 1 T Q = P C Q. 

.. the figures t Q, P Q, are similar ; and the figure which S seems to 
describe round P is similar, and equal to the figure which P seems to 
describe round S. 

418. PROP. LVIII. If S remained at rest, a figure might be de 
scribed by P round S, similar and equal to the figures which P and S 
seem to describe round each other, and by an equal force. 







Curves are supposed similar and Q R, q r indefinitely small. Let P and 
p be projected in directions P R, p r (making equal angles C P R, s p r) 
with such velocities that 

V V~S 

_ V CP _ V PQ 

P v sp ^ pq 

Then (si 

since a t = 


pq VPQ 

Vp q VPQ _ V QR 
V q r 



But in the beginning of the motion f = 

F _ QR jr l_ 
f : : ~qr Q R =: 1 

The same thing takes place if the center of gravity and the whole system 
move uniformly forward in a straight line in fixed space. 

419. COB. 1. If F cc D, the bodies will describe round the common 
center of gravity, and round each other, concentric ellipses, for such would 
be described by P round S at rest with the same force. 

Conversely, if the figures be ellipses concentric, F D. 

420. COR. 2. If F <x - the figures will be conic sections, the foci in 

the centers of force, and the converse. 

421. COR. 3. Equal areas are described round the center of gravity, 
and round each other, in equal times. 


422. COR. 3. Otherwise. Since the curves are similar, the areas, bounded 
by similar parts of the curves, are similar or proportional. 

.-. spq : C P Q : : sp 2 : C P 2 : : (S + P) 2 : s 2 in a given ratio; 


and T. through s p q : T. through CPQ:: VS + P: V S, in a given ratio 
and .-. : : T. through spv: T. through CPV 

.-. T. through C P Q : T. through CPV:: T. through spq : T. through spv 

: : s p q : s p v (by Sect. II.) 

.. the areas described round C are proportional to the times, and the 
areas described round each other in the same times, which are similar to 
the areas round C, are also proportional to the times. 

423. PROP. LIX. The period in the figure described in4ast Prop. 
: the period round C : : V S + P : V S ; for the times through similar 
arcs p q, P Q, are in that proportion. 

424. PROP. LX. The major axis of an ellipse which P seems to de 
scribe round S in motion (Force <x jrzl major axis of an ellipse which 

would be described by P in the same time round S at rest : : S + P : 
of two mean proportionals between S + P and S. 

Let A = major axis of an ellipse described (or seemed to be described) 
round S in motion, and which is similar and equal to the ellipse de 
scribed in Prop. LVIII. 

Let x = major axis of an ellipse which would be described round S at 
rest in the same time. 

period in ellipse round S in motion V S /p T TV\ 

period in same ellipse round Sat rest "" ^/~s^f^P r ^ 
and by Sect. Ill, 

period in ellipse round S at rest A * 

period in required ellipse round S at rest ~ f 


period in ellipse round S in motion A* V~S 

period in required ellipse round S at rest ~~ I v~S~^TP 
but these periods are to be equal, 

.-. A 3 S = x 3 .S~+~p 


.-. A:x:: V S + P: V S::S+ P: first of two mean proportionals 
(for if a, a r, a r 2 , a r 3 , be proportionals, V~o. : V a r 3 : : a : a r.) 

425. At what mean distance from the earth would the moon revolve 
round the earth at rest, in the same time as she now revolves round the 
earth in motion ? This is easily resolved. 

426. PROP. LXI. The bodies will move as if acted upon by bodies at 
the center of gravity with the same force, and the law of force with re- 


spect to the distances from the center of gravity will be the same as with 
respect to the distances from each other. 

For the force is always in the line of the center of gravity, and .-. the 
bodies will be acted upon as if it came from the center of gravity. 

And the distance from the center of gravity is in a given ratio to the 
distance from each other, .-. the forces which are the same functions of 
these distances will be proportional. 

427. P$,OP. LXII. Problem of two bodies with no initial Velocities. 

F oc _ . Two bodies are let fall towards each other. Determine the 


The center of gravity will remain at rest, and the bodies will move as 
if acted on by bodies placed at the center of gravity, (and exerting the 
same force at any given distance that the real bodies exert), 

.-. the motions may be determined by the 7th Sect. 

428. PROP. LXIII. Problem of two bodies with given initial Velo 

F ex j . Two bodies are projected in given directions, with given 

velocities. Determine the motions. 

The motion of the center of gravity is known from the velocities and 
directions of projection. Subtract the velocity of the center of gravity 
from each of the given velocities, and the remainders will be the velocities 
with which the bodies will move in respect of each other, and of the cen 
ter of gravity, as if the center of gravity were at rest. Hence since they 
are acted upon as if by bodies at the center of gravity, (whose magnitudes 
are determined by the equality of the forces), the motions may be deter 
mined by Prop. XVII, Sect. Ill, (velocities being supposed to be acquired 
down the finite distance), if the directions of projection do not tend to the 
center, or by Prop. XXXVII, Sect. VII, if they tend to or directly from 
the center. Thus the motions of the bodies with respect to the center of 
gravity will be determined, and these motions compounded with the uni 
form motion of the center of gravity will determine the motions of the 
bodies in absolute space. 

429. PIIOP. LXIV. F oc D, determine the motions of any number of 
bodies attracting each other. 


T and L will describe concentric 
ellipses round D. 

Now add a third body S. 

Attraction of S on T may be re 
presented by the distance T S, and 
on L by L S, (attraction at distance 
being 1) resolve T S, L S, into 
T D, D S ; L D, D S, whereof the 
parts T D, L D, being in given 
ratios to the whole, T L, L T, will 
only increase the forces with which 
L and T act on each other, and 

the bodies L and T will continue to describe ellipses (as far as respect 
these new forces) but with accelerated velocities, (for in similar parts of 
similar figures V 2 F.R Prop. IV. Cor. 1 and 8.) The remaining 
forces D S, and D S, being equal and parallel, will not alter the relative 
motions of the bodies L and T, .-. they will continue to describe ellipses 
round D, which will move towards the line I K, but will be impeded in 
its approach by making the bodies S and D (D being T + L) describe 
concentric ellipses round the center of gravity C, being projected with 
proper velocities, in opposite and parallel directions. Now add a fourth 
body V, and all the previous motions will continue the same, only accel 
erated, and C and V will describe ellipses round B, being projected with 
proper velocities. 

And so on, for any number of bodies. 

Also the periods in all the ellipses will be the same, for the accelerating 
force onT = L.TL+ S . TD = (T+L) . TD+S. T D = (T+L +S). 
T D, i. e. when a third body S is added, T is acted on as if by the sum 
of the three bodies at the distance T D, and the accelerating force on D 
towards C=S.SD = S.CS+S.DC = (T+L).DC+S.DC 
- (T + L + S). D C. 

. . accelerating force on T towards D : do. on D towards C : : T D : D C 


. . the absolute accelerating forces on T and D are equal, or T and D 
move as if they revolved round a common center, the absolute force the 
same, and varying as the distance from the center, i. e. they describe el 
lipses, in the same periods. 

Similarly when a fourth body V is added, T, L, D, S, C, and V, move 
as if the four bodies were placed at D, C, B, i. e. as if the absolute forces 
were the same, and with forces proportional to their respective distances 
from the centers of gravity, and .. in equal periods. 




And so on, for any number of bodies. 

430. PROP. LXVI. S and P revolve round T, S in the exterior orbit, 
P in the interior, 

F oc , find when P will describe round T an orbit nearest to the 

ellipse, and areas most nearly proportional to the times. 

(1st.) Let S, P, revolve round the greatest body T in the same plane. 
Take K S for the force of S on P at the mean distance S K, 

L S = S K . 

= force at p > 

resolve L S into L M, M S, 

L M is parallel to P T, and .-. tends to the center T, .-. P will con 
tinue to describe areas round T proportional to the times, as when acted 

on only by P T, but since L M does not oc p~ff~z > tne sum of L M and 

P T will not TZ , .-. the form of the elliptic orbit P A B will be 
disturbed by this force, L M, M S neither tends from P to the center 

T, nor oc 

. from the force M S both the proportionality of areas 

P T 2 

to times, and the elliptic form of the orbit, will be disturbed, and the 
elliptic form on two accounts, because M S does not tend to C, and be 
cause it does not p~q^i 

. . the areas will be most proportional to the times, when the force 
M S is least, and the elliptic form will be most complete, when the forces 
M S, L M, but particularly L M, are least. 

Now let the force of S on T = N S, then this first part of the force 
M S being common to P and T will not affect their mutual motions, .. the 

BOOK 1.] 



disturbing forces will be least when L M, M N, are least, or L M remain 
ing, when M N is least, i. e. when the forces of S on P and T are nearly 
equal, or S N nearly = S K. 

(2dly) Let S and P revolve round T in different planes. 

Then L M will act as before. 

But M N acting parallel to T S, when S is not in the line of the Nodes, 
(and M N does not pass through T), will cause a disturbance not only 
in the longitude as before, but also in the latitude, by deflecting P from 
the plane of its orbit. And this disturbance will be least, when M N is 
least, or S N nearly = S K. 

431. COR. 1. If more bodies revolve round the greatest body T, the 
motion of the inmost body P will be least disturbed when T is attracted 
by the others equally, according to the distances, as they are attracted by 
each other. 

432. COR. 2. In the system of T, if the attractions of any two on the 

third be as y^, , P will describe areas round T with greater velocity near 

conjunction and opposition, than near the quadratures. 

433. To prove this, the following investigation is necessary. 

Take 1 S to represent the attraction of S on P, 

n S T, 

Then the disturbing forces are 1 m (parallel to P T) and m n. 
Now - 


O I c, TJ 


SP~ (R 2 2Rrcos. 

V R 2 2Rrcos. A 

JL C0 ^: 4. l\ /i 2 r cos. A r 2 
R h RVV ~~KT r R- 

VOL. I. 


S / 2r 

S /. 3/2r r 2 x 3. 5 /2rcos. A rVo N 

= KA 1 + rw cos - A - RI) + 274 ( R wl &c -) 

S /. 3r /3 3.5 

= RTA 1 + Tr cos - A ~ (-2 - 2^ cos< 

S /. 3 r. cos. A\ 
= R 2 ^ ~R / 

where R is indefinitely great with respect to r. 

-Q Q^ ^ /, 3 r cos. A\ S S.Srcos. 
-Sn= w (l+ _^__)_ R2= __ 


and Ira = SI. - = ~ (R 2 2 R r cos. A + r 2 ) 

* (R 2 ~2 Rr cos. A + r 2 )- 

2 &c 


" R 3 R 

= -p^Y ultimately. 

434. Call 1 m the addititious force 
and m n the ablatitious force - 
and m n = 1 m 3 cos. A. 
Resolve m n into m q, q n. 

The part of the ablatitious force which acts in the direction m q 
= m n . cos. A 
3 . S . r. cos. 2 A 


= central ablatitious force. 

3 S r 
The tangential part r= m n . sin. A = ~WT~ sm - -^ cos - -A- 

o Q r 

= - . -j^ . sin. 2 A = tangential ablatitious force 

& JLv 

., i i r ., j- Tjrr, i S.r 3.S.r.cos. 2 A 

% . the whole force m the direction PT = lm mq = ~-, ^r^ 

it it 

= ^ (l _ 3 cos. 2 A) and the 
R 3 v 

3 S.r 
, whole force in the direction of the Tangent = q n = . ~^-j . sin. 2 A. 

til At 

435. Hence COR. 2. is manifest, for of the four forces acting on P, the 




three first, namely, attraction of T, addititious force, and central ablatiti- 
ous force, do not disturb the equable description of areas, but the fourth 
or tangential ablatitious force does, and this is -f- from A to B, from B 
to C, + from C to D, from D to A. /. the velocity is accelerated from A 
to B, and retarded from B to C, /. it is greatest at B. Similarly it is a 
maximum at D. And it is a minimum at A and C. This is Cor. 3. 
436. To otherwise calculate the central and tangential ablititious forces. 

On account of the great distance of S, S M, P L may be considered 
parallel, and 

.-. P T = L M, and S P = S K = S T. 

.-. the ablatitious force = 3 P T. sin. 6 = 3 P K. 
Take P m = 3 P K, and resolve it into P n, n m. 
P n =; P m . sin. 6 = 3 P T. sin. 2 6 = central ablatitious force 

= 3 p T. ] cos - 2 * 

n m = P m . cos, 6 3 P T. sin. 6 cos. 6 = ^ . P T. sin. 2 6 = tangential 


ablatitious force. 

The same conclusions may be got in terms of 1 m from the fig. in Art 
433, which would be better. 

437. Find the disturbing force on P in the direction P T. 

This = (addititious + central ablatitious) force = 1 m -f 3 1 m . sin. 2 6 
"I cos. 2 

i 01 /" 

= lm_31m( 

438. To Jind the mean disturbing force of S during a whole revolution 
in the direction P T. 

Let P T at the mean distance = m, then 1 m f 


1 3 cos. 2 


1m m , !! 

= -^ since cos. 2 6 is destroyed during a whole revo- 

- A 


439. The disturbing forces on P are 

(1) addititious = -=^- = A. 

(2) ablatitious = 3 . A . sin. 6 



3 . A 

which is (1) tangential ablatitious force * . cos. 2 & 

I cos> 2 

and (2) central ablatitious force = 3 A . - 


3 A 3 A 

.*. whole disturbing force in the direction P T = A -j - . cos. 2 & 

A , 3 A 

= Q- + . cos. 2 6. 

But in a whole revolution cos. 2 6 will destroy itself, .-. the whole dis 
turbing force in the direction P T in a complete revolution is ablatitious 
and = addititious force. 

The whole force in the direction P T = -^-j- (1 3 sin. 2 6) (Art. 433) 

multiply this by d.0, and the integral = -^-y (0 6 + . sin. 2 i\ 

= sum of the disturbing forces ; and this when 6 = ir becomes 


This must be divided by T, and it gives the mean disturbing force act- 


ing on P in the direction of radius vector = & ~t> s 

440. The 2d COR. will appear from Art. 433 and 434. 


For the tangential ablatitious force = . sin 2 6 . X addititious force, 

.. this force will accelerate the description of the areas from the quadra 
tures to the syzygies and retard it from the syzygies to the quadratures, 
since in the former case sin. 2 is +, and in the latter . 

441. COR. 3 is contained in COR. 2. (Hence the Variation in as 




442. P V is equivalent to P T, T V, and accelerates the motion ; 
p V is equivalent to p T, T V, and retards the motion. 

443. COR. 4. Cast, par., the curve is of greater curvature in the quadra 
tures than in the syzygies. 

For since the velocity is greatest in the syzygies, (and the central abla- 
titious force being the greatest, the remaining force of Pto T is the least) 
the body will be less deflected from a right line, and the orbit will be less 
curved. The contrary takes place in the quadratures. 

444. The whole force from S in the direction P T=~^ (1 3 sin. 2 6} 

(see 433) and the force from T in the direction P T = - 

rp O 

. . the whole force in the direction P T = i- + ^ (1 3 sin. 2 6) 

T S r 
and at A this becomes -V + - 

r 2 

at B 
at C 

r 2 


r 2 

. 2 

2 . S . r 

R 3 
R 3 

2 S. r 

r R 3 

(for though sin. 270 is , yet its syzygy is +). 

Thus it appears that on two accounts the orbit is more curved in the 
quadratures than in the syzygies, and assumes the form of an ellipse at 
the major axis A C. 



.*. the body is at a greater distance from the center in the quadratures 
than in the syzygies, which is Cor. 5. 

445. COR. 5. Hence the body P, caet. par., will recede farther from 
T in the quadratures than in the syzygies ; for since the orbit is less 
curved in the syzygies than in the quadratures, it is evident that the body 
must be farther from the center in the quadratures than in the syzygies. 

446. Con. 6. The addititious central force is greater than the ablati- 
tious from Q to P, and from P 7 to Q, but less from P to P , and from 
Q to Q , .". on the whole, the central attraction is diminished. But it 
may be said, that the areas are accelerated towards B and D, and .*. the 
time through P P may not exceed the time through P Q, or the time 
through Q Q exceed that through Q P. But in all the corollories, since 
the errors are very small, when we are seeking the quantity of an error, 
and have ascertained it without taking into account some other error, 
there will be an error in our error, but this error in the error will be an 
error of the second order, and may .*. be neglected. 

The attraction of P to T being diminished in the course of a revolution, 
the absolute force towards T is diminished, (being diminished by the 

S r r & 

mean disturbing force i _ s , 439,) .-. the period which . is 

R 3 V f 

increased, supposing r constant. 

But as T approaches S (which it will do from its higher apse to the 

lower) R is diminished, the disturbing force fwhich involves y] will be 

increased, and the gravity of P to T still more diminished, and .-. r will 
be increased ; . . on both accounts (the diminution of f and increase of r) 
the period will be increased. 

(Thus the period of the moon round the earth is shorter in summer 
than in winter. Hence the Annual equation in astronomy.) 

When T recedes from S, R is increased, and the disturbing force di 
minished and r diminished. . . the period will be diminished (not in com 
parison with the period round T if there were no body S, but in compari 
son with what the period was before, from the actual disturbance.) 

T 1 C 

447. COR. 6. The whole force of P to T in the quadratures = ^-+-, 1 

r 2 R s 

T 2Sr 

--- the syzygies = -- 

. . on the whole the attraction of P to T is diminished in a revolution. 
For the ablatitious force in the syzygies equals twice the addititious force 
in the quadratures. 


At a certain point the ablatitious force zr the addititious; when 

1 = 3 sin. 2 6 

sill - = V3 

A = 55, &c. 


(the whole force being then = j. 

Up to this point from the quadratures the addititious force is greater 
than the ablatitious force, and from this point to one equally distant from 
the syzygies on the other side, the ablatitious is greater than the addititious ; 
.. in a whole revolution P s gravity to T is diminished. 

Again since T alternately approaches to and recedes from S, the radius 

I* - 

P T is increased when T approaches S, and the period cc _____ ___ __ . 

V absolute force 

and since f is diminished, and .*. r increased, . . the periodic time is in 
creased on both accounts, (for f is diminished by the increase of the dis 

turbing forces which involve w.J If the distance of S be diminished, the 

absolute force of S on P will be increased, . .thedisturbingforces which QCyr-^ 
from S are increased, and P s gravity to T diminished, and .*. the periodic 
time is increased in a greater ratio than r 2 (because of the diminution of 

r f 
fin the expression -ry-yj and when the distance of S is increased, the dis 

turbing force will be diminished, (but still the attraction of P to T will be 
diminished by the disturbance of S) and r will be decreased, .*. the 


period will be diminished in a less ratio than r ^. 

448. COR. 7. To find the effect of the disturbing force on the motion 
of the apsides of P s orbit during one whole revolution. 


Whole force in the direction P T = -f TTT (1 ^ cos> * A) 
= T +T.c.r, (if T.c = 3 (l-3cos.A) = Tr + 3 - c - r4 > 

I i c 

. . the L. between the apsides =180 - - by the IXth Sect, which 

1 + 4 c 

is less than 180 when c is positive, i. e. from Q to P and from P to P, 


(fig. (446,)) and greater than 180 when c is negative, i. e. from P to P 
and from Q to Q , 

.. upon the whole the apsides are progressive, (regressive in the quadra 
tures and progressive in the syzygies) ; 

, T 3Sr 

force = -75 -- TTT" force m conjunction 

T 3 S i 1 

-f~ z -- ^ = force in opposition 


R 3 T 3Sr 3 A R 3 T 3Sr /3 
r R r 2 R 3 

differ most from and -=-$ 
r 2 r /z 

when r is least with respect to r , 

which is the case when the Apsides are in the syzygies. 

R 3 T+ Sr 3 R 3 T+ Sr 3 
r 8 R 8 ~?~ r R T ~ 

differ least from 2 an( ^ ~ when r is most nearly equal to r , 

449. COR. 7. Ex. Find the angle from the quadratures, when the apses 
are stationary. 

Draw P m parallel to T S, and = 3 P K, m n perpendicular to T P, 
resolve. P m into P n, n m, whereof n m neither increases nor diminishes 
the accelerating force of P to T, but P n lessens that force, .-. when P n 
= P T, the accelerating force of P is neither increased nor diminished, 
and the apses are quiescent, 

by the triangles PT:PK::PM=3PK:Pn-PT 
.*. in the required position 3 P K 2 = P T ~ 

P K = ~^= PT.sin. P, 
v o 


.. , 


6 = 35 26 . 
The addititious force P T P n is a maximum in quadratures. 

^ P 
F or P T : P K : : 3 P K : P n = 

.-. P T P n = PT 3 pJP , which is a maximum when P K = 0, 

or the body is in syzygy. 

450. COR. 8. Since the progression or regression of the Apsides de 
pends on the decrement of the force in a greater or less ratio than D 2 , from 
the lower apse to the upper, and on a similar increment from the upper 
to the lower, (by the IXth Sect.), and is .. greatest when the proportion 
of the force in the upper apse to that in the lower, recedes the most from the 
inverse square of D, it is manifest that the Apsides progress the fastest from 
the ablatitious force, when they are in the syzygies, (because the whole forces 
in conjunction and opposition, i. e. at the upper and lower apses being 

T 2 S r 

I -- rTT" > when the apsides are in the syzygies and when r is greatest 


at the upper apse, being least, and the negative part of the expression 

2 S r 
,, 3 being greatest, the whole expression is .. least, and when r is least, 


at the lower apse, ^ being greatest, and the negative part least, .. the 

whole expression is greatest, and .*. the disproportion between the forces at 
the upper and lower apse is greatest), and that they regress the slowest 

T S r 

in that case from the addititious force, (for + ^-^ , which is the whole 

v r 2 R 3 

force in the quadratures, both before and after conjunction, r being the 
semi minor axis in each case, differs least from the inverse square) ; there 
fore, on the whole the progression in the course of a revolution is greatest 
when the apsides are in the syzygies. 

