76 Sarva-Siddhanta •1B 7. (Fig. 4). The points B, A, M, १, , and ०, correspond with those simi larly marked in the 14ast figure (Fig. 3). £he centre of the eccentric circle is at , and IE, which equals Alis the eccentricity, which is given. Join e%; the angle wea equals MEA, the incun ४nomaly , ma be equals Mothe cquation. Extend Eig. 4 me to , where it ameets Eta per. pendicular let fall upotn it from E. Then, in the right-angle triangle e, the sie ME and the angles Eed equals * ९ •re en, to find he other witles, ed and .]] . Add && to , the dius; add the square of the sum to that of ED the Aguare rootb of t]uir sum j« ]F4 : 1hem.in the th-angla friangle Ed. all the sides and the right angle are lyan ( ir ]he १ngle Eth४ the equalon. This process is equivalent to a transfer of the epity¢l% from M to E; Er becomes the result from the basesine (bajjipeta}, an तe that from the perpendicular-xine (Motijipfted, and the angle of the equation is found in the 171 ner && is se !(! is found in the indu process next to be explained; while, in that which we have been considering , E
- {&6ared to be equal to ke
Ptolenmy nlso adds to the moon's orbit ann picycle, to account for her second inequality, the ovcation, the discovery of which does himn so much honor. Of this inequalify the Hindu take no notice. 4(). 'The result frobn he perpendicular-sine (kutiphala) of the distance from the conjunction is to be aded to radius, when tle distance (kendra) is in the half-orbit beginning with Capricorn; but when in that beginning with Cancer, the 1esult from the per ppendicula-sine is to be subtracted 41. To the square of this sum or difference add the square of the result from the ba-sine (alphala); tlho &quare root of their sum is the hypotheouse (koipe) called variable (cat). Multiply the PeBult from th basesine by radius, and divide by the variable hypotbenux : 42. he are corresponding to the quotient is, in minutes, etc., blhe equation of the conjunction (ligarya pottr); it is em