Similarly the regression is greatest when the apsides are in the quadra 
tures, but still it is not equal to the progression in the course of the re- 

451. COR. 8. Let the apsides be in the syzygies, and let the force 
at the upper apse : that at the lower, : : D E : A B, D A 



being the curve whose ordinate is inversely 
as the distance 2 from C, . . these forces being 
diminished, the force D E at the upper apse 

2 r S 
by the greatest quantity -oT~ > anc ^ tne f rce 

A B at the lower apse by the least quantity 


J5-J- ; the curve a d which is the new force 

curve has its ordinates decreasing in a 
greater ratio than ^^ . 

Let the apsides be in the quadratures, then the force E D will be increased 

by the greatest quantity ^ , and the force A B by the least quantity 

S r 

^-j- , /. the curve a d which is the new force curve will have its 

ordinates decreasing in a less ratio than = 2 . 

451. COR. 9. Suppose the line of apsides to be in quadratures, then while the 
body moves from a higher to a lower apse, it is acted on by a force which 

1 R 3 T -f- S r 3 

does not increase so fast as -^~ 9 (for the force = r-^-, , .. the 

r^ R, 3 

numerator decreases as the denominator increases), . . the orbit will be 
exterior to the elliptic orbit and the excentricity will be decreased. Also as 

the descent is caused by the force -rr-^ (1 3 cos. 2 A), the less this 


force is with respect to - , the less will the excentricity be diminished. 

Now while the line of the apsides moves from the line of quadratures, the 
force p 3 ( 1 3 cos. 2 A) is diminished, and when it is inclined at z_ 35 


16 the disturbing force = 0, and .. at those four points the excentricity 
is unaltered. After this, it may be shown in the same manner that the 
excentricity will be continually increased until the line of apsides coin 
cides with the line of syzygies. Here it is a maximum, since the disturb 
ing force is negative. Afterwards it will decrease as before it increased 
until the line of apsides again coincides with the quadrature, and then the 
excentricity = maximum. 
(Hence Evection in Astron.) 


452. LEMMA. To calculate that part of the ablatitious force which is 
employed in drawing P from the plane of its orbit. 

Let A = angular distance from syzygy. 

Q = angular distance of nodes from syzygy. 
I = inclination of orbit to orbit of S and T. 

3 S r 

Then the force required = -jp- . cos. A . sin. Q . sin. I. (not quite 


When P is in quadratures, this force vanishes, since oos. A = 0. 

When nodes are in syzygy, since sin. Q = 0, 

quadratures, this force (cast, par.) = maxi 
mum, since sin. Q = sin. 90 = rad. 

453. COR. 12. The effects produced by the disturbing forces are all 
greater when P is in conjunction than when in opposition. 

For they involve -, .-. when R is least, they are greatest. 

454. COR. 13. Let S be supposed so great that the system P and T re 
volve round S fixed. Then the disturbing forces will be of the same kind 
as before, when we supposed S to revolve round T at rest. 

The only difference will be in the magnitude of these forces, which will 
be increased in the same ratio as S is increased. 

455. COR. 14. If we suppose the different systems in which S and S T 
oc, but P T and P and T remain the same, and the period (p) of P round 

T remains the same, all the errors p~3 a ~^7 , if A = density of S, 

and d its diameter, 

a <3 3 , if A given, and 3 = apparent diam. 

TTs a o~3 ^ P = period of T round S, 
.. the errors oc . 

These are the linear errors, and angular errors oc in the same ratio, 
since P T is given. 

456. COR. 15. If S and T be varied in the same ratio, 

S T 

Accelerating force of S : that of T : : rf -z : the same ratio as before. 

R 2 r- 

. . the disturbances remain the same as before. 

(The same will hold if R and r be also varied proportionally.) 
.. the linear errors described in P s orbit oc P T, (since they involve r), 

if P T oc, the rest remaining constant. 


i ,1 i r T> /> m linear errors P T 
also the angular errors of P as seen from T oc a __ oc i } 

and are . . the same in the two systems. 

The similar linear errors a f . T 2 , .-. P T a f . T \ and f 

P T P T 

-Fp-g- , but f a accelerating force of T on P oc , (p = period of P 

round T,) 

.-.Tap and .-. oc P 
c S P 3 

\ o T 1 Jr / 

COR. 14. In the systems 

S, T, P, Radii R, r Periods P, p 
S , T, P R , r P , p. 

Linear errors dato t. in 1st : do. in second : : p- 2 : p^ 

.*. angular errors in the period of P : : : - : -pj^ . 

COR. 15. In the systems 

S T P F? r P r 

J - 1 J x J "> - 1 " ~ * 9 P 

S , T, P R , r F, p , 


.%* =2.. 

, S T , R r 
so that -^ = ;=- and ^ 
o R r 


Linear errors in a revolution of P in 1 st. : do. in second : : r : r 
angular errors : ::!:!. 

COR. 16. In the systems 

S, T, P, R, r P, p 

S, T , P, R, i j P, p . 

Linear errors in a revolution of P in 1st. : do in second : : r p 2 : r p /s 
angular errors in a revolution of P : : : p 2 : p 2 . 

To compare the systems 

(1) S, T, P R, r P, p 

/O\ O/ TV T)/ T>/ ,,/ ID/ y-/ 

I ^ I O j J j JL *" -- JLV I ~" " " - -- "~ A , Li 

Assume the system 

(Q\ C/ T 1 p T} r p/ n 

l I ^ J J. j JL ^^ At* 5 J. JL A U 

.*. by (14) angular errors in P S revolution in (1) : in (3) . : -51 p7 Z 
by (16) angular errors in (3) : in (2) : : p 2 : p /2 

~ p/2 

therefore errors in (1) : in (2) : : p- 2 : ^- z 


Or assume the system (3) 2, T, P g, r n, p 

2 T Q r 

so that ~T- = -, -, = , 


/. the errors in (1) : errors in (3) : 

(3) : (2} 

I I S 

2 S R 3 

P 2 n 2 " R 3 

e 3 " 2 s 3 

:: 1 : 1 

. S S . R 3 R 3 . 

S T R 3 

r /3 

"S 7 2 R 3 3 * 

s , T R , 3 - 

r 3 

S r 3 . S r 73 

..P 2 .]. 

: : R 3 T : n f 3 * T 

pa p/ 2 * 

457. COR. 16. In the different systems the mean angular errors of 
P a ^~ whether we consider the motion of apses or of nodes (or errors 

in latitude and longitude.) 

For first, suppose every thing in the two different systems to be the same 
except P T, . . p will vary. Divide the whole times p, p , into the same 
number of indefinitely small portions proportional to the wholes. Then if 
the position of P be given, the disturbing forces all cc each other cc P T 
and the space cc f . T 2 , .*. the linear errors generated in any two corre 
sponding portions of tune cc P T . p 2 . 

.. the angular errors generated in these portions, as seen from T, oc p 2 . 

.. Cornp . the periodic angular errors as seen from T x p 2 . 

Now by Cor. 14, if in two different systems P T and .. p be the same, 
every thing else varying, the angular errors generated in a given time, as in 


.. neutris datis, in different systems the angular errors generated in the 

P 2 
time p oc jl^ . 


// . // . . P_ 2 . JL 


.*. the angular errors generated in 1" (or the mean angular errors) or . 

Hence the mean motion of the nodes as seen from T cc mean motion 

of the apses, for each oc 

458. COR. 17. 

Mean addititious force : mean force of P on T : : p z : P 2 . 

mean addititious force : force of S on T : : P T : S T, 



Sr S 



S T 
force of S on T : mean force of T on P: : r- : ^ { *"- 


force oc 




.-. mean addititious force : mean force of T on P: : p 2 : P 2 

.*. ablatitious force : mean force of T on P: : 3 cos. 6 . p 
Similarly, the tangential and central ablatitious and all the forces may 
be found in terms of the mean force of T on P. 

459. PROP. LXVII. Things being as in Prop. LXVI, S describes 
the areas more nearly proportional to the times, and the orbit more ellipti 
cal round the center of gravity of P and T than round T. 

P T 

For the forces on S are 




.-. the direction of the compound force lies between S P, S T; and T 
attracts S more than P. 

.. it lies nearer T than P, and .. nearer C the center of gravity of T 
and P. 

. . the areas round C are more proportional to the times, than when 
round T. 

Also as S P increases or decreases, S C increases or decreases, but S T 
remains the same ; .*. the compound force is more nearly proportional to 
the inverse square of S C than of S T; . . also the orbit round C is move 
nearly elliptic (having C in the focus) than the orbit round T. 




460. To find the axis major of an ellipse, whose periodic time round 
S at rest would equal the periodic time of P round S in motion. 

Let A equal the axis major of an ellipse described round P at rest 
equal the axis major of P Q v. 

Let x equal the axis major required, 

P. T. of P round S in motion : p S at rest : : V S : V S + P 

3 3 

P. T. of p in the elliptic axis A : P. T. in the elliptic axis x : : A 2 : x * 
.-. P. T. of P round S in motion : P.T. in the x : : V A 3 !* : Vx 3 (S+P). 
By hyp. the 1st term equals the 2d, 

.-. A 3 S = x 3 . S + P 

461. PROP. LXIII. Having given the velocity, places, and directions 
of two bodies attracted to their common center of gravity, the forces vary 
ing inversely as the distance 2 , to determine the actual motions of bodies in 
fixed space. 

Since the initial motions of the bodies are given, the motions of the center 
of gravity are given. And the bodies describe the same moveable curve 
round the center of gravity as if the center were at rest, while the center 
moves uniformly in a right line. 

* Take therefore the motion of the center proportional to the time, 
i. e. proportional to the area described in moveable orbits- 

* Since a body describes some curve in fixed space, it describes areas in proportion to the times 
in this curve, and since the center moves uniformly forward, the space described by it is in pro 
portion to the time, therefore, &c. 




462. Ex. 1. Let the body P describe a circle round C, while the center C 
moves uniformly forward. Take C G : C P : : v of C : v of P, and with the 

center C and rad. C G describe a circle G C N, and suppose it to move 
round along G H, then P will describe the trochoid P L T, and when P 
has described the semicircle P A B, P will be at the summit of the trochoid 

.*. every point of the semicircumference G F N will have touched G H, 

.. G H equals the semicircumference G F N, 

.-. v of P : v of C : : P A B semicircumference : C 11 = G F N semicircle 
* : : C P : C G Q. e. d. 

463. Ex. 2. Let the moveable curve 
be a parabola, and let the center of gravity 
move in the direction of its primitive 
axis. When the body is at the vertex 
A , let S be the position of the center 
of gravity, and while S has described 
uniformly S S, let A have described the 
arc of the parabola A P. 

Let A N = x, N P = y, be the ab-A S 
scissa and ordinate of the curve A P in fixed space. 

Let 4 p equal the parameter of the parabola A P. 

.-. A N = f- , A S = S S = x _ = 
4p 4p 

SN = AN A S = A N p = -? 





= s . Xl __ i y 3 4 P y _ y 3 + I2p g y 

3 4p ^ 4 p 24 p 

By Prop. S S oo A S P ; therefore they are in some given ratio. 

Let A S P : S S : : a : b : : 

24 p 

4 p 

* If C P = C G the curve in fixed space becomes the common cycloid. 
If C P > C G -- - --- the oblongated trochoid. 




. . y 3 -f 12p 2 y = 4pax ay* 
.-. y 3 + ay 2 + 12 p 8 y 4pax == 0. 
Equation to the curve in fixed space. 
464. Ex. 3. * Let B B be the orbit of the earth round the sun, M A 

that of the moon round the earth, then the moon will, during a revolution, 
trace out a contracted or protracted epicycloid according as A L has a 
greater or less circumference than A M, and the orbit of the moon round 
the sun will consist of twelve epicycloids, and it will be always concave to 
the sun. For 

R r 

F of the earth to the sun : F of the moon to the earth : : p-j : t 

400 1 

(365) 2 (27) 2 

in a greater ratio than 2:1. But the force of the earth to the sun is 
nearly equal to the force of the moon to the sun, . .the force of the moon 
to the earth, .-. the deflection to the sun will always be within the tan 
gential or the curve is always concave towards the sun. 

465. PROP. LXVI. If three bodies attract each other with forces 


varying inversely as the square of the distance, but the two leas: revolve 

To determine the nature of the curve dwribed by the moon with respect to the sun. 
VOL. I. Z 


about the greatest, the innermost of the two will more nearly describe the 
areas proportional to the time, and a figure more nearly similar to an el 
lipse, if the greatest body be attracted by the others, than if it were at rest, 
or than if it were attracted much more or much less than the other bodies. 
(L M : P T : : S L : S P, 

.-. L M oc 
.-. L M = 

SP 3 * 

S P S P 3 

.-. S K 2 : SP* : : SL : S P). 

Let P and S revolve in the same plane about the greatest body T, and 
P describe the orbit P A B, and S, E S E. Take S K the mean distance 
of P from S, and let S K represent the attraction of P to S at that dis 
tance. Take SL : SK :: SR 2 : SP 2 , and SL will represent the 
attraction of S on P at the distance S P. Resolve it into two S M, and 
L M parallel to P T, and P will be acted upon by three forces P T, L M, 
S M. The first force P T tends to T , and varies inversely as the dis 
tance 2 , .. P ought by this force to describe an ellipse, whose focus is T. 
The second, L M, being parallel to P T may be made to coincide with it 
in this direction, and .. the body P will still, being acted upon by a centri 
petal force to T, describe areas proportional to the time. But since L M 
does not vary inversely as P T, it will make P describe a curve different 
from an ellipse, and .*. the longer L M is compared with P T, the more 
will the curves differ from an ellipse. The third force S M, being neither 
in the direction P T, nor varying in the inverse square of the distance, will 
make the body no longer describe areas in proportion to the limes, and the 
curve differ more from the form of an ellipse. The body P will .*. describe 
areas most nearly proportional to the times, when this third force is a 
minimum, and P A B will approach nearest to the form of an ellipse, when 
both second and third forces are minima. Now let S N represent the 
attraction of S on T towards S, and if S N and S M were equal, P and 
T being equally attracted in parallel directions would have relatively the 
same situation, and if S N be greater or less then S M, their difference 
M N is the disturbing force, and the body P will approach most nearly 
the equable description of areas, and P A B to the form of an ellipse, 
when M N is either nothing or a minimum. 

Case 2. If the bodies P and S revolve about T in different planes, L M 
being parallel to P S will have the same effect as before, and will not 




tend to move P from its plane. But N M acting in a different plane, 
will tend to draw P out of its plane, besides disturbing the equable des 
cription of areas, &c. and as before this disturbing force is a minimum, 
when M N is a, minimum, or when S N = nearly S K. 

466. To estimate the magnitude of the disturbing forces on P, when P 
moves in a circular orbit, and in the same plane with S and T. 

Let the angle from the quadratures P C T = S, 

S T = d, P T = r, F at the distance (a) = M, 

F on P - Ma2 

. . From P in the direction S P : 

. . F in the direction P T = ^^] x 
But S P 2 = d 2 + r 2 2 d r sin. 0, 
.-. F in the direction P T = 

P T : : S P : P T, 


M a*r 

(d 2 + r * 2 d r sin. 6} f 

M a 2 r 


2 d r sin. 6 

d 3 r d 

IM. u. ~ r 

= 3-3 = A nearly, since d being indefinitely great compared with r 
in the expansion, all the terms may be neglected except two. First -i 
vanishes when compared with -r- 3 , .-. the addititious force in the direction 

T = A. By proportion as before, force in the direction S T 

Ma 2 ST Mad f 

: SP* SP " d 3 (1 + (r 2dr sin. 6 

Mji^ / 3 r 8 - 2 d r sin. 

d* \ ~ 2 d > 

_M a 2 3 M a 8 r 8 3 M a*r sin, t) 
d* 2 d 4 + " d 3 




.-. force in the direction S T = 


3 M a 2 r 

sin. t nearly, since 

it *-* 

1 1 Ma 2 

-, vanishes when compared with -, , and the force of S on T = rr- , 
d * d 3 d * 

Ma 2 3 M a r . Ma 2 

.-. ablatitious F = TV; }- rz sin - d Tr~ 

d- d* d* 

= 3 A . sin. 0. 

If P T equal the addititious force, then the ablatitious force equals 3 P K, 
for P K: PT: : sin. 6 : (1 = r), 

.-. 3 P K = 3 P T . sin. 6 = 3 A . sin. 6. 
To resolve the ablatitious force. Take 

P m : P n : : P T : T K : : 1 : cos. 6, 

3 A 

.-. P n = P in X cos. 6 = 3 A X sin. 6 cos. 6 = . sin. 2 6 

m n = P m X PK = 3A. sin. 2 6 = 3 A . * ~ C S> 2 *, 


.. the disturbing forces of S on P are 

M a 2 r 

1. The addititious force = p = A. 

2. The ablatitious force which is resolved into the tangential part 

q A J 2 COS A 

= - . sin. 2 6, and that in the direction T P = 3 A . = - , 

*^ ^ 

.. whole disturbing force in the direction P T = A 3 A . ^ - 

A 3 A 3 A ASA i-*iii 

= A j . cos. 2 6 = H ~ . cos. 2 6, and in the whole 

22 22 

revolution the positive cosine destroys the negative, therefore the whole 
disturbing force in a complete revolution is ablatitious, and equal to one 
half of the mean addititious force. 
467. To compare N M and L M. 

L M : P T : : (S L = |^) : S P, 
.-. L M = f p, X P T 


MN = 

3_SP 3 

v S T _ S T 

SP 3 S P 

SK 3 -(SK-KP) 3 

S P 3 
S K 3 S K* + 3 S R 2 x K P 

S P 3 
3 S K* x P K 


X ST nearly 

S P 

X S T nearly = 


= -g-pr X P T X sin. 6, 

.-. M N : L M : : 1 : 3 sin. 6. 

S P 

X P K 


468. Next let S and P revolve about T in different planes, and let 
N P N be P s orbit, N N the line of the nodes. Take T K in T S = 
3 A . sin. 6. Pass a plane through T K and turn it round till it is per 
pendicular to P s orbit. Let T e be the intersection of it with P s orbit. 
Produce T E and draw K F perpendicular to it, .-. K F is perpendicular 
to the plane of P s orbit, and therefore perpendicular to every line meet 
ing it in that orbit, T in the plane of S s orbit ; draw K H perpendicular 
to N N produced ; join H F, then F H K equals the inclination of the 
planes of the two orbits. For K H T, K F T, K F H being all right angles, 

KT* = K H* + HT* 
K F * + H = K F 2 + F H * + H T , 
* .-. F T * = F H 2 + H T , 

.. F H is perpendicular to H T. 
Since P T = A, T K = A x sin. 6 

Let the angle K H T = T, II T K e= <p = angular distance of the line of the no<!c 
from S y z. 







3 sin. t) 
sin. <p 
sin. T, 
3 sin. d . sin. 



/. ablatitious force perpendicular to P s orbit = K F 
= 3 P T X sin. 6. sin. p x sin. T = 3 A X sin. 6. sin. <p X sin. T. 
2d. Hence it appears that there are four forces acting on P. 


1. Attraction of P to T a 

2. Addititious F in the direction P T = 

3. Ablatitious F in the direction P T = 

M a*r 
d 3 * 
3 Ma 2 r 

sin. z 6. 

4. Tangential part of the ablatitious force = f . 

Ma ! 

sin. 2 6. 

Of these the three first acting in the direction of the radius-vector do 
not disturb the equable description of areas, the fourth acting in the di 
rection of a tangent at P does interrupt it. 

Since the tangential part of F is formed by the revolution of P M = 3 A X 
sin. & at C, 6 = 0, therefore P m = 0, and consequently the tangential 
F = ; from C to A, P n is in consequentia, and therefore accelerates 
the body P at A, it again equals 0, and from A to D is in antecedentia, 
and therefore retards P ; from D to B it accelerates; from B to C it re 

Therefore the velocity of P is greatest at A and B, because these are 
the points at which the accelerations cease and retardations begin, and 
the velocity is least at D and C. To find the velocity gained by the ac 

tion of the tangential force.* 

sin. 26d6 

* F in the direction P T is a maximum at the quadrature, because die ablatitious F in tie 
quadrature is 0, and at every other point it is something. 


sin. 2 6 X 20 = (cos. 2 0) , 

v 2 
. . Z = = Cor. | A. cos. 2 6. 


But when 6 = 0, the tangential F = 0, and no velocity is produced, 
.-. cos. 2 = R = ], 

(1 cos. 2 6} = | A. 2 sin. 2 6, 


.-. v 2 = 3g A. sui. 2 0, 
/. v = V 3 g A. sin. d, 
. . v a (sin. 0) , 

. . whole f on the moon at the mean distance : f of S on T : : - 2 : p^ 

* r 

and the force of S on T : add. f at the mean distance (m) : : :"4*s 

d d 

.*. whole f at the mean distance : m : : P s : p 2 and ~- t X whole f &c. = in. 

f or 
Now f on the moon at any distance (r) = ^-j- 3 and at the mean 

distance (1) = f ^L- 3 = f , 

_ p 2 f m p 1 

.*. m = 


JL ** A 

2p 2 f 
2 P 8 + p 

and therefore nearly = ~ ^ p4 , 

( p 2 2 p 4 ) 
.\ in r (which equals the addititious force) = | rfl BT" J 

469. To compare the ablatitious and addititious forces upon the moon, 
with the force of gravity upon the earth s surface. (Newton, Vol. III. 
Prop. XXV.) 

add. f : f of Son T :: PT : ST 

S T P V P T 

f of S on T : f of the earth on the moon : : -. Tj - : ^- = , 

.. add. f : f of the earth on the moon : : p 2 : P 2 
f of the earth on the moon : force of gravity :: 1 ; 60 5 , 

.% add. f : force of gravity :: p* : P 2 . GO 2 . . . (]) 
Also ablat. f : addititious force : : 3 P K : P T, 

.-. ablat. f : addititious force : : 3 P K . p * : 60 2 . P T. P s . (2) 

470. Con. 2. In a system of three bodies S, P, T, force oc* -,- the 



body P will describe greater areas in a given time at the syzygies than at 
the quadrature. 

The tangent ablatitious f = f . P T . sin. 2 6 ; therefore this force will 
accelerate the description of areas from quadratures to syzygies and retard 
it from syzygies to quadratures, since in the former case sin. 2 6 is positive, 
and in the latter negative. 

COR. 3. is contained in Cor. 2. 

The first quadrant d. sin. being positive the velocity increases, 
in the second d. sin. negative the velocity decreases, &c. for the 1st Cor. 
2d Cor. &c. 

Also v is a maximum when sin. 8 is a maximum, i. e. at A and B. 

471. COR. 4. The curvature of P s orbit is greater in quadratures than 
in the syzygy. 

Ma 2 Ma e r 3Mar.. B - 

The whole F on P = -^7- -\ -- -p --- ~2~[3~ ( l ~~ cos> ) X 

/3 M a 3 r . sin. 2 6\ 
\ 2 d 3 / 

In quadratures sin. 20=0, 

F M a 2 M a * r 
~^~ ~d^~ 
And in syz. 29= 180, 

.-. sin. 20 = 0, cos. 201 

3Ma g r 3 M a g r 

TTF""*" d 3 

, , v . M a J 2 M a * r 

.*. the whole if on P in the svz. = - r- --- , 

r 2 d 

.. F is greater in the quadratures than in the syzygies; and the velocity 
is greater in the syzygies than in the quadratures. 

1 T* 

But the curvature a p-^r cc v 2 , .. is greatest in the quadratures and 

least in the syzygies. 

472. COR. 5- Since the curvature of P s orbit is greatest in the quadra 
ture and least in the syzygy, the circular orbit must assume the form of an 
ellipse whose major axis is C D and minor A B- 

.*. P recedes farther from T in the quadrature than in the syzygy. 

473. COR. 6. 

The whole F on P in the line PT = 

.Ma 2 
= in quad. 5 

BOOK i.] 



M a * 2 M a 2 r 
and in syz. = o 

let the ablatitious force on P equal the addititious, and 
M a 2 r 3 M a 2 r 

. sin. 2 6 


/. sin. Q = =- sin. 35 . 16. 
V 3 

Therefore up to this point from quadrature the ablatitious force is less 
than the addititious, and from this to one equally distant from the other 
point of quadrature, the ablatitious is greater than the addititious, therefore 
in a whole revolution the gravity of P to T is diminutive from what it 


would be if the orbit were circular or if S did not act, and P a - , - ~ 

\ abl. r 

and since the action of S is alternately increased or diminished, therefore 
P ex from what it would be were P T constant, both on account of the 
variation, and of the absolute force. 

474. COR. 7. * Let P revolve round T in an elliptic orbit, the force on 

Ma 2 , Ma 2 r , b 
P in the quad. = --,- H ^ + - 2 + c r. 

.-. G + 180 

and since the number is greater than the de- 

b + 4 c 

nomination G is less than 180. . . the apsides are regressive if the same 
effect is produced as long as the addititious force is greater than the abla 
titious, i. e. through 35. 16 . 

The force on P in the syz. = 


2Ma l r 

* Since P a 


and in whiter the sun is nearer the earth than in summer, 

V ablatitious force 

R Js increased in winter, and A i diminished, therefore the lunar months are shorter in vrintor 
than in summer. 


= 180 . /, ~ I C > 180 
V b 8 c 

m c 

.*. in the syz. the apsides are progressive, and since / : will be 

an improper fraction as long as the ablatitious force is greater than the 
addititious, and when the disturbing forces are equal, m c = n c, therefore 
G = 180, i. e. the line of apsides is at rest (or it lies in V C produced 
9th.) .*. since they are regressive through 141. 4 and progressive 
2 18. 56 they are on the whole progressive. 

To find the effect produced by the tangential ablatitious force, on the 
velocity of P in its orbit. Assume u = velocity of a body at the mean 

distance 1, then = velocity at any other distance r nearly, the orbit 

being nearly circular. 

Let v be the true velocity of P at any distance (r), vdv = gFdx 

( f = 16 12 For the tan S ent ablatitious f = f . P T . 2 0, and x = r 
= 3 P T . m r . sin., 

.-. v 2 = 3 P T m r cos. 2 6 + C, 


v 2 - - frr 

V n C\A - 

f " 

Hence it appears that the velocity is greatest in syzygy and least in 
quadrature, since in the former case, cos. 2 d is greatest and negative, and 
in the latter, greatest and positive. 

To find the increment of the moon s velocity by the tangential force 
while she moves from quadrature to syzygy. 

v 2 = 3 P T . m . r . cos. 2 6 + C, 

but (v) the increment = 0, when 6 = 0, 
.-. C = 3 P T . m . r, 

.-. v 2 = 3 P T . m . r (1 cos. 2 6) = G P T. m. r. sin. 8 0, 
and when d = 90, or the body is in syzygy v " = 6 P T rn . r. 

475. COR. 6. Since the gravity of P to T is twice as much diminished 
in syzygy as it is increased in quadrature, by the action of the disturbing 
force S, the gravity of P to T during a whole revolution is diminished. 
Now the disturbing forces depend on the proportion between P T and 
T S, and therefore they become less or greater as T S becomes greater 


or less. If therefore T approach S, the gravity of P to T will be still 
more diminished, and therefore P T will be the increment. 

Now P. T cc - ; since, therefore, when S T is di- 

V absolute force 

minished, R is increased and the absolute force diminished (for the ab 
solute force to T is diminished by the increase of the disturbing force) the 
P . T is increased. In the same way when S T is increased the P . T is 
diminished, therefore P. T is increased or diminished according as S T 

* O 

is diminished or increased. Hence per. t of the moon is shorter in winter 
than in summer. 


476. COR. 7. To find the effect of the disturbing force on the motion 

of the apsides of P s orbit during a whole revolution. 

Let f = gravity of P to T at the mean distance ( 1 ), then = gravity 

of P at any other distance r. 

f f 

Now in quadrature the whole force of P to T = - a -f- add. f = 2 + r 

= 3 and with this force the distance of the apsides = 180 / ^ 

which is less than 180, therefore the apsides are regressive when the 


body is in quadrature. Now in syz. the whole force of P to T = 

r 2 
f r g r 4 

2 r = - y , therefore the distance between the apsides = 180 

, f 2 

fij f 8 which is greater than 180, therefore the apsides are progressive 

when the body is in syzygy. 

But as the force (2 r) which causes the progression in syzygy is double 
the force (r) which causes the regression in quadrature, the progressive 
motion in syzygy is greater than the regressive motion in the quadrature. 
Hence, upon the whole, the motion of the apsides will be progressive 
during a whole revolution. 

At any other point, the motion of the apsides will be progressive or 

P T S P T 

retrograde, according as the whole central force + ^ . cos. 2 i) 

t & 

is negative or positive. 




477. COR. 8. To calculate the disturbing force when P s orbit is ex- 


P T 3 P T 

The whole central disturbing force = -f- cos. 26=. 

-\ s . cos. 2 6 (m is the mean add. f). Now r = 

1 e 

= by div. 1 e 2 + e . cos. u + e 2 . cos. 2 u, &c. neglecting terms in- 

e 2 e 2 

volving e 3 , &c. = 1 + e . cos. u + . cos. 2 u ; therefore the 

whole central disturbing force = 


m e 

m . e . cos. u 

me 8 cos. 2 u , 3 3 in e - o 

-, - + -~- ni cos. 2 6 . cos. 2 6 + m e . cos. u . cos. 2 6 

^r *w * 

-f | m e ". cos. 2 u . cos. 2 6. 

478. COR. 8. It has been shown that the apsides are progressive in 
syzygy in consequence of the ablatitious force, and that they are regres 
sive in quadrature from the effect of the ablatitious force, and also, that 
they are upon the whole progressive. It follows, therefore, that the 
greater the excess of the ablatitious over the addititious force, the more will 
the apsides be progressive in the course of a revolution. Now in any 
position m M of the line of the apsides, the excess of the ablatitious in 
conjunction 2 A T in opposition = T B, therefore the whole excess 
= 2 A B. Again, the excess of the addititious above the ablatitious force 
in quadrature = C D. Therefore the apsides in a whole revolution will 
be retrograde if 2 A B be less than C D, and progressive if 2 A B be 
greater than C D. Also their progression will be greater, the greater the 
excess of 2 A B above C D ; but the excess is the greatest when M m is 
in syzygy, for then A B is greatest and C D the least. Also, when M in 
is in syzygy the apsides being progressive are moving in the same direc 
tion with S, and therefore will remain for some length of time in syzygy. 
Again, when the apsides are in quadrature A B = P p, and C D = M m, 



but if the orbit be nearly circular, 2 A B is greater than C D ; therefore 
the apsides are still in a whole revolution progressive, though not so 

much as in the former case. 


In orbits nearly circular it follows from G = = when F a AP- S , 

V r 

that if the force vary in a greater ratio than the inverse square, the 
apsides are progressive. If therefore in the inverse square they are sta 
tionary, if in a less ratio they are regressive. Now from quadrature to 
35 a force which <x the distance is added to one varying inversely as 
the square, therefore the compound varies in a less ratio than the inverse 
square, therefore the apsides are regressive up to this point. At this point 

F <x -T. ; , therefore they are stationary. From this to 35 from 

distance 2 

another Q a quantity varying as the distance is subtracted from one 
varying inversely as the square, therefore the resulting quantity varies 
in a greater ratio than the inverse square, therefore the apsides are 
progressive through 218. 


479. COR. 8. It has been shown that the apsides are progressive in 
syzygy in consequence of the ablatitious force, and that they are regressive 
in the quadratures on account of the addititious force, and they are on the 
whole progressive, because the ablatitious force is on the whole greater 
than the addititious. . . the greater the excess of the ablatitious force 
above the addititious the more will be the apsides progressive. 

In any position of the line A B in conjunction the excess of the ablati 
tious force above the addititious is 2 P T, in opposition 2 p t. .*. the whole 
excess in the syzygies = 2 P p. In the quadratures at C the ablatitious 
force vanishes. /. the excess of the addititious = additious = C T. 
.*. the whole addititious in the quadratures = C D. 

Now the apsides will, in the whole revolution, be progressive or regres 
sive, according as 2 Pp is greater or less than C D, and then the progres 
sion will be greatest in that position of the line of the apses when 2 P p 
C D is the greatest, i. e. when A B is in the syzygy, for then 2 P p 
2 A B, the greatest line in the ellipse, and C D = R r =r ordinate = 
least through the focus. .*. 2 P p CD is a maximum. Also when 
A B is in the syzygy, the line of apsides being progressive, will move the 
same way as S. .. it will remain in the syzygy longer, and on this account 
the apsides will be more progressive. But when the apsides are in the 
quadratures S P = R r and C D = A B, and the orbit being nearly 
circular, R r nearly equals A B. . . 2 P p C D is positive, and the 


apsides are progressive on the whole, though not so much as in the last 
case ; and the apsides being regressive in the quadratures move in the op 
posite direction to S, .*. are sooner out of the quadratures, .. the regres 
sion in the quadrature is less than the progression in the syzygy. 

480. COR. 9. LEMMA. If from a quantity which GC -r-^ any quantity 


be subtracted which a A the remainder will vary in a higher ratio than 

the inverse square of A, but if to a quantity varying as ^- z another be 


added which a A, the sum will vary in a lower ratio than -r-g . 

1 j c A 2 

If be diminished C A = 7-= . If A increases 1 c A * 

A 2 A z 

decreases, and -r-j increases. . . the quantity decreases, 1 c A increases 


and -r-j- increases. .-. increases from both these accounts. . . the whole 

A i 

quantity varies in a higher ratio than -^ . 

1 4- c A 2 

If C A be added -r-g , as A is increased the numerator increases, 

and -j-g decreases. . . the quantity does not decrease so fast as -j- s , and 
A. A 

if A be diminished 1 + c A 2 is diminished, and -^ increased. . . the 
quantity is not increased as fast as -r- 2 . .-. &c. Q. e. d. 


481. COR. 9. To find the effect of the disturbing force on the excen- 

tricity of P s orbit. If P were acted on by a force a -j- z , the excentricity 

of its orbit would not be altered. But since P is acted on by a force vary 
ing partly as r z and partly as the distance, the excentricity will continual 
ly vary. 

Suppose the line of the apsides to coincide with the quadrature, then 
while the body moves from the higher to the lower apse, it is acted upon 

by a force which does not increase so fast as -p } for the force at the quad- 


rature = + m r, and /. the body will describe an orbit exterior to the 
elliptic which would be described by the force a - . Hence the body 


will be farther from the focus at the lower apse than it would have been 
had it moved in an elliptic orbit, or the excentricity is diminished. Also 
as the decrease in excentricity is caused by the force (m r), the less this 

force is with respect to z , the less will be the diminution of excentricity. 

Now while the line of apsides moves from the line of quadratures, the force 
(m r) is diminished, and when it is inclined at an angle of 35 16 the 
disturbing force is nothing, and .*. at those four points the excentricity 
remains unaltered. After this it may be shown in the same manner that 
the excentricity will be continually increased, until the line of apsides 
coincides with the syzygies. Hence it is a maximum, since the disturbing 
force in these is negative. Afterwards it will decrease as before it in 
creased, until the line of apsides again coincides with the line of quadra 
ture, and the excentricity is a minimum. 

COR. 14. Let P T = r, S T = d, f = force of T on P at the distance 
1, g = force of S on T at the distance, then the ablatitious force 

= ~n J if " the position of P be given, and d varies, the ablati 
tious force cc -p . But when the position of P is given, the ablatitious 
: addititious : : in a given ratio, . . addititious force cc -p , or the dis 
turbing force cc ^ . Hence if the absolute force of S should x the dis- 

i if 
turbing force cc r^ - . Let P = the periodical time of T about S, 

.. p-- cc -j^ * . Let A = density, 8 = diameter of the sun, then the 

A .X 3 1 

absolute force <x A d 3 , then the disturbing force a j cc p-^ cc A (ap 
parent diameter) 3 of the sun. Or since P T is constant, the linear as well 
as the angular errors oc in the same ratio. 

483. Con. 15. If the bodies S and T either remain unchanged, or their 
absolute forces are changed in any given ratio, and the magnitude of the 
orbits described by S and P be so changed that they remain similar to 
what they were before, and their inclination be unaltered, since the accel- 

c rr-rr. i A - r r o absolute force of T 
crating force ot P to i : accelerating force of S : : p : 

absolute force of S , , r . , 

r r z , and the numerators and denominators of the last 

o JL 

terms are changed in the same given ratio, the accelerating forces remain 
in the same ratio as before, and the linear or angular errors cc as before, 




i. e. as the diameter of the orbits, and the times of those errors oc P T s 
of the bodies. 

COR. 16. Hence if the forms and inclinations of the orbits remain, and 
the magnitude of the forces and the distances of the bodies be changed ; to 
find the variation of the errors and the times of the errors. In Cor. 14. 

it was shown, how that when P T remained constant, the errors oc ^ . 

Now let P T also a , then since the addititious force in a given position 
of P oc P T, and in a given position of P the addititious : ablatitious in 
a given ratio. 

COK. If a body in an ellipse be acted upon bv a force which varies 
in a ratio greater than the inverse 
square of the distance, it will in de 
scending fromthe higher apse Bto the 
lower apse A, be drawn nearer to the ^ 

center. .*. as S is fixed, the excen- 
tricity is increased, and from A to B 
the excentricity will be increased 
also, because the force decreases the faster the distance 2 increases. 

484. (CoR. 10.) Let the plane of P s orbit be inclined to the plane of T s 
orbit remaining fixed. Then the addititious force being parallel to P T, 
is in the same plane with it, and . . does not alter the inclination of the 
plane. But the ablatitious force acting from P to S may be resolved into 
two, one parallel, and one perpendicular to the plane of P s orbit. The 
force perpendicular to P s orbit = 3 A X sin. 6 X sin. Q X sin. T 
when d perpendicular distance of P from the quadratures, Q = angular 
distance of the line of the nodes from the syzygy, T = first inclination of 
the planes. 

Hence when the line of the nodes is in the syzygy, 6 0, 
.. no force acts perpendicular to the plane, 
and the inclination is not changed. When 
the line of the nodes is in the quadratures, 
d = 90, /. sin. is a maximum, . . force per 
pendicular produces the greatest change / 
in the inclination, and sin. & being posi 
tive from C to D, the force to change the 
inclination continually acts from C to D 
pulling the plane down from D to C. Sin. d 
is negative, .*. force which before was posi- 

sin. = 



tive pulling down to the plane of S s orbit (or to the plane of the paper) 
now is negative, and . . pulls up to the plane of the paper. But P s orbit is 
now below the plane of the paper, . . force still acts to change the inclina 
tion. Now since the force from C to D continually draws P towards the 
plane of S s orbit, P will arrive at that plane before it gets to D. 

If the nodes be in the octants past the quadrature, that is between C 
and A. Then from N to D, sin. 6 being positive, the inclination is di 
minished, and from Dto N increased, .*. inclination is diminished through 
270, and increased through 90, . . in this, as in the former case, it is 
more diminished than increased. When the nodes are in the octants be 
fore the quadratures, i. e. in G H, inclination is decreased from H to C, 
diminished from C to N, (and at N the body having got to the highest 
point) increased from N to D, diminished from D to N , and increased 
from 2 N to H, . . inclination is increased through 270, and diminished 
through 90, /. it is increased upon the whole. Now the inclination of 
P s orbit is a maximum when the force perpendicular to it is a minimum, 
i. e. when (by expression) the line of the nodes is in the syzygies. When 
is the quadratures, and the body is in the syzygies, the least it is increased 
when the apsides move from the syzygies to the quadratures ; it is dimin 
ished and again increased as they return to the syzygies. 

485. (CoR. 11.) While P moves from the quadrature in C, the nodes 
being in the quadrature it is drawn towards S, and .*. comes to the plane 
of S s orbit at a point nearer S than N or D, i. e. cuts the plane before it 
arrives at the node. . . in this case the line of the nodes is regressive. In 
the syzygies the nodes rest, and in the points between the syzygies and 
quadratures, they are sometimes progressive and sometimes regressive, 
but on the whole regressive; .. they are either retrograde or stationary. 

486. (CoR. 12.) All the errors mentioned in the preceding corollaries are 
greater in the syzygies than in any other points, because the disturbing 
force is greater at the conjunction and opposition. 

487. (CoR. 13.) And since in deducing the preceding corollaries, no re 
gard was had to the magnitude of S, the principles are true if S be so 
great that P and T revolve about it, and since S is increased, the disturbing 
force is increased ; .-. irregularities will be greater than they were before. 

Ma 2 r ^ T VT ^ r 3 Ma 


488. (CoR. 14.) L M = ^j^- = N N M = " ^ , sin. 6, .-. in 
a given position of P, if P T remain unaltered, the forces N M and L M 

VOL. T. A a 


cc -.-. X absolute force cc --^ - of T for (sect. 3 . P 2 oc 
j 2 

-.-. --^ - . . 

d j (Per. T) 2 absolute f. 

whether the absolute force vary or be constant. Let D = diameter of S, 
<3 = density of S, and attractive force of S cc magnitude or quantity of 
matter oc D 3 3, 

D 3 & 

/. forces L M and N M cc -TT-. 

d 3 

But r = apparent diameter of S, 

.-. forces cc (apparent diameter) 3 3 another expression. 

489. (CoR. 15.) Let another body as P revolve round T in an orbit 
similar to the orbit of P round T, while T is carried round S in an orbit 
similar to that of T round S, and let the orbit of P be equally inclined to 
that of T" with the orbit P to that of T. Let A, a, be the absolute forces 
of S, T, A , a , of S , T , 

A a 

accelerating force of P by S : that of P by T : : ~ p 2 : p ^ , 

and the orbits being similar 

A a 

accelerating force of P by S : that of P by T : : ~ p/ 2 : p}-^ , 

.. if A : a : : A : a, and the orbits being similar, 

S P : P T * : : S F : F T , 
accelerating force of P by S : that of P by T 
: : force on P by S : force on P by T , 
and the errors due to the disturbing forces in the case of P are as 

A A 

cT>t r 3 x r i n l ^ e case f -f" an d S are as Q , ^3 X R, 
o L o JL 

.. linear errors in the first case : that in the second : : r : R. 
sin. errors 

Angular errors cc 


in the first cas 

linear errors 

angular errors in the first case : that in the second : : 1 : 1. 

Now Cor. 2. Lem. X. T 2 a 

T C 

angular errors 

.\ T 2 x angular errors, 
.-. angular errors : 360 : : T 2 : P 2 , 

.-. T 2 a P 2 X angular errors, 
.-. T oc P for = angular errors. 


490. (Con. 16.) Suppose the forces of S, P T, ST to vary in any man 
ner, it is required to compare the angular errors that P describes in simi 
lar, and similarly situated orbits. Suppose the force of S and T to be 
constant, . . addititious force x P T, . . if two bodies describe in similar 
orbits = evanescent arcs. Linear errors x p 2 X P T. 

.-. angular errors x p 2 (p = per. time of P round T, P = that of T 
round S). But by Cor. 14. if P T be given, the absolute force of A and 

Angular errors x -yyy 

.*. if P T, S T and the absolute force alternately vary, 
angular errors x ~- , 

/P = per. time of P round T\ f M a 2 r 

Vp = per. time of T round S J ~dP~ 

, linear errors 

angular errors x p . 


M a 2 r 

.-. lin. errors x force T ! a pr X P 2 by last Cor. 

d 3 

, rP 2 P\ 

/. angular errors x x r ) . 

d 3 X r p 2 / 

M a 2 
Now the errors d t X p = whole angular errors x -L , 

.*. error d t x -,y- 2 thence the mean motion of the apsides x mean motion 

of the nodes, for each x J , for each error is formed by forces varying as 

proof of the preceding corollaries, both the disturbing forces, and .-. the 
errors produced by them in a given time will x P T. Let P describe an 
indefinite small angle about T (in a given position of P), then the linear 
errors generated in that time x force T P time 2 , but the time of describ 
ing = angles about T x whole periodic time (p), . . linear errors x 
P T p *, and as the same is true for every small portion, similar; the 
linear errors during a whole revolution x P T p 2 . Angular errors 

lincni* cr 
x -j .-. oc p * . when S T, P T, and the absolute force vary, the 

p 2 absolute p * p * 
angular errors a p~ a g ^ 3 a g*,_ , (when the absolute force is 

A a2 


given.) Now the error in any given timex p varies the whole errors during 

P 2 P 

a revolution a ~- z . .*. the tfrrors in any given time oc p- 2 . Hence the 

mean motion of the apsides of P s orbit varies the mean motion of the 
nodes, and each will a -~ 3 the excentricities and inclination being small 

and remaining the same. 

491. (CoR. 17.) To compare the disturbing forces with the force of 

FofSonT:FofPonT: absoluteF a 


ST 2 T P ! 

absolute F . A. ST . aTP 

axis major 3 SS 3 T P s 

. S.T . TP . ^L 

* * P 2 " D * " " p 2 

mean add. F : F of S on T : : ^^ : ^- : : 

.-. mean add. F : F P on T : : p 2 : P . 

492. To compare the densities of different planets. 

Let P and P be the periodic times of A and B, r and r their distances 
from the body round which they revolve. 

F of A to S : F of B to S : : ~ : ^ 

quantity of matter in A do. in B m D 3 of A X density ^ D 3 of Bx density 
distance 2 distance 2 distance 8 distance * 

r r> 

p 2 p/ 2 

D 3 xd 

D /3 xd 1 1 

r 3 

r 3 p e p/ 2 

r 3 r /3 

A V 

..a. a > -p 3 p s j-j/ 3 p/ E 

1 1 

* S 3 P 2 3 p/ J 

where S and S represent the apparent diameters of the two planets. 

493. In what part of the moon s orbit is her gravity towards the earth 
unaffected by the action of the sun. 

Ma 2 r 3Ma 2 r U cos. 2 ^ + 3 Ma r^ ^ 

2 ~ 2 d 3 

and when it is acted upon only by the force of gravity = for the 
other forces then have no effect. 




M a*r 



a 2 

T 1 COS 

. 2 

1 3 

M a 2 r . 

) n 

d 3 




1 2 

d J 




cos. 2 6 t 

"3 s 

;in. 2 6 










cos. 2 6 + 


sin. 2 

a = o 




1 sin. 

2 C 






+ 2 

Let x = sin. 6, 

(.-. 1 f + | | sin. * + | X 2 sin. x cos. d = 0) 

3x 2 


+ 3 x V 1 x 


An equation from which x may be found. 

494. LEMMA. If a body moving towards a plane given in position, be 
acted upon by a force perpendicular to its motion tending towards that plane, 
the inclination of the orbit to the plane will be increased. Again, if the body 
be moving from the plane, and the force acts from the plane, the inclina 
tion is also increased. But if the body be moving towards the plane, and 
the force tends from the plane, or if the body be moving from the plane, 
and the force tends towards the plane, the inclination of the orbit to the 
plane is diminished. 

495. To calculate that part of the ablatitious tangential force which is 
employed in drawing P from the plane of its orbit. 

Let the dotted line upon the ecliptic N A P N be that part of P s orbit 
which lies above it. Let C D be the intersection of a plane drawn per 
pendicular to the ecliptic ; P K perpendicular to this plane, and there- 





fore parallel to the ecliptic. Take T F = 3 P K ; join P F and it will 
represent the disturbing force of the sun. Draw P i a tangent to, and 
F i perpendicular to the plane of the orbit. Complete the rectangle i m, 
and P F may be resolved into P m, P i, of which P m is the effective force 
to alter the inclination. Draw the plane F G i perpendicular to N N ; 
then F G is perpendicular to N N . Also F i G is a right angle. As 
sume P T tabular rad. Then 

: : R : s >- . 
: : R : i J * 

PT: Pm :: R 3 : 3g. s. i 
_ PT.3g. s. i 

Pm = 


PT: TF:: 
T F : F G 
FG: Pm 

g = sin. 6 =r sin. L dist. from quad. 

s = sin. <p = sin. /_ dist. of nodes from syz. 

i =r sin. F T i = sin. F G i = sin. inclination of orbit to ecliptic. 

Hence the force to draw P from its orbit = 


when P is in 

the quadratures. Since g vanishes this force vanishes. When the nodes 
are in the syzygies s vanishes, and when in the quadratures this force is a 
maximum. Since s = rad. cotan. parte. 

496. To calculate the quantity of the forces. 

Let S T = d, P T = r, the mean distance from T = i. The force 

of T on P at the mean distance = f; the force of S on P at the mean 
distance = g. 

Then the force S T = - , and the force S T : f. P T : : d : r, 

IT r f? r 3 " r 

.-. force P T = ^r, hence the add. f = >; ablat. f = j? 3 sin. 0, the 
d 3 d 3 d 3 

mean add. force at distance 1 = -K , the central ablat. = , ,- sin. 2 6, the 

d* d 3 

3 rr r 

tangential ablat. f = S"jnT * S " T> ^ " 


* ~ f? i* 3 0* r 
The whole disturbing force of S on P = ~o~T 3 ^ 9 1 3 cos> ^ ^ > l ^ e 

mean disturbing f = ^ 3 - (since cos. 2 & vanishes) = by supposi 

Hence we have the whole gravitation of P to T = *3t + oiT * 

r ci cl i& ci 

cos. 2 0, and the mean = n _- (since cos. 2 vanishes). 

r a 2 d* v 


497. Required the whole effect, and also the mean effect of the sun to 
diminish the lunar gravity; and show that if P and p be the periodic 
times of the earth and moon, f the earth s attraction at the mean 
distance of the moon, r the radius-vector of the moon s orbit ; the additi- 

fp 2 P 4 1 

tious force will be nearly represented by the formula \ \.~ ^n4 \ f r - 

v X A * 

P n = 3 P T. sin. 8 6, and P T 3 P T . sin. 8 d = 2 + JL p T X 

cos. 26 = whole diminution of gravity of the moon, and the mean di- 

P T g r, 
mmution = -f- ^ 3 by supposition. 


P 1 a d 3 
.ab. f ^_ 

498. To find the central and ablatitious tangential forces. 


Take Pm = 3PK = 3PT. sin. 6 = ablatitious force. 
Then P n = P m . sin. 6 = 3 P T . sin. * Q = central force 
m n = P m . cos. 6 = 3 P T . sin. 6 . cos. 6 

= | . P T sin. 2 6 = tangential ablatitious force. 
To find what is the disturbing force of S on P. 

A a 1 


The disturbing force = P T 3 P T . sin. * 6 = (~ ! + 3cos - 2 *\ x 
P T" ^ 

P T = A-i + - P T. cos. 2 6. 

d ti 

To find the mean disturbing force of S during a whole revolution. 

P T 3 

Let P T at the mean distance = m, then 1 . P T cos. 2 6 

id ft 

g = H since cos. 2 6 is destroyed during a whole revolution. 

499. To find the disturbing force in syzygy. 

SAT A T = 2 A T = disturbing force in syzygy; 
the force in quadrature is wholly effective and equal P T, 
/. force in quadrature : f in syzygy : : P T : 2 P T : : 1 : 2. 

To find that point in P s orbit when the force of P to T is neither 
increased nor diminished by the force of S to T. 

In this point Pn= P T or 3 P T sin. 2 6 = P T, 

.*. sin. 6 = -== 
V 3 


6 = 35 W." 
To find when the central ablatitious force is a maximum. 

P n = 3 P T . sin. 2 & = maximum, 
. . d . (sin. 2 6) or 2 sin. 6 . cos. & d 6 = 0, 

. . sin. 6 . cos. 6 = 0, 

sin. 6 . V 1 sin. 2 6 = 0, 

sin. 0=1, 

or the body is in opposition. 
Then (Prop. LVIII, LIX,) 

T 2 : t 2 : : S P : C P : : S + P : S 

T 2 : t 2 : : A 3 : x 3 

. A 3 : x 3 :: S+ P : S 


A : x :: (S+ P) ^ : S*. 

500. PROB. Hence to correct for the axis major of the moon s orbit. 
Let S be the earth, P the moon, and let per. t of a body moving in a 
secondary at the earth s surface be found, and also the periodic time of 


the moon. Then we may find the axis major of the moon s orbit round 
the earth supposed at rest = x, by supposition. Then the corrected axis 

or axis major round the earth in motion : x : : (S + P) : S s 

(S + 
. . axis major round the earth in motion = x . S 

= y. 

Hence to compare the quantity of matter in the earth and moon, 

y:x:: VS+P: V S 
... y 3_ x 3 : X 3 :: p : s. 
501. To define the addititious and ablatitious forces. Let S T repre 

sent the attractive force of T to S. Take 

SL: ST:: 



-: : ST 8 : S P 1 

S P 2 S T 

and S L will represent the attractive force of P to S. Resolve this into 
S M, and L M ; then L M, that part of the force in the direction P T 
is called the addititious force, and S M S T = NMis the ablatitious 

502. To compare these forces. 

Since SL:ST::ST 2 :SP 2 , .-. SL = |i| = attractive force of 

P to S in the direction S P, and S P : S T : : |- 

= attractive 

force of P to S in the direction TS = ST 4 (ST PK)~ =ST 
+ 3 P K = S M nearly, 

.-. 3PK = TM = PL = ablatitious force = 3 P T . sin. 6. 

c T 3 e T 3 
Also S P P T - - 

SP- ST" 1 

P T = attractive force of P to S in the direction L M = P T nearly. 
Hence the addititious force : ablatitious force : : P T : 3 P T . sin. 6 : 1 

. 3 sin. 6. Q. e. d. 


1. PROP. I. All secondaries are found to describe areas round the 
primary proportional to the time, and these periodic times to be to each 
other in the sesquiplicate ratio of their radii. Therefore the center of 

force is in the primary, and the force cc =Y . 

2. PROP. II. In the same way, it may be proved, that the sun is the 
center of force to the primaries, and that the forces oc ,.- - . Also the 

Aphelion points are nearly at rest, which would not be the case if the 
force varied in a greater or less ratio than the inverse square of the dis 
tance, by principles of the 9th Section, Book 1st. 

3. PROP. III. The foregoing applies to the moon. The motion of the 
moon s apogee is very slow about 3 3 in a revolution, whence the force 

will x -vs-jTg ~Az It was proved in the 9th Section, that if the ablatitious 

force of the sun were to the centripetal force of the earth : : 1 : 357.45, 
that the motion of the moon s apogee would be ^ the real motion. 
.*. the ablatitious force of the sun : centripetal force : : 2 : 357.45 

: : 1 : 178 f. 

This being very small may be neglected, the remainder x ^ . 

4. COR. The mean force of the earth on the moon : force of attraction 

; : 177 f I : 178 fg. 

The centripetal force at the distance of the moon : centripetal force at 
the earth:: 1 : D*. 

5. PROP. IV. By the best observations, the distance of the moon from 
the earth equals about 60 semidiameters of the earth in syzygies. If the 
moon or any heavy body at the same distance were deprived of motion in 
the space of one minute, it would fall through a space = 16 /^feet. For the 




deflexion from the tangent in the same time = 16 T L feet. Therefore the 
space fallen through at the surface of the earth in I" = 16 T V feet. 
For 60" : t : : D : 1, 


thence the moon is retained in its orbit by the force of the earth s gravity 
like heavy bodies on the earth s surface. 

6. PROP. XIX. By the figure of the earth, the force of gravity at 

the pole : force of gravity at the equator : : 289 : 288. Suppose A B Q q 
a spheroid revolving, the lesser diameter P Q, and A C Q q c a a canal 
filled with water. Then the weight of the arm Q q c C : ditto of 
A a c C : : 288 : 289. The centrifugal force at the equator, therefore 1 
suppose 2^-g f tne weight. 

Again, supposing the ratio of the diameters to be 100 : 101. By com 
putation, the attraction to the earth at Q : attraction to a sphere whose 
radius == Q C : : 126 : 125. And the attraction to a sphere whose ra 
dius A C : attraction of a spheroid at A formed by the revolution of an 
ellipse about its major axis : : 126 : 125. 

The attraction to the earth at A is a mean proportional between the at 
tractions to the sphere whose radius =r A C, and the oblong spheroid, 
since the attraction varies as the quantity of matter, and the quantity of 
matter in the oblate spheroid is a mean to the quantities of matter in the 
oblong spheroid and the circumscribing sphere. 

Hence the attraction to the sphere whose radius = A C : attraction to 
the earth at A : : 126 : 125 $. 

. . attraction to the earth at the pole : attraction to the earth at the equa 
tor : : 501 : 500. 

Now the weights in the canals cc whole weights a magnitudes X gra- 


vity, therefore the weight of the equatorial arm : weight of the polar 
: : 500 X 101 : 501 X 100 
: : 505 : 501. 

Therefore the centrifugal force at the equator supports ^-^ to make an 


But the centrifugal force of the earth supports 

41 11 

* 505 : 289 : : 100 : 229 = the GXCeSS f the e< l uatorial over the P olar 

Hence the equatorial radius : polar : : 1 + ^^r : 1 

: : 230 : 229. 

Again, since when the times of rotation and density are different the 


difference of the diameter oc -, - . and that the time of the earth s rota- 


tion = 23h. 56 . 

The time of Jupiter s rotation = 9h. 56 . 

The ratio of the squares of the velocity are as 29 : 5, and the density 
of the earth : density of Jupiter : : 400 : 94.5. 

d the difference of Jupiter s diameter is as - X jrj-p X -rr- , 

5 94.5 229 

.-. d : Jupiter s least diameter : : - x ^j-r X ^5 : : 29 X 80 : 94.5 X 229 

> .Jr..) - 

: : 2320 : 21640 
: : 232 : 2164 
:: 1 : 9| 

The polar diameter : equatorial diameter : : 9| : 10^ 



1. The interval between two succeeding high waters is 12 hours 25 
minutes. The diminution varies nearly as the squares of the times from 
high water. 

2. Twenty- four hours 50 minutes may be called the lunar day. The 
interval between two complete tides, the tide day. The first may be call- 




ed the superior, the other inferior, and at the time of new moon, the 
morning and evening, 

3. The high water is when the moon is in S. W. to us. The highest tide 
at Brest is a day and a half after full or change. The third full sea after 
the high water at the full moon is the highest ; the third after quadrature 
is the lowest or neap tide. 

4. Also the highest spring tide is when the moon is in perigee, the next 
spring tide is the lowest, since the moon is nearly in the apogee. 

5. In winter the spring tides are greater than in summer, and from the 
same reasoning the neap tides are lower. 

6. In north latitude, when the moon s declination is north, that tide in 
which the moon is above the horizon is greater than the other of the same 
day in which the moon is below the horizon. The contrary will take 
place if either the observer be in south latitude or the moon s declination 

7. PROP. I. Suppose P to be any 
particle attracted towards a center E, 
and let the gravity of E to S be repre 
sented by E S. Draw B A perpendi 
cular to E S, which will therefore re 
present the diameter of the plane of il 
lumination. Draw Q P N perpendicu 
lar to B A, P M perpendicular to E C. 
Then take E I = 3 P N, and join P I, 
P I will represent the disturbing force 
of P. PI may be resolved into the 
two P E, P Q, of which P E is counter 
balanced by an equal and opposite force, 
P Q acts in the direction N P. 

Hence if the whole body be supposed 
to be fluid, the fluid in the canal N P 
will lose its equilibrium, and therefore 
cannot remain at rest. Now, the equi 
librium may be restored by adding a 
small portion P p to the canal, or by 
supposing the water to subside round 
the circle B A, and to be collected to 
wards O and C, so that the earth may put on the form of a prolate sphe 
roid, whose axis is in the line O C, and poles in O and C, which may be 


the case since the forces which are superadded a N P, or the distance 
from B A, so that this mass may acquire such a protuberancy at O and C, 
that the force at O shall be to the force at B : : E A : E C ; and by the 
above formula 

_ 5JC __ E C E A 

r ~ 4 g ~ E A 

8. PROP. II. Let W equal the terrestrial gravitation of C; G equal its 
gravitation to the sun ; F the disturbing force of a particle acting at O and 
C ; S and E the quantities of matter in the sun and earth. 

3 S C 

.-. F : W : : 

CS* X CG C E 3 

Since the gravitation to the sun oc s 

C S 2 : E S 2 : : ES: C G 

/. CG X C S 2 = ES 3 . 

. F . W . . ?A . _A 

E S 3 C E 3 


E : S : : 1 : 338343 

E C:ES: : 1 : 23668 
. 3 S . _]?_. - 1 12773541 F W 

" * E s s cnr^ * iw**** . . , . 

.-. 4 W : 5 F : : C E : E C E A. 

4 d 3d 
Attraction to the pole : attraction to the equator : : 1 : 1 

O t) 

Quantity of matter at the pole : do. at equator : : 1 : 1 d. 

Weight of the polar arm : weight of the equatorial arm : : 1 : 1 - 

O D 

. Excess of the polar = attractive force : weight of the equator 


mean weight W : : : 1 


9. PROP. III. Let A E a Q be the spheroid, B E b Q the inscribed 




sphere, A G a g the circumscribed sphere, and D F d f the sphere equal 
(in capacity) to the spheroid. 



Then since spheres and spheroids are equal to f of their circumscribing 
cylinder, and that the spheroid = sphere D F d f. 
CF 2 xCD = CE 2 xCA 
CE: C F 2 : : CD: C A, 

and make 



.-.C E 2 : C F 2 : : C E : Cx 
/. CD:CA::CE:Cx 
.-. CD:CE::CA:Cx 

C D = C E nearly 
.-. C A = C x. 

E x = 2 E F nearly 
.-. A D = 2 E F.* 

Let C E = a, C F = a + x, 

_ aM-2a*+x a _ a* + 2 * 
~~T~ a 

= a + 2 x nearly 
.% E x = 2 x nearly. 


PROP. IV. By the triangles p I L, C I N, 

A B : I L : : r 2 : (cos.) z L. T C A 
.-. I L = A B x (cos.) 2 z_ I C A = S X (cos.) ? x 
(if S = A B and x = angular distance from the sun s place.) 

G E : K I : : r 2 : (sin.) L. T C A 
.-. K I = S X (sin.) 2 . K. 
COR. 1. The elevation of a spheroid above the level of the undisturbed 

c _ 

ocean = 1 i 1 m = S X (cos.) 2 x \- = S X (cos.) 2 x 


The depression of the same = S X (sin.) z x S = S X (sin.) 2 x f. 
COR. 2. The spheroid cuts the sphere equal in capacity to itself in a 


point where S X (cos.) 2 x = = 0, or (cos.) " x = . 


. . cos. x = .57734, &c. 

= cos. 54. 44 . 

10. PROP. V. The unequal gravitation of the earth to the moon is 
(4000) 3 times greater than towards the sun. 

Let M equal the elevation above the inscribed sphere at the pole of 
the spheroid, 7 equal the angular distance from the pole. 

/. the elevation above the equally capacious sphere = M X (cos.) z / 

the depression --- ---- = M X (sin.) * 7 |. 

Hence the effect of the joint action of the sun and moon is equal to the 
sum or difference of their separate actions. 

.-. the elevation at any place = S X (cos.) 3 x -f M X (cos.) 2 7 S + 5T 
the depression -- = S X (sin.) " x + M X (sin.) 2 7 f S + M. 

1. Suppose the sun and moon in the same place in the heavens. 
Then the elevation at the pole = S + M S + M = | S + M, and 
the depression at the equator = S + M S + M = f, S + M, 

. . the elevation above the inscribed sphere = S + M. 

2. Suppose the moon to be in the quadratures. 

The elevation at S = S i S + M = f S $ M. 
the depression at M = S S + M = $ S M, 
the elevation at S above the inscribed sphere = S M, 
the elevation at M (by the same reasoning) = M S. 
But (by observation) it is found that it is high water under the moon 
when it is in the quadratures, also that tlie depression at S is below the 
natural level of the ocean ; hence M is more than twice S, and although 

VOL. I. B b 




the high water is never directly under the sun or moon, when the moon is 
in the quadratures high water is always 6 hours after the high water at 
full or change. 

Suppose the moon to be in neither of the former positions. 

Then the place of high water is where the elevation =r maximum, 
or when S X cos. 2 x + M X cos. 2 y = maximum, 
and since 

cos. * x = + \ cos. 2 x, 

cos. y = + \ cos. 2 y, 

elevation = maximum, when S X cos. 2 x + M X cos. 2 y = max 

Therefore, let A B S D be a great circle of the earth passing through 
S and M, (those places on its surface which have the sun and moon in the 
zenith). Join C M, cutting the circle described on C S in (m). Make 
S d : d a : : force of the moon : force of the sun (which force is supposed 


known). Join ma, m d, and let H be any point on the surface of the 
ocean. Join C H cutting the circle C m S in (h) ; draw the diameter 
h d h , and draw m t, a x perpendicular to h h , and a y parallel to it. 

M=Sd, S=ad 


.-. d t = M X cos. 2 y, d x = S X cos. 2 x, 
.. elevation = maximum when t x = a y = maximum, 
or when a y = a m, i. e. when h h is parallel to a m, hence 



S d : d a : : M : S, 

and join m a, draw h h parallel to a m, and from C draw C h H cutting 
the surface of the ocean in H, which is the point of hi^h water. 

Again, through h 7 draw L C h , meeting the circle in L, L ; these are 
the points of low water. For let 

L C S = u, L C M = z . 

cos. L a d x = cos. A S d h = cos. 2 u S C h"!= cos. 2 u = d x 

cos. 2 z = cos. 2 L C M = d t. 
.-. S X cos. 2 u + M X cos. 2 z = max. 

COR. If d f be drawn perpendicular to a m, a m represents the whole 
difference between high and low water, a f equals the point effected by the 
sun, m f that by the moon. 

sin. * u = cos. 2 x, 
sin. 2 y = cos. 2 x. 

.*. elevation + depression = S X : cos. - x + M X : cos. i y 

+ S X cos. 2 x -^- $ 
+ M X : cos. y f = S X : 2 cos. x 1 + M X : 2cos. y 1 

= S X cos. 2 x + M x cos. 2 y 

d t = M X cos. 2 y 
d x = S X cos. 2 x. 


12. Conclusions deduced from the above (supposing that both the sun 
and moon are in the equator.) 


1. At new and full moon, high water will be at noon and midnight. 
For in this case C M, a m, C S, d h, C H, all coincide. 

2. When the moon is in the quadrature at B, the place of high water is 
also at B under the moon, when the moon is on the meridian, for C M is 
perpendicular to C S, (m) coincides with C, (a m) with (a C), d h with 
d C. 

3. While the moon passes from the syzygy to the quadrature the place 
of high water follows the moon s place, and is to the westward of it, over 
takes the moon at the quadratures, and is again overtaken at the next 
syzygy. Hence in the first and third quadrants high water is after noon 
or midnight, but before the moon s southing, and in second and fourth vice 

4. ZL M C H = max. when S C H = 45. S d h = 90. and m a 
perpendicular to S C, and a m d = max., and a m d m d h = 2y . 


Hence in the octants, the motion of the high water = moon s easterly 
motion ; in syzygy it is slower ; in quadratures faster. Therefore the tide 
day in the octants = 24h. 50 = the lunar day ; in syzygy it is less = 24h. 
35 ; in quadratures = 25h. 25 . 

For take any point (u) near (m), draw u a, u d, and d i parallel to a u 
and with the center (a) and radius a u, describe an arc (u v) which may 
be considered as a straight line perpendicular to am; u m and i h are 
respectively equal to the motions of M and H, and by triangles u m v, 

u m : i h : : m a : m f. 

Therefore the synodic motion of the moon s place : synodic motion ot 
high water : : m a : m f. 

COR. 1. At new or full moon, m a coincides with S a, and m f with S d ; 
at the quadratures, m a coincides with C a, and m f with C d ; therefore 
the retardation of the tides at new or full moon : retardation at quadra 
tures ::Sa:Ca::M + S:M S. 

Con. 2. In the octants, m a is perpendicular to S a, therefore m a, m f 
coincide. Therefore the synodic motion of high water equals the synodic 
motion of the moon. 

COR. 3. The variation of the tide during a lunation is represented by 
(m a) ; at S, m a = S a, at C = C a. 

Therefore the spring tide : neap tide : : M -f- S : M S. 

COR. 4. The sun contributes to the elevation, till the high water is in 
the octants, after which (a f ) is v e, therefore the sun diminishes the 

COR. 5. Let m u be a given arc of the moon s synodic motion, in v is 
the difference between the tides m a, u a corresponding to it. 
Therefore by the triangles m u v, m d f. 

m u : m v : : m d : d f. 

.*. m v <x d f ; 
and since 

m d : d f : : r : sin. dmf:: r : sin. m d h : : r : sin. 2 M C H 
m v oc sin. 2 arc M H. 

13. PROP. VI. In the triangle m d a, m d, d a and Z. m d a are known 
when the proportion M : S is known and the moon s elongation. 

Let the angle m d a = a, 
and make 

M + S : M S : : tan. a : tan. b 



a b a + b 



y = -g-,x:= 2 

M+ S:M S::md + da:md da 

mad+amd mad amd 
: : tan. ^ : tan. 

2 x + 2 y 2x 2y 

: : tan. = ; : tan. ~ 

: : tan. x -f- y : tan. x y 

: : tan. a : tan. b, 
. . x + y : x y : : a : b, 
.-. 2 x = a + b, 2 y = a b, 

. x - 

~ b 

2 * 

14. PROP. VII. To find the proportion between the accelerating forces 
of the moon and sun. 1st. By comparing the tide day at new and full 
moon with the tide day at quadratures. 

35 : 85 : : M : S, 

. . . . . . . . . 

Also, at the time of the greatest separation of high water from the moon 
in the triangle m d a, m d : d a : : r : sin. 2 y : : M : S, 

.-. jgj = sin. 2 y, 

at the octants y is found =12 SO , 
.. ^ = sin. 25, 


. . M : S : : 5 : 2} nearly. 
Hence taking this as the mean proportion at the mean distances of the 

moon and sun (if the earth =1) the moon = . 

COR. 1. If the disturbing forces were equal there would be no high or 
low water at quadratures, but there would be an elevation above the in 
scribed spheroid all round the circle, passing through the sun and moon 


COR. The gravitation of the sun produces an elevation of 24 inches, 
the gravitation of the moon produces an elevation of 58 inches. 
.. the spring tide = 82 inches, and the neap tide = 33| inches. 

15. COR. 3. Though M : S : : 5 : 2, this ratio varies nearly from (6:2) 
to 4 : 2, for supposing the sun and moon s distance each = 1000. 

In January, the distance of the sun = 983, perigee distance of the 
moon = 945. 

In July, the distance of the sun = 1017, apogee distance of the moon 
= 1055. 

Disturbing force oc ~- 3 ; hence 












rr.i 5 A 3 d 3 

The general expression is M = S X pr 3 X 7-5 

JL) o 

To find the general expression above. 

Disturbing force of different bodies (See Newton, Sect, llth, p. G6, 
Cor. 14.) a jL, 

.-. disturbing force S : disturbing force at mean distance : : D 3 : A 3 
disturbing force M : disturbing force at mean distance : : d 3 : 8 3 , 

M 5 d_*_ <P 
S : 2 :: D 3 * A~ 3 

M ^ Aj> (P 

* ~S > : 2 X D 1 X ^ 

(or supposing that the absolute force of the sun and moon are the same). 

16. PROP. VIII. Let N Q S E be the earth, N S its axis, E Q its equa. 
tor, O its center ; let the moon be in the direction O M having the de 
clination B Q. 

* The solar force may be neglected, but the variation of the moon s distance, and proportion 
ally the variation of its action, produces an effect on the times, and a much greater on the heights 
of the tides. 


[BooK III. 

Let D be any point on the surface of the earth, D C L its parallel of 
latitude, N D S its meridian ; and let B F b f be the elliptical spheroid 
of the ocean, having its poles in O M, and its equator F O f. 


As the point D is carried along its parallel of latitude, it will pass 
through all the states of the tide, having high water at C and L, and low 
water when it comes to (d) the intersection of its parallel of latitude with 
the equator of the watery spheroid. 

Draw the meridian N d G cutting the terrestrial equator in G. Then 
the arc Q G (converted into lunar hours) will give the duration of the 
ebb of the superior tide, G E in the same way the flood of the inferior. 
N. B., the whole tide G Q C , consisting of the ebb Q G, and the flood 
G Q is more than four times G O greater than the inferior tide. 

COR. If the spheroid touch the sphere in F and f, C C is the height 
at C, L I/ the height at L, hence if L q be a concentric circle C q will 
be the difference of superior and inferior tides. 


1. If the moon has no declination, the duration of the inferior and su 
perior tides is equal for one day over all the earth. 

2. If the moon has declination, the duration of the superior will be 
longer or shorter than the duration of the inferior according as the 
moon s declination and the latitude of the place are of the same or differ 
ent denominations. 

3. When the moon s declination equals the colatitude or exceeds it, 


there will only be a superior or inferior tide in the same day, (the paral 
lel of latitude passing through f or between N and f.) 

4. The sin. of arc G O = tan. of latitude X tan. declination. 

rad. : cot. d O G : : tan. d G : sin. G O, 
.-. sin. G O = cot. d O G X tan. G d 

= tan. declination X tan. latitude. 

17. PROP. IX. With the center C and radius C Q (representing the 


whole elevation of the lunar tide) describe a circle which may represent 
the terrestrial meridian of any place, whose poles are P, p, and equator 
E Q. Bisect P C in O, and round O describe a circle P B C D ; let M 
be the place on the earth s surface which has the moon in its zenith, Z 
the place of the observer. Draw M C m, cutting the small circle in A, 
and Z C N cutting the small circle in B ; draw the diameter BOD and 
A I parallel to E Q, draw A F, G H, IK perpendicular to B D, and 
join I D, A B, A D, and through I draw C M cutting the meridian in 
M . Then after a diurnal revolution the moon will come into the 
situation M , and the angle M C N ( = the nadir distance) = supplement 
the angle ICB = ^IDB. 

Also the .ADB = BCA = zenith distance of the moon. 


Hence D F, D K cc cos. * of the zenith and nadir distances to rad. D B. 
oc elevation of the superior and inferior tides. 


1. The greatest tides are when the moon is in the zenith or nadir of the 
observer. For in this case (when M approaches to Z) A and I move to 
wards D, B, and F coincides with B ; but in this case, the medium tide 
which is represented by D H (an arithmetic mean to D K, D F) is di 

If Z approach to M, D and I separate ; and hence, the superior and 
inferior and the medium tides all increase. 

2. If the moon be in the equator, the inferior and superior tides are 
equal, and equal M X (cos) 2 latitude. For since A and I coincide with 
C, and F and K with (i) D i = D B X (cos.) 8 B D C = M X (cos.) * 

3. If the observer be in the equator, the superior and inferior tides are 
equal every where, and = M X (cos.) 2 of the declination of the moon. 
For B coincides with C, and F and K with G ; P G = P C X cos. 2 of 
the moon s declination = M x (cos.) z of the moon s declination. 

4. The superior tides are greater or less than the inferior, according as 
the moon and place of the observer are on the same or different sides of 
the equator. 

5. If the colatitude of the place equal the moon s declination or is less 
than it, there will be no superior or inferior tide, according as the latitude 
and the declination have the same or different denominations. For when 
P Z = M Q, D coincides with I, and if it be less than M Q, D falls between 
I and C, so that Z will not pass through the equator of the watery spheroid. 

6. At the pole there are no diurnal tides, but a rise and subsidence 
of the water twice in the month, owing to the moon s declining to both 
sides of the equator. 

18. PROP. X. To find the value of the mean tide. 

A G = sin. 2 declination (to rad. = O C.) 

O G = cos. 2 declination (to the same radius). 

..OH = cos. 2 declination X cos. 2 lat. X -_- t 


.-. D H = O D + O H 

M / 1 + cos. 2 lat. X cos. 2 declination 
._ J.VI X x-, 


Now as the moon s declination never exceeds 30, the cos. 2 declination 
is always + v 2 , and never greater than ; if the latitude be less than 45, 
the cos. 2 lat. is + v e, after which it becomes v e. 


1. The mean tide is equally affected by north and south declination of 
the moon. 

2. If the latitude = 45, the mean tide M. 

3. If the lat. be less than 45, the mean tide decreases as the declina 
tion increases. 

4. If the latitude be greater than 45, the mean tide decreases as the 
declination diminishes. 

. Tr . , , . , ,, 1 + cos. 2 declination 

5. If the latitude = 0, the mean tide = M X 5 



503. PROP. LXX. To find the attraction on a particle placed within 
a spherical surface, force ce g . y - g . 

Let P be a particle, and through P draw H P K, 
I P L making a very small angle, and let them 
revolve and generate conical surfaces I P H, 
L P K. Now since the angles at P are equal 
and the angles at H and L are also equal (for 
both are on the same segment of the circle), 
therefore the triangles H I P, P L K, are similar. 

.-. HI:KL::HP:PL 

Now since the surface of a cone GC (slant side) 2 , 

.. surface intercepted by revolution of I P H : that of L P K : : P H : P L 

:: HI 2 : KL 

and attractions of each particle in I P H : that of L P K 

P2 r> T 
Jti J. Jr \~ 


but the whole attraction of P oc the number of particles X attraction of 

HI* K L* 

.. the whole attraction on P from H I : from K L : : ^rm ir T . 

rl 1 T Jv L, * 

:: J : 1; 

and the same may be proved of any other part of the spherical surface ; 
.*. P is at rest. 

504. PROP. LXXL To find the attraction on a particle placed without 

a spherical surface, force cc g . -p - . 

distance * 




Let A B, a b, be two equal spherical surfaces, and let P, p be two 
particles at any distances P S, p s from their centers; draw P H K, 


P I L very near each other, and S F D, S E perpendicular upon them, and 
from (p) draw p h k, p i 1, so that h k, i 1 may equal H K, I L respective 
ly, and s f d, s e, i r perpendiculars upon them may equal S F D, S E, 
I R respectively ; then ultimately PE = PF = pe = pf, and D F 
= d f. Draw I Q, i q perpendicular upon P S, p s. 

PI: PF:: IR : DF") 

V.-. PI pf:pi.PF::IR:ir::IH:ih 
: : d f : i r I 


pf:p i : : 


PI: PS:: IQ: SF 


.-. ps: (pi) 2 .PF. PS:: IQ.IH:iq.ih 
: : circumfer. of circle rad. I Q X I H : circumfer. of circle rad i q X i h 
: : annulus described by revolution of I Q : that by revolution of i q. 

-. . 

attraction on 1st annulus : attraction on 2d 

attraction on the annulus : attraction in the direction P S 

P F 

.. attraction in direction PS = p f. p s. ^-~ 

P ] 
.-. whole att n . of p to S : whole att n . of (p) to s : : p f . p s . p-; 

1st annulus ^ 2d annulus 
distance 2 distance 2 (pi)*.PF. PS 

PI 2 (pi) 2 

:: pf. ps :PF.PS. 

P I : P Q 
P S : P F 

: P F . P S . - 

PS 2 ps 2 


and the same may be proved of all the annul! of which the surfaces are 

-^-- - 

composed, and therefore the attraction of P cc p-qi cc -^-- - j from 

the center. 

COR. The attraction of the particles within the surface on P equals the 
attraction of the particles without the surface. 

For K L : I H : : P L : P I : : L N : I Q. 

.*. annulus described by I H : annulus described by K L 
:: IQ.IH: K L. L N : : P P : P L 2 

.*. attraction on the annulus I H : attraction on the annulus K L 

PI 2 PL 2 
: P I s : P L 8 

and so on for every other annulus, and one set of annuli equals the part 
within the surface, and the other set equals the part without. 

506. PROP. LXXII. To find the attraction on a particle placed with 

out a solid sphere, force oc g - -p - r. 

distance 2 

Let the sphere be supposed to be made up of spherical surfaces, and 

the attraction of these surfaces upon P will x -TT- -- r, and therefore 

distance z 

the whole attractions 

number of surfaces content of sphere diameter 3 

P~W~ PS 2 PS 2 " 

and if P S bear a given ratio to the diameter, then 

the whole attraction on P oc -, -,<x diameter- 


507. PROP. LXXIIL To find the attraction on the particle placed 

Let P be the particle ; with rad. S P describe 
the interior sphere P Q ; then by Prop. LXX. 
(considering the sphere to be made of spherical 
surfaces,) the attraction of all the particles con- 
tained between the circumferences of the two 
circles on P will be nothing, inasmuch as they 
are equal on each side of P, and the attraction 

PS 3 
of the other part by the last Prop, oc rr^i a P S. 



[SECT. X1J. 

508. PROP. LXXIV. If the attractions of the particles of a sphere 

<x T . : =. and two similar spheres attract each other, then the spheres 

distance z 


will attract with a force x g as 

distance 3 

of their centers. 

For the attraction of each particle cc -~- = from the center of the 

distance 2 

attracting sphere (A), and therefore with respect to the attracted particle 
the attracting sphere is the same as if all its particles were concentrated 
in its center. Hence the attraction of each particle in (A) upon the 

whole of (B) will a -^ of each particle in B from the center of P, 

distance 2 

and if all the particles in B were concentrated in the center, the attraction 
would be the same; and hence the attractions of A and B upon each other 
will be the same as if each of them were concentrated in its center, and 

therefore cc 

distance 2 

509. PROP. LXXVI. Let the spheres attract each other, and let 
them not be homogeneous, but let them be homogeneous at correspond 
ing distances from the center, then they attract each other with forces 




Suppose any number of spheres C D and E F, I K and L M, &c. to 
be concentric with the spheres A B, G H, respectively; and let C D and 
I K, E F and L M be homogeneous respectively ; then each of these 

spheres will attract each other with forces cc g . T ; Now suppose 

distance * 

the original spheres to be made up by the addition and subtraction of 
similar and homogeneous spheres, each of these spheres attracting each 


other with a force a *. -7: - a , 

distance a 

each other in the same ratio. 



then the sum or differences will attract 

510. PROP. LXXVII. Let the force cc distance, to find the attraction 
of a sphere on a particle placed without or within it. 

Let P be the particle, S the center, draw two planes E F, e f, equally 
distant from S ; let H be a particle in the plane E F, then the attraction 
of H on P oc HP, .and therefore the attraction in the direction S P a 
P G, and the attraction of the sum of the particles in E F on P towards 
S a circle E F . P G, and the attraction of the sum of the particles in 
(e f) on P towards S cc circle e f . P g, therefore the whole attraction of 
E F, e f, a circle EF(PG+Pg)cc circle E F . 2 P S, therefore the 
whole attraction of the sphere cc sphere X P S. 

When P is within the sphere, the attraction of the circle E F on P to 
wards S x circle E F . P G, and the attraction of the circle (e f ) towards 
S cc circle e f . P g, and the difference of these attractions on the whole 
attraction to S cc circle E F (P g P G) cc circle E F . 2 P S. There 
fore the whole attraction of the sphere on P cc sphere X P S. 

511. LEMMA XXIX. If any arc be described with the center S, rad. 

S B, and with the center P, two circles be described very near each other 

Vot. I. C c 




cutting, first, the circle in E, e, and P S in F, f; and E D, e d, be drawn 
perpendicular to P S, then ultimately, 

Dd: Ff: : PE: PS. 

Dd: Ee:: 

DT: ET:: DE: ES 


Ee: Ff :: 


D rl F f - 

T> E : S G ; : 

P E : P S. 

512. PROP. LXXIX. Let a solid be generated by the revolutions of at. 
evanescent lamina E F f e round the axis P S, then the force with which 
the solid attracts PocDE 2 . Ffx force of each particle. 

Draw E D, e d perpendiculars upon PS; let e d intersect E F in r; 
draw r n perpendicular upon E D. Then E r : n r : : P E : ED, .*. 
Er.ED = nr.PS = Dd.PE, . . the annular surface generated by 
the revolution of Era Er.EDacDd.PE, and (P E remaining the 
same) a D d. But the attraction of this annular surface on P ex D d . 
P E, and the attraction in the direction P E : the attraction in the direc 
tion P S : : P E : P D, 

.. the attraction in the direction P S oc 


.Dd. PE oc PD.Dd 

and the whole attraction on P of the surface described by E F a sum of 
the PD.Dd. 

Let P E = r, D F = x, 
.-. P D = r x, 

. P D . D d = r d x x < x, 

..sumofPD.DdS=/rdx xdx = 

D E 1 , 

and therefore the attraction of lamina cc D E *. Ff X force of each particle. 



D E*. P S 

513. PROP. LXXX. Take D N proportional to 

X force 

of each particle at the distance P E, or if ^ represent that force, let D N 

~T) "p 2 p C 

a P E V tnen tne area trace d out by D N will be proportional to 
the whole attraction of the sphere. 

For the attraction of lamina EFfeaDE 2 . Ffx force of each parti- 

ID E 2 P S 
cle a (LEMMA XXIII) - - -- . D d x force of each particle, or 

D E 2 PS 

d " 

a attraction of lamina E F f e, and the 

p E. V 

sum of these areas or area A N B will represent the whole attraction of 
the sphere on P. 

514. PROP. LXXXI. To find the area A N B. 

Draw the tangent P H and H I perpendicular on P S, and bisect P I 
in L ; then 




SE S = SH 2 = PS.SI, 
.-. PE 2 = P S 2 + PS.SI + 2PS.SD 
= PS{PS + SI + 2SD} 
= P S J(P I + I S) + S I + 2 S DJ 

DE*= SE 2 SD 2 = SE 2 (LD LS) 2 
= SE 2 LD 2 LS 2 + 2LD.LS 
-2LD.LS LD 2 (LS+SE)(LS SE) 

.*. D N oc 

PE.V V 2 SD.P S. V 

V 2 L D . P S". V V2LD.PS.V 

and hence if V be given, D N may be represented in terms of L D and 
known quantities. 

515. Ex. 1. Let the force a ^-. - ; to find the area A N B. 



, LD A L . L B 
~2~* 2LD 

, _ , L D . D d AL.LB. D d 
.-. D N . D d, or d . area GC L b . D d -- ^ 2 ^ ^ - > 

., area AND between the values of L A and L B 

n TAX LB 2 -LA 2 AL.LB .LB 
= LS.(LB~LA) -- j- -g- ILA- 


L B 2 L A 2 = (L B + L A) . (LB LA) 

= (LS + AS + LS AS)AB = 2LS.AB, 

A XT -r^ A B . AL.LB . L B 

.-. area AND = LS.AB -- ^ --- 2 - 1 j^ 

L S . A B AL.LB . L B 
~~2~ 2 L~A* 




516. To construct this area. 

To the points L, A, B erect L 1, A a, B b, 
perpendiculars, and let A a = L B, and B b 
= L A, through the points (a), (b), de 
scribe an hyperbola to which L 1, L B are 
asymptotes. Then. by property of the hy 
perbola, AL.Aa = LD.DF, 



A L . L B . D d 

L A 

.-. D F = 
.-. DF.Dd = 

.-. area A a F D =/D F. D d = A L. L B/L D, 

. . hyperbolic area Aaf b B= A L L B f^L^. 

J L A* 

The area A a B b == B b A B 4- A B> a n 



+ L A 

= ^^AB 

AB = LS.AB, 
. . area a f b a = area A a B b -area A a f b B 

517. Ex. 2. Let the force a 

n TO 

Let V = 

, to find the 

2 A S* 

. .DN= 



V.PE = JLJ^ := !P_SjiI^_ 


A K9 

. . DN =^i^J[ AL.LB. SI i 

LD 2 ~2T7IP = 2PS. g L.LD , 

N.x = SI.L S/LD ^JjiPj. AL.LB. SI 

2 ~2TT) 

. . area between the values of L A and L B 

S /-^? !iiyLzi_LAJ_ /L^SJ AL.SI 

AJ A 2 v^ o ~"~ : S 




[SECT. xir. 

To construct this area. 
1 a 

Take S I = S s, and describe a hyperbola passing through a, s, b, to which 
L 1, L B are asymptotes; then as in the former case, the area A a n b B 

.-. the area A N B = S I . L S SLAB. 

518. PROF. LXXXII. Let I be a particle within the sphere, and P 
the same particle without the sphere, and take 

S P : S A : : S A : S I, 

then will the attracting power of the sphere on I : attracting power of the 
sphere on P _ _ 

: : V S I. V force on I : V S P. V forpe on P. 
D N force on the point P : D N 7 force on the point I 

D E 2 P S D E 2 I S 
:: ~FE7V~ : TE.V 
: : P S . I E . V : I S . P E . V. 


V : V :: P E n : I E", 



DN : D N :: PS.IE.IE n :IS.PE.PE", 

and the angle at S is common, 

.. triangles P S E, I S E are similar, 
.-. P E : I E : : P S : S E : : S E : S I, 
.-. D N : D N :: PS.SE.I E n : PS. SI. P E ", 
: : SE.I E n : S I.P E n 


: : A/S P.I E n : VSI.PE" 

:: VSP : SI VSI.PS*. 

519. PROP. LXXXIII. To find the attraction of a segment of a spheie 
.upon a corpuscle placed within its centre. 

Draw the circle F E G with the 
center P, let R B S be the segment of 
the sphere, and let the attraction of the 
spherical lamina E F G upon P be 
proportional to F N, then the area de 
scribed by F N oc whole attraction of 
the segment to P. 

Now the surface of the segment 
E F G a P F D F, and the content 
of the lamina whose thickness is O a 
PF D F O. 



Let F oc 


- and the attraction on P of the particle in that 
DE ! 

spherical lamina, cc (Prop. LXXIII.) -p -pr^- 
f2 P F F D F D 2 ) O 


PF n 

2FD O FD 2 O 

P F " - ! P F n 

.. if F N be taken proportional to p ,., n _, 
out by F N will be the whole attraction on P. 

F D * 

-- , the area traced 

520. PROP. LXXXIV. To find the attraction when the body is placed 
in the axis of the segment, but not in the center of the sphere. 




Describe a circle with the radius P E, and the segment cut off by the 
revolution of this circle E F K round P B, will have P in its center, and 


the attraction on P of this part may be found by the preceding Proposi 
tion, and of the other part by PROP. LXXXI. and the sum of these at- 
tractions will be the whole attraction on P. 


521. PROP. LXXXV. If the attraction of a body on a particle placed 
in contact with it, be much greater than if the particle were removed at 
any the least distance from contact, the force of the attraction of the par 
ticles a in a higher ratio than that of-p . 

distance z 

For if the force oc -rr j , and the particle be placed at any distance 

from the sphere, then the attraction oc -^ from the center of the 

distance 2 

sphere, .and .. is not sensibly increased by being placed in contact with 
the sphere, and it is still less increased when the force a in a less ratio 

, and it is indifferent whether the sphere be homo- 

than that of -p 


geneous or not ; if it be homogeneous at equal distances, or whether the 
body be placed within or without the sphei e, the attraction still varying in 
the same ratio, or whether any parts of this orbit remote from the point of 
contact be taken away, and be supplied by other parts, whether attractive 
or not, . . so far as attraction is concerned, the attracting power of this 
sphere, and of any other body will not sensibly differ ; . . if the pheno- 


mena stated in the Proposition be observed, the force must vary in a higher 

ratio than that of -p . 

distance 2 

522. PROP. LXXXVI. If the attraction of the particles cc in a higher 

ratio than T. , or oc -7: 5 . then the attraction of a body placed 

distance 3 distance d 

in contact with any body, is much greater than if they were separated 
even by an evanescent distance. 

For if the force of each particle of the sphere oc in a higher ratio than 

that of -j = , the attraction of the sphere on the particle is indefinitely 


increased by their being placed in contact, and the same is the case for 
any meniscus of a sphere; and by the addition and subtraction of attrac 
tive particles to a sphere, the body may assume any given figure, and 
.*. the increase or decrease of the attraction of this body will not be sensi 
bly different from the attraction of a sphere, if the body be placed in con 
tact with it. 

523. PROP. LXXXVII. Let two similar bodies, composed of particles 
equally attractive, be placed at proportional distances from two particles 
which are also proportional to the bodies themselves, then the accelerat 
ing attractions of corpuscles to the attracting bodies will be proportional 
to the whole bodies of which they are a part, and in which they are simi 
larly situated. 

For if the bodies be supposed to consist of particles which are propor 
tional to the bodies themselves, then the attraction of each particle in one 
body : the attraction of each particle in the other body, : : the attraction 
of all the particles in the first body : the attraction of all the particles in 
the second body, which is the Proposition. 

COR. Let the attracting forces cc -p , then the attraction of a 

distance n 

particle in a body whose side is A : B 

A 3 B 3 

distance n from A distance n from B 
A 3 B^ 
A" : B" 
1 1 

A n - 3 B n ~ 3 

if the distances oc as A and B. 




524. Paop. LXXXVIII. If the particles of any body attract with a 
force a distance, then the whole body will be acted upon by a particle 
without it, in the same manner as if all the particles of which the body is 
composed, were concentrated in its center of gravity. 

Let R S T V be the body, Z the par 
ticle without it, let A and B be any 
two particles of the body, G their cen 
ter of gravity, then A A G = B B G, 
and then the forces of Z of these parti 
cles oc A A Z, B B Z, and these 
forces may be resolved into A A G + 
A G Z, B B G + B G Z, and A A G 
being = B B G and acting in opposite 
directions, they will destroy each other, 
and . . force of Z upon A and B will be 

proportional to A Z G + B Z G, or to (A + B) Z G, .-. particles A 
and B will be equally acted upon by Z, whether they be at A and B, or 
collected in their center of gravity. And if there be three bodies A, B, 
C, the same may be proved of the center of gravity of A and B (G) and 
C, and . . of A, B, and C, and so on for all the particles of which the 
body is composed, or for the body itself. 

525. PROP. LXXXIX. The same applies to any number of bodies 
acting upon a particle, the force of each body being the same as if it 
were collected in its center of gravity, and the force of the whole system 
of bodies being the same as if the several centers of gravity were collected 
in the common center of the whole. 

526. PROP. XC. Let a body be placed in a perpendicular to the plane 
of a given circle drawn from its center ; to find the attraction of the circu 
lar area upon the body. 

With the center A, radius = A D, let 
a circle be supposed to be described, to 
whose plane A P is perpendicular. From 
any point E in this circle draw P E, in 
P A or it produced take P F = P E, and 
draw F K perpendicular to P F, and let 
F K oc attracting force at E on P. Let 
J K L be the curve described by the point 
K, and let I K L meet A D in L, take 
P H = P D, and draw H I perpendicular 


to P H meeting this curve in I, then the attraction on P of the circle 
a A P the area A H I L. 

For take E e an evanescent part of A D, and join P e, draw e C per 
pendicular upon P E, .-. E e : E C : : P E : A E, .-. E e . A E = E C x 
P E cc annulus described by A E, and the attraction of that annul us in 

P A 

the direction P A oc E C . P E . ^-^ X force of each particle at E cc E C X 

lr ilj 

P A X force of each particle at E, but E C = F f, .-. F K . F f cc E C x 
the force of each particle at E, . . attraction of the annulus in the direction 
PA cc PA.Ff. FK, and .-.PA X sum of the areas F K . Ff or P A 
the area A H I L is proportional to the attraction of the whole part de 
scribed by the revolution of A E. 

527. COR. 1. Let the force of each particle a T - 3, at P F = x. 

distance 2 

let b = force at the distance a, 

b a 2 
. . F K the force at the distance x = r , 

F K Ff ka dx 
. . r A., f i , 

.-. attraction = PA.FK.Ff=PA /"-- 2 

J x 

cc PA - x A p- p , 

and between the values of P A and P H, the attraction 

P A _L l ?- A 

L PA~~PH ~PH* 

528. COR. 2. Letthe force cc ^^ - . , then T K = ^ , 

distance n x n 

^ /.b a n , PA 1 

. . attraction = P A / d x cc - r X -- r+ Cor., 
/x n n 1 x " 

and between the values of P A and P H, 

PA r i 1 

.* * 

attraction = -- 


1 P A 

529. COR. 3. Let the diameter of a circle become infinite, or P II 

cc co, then the attraction cc . . 

1 A 

530. PROP. XCI. To find the attraction on a particle placed in the 
axis produced of a regular solid. 


R E 

[Sr-CT. XIII. 

Let P be a body situated in the axis A B of the curve D E C G, by 
the revolution of which the solid is generated. Let any circle 11 F S 
perpendicular to the axis, cut the solid, and in the semidiameter F S of 
the solid, take F K proportional to the attraction of the circle on P, then 
F K . F f o: attraction of the solid whose base = circle R F S, and depth 
= F f, let I K L be the curve traced out by F K, .. A L K F a at 
traction of the solid. 

COR. 1. Let the solid be a cylinder, the force varying as j 

2 * 


Then the attraction of the circle R F S, or F K which is proportional 

to that attraction a 1 


Let P F = x, F R = b, 
. . F K a 1 - 

x x 

. . FK. Ff ac dx 

.. area cc x Vx 2 + b * . 




Now if P A = x, attraction = 0, 

.-. Cor. = PD P A, 

.-. whole attraction = P B P E + PD PA 

= AB PE + PD. 
Let AB= oo = P E = P D, 

. . atraction = A B. 

531. COR. 3. Let the body P be placed 
within a spheroid, let a spheroidical shell 
be included between the two similar 
spheroids DOG, K N I, and let the 
spheroid be described round S which 
will pass through P, and which is simi 
lar to the original spheroid, draw D P E, 
F P G, very near each other. Now P D 
= BE, PF = CG, P H = B I, P K 
= CL. 

.-. F K = L G, and D H = I E, 

and the parts of the spheroidical shell which are intercepted between these 
lines, are of equal thickness, as also the conical frustums intercepted by 
the revolution of these lines, and 

.*. attraction on P by the part D K : . . . . G I 

number of particles in D K __ ... G 2 




PD ? 
PG 2 


: : 1 : 1, 

PD 2 PG ! 

arid the same may be proved of every other part of a spheroidical shell, and 
,\ body is not at all attracted by it; and the same may be proved of all the 
other spheroidical shells which are included between the spheroids, A O G, 
and C P M, and . . P is not affected by the parts extei-nal to C P M, and 
.-. (Prop. LXXIL), 

attraction on P : attraction on A : : P S : A S. 

532. PROP. XCIII. To find the attraction of a body placed without an 

infinite solid, the force of each particle varying as T. , where n is 

distance n 

greater than 3. 

Let C be the body, and let G L, H M, K O, &c. be the attractions 
at the several infinite planes of which a solid is composed on the 




body C; then the area G L O K equals the whole attraction of a solid 












Now if the force cc T . n , 



H M a c ^ n _ a (Cor. 3. Prop. XC) 

.-./H M . d x a /*-4^i cc L_^ + Cor. 

J .j -V n * xr n d * 


C G n ~ 3 C H n ~ 

and. if H C = GO 

then the area G L O K a ^-^ - . 

(j (_, " ~ d 

Case 2. Let a body be placed within the solid. 


I K 



Let C be the place of the body, and take C K = C G ; the part of 
the solid between G and K will have no effect on the body C, and there 
fore it is attracted to remain as if it were placed without it at the distance 

.*. attraction cc 





534. PROP. XCIV. Let a body move through a similar medium, ter 
minated by parallel plane surfaces, and let the body, in its passage through 
this medium, be attracted by a force varying according to any law of its 
distance from the plane of incidence. Then will the sine of inclination be 
to the sine of refraction in a given ratio. 

R a 

Let A a, B b be the planes which terminate the medium, and G H be 
the direction of the body s incidence, and I R that of its emergence. 

Case 1. Let the force to the plane A a be constant, then the body will 
describe a parabola, the force acting parallel to I R, which will be a diameter 
of the parabola described. H M will be a tangent to the parabola, and if 
K I be produced I L will also be a tangent to the parabola at I. Let K I 
produced meet G M in L with the center L, and distance L I describe 
a circle cutting I R in N, and draw L O perpendicular to I R. Now by a 
property of the parabola M I =. I v, 

.-. M L = H L, /. M O = O R, and .-. M N = I R. 

The angle L M I = the angle of incidence, and the angle M I L = sup 
plement of M I K = supplemental angle of emergence. 

L . M I = M H 2 = 4 M L * 




__ 1V/T T 2 T {^\ 

. M j = ML 2 ^-LQ 2 

.-. L:IR::4ML 2 :ML 2 LQ 1 
but L and I R are given 

.-.4 ML 2 a ML 2 LQ 1 

.-.ML 2 aLQ 2 a LI 2 

.% M L a L I or sin. refraction : sin. inclination in a given ratio. 
Case 2. Let the force vary according to T G/ 

H / a 

any law of distance from A a. g j/ ~ b 

Divide the medium by parallel planes A a, c K/ c 

B b, C c, D d, &c. and let the planes be at ^_ 
evanescent distances from each other, and 
let the force in passing from A a to B b, 
from B b to C c, from C c to D d, &c. be 

. . sin. I at H : sin. R at H : : a : b 

sin. R or I at I : sin. R at K : : c : d 
sin. R or I at K : sin. R at R : : e : f, and so on. 

. . sin. I at H : sin. RatR::a.c.e:b.d.f and in a constant pro 

535. PROP. XCV. The velocity of a particle before incidence : velocity 
after emergence : : sin. emergence : sin. incidence. 





Take A H = I d, and draw A G, d K perpendicular upon A a, D d, 
meeting the directions of incidence and emergence in G, K. Let the 
motion of the body be resolved into the two G A, A H, Id, d k, the ve- 


locity perpendicular to A a cannot alter the motion in the direction A a ; 
therefore the body will describe G H, I K in the same time as the spaces 
A H, I d are described, that is, it will describe G H, I K in equal times 
before the incidence and after the emergence. 

Velocity before incidence : velocity after emergence : : G H : I K 

A H Id 

" sin/incidence sin. emergence 
: : sin. emergence : sin. incidence. 

536. PROP. XCVI. Let the velocity before incidence be greater than 
the velocity after emergence, then, by inclining the direction of the inci 
dent particle perpetually, the ray will be refracted back again in a similar 
curve, and the angle of reflection will equal the angle of incidence. 

ri 2 


A P hXa 

B \P P/ b 




Let the medium be separated by parallel planes A a, B b, C c, D d, 
E e, &c. and since the velocity before incidence is greater than the 
velocity after emergence. .*. sin. of emergence is greater than sin. of in 
cidence. . . H P, P Q, Q R, &c. will continually make a less angle with 
H a, P b, Q c, R d, &c. till at last it coincides with it as at R ; and after 
this it will be reflected back again and describe the curve R q p h g simi 
lar to R Q P H G, and the angle of emergence at h will equal the angle 
of incidence at H. 

537. PROP. XCVII. Let sin. incidence : sin. refraction in a given ra 
tio, and let the rays diverge from a given point ; to find the surface of 
medium so that they may be refracted to another given point. 


Let A be the focus of incident, B of refracted rays, and let C D E 
be the surface which it is required to determine. Take D E a small arc, 

VOL. I. D d 




and draw E F, E G perpendiculars upon A D and D B; then D F, D G 
are the sines of incidence and refraction ; or increment of A D : decrement 
of B D : : sin. incidence : sin. refraction. Take .*. a point C in the axis 
through which the curve ought to pass, and let C M : C N : : sin. inci 
dence : sin. refraction, and points where the circles described with radii 
A M, B N intersect each other will trace out the curve. 

538. COR. 1. If A and B be either of them at an infinite distance or at 
any assigned situation, all the curves, which are the loci of D in different 
situations of A and B with respect to C, will be traced out by this 


A C B 

539. COR. 2. Describe circles with radii A C and C B, meeting A D, 
B D in P and Q ; then P D : D Q : : sin. incidence : sin. refraction, since 
P D, D Q are the increments of B C and A C. 



1. PROP. I. Suppose the resistance oc velocity, and supposing the whole 
time to be divided into equal portions, the motion lost will velocity, and 
oc space described. Therefore by composition, the whole decrement of the 
velocity cc space described. 

COR. Hence the whole velocity at the beginning of motion : that part 
which is lost : : the whole space which the velocity can describe : space 
already described. 

2. PROP. II. Suppose the resistance oc velocity. 

Case 1. Suppose the whole time to be divided into equal portions, and 
at the beginning of each portion, the force of resistance to make a single 
impulse which will oc velocity, and the decrement of the velocity 
cc resistance in a given time, oc velocity. Therefore the velocities 
at the beginning of the respective portions of time will be in a con 
tinued progression. Now suppose the portions of time to be diminished 
sine limite, and then the number increased ad injinitum, then the force of 
resistance will act constantly, and the velocity at the beginning of equal 
successive portions of time will be in geometric progression. 

Case 2. The spaces described will be as the decrements of the velocity 
oc velocity. 

3. COR. 1. Hence if the time be represented by any line and be divid 
ed into equal portions, and ordinates be drawn perpendicular to this 
line in geometric progression, the ordinates will represent the velocities, 
and the area of the curve which is the logarithmic curve, will be as the 
spaces described. 

Dd 2 



[SECT. 1. 

Suppose L S T to be the logarithmic curve to the asymptote A Z. 
A L, the velocity of the body at the beginning of the motion. 

P Q 

h H 

K Z 

The space described in the time A H with the first velocity continued 
uniform : space described in the resisting medium, in the same time : : 
A H P L : area A L S H : : rect. A L X P L : rect. A L X PS* 

: : P L : P S (if A L = subtan. of the curve). 

Also since H S, K T representing the velocities in the times A H, A K ; 
P S, Q T are the velocities lost, and therefore oc spaces described. 

4. COR. 1. Suppose the resistance as well as the velocity at the begin 

ning of the motion to be represented by the line C A, and after any time by 
the line C D. The area A B G D will be as the time, and A D as the 
space described. 

For if A B G D increase in arithmetical progression the areas being 
the hyperbolic logarithms of the abscissas, the abscissa will decrease in 
geometrical progression, and therefore A D will increase in the same 

5. PROP. III. Let the force of gravity be represented by the rectangle 

* Let the subtangent = M. Then the whole area of the curve = M X A L. 

.-. the area ALSH = MXAL MXHS = MXPS=ALXPS. 




BACH, and the force of resistance at the beginning of the motion by 
the rectangle B A D E on the other side of A B. 





Describe the hyperbola G B K between the asymptotes A C and C H 
cutting the perpendiculars D E, d e, in G and g. 

Then if the body ascend in the time represented by the area D G g d, 
the body will describe a space proportional to the area E G g e, and the 
whole space through which it can ascend will be proportional to the area 
E G B. 

If the body descend in the time A B K I, the area described is B F K. 

For>euppose the whole area of the parallelogram B A C H to be di- 

A a K L M N I 

vided into portions, which shall be as the increments of the velocity in 
equal times, therefore A k, A 1, A m, A n, &c. will <x velocity, and there 
fore cc resistances at the beginning of the respective times. 

Let A C : A K : : force of gravity : resistance at the beginning of the 
second portion of time, then the parallelograms B A C H, k K C H, &c. 
will represent the absolute forces on the body, and will decrease in geome 
trical progression. Hence if the lines K k, L 1, &c. be produced to meet 

D d 3 


the curve in q, r, &c. these hyperbolic areas being all equal will repre 
sent the times, and also the force of gravity which is constant. But the 
area B A K q : area Bqk::Kq:4kq::AC:|AK:: force of 
gravity : resistance in the middle of the first portion of time. 

In the same way, the areas q K L r, r L M s, &c. are to the areas 
q k 1 r, r 1 m s, &c. as the force of gravity to the force of resistance in the mid 
dle of the second, third, &c. portions of time. And since the first term is 
constant and proportional to the third, the second is proportional to the 
fourth, similarly as to the velocities, and therefore to the spaces described. 

. . by composition B k q, B r 1, B s m, &c. will be as the whole spaces 
described, Q. e. d. 

The same may be proved of the ascent of the body in the same way. 

6. COR. 1. The greatest velocity which the body can acquire : the velo 
city acquired in any given time : : force of gravity : force of resistance 
at the end of the given time. 

7. COR. 2. The times are logarithms of the velocities. 

8. COR. 4. The space described by the body is the difference of the space 
representing the time, and the area representing the velocity, which at the 
beginning of the motion are mutually equal to each other. 

Suppose the resistance to <x velocity. 

r v ~ 

. . C E : v 2 : : r : j- = retarding force corresponding with the velocity (v) 

.-. x = b X 1 v + C, 

.-. t = b X + Cor. 

= X cc- -, 

.. the times being in geometiical progression, the velocities C, d, E, &c. 
will be in the same inverse geometrical progression. 

Also the spaces will be in arithmetical progression. 




9. PROP. IV. Let D P be the direction of the projectile, and let it 
represent the initial velocity ; draw C P perpendicular to C D, and 



let D A : A C : : resistance : gravity. Also DP: C P : : resistance : 
gravity, .-. DAxDP:CPxCA::R:G. Between D C, C P de 
scribe a hyperbola cutting D G and A B perpendicular to D C in G and B, 
from R draw R V perpendicular cutting D P in V and the hyperbola in T, 
complete the parallelogram G K C D and make N : Q B : : C D : C P. 


V r = - N or R r = ^ , 

for s*ince 

R V = 





~~ ~" 

in the time represented by D R T G the body will be at (r), and the great 
est altitude = a, and the velocity cc r L. 

For the motion may be resolved into two, ascending and lateral. The 
lateral motion is represented by D R, and the motion in ascent by 11 r, 

a D R x QB GTt, 

D R X A B D G . R T 




D R X A B D R x AQ 

D R : R r : : N : A B A Q, or Q B 

: : C D : C P, 

: : lateral motion . ascending motion at the beginning, 
(r) will be the place of the body required. 


10. PROP. V. Suppose the resistance to vary as the velocity 2 . 
Then as before, the decrement of velocity a resistance a velocity ! . 


Let the whole time A D be divided into a great number of equal por 
tions, and draw the ordinates A B, K k, L 1, M m, &c. to the hyperbola 
described between the two rectangular asymptotes, C H, CD; then by the 
property of the hyperbola, 

/. ABKk:Kk::AK:CA 

.-. AB KkaABxKk. 
In the same way 

Kk LI a Kk 2 , &c. 

A B 2 , K k , L 1 2 , &c. 
are proportional to their differences. 

. . velocities will decrease in the same proportion. Also the spaces de 
scribed are represented by the areas described by the ordinates ; hence in 




the time A M the space described may be represented by the whole area 
A M mB. 

Now suppose the lines C A, C K, &c. and similarly A K, K L, &c. in 
geometrical progression, then the ordinates will decrease in the inverse 
geometrical progression, and the spaces will be all equal to each other. 

Q. e. d. 

1 1. COR. 1. The space described in the resisting medium : the space de 
scribed with the first velocity continued uniform for the time AD:: the 
hyperbolic area A D G B : rectangle A B X AD. 

12. COR. 3. The first resistance equals the centripetal force which would 
generate the first velocity in the time A C, for if the tangent B T be drawn 
to the hyperbola at B, since the hyperbola is rectangular AT = AC, and 
with the first resistance continued uniform for the time A C the whole 
velocity A B would be destroyed, which is the time in which the same ve 
locity would be generated by a force equal the first resistance. For the 
first decrement is A B K k, and in equal times there would be equal de 
crements of velocity. 

13. COR. 4. The first resistance : force of gravity : : velocity generated 
by the force equal the first resistance in the time A C : velocity generated 
by the force of gravity in the same time. 

14. COR. 5. Vice versa, if this ratio is given, every thing else may be 


P L K I A 

15. PROP. VIII. Let C A represent the force of gravity, A K the resis 
tance, . . C K represents the absolute force at any time (if the body de 
scend) ; A P, a mean proportional to A C and A K, represents the velo 
city ; K L, P Q are contemporaneous increments of the resistance and 
the velocity. 

Then since 





the increment of velocity cc force when the time is given, 

.-. K L x K N a A P x K C x K N, 

.. ultimately K L O N (equal the increment of the hyperbolic area) 
GC A P cc velocity, cc space described, and the whole hyperbolic area = 
the sum of all the K L O Ns which are proportional to the velocity, and 
.*. space described. .*. If the whole hyperbolic area be divided into equal 
portions the absolute force C A, C I, C K, &c. are in geometrical pro 
gression. Q. e. d. 

16. COR. 1. Hence if the space described be represented by a hyper 
bolic area, the force of gravity, velocity, and resistance, may be repre 
sented by lines which are in continued proportion. 

17. COR. 2. The greatest velocity = A C. 

18. COR. 3. If the resistance is known for a given velocity, the greatest 
velocity : given velocity : : V force of gravity : V given resistance. 

19. PROP. IX. Let A C represent the greatest velocity, and A D be per- 


pendicular and equal to it. With the center D and radius A D describe 
the quadrant A t E and the hyperbola A V Z. Draw the radii D P, D p. 

Case 1. If the body ascend ; draw D v q near to D p, .-. since the sector 
and the triangle are small, 

D v t : Dp q: : D t* : D p* 

q p 


v t oc 



& A D X p q p q 

* AD 2 + ADxAK a C K 

cc increment of the time. 

.-. bv composition, the whole sector a whole time till the whole 
V = 0. 

Case 2. If the body descend ; as before 

D VT: D P Q: : D T 2 : D P 2 

: : DX 4 : D A*: : T X 2 : A P* 
: : DX 2 TX 2 : DA 2 AP 1 
: : A D 2 : A D 2 ADx AK 
: : A D : C K. 
By the property of the hyperbola, 

T X 2 = D X 2 D A 2 
.-. D A 2 = DX 2 TX 2 



oc increment of the time. 

.-. by composition, the whole time of descent till the body acquire its 
greatest V = the whole hyperbolic sector DAT. 

20. COR. 1. If A B = \ A C. 

The space which the descending body describes in any time : space 
which it would describe in a non-resisting medium to acquire the greatest 
velocity : : area A B N K : A A T D, which represents the time. For 
since AC:AP::AP:AK 




: : vol. of the body at any time : the greatest vel. 
Hence the increments of the areas cc velocity cc spaces described. 
.-. by composition the whole A B N K : sector A T D : : space described 
to acquire any velocity : space described in a non-resisting medium for 
the same time. 

21. COR. 2. In the same way, if the body ascend, the space described 
till the velocity = A p : space through which a body would move : : 
A B n k : A D t. 

22. COR. 3. Also, the velocity of a body falling for the time A T D : 
velocity which a body would acquire in a non-resisting medium in the 
same time : : A A D P : sector T D A ; for since the force is constant, 


the velocity in a non-resisting medium cc time, and the force in a resist 
ing medium ocAPccAADP. 

23. COR. 4. In the same way, the velocity in the ascent : velocity with which 
a body should move, to lose its whole motion in the same time : : A A p D 
: sector A t D : : A p : arc A t. 

For let A Y be any other velocity acquired in a non -resisting medium 
in the same time with A P. 

.-. A P : A C : : A P D : this area 


Therefore the area which represents the time of acquiring the greatest 
velocity in a non-resisting medium = A C D. 

In the same way, let Ay be velocity lost in a non-resisting medium in 
the same time as A p in a resisting medium. 

.*. Ap:Ay::AApD: area which represents the time of losing the 
velocity A p. 

.. time of losing the velocity A y = A A p D. 

24. COR. 5. Hence the time in which a falling body would acquire the 
velocity A P : time in which, in a non-resisting medium, it would acquire 
the greatest velocity : : sector A D T : A C A D. 

Also the time in which it would lose the velocity A p : time in which, 
in a non-resisting medium, it would lose the same velocity : : arc A t : 
tangent A p. 

25. COR. 6. Hence the time being given, the space described in ascent 
or descent may be known, for the greatest velocity which the body can 
acquire is constant, therefore the time in which a body falling in a non- 
resisting medium, would acquire that velocity is also known. Then the 
sector ADTorADtrAADC:: given time : time just foundj there 
fore the velocity A P is known or A p. 

Then the area ABNKorABnk:ADTorADt:: space sought 
for : space which the body would describe uniformly with its greatest 

26. COR. 7. Hence vice versa, if the space be given, the time will be 


27. PROP. X. Let P F Q be the curve meeting the plane P Q. Let 


B C D E Q 

G, H, I, K be the points in the curve, draw the ordinates ; let B C = C D 
= D E, &c. 

Draw H N, G L tangents at H and G, meeting the ordinates produced 
in L and N, complete the parallelogram C H M D. Then the times 
cc V L H and V N I, and the velocities oc G H and H I, and the times 


cc ; let T and t = times, and the velocities a ~j and - , therefore 

the decrement of the velocity arising from the retardation of resistance and 

G H H T 

the acceleration of gravity cc ~, , also the accelerating force of 

gravity would cause a body to describe 2 I N in the same time, therefore 

the increment of the velocity from G = 


again the arc is increased 

by the space = HI HN = RI = - =5-= - , therefore the de- 


crement from the resistance alone = ~ -- -- 1 ---- =-= , .. 

GHxt T 

resistance : gravity : : - -- H 1 


2 M I x N I v T 
HI - - : 2 N L 

Again, let 

A B, C D, C E, &c. be o + o, 2o, 3o, &c. 
C H = P 


.-. D I = P 

EK = P 

Q o + &c. 

2Qo 4Ro 2 &c. 



(BG CH) 2 + B C 2 (= G H 2 ) = o 2 + Q*o 2 + 3QRo 3 -f &c. 
.-. G H 2 = 1 + Q 2 x o 2 + 3 Q R o 3 , 

Q Ro 2 

.-. G H = V 1 + Q 2 x o + 

i + Q 


Subtract from C H the sum G B and D I, and R o 2 and R o 2 + 
3 S o 3 will be the remainder, equal to the sagittae of the arcs, and which 
are proportional to L H and N I, and therefore, in the subtracted num 
ber of the times, 

. . ^ a / 

R + 3 S o R + f So ^ j 3 S o 
R " a 2 R " * + 2 R 

Q" 2 2 R 

S o 3 

HI = o. V 1 + Q 4 + 

Q R o 2 

M I x NI__ Ro 2 x_Qo_+ Ro 2 H- &c. 
HI = o. V l~+ Q* Q Ro 2 

I ^ ; 

l + Q 2 

GHxt HT ,2MIxNI 
.-. resistance : gravity : : Fp H 1 H rrr ^~ : " N I 

: : 3 S V 1 + Q 2 : 4 R 2 . 

The velocity is equal to that in the parabola whose diameter rr H C, 

H N 2 1 + Q * 

and the lat. rect. = , or n The resistance oc density x V e , 

e , , resistance 3 S V 1 + Q 2 v R 

therefore the density ^j-^ oc o ^ directly oc _ 

V s * K " ^14-Q S 

directly oc 

R V 1 + Q 2 

28. Ex. 1 . Let it be a circular arc, C H = e, A Q =r n, A C a, 
CD = o, 
.-. D I 2 = n 2 (a+o) 2 = n 2 a 2 2ao-o 8 =e 2 Sao o*, 


and therefore 


2 3 

_ e 

a o n o 
_ - - --5- 

a n o 

r /" t? 

P = c, Q = -, R = ^ 

S = 

a n : 

.-. density oc 


R V 1 + Q 2 " 2e5 

2 e 5 
a n 2 2 e 3 e 


a a sin. 

a a a oc tangent. 

n e e cos. 

3 a n " n n 4 
The resistance : gravity : : g Q . X : 5 : : 3 a : 2 n. 

29. Ex. 2. Of the hyperbola. 

P I X b - P D 2 , 
.-. put P C = a, C D = o, Q P = c, 

.. a + o X c a o ac a 2 2ao + co o 2 

a c a 

.-. D I = 

2 a + c o 2 

r TT- .""B 1 

and since there is no fourth term, 

S = 0, 

.*. draw y = 0. 
30. PROP. XIII. Suppose the resistance to V + V 2 . 

A Q P 


D F 

Case 1. Suppose the body to ascend ; with the center D and rad. D B, 




describe the quadrant B T F; draw B P an indefinite line perpendicular 
to B D, and parallel to D F. Let A P represent the velocity ; join D P, 
D A, and draw D Q near D P. 

.. resistance AP 2 + 2BAxAP, suppose gravity oc D A *, 

. . decrement of V oc gravity + resistance AD 2 +AP 2 + 2BAxAP. 

a D P 2 

DPQ( PQ) :D T V::D P 2 :DT 2 , 
.-. D T Va D T 2 <x l, 
therefore the whole sector E T D, is proportional to the time. 

Case 2. Suppose the force of gravity proportional to a less quantity 
than DA 2 , draw B D perpendicular to B P, and let the force of gravity 

P Q 


oc A B 2 B D 2 . Draw D F parallel to P B and = D B and with the 
center D axis-major = axis-minor = D B, describe a hyperbola 
from the vertex F, cutting A D produced in E, and D P, D Q in T, V. 

Now since the body is supposed to ascend. 

2AB X AP + AB 2 
B 2 + 2AB x BP). 

Also, DTV:DPQ::DT 2 :DP 2 (by similar triangles) 

::TG 2 :BD 2 (TG perpendicular to G) 
: : D F 2 : PB 2 D B 2 . 

Now D P Q cc decrement of velocity oc P B 2 D B 2 , 

.. DTVocDF 2 al a increment of the time, since the time flows uni 

The decrement of the velocity ccAP 
B D 2 oc BP 2 BD 2 BP 2 = AP 2 


Case 3. If the body descend ; let gravity oc B D J A B *. 

With center D and vertex B, describe the rectangular hyperbola B T V, 
cutting the lines D A, D P, D Q produced in E, T, V. 

The increment of V B D 2 A B 2 2 A B x AP _ A P * 
oc B D 2 (A B + AP) 2 oc B D 2 B P 1 
DTV:DPQ(ocpQ)::DT 2 :DP 2 

::GT S :BP*::GD 2 BD 2 :BP 2 
:: GD 2 : BD 2 :: BD 2 : BD 2 EPS 

.-. DT Voc BD oc i, 
.. the whole sector E D T oc time. 

31. COR. With the center C and distance D A describe an arc similar 
to B T. 

Then the velocity A P : the velocity which in the time E D t a body 
would lose or acquire in a non-resisting medium : : A D A P sector 
AD t. 

For V in a non-resisting medium oc time. 

32. In the case of the ascent, 

Let the force of gravity I. Resistance oc 2 a v -f- v 

. . d v oe 1 + 2 a v + v* 
d v 

. . by Demoivre s first formula, 
f. or time = 


VOL. I. 

= ~l X cir. arc. rad. = g and 
tangent = v + a 



The whole time .*. when v = = -, X cir. arc rad. = a 


and tangent z= a -f- C. 

.*. cor r . time = ; X cir. arc rad. = g and tangent v -f a cir. arc rad. 


= g and tangent a. 
.-. the time of ascent = sector EDT g s = 1 a*. 

33. In the case of descent, 

dv cc 1 2 a v v* 

v + a = x 
.*. d v = d x 
.-. \ z -f 2 a v -f a 2 = x s 

.-. 1-r-a 2 x 2 = 1 2 a v v * 

Time = 0, v = 0, 
/. x = a, 

.-. Cor 1 , time X ft- - ffi^- . 

2 g J g x J g a 

34- PROP. XIV. Take A C proportional to gravity, and A K to the 
esistance on contrary sides if the body ascend, and vice versa. 
Between the asymptotes describe a hyperbola, &c. &c. 
Draw A b perpendicular to C A, and 

Ab:DB::l)B 2 :4BA X A C. 
The area A b N K increases or decreases in arithmetic progression it 
the forces be taken in geometric progression. 

A K a resistance a 2 B A P + A P 2 . 


. 2BAP + AP 2 
A K. r= y 

.*. Jv JL T/ > 






KL = 

2 B P Q 

N T ow 

DB:Ab::4BAx CAtDB* 
BD 3 

.-. L O = 

4 B A x C K 

. K-T nv 2PB x PQ x BD 3 

. . IV JL \J IS =: 7~rr~ i >S- i=i . 

4B A x CK x Z 

Case 1. Suppose the body to ascend, 

gravity ex A B + B D 2 = A B + BD 





.-.DP l = CKx Z. 
.-. DT 2 :DP*::DB :CKxZ 
and in the other two cases the same result will obtain. 

DTV = DBx ra. 

.-.DBxm:iDBx PQ::DB*:CK X Z 
.-. BD 3 xPQ = 2BDxmxCKxZ. 


it will represent the space. 

A P.* velocity. 


35. PROP. XV. LEMMA. The 

. O P Q = a rectangle = L. O Q R 

L. S P Q = L. of the spiral = A. S Q R 

.-. L. O P S = L- O Q S. 

.-. the circle which passes through the points P, S, O, also passes 
through Q. Also when Q coincides with P, this ^^- touches the spiral. 

.-. L. P S O L. in a 

whose diameter = P O. 



TQ : PQ :: PQ : 2 PS. 
.r. PQ-- 2PS x TO 

which also follows from the general property of every curve. 
PQ 2 = P V x Q R. 


QK -TW- 

36. Hence the resistance density X square of the velocity. 

37. Density oc -j-- centripetal force oc density 2 -p -. 

J distance distance 2 

Then produce S Q to V so that S V = S P, and let P Q be an arc 
described in a small time, P R described in twice that time, .. the decre 
ments of the arcs from what would be described in a non-resisting me 
dium a T 2 . 

.. decrement of the arc P Q = \ decrement of the arc P R 

.-. decrement of the arc P Q = R r (if Q S r = area P S Q). 

For let P q, q v be arcs described (in the same time as P Q, Q R) in a 
non-resisting medium, 

PSq PSQ = QSq = qSv Q S r 

-rSv QSq 
.-. 2 Q S q = r S v 

.-. if S T ultimately = S t be the perpendicular on the tangents 
STxQq = Stxrv 

.-. 2 Q q = r v 

R v = 4 Q q. 
. . 2 Q q = R r. 

Resistance : centripetal force : : R r : T Q, 

T Q X S P 2 a time 2 , (Newt. Sect. II.) 
.-.PQ 2 X S P a time 2 

/. time a P Q x V fc> I 

.-. V a 

V at Q oc 


C J 


PQ: Q r : : SQ: SP 

since the areas are equal, and the angles at P and Q are equal. 
.-. P Q : R r : : S Q : S P V S Q x S P 

: : S Q : f V Q 

.-. S Q x S P = S P 2 V Q x SP 

.-. V SQx SP = SP J V Q_Z^_&c. 

.-. V Q ultimately = S P V S P X S Q 

T-, . decrement of -V R r 

Resistance oc = 5 cc 

time 2 P Q 2 X S P 



1 Q O 

S Q = S P cc QJ f x gp2 

O S 

.-. density X square of the velocity cc resistance cc Typ q- 

/. density a /Y15 o~ 

O S 

and in the logarithmic spiral ^r-p is constant 

.*. density cc ^-g . Q. e. d. 

88. ("OR. 1. V in spiral = V in the circle in a non -resisting medium at 
he same distance. 

39. COR 3. Resistance : centripetal force : : - R r : T Q 

jVQx PQ ^PQ 2 


: : I O S : O P. 

. . the ratio of resistance to the centripetal force is known if the spiral be 
given, and vice versa. 

40. Con- 4. If the resistance exceed the centripetal force, the body 
cannot move in this spiral. For if the resistance equal | the centripetal 


force, O S = O P, . .the body will descend to the center in a straight 
line P S. 

V of descent in a straight line : V in a non-resisting medium of de 
scent in an evanescent parabola : : 1 : V 2 ; for V in the spiral = V in the 
circle at the same distance, V in the parabola = V in the circle at 
| distance. 

Hence since time a v , 

time of descent in the 1st case : that in 2d : : V 2 : 1. 

41. Con. 5. V in the spiral P Q R = V in the line P S at the same 
distance. Also 

P Q R : P S in a given ratio : : P S : P T : : O P : O S 
.-. time of descending P Q R : that of "P S : : O P : O S.* 
Length of the spiral = T P = sector of the L. T P S. 

a : b : : b : c : : c : d : : d : e 
a + b + c + &c. : b + c + d + &c. : : a : b 

.*. a -f- b + c -} &c. : a : : a : a b. 

42. COR. 6. If with the center S and any two given radii, two 
circles be described, the number of revolutions which the body makes 
between the two circumferences in the different spirals <x tangent ot the 

angle of the spiral cc 

The time of describing the revolution : time down the difference of the 
radii : : length of the revolution : that difference. 

2d ex 4th, 
/. time cc length of the revolution oc secant of the angle of the spiral 


p q : p t : : S p : S y 

p (1 x 

d w : : : x : p. 

r. .- t 


43. Con. 7. Suppose a body to revolve as in the proposition, and to cut 

the radius in the points A, B, C, D, the intersections by the nature of the 
spiral arc in continued proportion. 

Times of revolution a Perimetersdescribed 

and velocity oc 



aA W T} Q ST ^ G 2 
i*. O J.) O V^ O 

. . the whole time : time of one revolution : : A 

: : A 
44. PROP. XVI. Suppose the centripetal force x J n , 

time a P Q x S P 

and velocity ex 

&c. : A S 

: A S B S *. 



Qr:PQ::SP :SQ 

Qr : Q R 
. . Q r : R r 


S Q $ - l : S Q *- > _ S P S ~ 
S Q : l^TfiT. V Q. 

S P = S Q + V Q, 


*- 1 + 1. VQ x SQ*- 2 + &c. 

... SQ2- _SP- = 1 x VQ x SQ?- 2 . 
Then as before it may be proved, if the spiral be given, that the density 
^rp. Q. e. d. 
45. COR. 1. 


Resistance : centripetal force : : 1 n . O S : O P, 
fur the resistance : centripetal force : : | II r : T Q 

X VQx PQ PQ ! 

Q " TiT 

x VQ:PQ 

: : l - x O S: OP. 


46. COR. 2. If n + 1 = 3, 1 ~ = 0, 


.. resistance = 0. 
COR. 3. If n + 1 be greater than 3, the resistance is propelling. 


47. PROP. XXIV. The distances of any bodies centers, of oscillation from 
the axis of motion being the same, the quantities of matter CD weight 
X squares of the times of oscillation in vacua. 

T, t i i -, force X time ,, ,. 

1< or the velocity generated GC -, - . r orce on bodies at 

quantities 01 matter 

c(jual distances from the lowest points GO weights, times of describing 
corresponding parts of the motion cc whole time of oscillation, 

c force X time of oscil. 

.-. quantities of matter cc -, .-, 


co weights X squares of the times, 

since the velocities generated cc -: for equal spaces. 


48. COR. 1. Ilence the times being the same, the quantities of matter 
co weights. 

Cou. 2. If the weights be the same, the quantities of matter co time % 

COR. 3. If the quantities of matter be the same, the weights cc -: -. 

time * 


49. Cou. 4. Generally the accelerating force cc - p .^ of matter 


and L oo T T 2 , 
T WxT* 
W x T 2 

.-. Q cc 


.\ if W and Q be given L co T 2 . 
If T and Q be given L oo W. 

CA ~ _ . ... c weight X time 2 of oscillation 
50. COR. 5. generally the quantity or matter cc a 1 -= . 

51 PROP. XXV. Let A B be the arc which a body would describe in a 

non-resisting medium in any time. Then the accelerating force at any 
point D oc C D ; let C D represent it, and since the resistance cc time, 
it may be represented by the arc C o. 

.*. the accelerating force in a resisting medium of any body d, = o d. 



Therefore at the beginning of motion, the accelerating force will be in 
this ratio, .*. the initial velocities and spaces described will be in the some 
ratio, .. the spaces to be described will also be in the same ratio, and 
vanish together, . . the bodies will arrive at the same time at the points 
C and o. 

In the same way when the bodies ascend, it may be proved that they 
will arrive at their highest points at the same time. .-. If A B : a B in 
the ratio. C B : o B, the oscillations in a non-resisting and resisting me 
dium will be isochronous. Q. e. d. 




Con. The greatest velocity in a resisting medium is at the point o. 
The expression for the J- time of an oscillation in vacuo, or time of de 
scent down to the lowest point a quadrant whose radius = 1. Now 

suppose the body to move in a resisting medium when the resistance 
: force of gravity : : r : 1. 

Then vdv = gFdx + grdz = gd 2 x + grdz. Now by 

a property of the cycloid, if - be the axis, d x : d z : : x : \ : : z : a, 


z d z 

. . d x =r , 


. . v d v = i - x z d z -f- grdz ~ 

= f X z 2 + grz, 

. . v 



r= d, V = o, 

.-. v 2 = . xd 2 z 2 _2grxd z 

= - x T r 4 a r d + 2 a J r z z*," 

2 2 a r d -f 2 a r z z s , 
a d z 

Vd z 2 a r d + 2 a r z z *. 


z a r = y, 

... z - 2 a r z + a * r * = y\ 

.*. 2 a r z z * = a s v * y f , 

d 2 a r d -f 2 a r z z = (d a r) 2 y ! = (b * y 5 



d z =r d y 


i r u Y 

.-. d t = / X -- ^- J 

J g Vb 2 y 8 

.-. t = f x circular arc, radius = 1, 

J % 

z a r 

cos. = , -f C and C = o. 

d a r 

/. the whole time of descent to the lowest point = f - X circular arc 

, a r . . 

whose cos. = -; , .-. time in vacuo : tune in resisting medium 

d a r 

- _. - o 

: : quadrant : arc whose cos. -: 

d a 

a r 


Cou. 1. Time of descent to the point of greatest acceleration is constant, 
for in that case z = a r, 

t = f x quadrant, for d v = 0, 


.-. v d v = 0, 

/. g z d z + g a r i = 0, 

/. z = a r, 
.-. z : r : : a : 1. 

COR. 2. To find the excess of arc in descent above that in ascent. 
v d v -f- g T d x + g r d z, 

z d z 
. v d v = -- s r d z 

v 2 m z 2 

.-. v 2 = &- (d- z 2 ) (z d) x 2 a r 

= - X (d * 2 a r d) (2 a r z z ) 

which when the body arrives to the highest point = 0, 
d ~ 2 a r d 2 a r z z 2 = 0, 

,1 " 9 a i* rl -7 2 I O .1 T r, 

.-. d 5 2ard = z*+2a r z, 
.-. z + a r = d a r, 
.-. z = d 2 a r, 
.-. d z = 2 a r. 




52. PROP. XXVI. Since V oc arc, and resistance a V, resistance a arc. 
.-. Accelerating force in the resisting medium GC arcs. 

Also the increments or decrements of V a accelerating force. 

.. the V will always <x arc. 

But in the beginning of the motion, the forces which oo arcs will generate 
velocities which are proportional to the arcs to be described. .-. the velo 
cities will always co arcs to be described. 

.*. the times of oscillation will be constant. 

53. PROP- XXVIII. Let C B be the arc described in the descent, C a 
in the ascent. 

.-. A a = the difference (if A C = C B) 
Force of gravity at D : resistance : : C D : C O. 
C A = C B 
Oa = O B 
. . CA OaorAa eO = CB OB = CO 

.-. C O = A a 

. . Force of gravity at D : resistance : : C D : A a 
. . At the beginning of the motion, 

Force of gravity : resistance : : 2 C B : A a 

: : 2 length of pendulum : A a. 
54. PROB. To find the resistance on a thread of a sensible thickness. 

Resistance CD V * X D * of suspended globe. 

.*. resistance on the whole thread : resistance on the globe C : : 


::2a s V. (a b) 8 : a 3 r 2 c 2 r 2 c 2 . (a 2 b) 3 , c = a + r. 

:: a 3 b 2 . (a b) * : 3a 2 r 2 c 2 b bab 2 r*c 2 -f-4b 3 r 2 c*, 
:: a b . (a b) 2 : 3a z r 2 c 2 ba b r * c 2 + 4 b * r 2 c\ 
.. resistance on the thread : whole resistance 
::a 3 b. (a b) a : r 2 c*.(3a ! bab+ 4b 3 ). 

COR. If the thickness (b) be small when compared with the length (a) 
bab4 4b 2 =3a 2 bab + 3 b 2 (nearly) = 3. (a b) -. 


3 a 

. . Resistance on the whole thread : resistance on the globe 
: : a 3 b : 3r a c 

Resistance on the thread : whole resistance to the pendulum 

Suppose, instead of a globe, a cylinder be suspended whose ax. = 2 r. 
Now by differentials 

the resistance on the circumference : resistance on the base : : 2 : 3. 

By composition the resistance to the cylinder : resistance on the square 
= 2 r : : 2 : 3. 

Resistance a x 2 x , 
. . resistance ax 3 , 

.. resistance to the whole thread ot x 3 . 
Resistance on A E a (a 2 b) 3 if 2 b = E D. 
. . Resistance on the thread : resistance of the globe 

: : 16 . a 3 b 2 . (a b) * ; 3 p . a 3 (a 2 b) 3 x r s . (a + i) *. 

55. PROP. XXIX. B a is the whole arc of oscillation. In the line OQ 
take four points S, P, Q, R, so that if O K, S T, P I, Q E be erected 




perpendiculars to O Q meeting a rectangular hyperbola between the 
asymptotes O Q, O K in T, I, G, E, and through I, K F be drawn 

O S P rRQ M 

parallel to O Q, meeting Q E produced in F. The area P I E Q may 
be : area P I S T : : C B : C a. Also I E F : I L T : : O R : O S. 

Draw M N perpendicular to O Q meeting the hyperbola in N, so that 
P L M N may be proportional to C Z, and P I G R to C D. 

Then the resistance : gravity -QQ X TEF IGH:PINM. 

Now since the force cc distance, the arcs and forces are as the hyper 
bolic areas. .*. D d is proportional to R r G g. 

Now by taking the differentials the increment of (Q-Q T E F I G H) 

P ,. T TTT? T V V 

= G H g h - 
H G I E I 


: R rX G R : : H G Q : G R : : O R X 

O P x 
O R 


x IEF:OPx PI. 
O R 

NowifTs g-^XIEF I GH, the increment Y a PIG R Y. 

Let V = the whole from gravity. .*. V R = actual accelerating 
force. . . Increment of the velocity a V R X increment of the time. 
As the resistance cc V 2 the increment of resistance a V X increment of 

, . , , . . increment of the space f 

the velocity, and the velocity a - ?. t . .-. Increment of 

increment ot the time 

resistance a V R if the space be given, co P I G R Z, if Z be the 
area which represents the resistance R e. 

Since the increment Y a PIGR Y, and the increment of Z 




ccPIGR Z. IfY and Z be equal at the beginning of the motion and 
begin at the same time by the addition of equal increments, they will still 
remain equal, and vanish at the same time. 

Now both Z and Y begin and end when resistance = 0, i. e. when 
O R 


. I E F I G H = 


xOR IGH = 0. 

O R x I E F 

I G H = Z 

.-. Resistance : gravity : : g-| . I E F I G H : P M N I. 

66. PROP. XLIV. The friction not being considered, suppose the mean 




altitude of the water in the two arms of the vessel to be A B, C D. Then 
when the water in the arm K L has ascended to E F, the water in the arm 
M N will descend to G H, and the moving force of the water equals the 
excess of the water in one arm above the water in the other, equals twice 
A E F B. Let V P be a pendulum, R S a cycloid = length of the 
canal, and P Q = A E. The accelerating force of the water : whole 
weight : : A E or P Q : P R. 


Also, the accelerating force of P through the arc P Q : whole weight 
of P : : P Q : P R ; therefore the accelerating force of the water and P 
cc the weights. Therefore if P equal the weight of the water in the canal, 
the vibration of the water in the canal will be similar and cotemporaneous 
with the oscillations of P in the cycloid. 

COR. 1. Hence the vibrations of the water are isochronous. 

Con. 2. If the length of the canal equal twice the length of the 
pendulum which oscillates in seconds; the vibrations will also be performed 
in seconds. 

COR. 3. The time of a vibration will <* V L. 
Let the length = L, A E = a, 

then the accelerating force : whole weight : : 2 a : L, 

.*. accelerating force = -y- ; 


2 A 
.. when the surface is at 0, the accelerating force = ^ 

Put E = x, 

A = a x, 

, .. c 2 a 2 x 
.. accelerating torce = = . 

g . 2 a d x 2 x d x 
* _ 

X 2 a x x 2 , 

x adx 

V 2 a x x s 

*. t ss^J ^ 5 X cir. arc rad. =a, and vers. = x 

~ ^ g a 

cor n . and cor". =r 0, 

v t = 0, x = 0, 
.-. ifp = 3. 14159, &c. 

= J 

(x) = (a)} = /-L X - P - 
ga 2 V2ga 


. . time of one entire vibration = p X 7-5 = time of one entire vi- 

V 2 o- 

bration of a pendulum whose length = . 


\ oi. I, Ff 




57. COR. 1. Since the distance (a) above the quiescent surface docs 
not enter into the expression. The time will be the same, whatever be 
the value of A E. 

58. COR. 2. The greatest velocity is at A = -^ x a, a a / - 

\ 1* L A V I 

59. PROP. XLVIL Let E, F, G be three physical points in the lin 
B C, which are equally distant; E e, F f, 
G g the spaces through which they move 
during the time of one vibration. Let e, <p, y 
be their place at any time. Make P S = 
E e, and bisect it in O, and with center O 
and radius O P = O S, describe a circle. 
Let the circumference of this circle repre- H 
sent the time of one vibration, so that in 
the time P H or P H S h, if H L or h 1 
be drawn perpendicular to P S and E be 
taken =r P L or P 1, E s may be found in 
E ; suppose this the nature of the medium. 
Take in the circumference P H Sh, the arcs 
H I, I K, h i, i k which may bear the 
same ratio to the circumference of the circle as E F or F G to 
B C. Draw I M, K N or i m, k n perpendicular to P S. Hence 
PI, or P H S i will represent the motion of F . and P K or 
P H S k that of G . E , Fp, G 7 = P L, P M, P N or P 1, 
P m, P n respectively. 

Hence s 7 or E G + G 7 E e = GE L N = expan 
sion at s 7 ; or = E G + 1 n. 

. . in going, expansion : mean expansion : : G E L N : E G 

In returning, 

: : : E G + In : E G 

Now join I O, and draw K r perpendicular to H L, UK r, 
I O M are similar triangles, since the^KHr = ^KOk=^ 
I O i = L. I O P and ^ at r and M = 90, 
.-. L N : K H : : I M : I O or O P, and by supposition K H : 
EG:: circumference PSLP:BC::OP:V = radius of 
the circle whose circumference = B C. 
.. by composition L N : G E : : I M : V. 

.% expansion : mean expansion : : V I M : V, 







Let A C and E be the respective places of the object, eye, and reflector 
at first, and B Q and F their places at any other time, or if K F = F Q 
= C E, K may also be the place of the eye, and since K F always = C E, 
and that B F is constant, K will trace out an ellipse by next problem. 
Also by optics the angle K F H = H F Q, and from similar triangles, 
K H : K F : : K D : K B, 

.-. KH + DH:KF + BF::KD:KB, 

D Q : D K : : K F + B F : K B in a given ratio, 
*. Q traces an ellipse. 

To determine the quantity of fluid issuing through an orifice of a 
given form and magnitude, in the side of a cylindrical vessel, supposed to 
be kept constantly full. 


S B = h, S A = h , A P = x, 
P M = y, 
.. velocity of the efflux in M N 

= V g (h + x) 

and the area of the lamina = 2 y x 
and the time = t, 

.*. the quantity of fluid through M N 
in n = area of the section x vel. X t, 

= 2 y x V g (h + x) X t, 

. . the quantity effluent through the whole area A m S t A = sum of 

all the portions effluent through M N = / 2 y x V g h ^f~xt 2t 

^gy^h -f-x-fC connected between the values x = 0, and 
x =r h - h . 


_ f/y x 

[y~x ~~+~C p 

mean height. 


.-. (ra b*) 8 xdx s = 2 r a b dy b 4 d y *, 

.-. r* a z dx* = 2 rab dy 8 
if (b) be small compared to (aj, 
r ad x* 

d y - VKT 

V r a X d x /jr_ _adx 

^ " " V 2 a x x 2 / N/a v V2ax x 2 

.\ v = / x circular arc whose rad. = a, and vers. = x 

\l a 

C, and cor". = 0, 
because when y = 0, x = 0, 
.. arc = 0. 

.-. C D = x quadrant B N E, 

and therefore 


V a " 


B N x k 

60. PROP. XLIX. Put A = attraction of a homogeneous atmosphere 
when the weight and density equal the weight and density of the medium 
through which the physical line E G is supposed to vibrate. Then every 
thing remaining as in Prop. XL VI I. the vibration of the line E G will 
be performed in the same times as the vibrations in a cycloid, whose 
length = P S, since in each case they would move according to the Fame 
law, and through the same space. Also, if A be the length of a pendulum, 
since T a V L 

The time of a vibration : time of oscillation of a pendulum A 
: : V~T~O : V ~A. 

Also (PROP. XLVIL), the accelerating force of E G in medium : ac 
celerating force in cycloid 

since H K : G E : : P O : V. 

: : PO X A : V 2 . 
Ff 3 



T x ji ~- when L is given. 

.. the time of" vibration : time of oscillation of the pendulum A 
: : V : A 
: : B C : circumference of a circle rad. = A. 

Now B C = space described in the time of one vibration, therefore 
the circumference of the circle of radius A = space described in the time 
of the oscillation of a pendulum whose length = A. 

Since the time of vibration : time of describing a space =r circum 
ference of the circle whose rad. = A : : B C : that circumference. 

COR. 1. The velocity equals that acquired down half the altitude of 
A. For in the same time, with this velocity uniform, the body would de 
scribe A ; and since the time down half A : time of an oscillation : : r : 
circumference. In the time of an oscillation the body would describe the 

Con. 2. Since the comparative force or weight cc density X attraction 

of a homogeneous atmosphere, A GO -, , and the velocity 00 V A. 

V elastic force 

ff , 

*JU ^- 

V density 


61. PROP. XLIX. Sound is produced by the pulses of air, which 
theory is confirmed, 1st, from the vibrations of solid bodies opposed to it. 
2d. from the Coincidence of theory with experiment, with respect to the 
velocity of sound. 

The specific gravity of air : that of mercury : : 1 : 11890. 

Now since the alt. oc - , .-. 1 : 11890 : : 30 inches : 29725 feet = 

sp. gr. 

altitude of the homogeneous atmosphere. Hence a pendulum whose 
length = 29725, will perform an oscillation in 190", in which time by 
Prop. XLIX, sound will move over 186768 feet, therefore in I" sound 
will describe 979 feet. This computation does not take into considera 
tion the solidity of the particles of air, through which sound is pro 
pagated instantly. Now suppose the particles of air to have the same 
density as the particles of water, then the diameter of each particle : dis- 


.-. elasticity : mean elasticity : : : . In the same way, for the 

points E and G, the ratio will be ^7 ^-^ : _ a \ . JL 

V rlL, V V KN V 

: : excess of elasticity of E : mean elasticity 

H L K N 1 

V 2 HLxV KNx V + HLx KN : T 
: : H L K N : V. 


V a 1. 

.-. the excess of E s elasticity cc H L K N, and since H L K N 
= H r : H K : : O M : O P, 

.-. H L K N a O M, 

/. excess of E s elasticity cc O M. 

Since E and G exert themselves in opposite directions by the arc s ten 
dency to dilate, this excess is the accelerating force of e 7, .. accelerating 
force co O M.* 


Since the ordinates in the harmonic curve drawn perpendicular to the 
axis are in a constant ratio, the subtenses of the angle of contact will be 

in the same given ratio. Now the subtenses oc . , and when 

rad. of curv. 

the curve performs very small vibrations, the arcs are nearly equal. 

Now the curv. cc ,- , .*. subtense cc curvature, 

Hence the accelerating force on any point of the string cc curvature at 
that point. 

* Now bisect F f in n, 

.-. O M = n<p 

O M = O T PM=nF F = n ? 
i. e. the accelerating force cc distance from f) the middle point. Q. e. d. 


To find the equation to the harmonic curve. 

C S 

E D 

Let A C be the axis of the harmonic curve C B A, D the middle point, 
draw B D perpendicular cutting the curve in B; draw P M perpendi 
cular to B D cutting the curve in P, and cutting the quadrant described 
with the center D and radius D B in N. Draw P S perpendicular to A C- 

BD = a, PM = y, B M = x, 
.-. D M = a x = P S. 

r = rad. of curv. at B, B P = z, 
d z d x 

. . rad. of curv. = 







(if d K be constant). 

a : a x : 

: curvature at B : curvature at P 
: rad. of cur. at P : rad. at B 

d z d x 

d y 
.*. r a d * y + adzdx xdxdz = 0, 

.\ rady + adzx = + C. 

x = 0, d y = d x, 
radz = + C = C, 

rady + axdz 


= r a d z. 

. . r a d y = r a b 2 d z, 
.-.r a dy ir (ra b 2 ) 2 X d x 2 + r a 8 dy 2r a b ! d y ! + b 4 d y % 



L t 
D d : - - = rad. of curve : : the moving force of D d : P 

.-. the moving force of D d = P x D T d X ap * 

L w 

. . accelerating force = P X Dd X a p* L 

L* Dd X w 

P X a p * 

if D O = x, D C = a, O C =r a x, 

.*. the accelerating force at O = T" . 
_ g. Pp 

v A * - v i - i 

. . v a s _ j- x a d x x d x 

P r>* 

... v z = fe ^ X 2ax 
L w 

g pl 

T /> V 2 ax x . 

L w 

.-. C and 1 = 0, 

d x / L w d x 

. . d t = . / 75 rX -; 

v VgPp 1 V 2 a x - 

L w 

rs , X cir. arc rad. = 1 



vers. sine = , 

when x = a, 
t = 0. 

^ r X -quadrant ss ./ ^ - X 

g P p 9 V g P p * 2 

= * x \J "^F* 

.". time of a vibration = / rr- I" 

/V g L 

. . number of vibrations in 1 " = ^ / -$ . 

V L w 

COR. Time of vibration =r time of the oscillation of a pendulum whose 
L w 




For this time = ./- 

64. PROP. LI. Let A F be a cylinder moving in a fluid round a 
fixed axis in S, and suppose the fluid divided into a great number of solid 

orbs of the same thickness. Then the disturbing force cc translation of 
parts X Surfaces. Now the disturbing forces are constant. . . Transla 
tion of parts, from the defect of lubricity a T. . Now the differ- 


r-.i ! . translation 1 * , 

ence ot the angular motions cc p ex -: - . On A Q draw 

distance d:stance* 

A a, B b, C c, &c. : : 
a hyperbolic area. 
. . periodic time cc 

distance - 

then the sum of the differences 



cc distance. 

angular motion hyperbolic area 
In the same way, if they were globes or spheres, the periodic time 
would vary as the distance *. 



tance between their centers : : 1 : 9, or 1 : 10 nearly. (For if there are 
two cubes of air and water equal to each other, D the diameter of the par 
ticles, S the interval between them, S + D = the side of the cube, and if 
N = N. N S + N D = N. in the side of the cube, N. in the cube 
jo N 3 . Also, if M be the N. in the cube of water, M D the side of the 
cube and the N. in the cube cc M 3 . 

Put 1 : A : : N 3 : M 3 , 

.-. M = A * N, 
By Proposition 

.-. S = D X A a 1, 
.-. S: D: : A 3 1 : 1, 

.-. S + D : D : : A 3 : 1 : : 9 : 1 if A = 870 

or 10: 1 if A = 1000). 

Now the space described by sound : space which the air occupies : : 9 : 11, 


.. space to be added = -^ = 108 or the velocity of sound is 1088 

feet per 1". 

Again, also the elasticity of air is increased by vapours. Hence since 

the velocity oc e . a - ^ ; if the density remain the same the velocity 
V density 

oc V elasticity. Hence if the air be supposed to consist of 11 feet, 10 of 
air, and 1 of vapour, the elasticity will be increased in the ratio of 1 1 : 10, 
therefore the velocity will be increased in the ratio of 11| : 10| or 21 : 20, 
therefore the velocity of sound will altogether be 1 142 feet per 1", which 
is the same as found by experiment. 

In summer the air being more elastic than in winter, sound will be 
propagated with a greater velocity than in winter. The above calculation 
relates to the mean elasticity of the air which is in spring and autumn. 
Hence may be found the intervals of pulses of the air. 

By experiment, a tube whose length is five Paris feet, was observed to 
give the same sound as a chord which vibrated 100 times in 1", and in 
the same time sound moves through 1070 feet, therefore the interval of 
the pulses of air = 10.7 or about twice the length of the pipe. 

Ff 4 


62. On the vibrations of a harmonic string. 

The force with which a string tends to the center of the curve : force 
which stretches the string : : length : radius of curvature. Let P p be a 

small portion of the string, O the center of the curve ; join O P, O p, and 
draw P t, p t, tangents at P and p meeting in t, complete the parallelo 
gram P t p r. Join t r, then P t, p t represent the stretching force of 
the string, which may be resolved into P x, t x and p x, t x of which 
P x, p x destroy each other, and 2 t x = force with which the string 
tends to the center O. Now the /LtPr= z. P O p, . . z. t P x = . 
P O p, .*. t r : P t : : P p : O P, i. e. the force with which any particle 
moves towards the center of the curve : force which stretches it : : length 
: radius. 

63. To find the times of vibration of a harmonic string. 


Let w = weight of the string. L = length. 
D d : L : : weight D d : w 

1* TTAJ D d X W 

. . weight or D d = _ 

K 1 1 U KIN Astronomy Mathematics Statistics Computer Science Library 

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