﻿OF THE HINDUS. 265 



part of the operation differs in no respect that I know 

 of from the method of European astronomers to 

 compute a lunar eclipse. The translation of the For- 

 mula for this purpose, in the Surya Siddhanta, is as 

 follows : «' The earth's shadow is always six signs 

 " distant from Surya ; and Chandra is eclipsed when- 

 <c ever at the purnima the pata is found there; as is 

 " also Szirya, whenever at the end of the amavasya the 

 " pata is found in the place of Surya ; or, in either 

 " case, when the pata is nearly so situated. At the 

 *' end of the amavasya tifhi the signs, degrees, 

 <c and minutes of Surya and Chandra are equal ; and 

 <( at the end of the purnima tifhi the difference is ex- 

 <c actly six signs; take therefore the time unexpired 

 V of either of those tifhis, and the motion for that 

 *' time add to the madhyama, and the degrees and mi- 

 " nutes of Surya and Chandra will be equal. For 

 *' the same instants of time compute the place of the 

 ** pata in its retrograde motion, and, if it should be in 

 *' conjunction with Surya and Chandra, then, as from 

 tc the intervention of a cloud, there will be an obscu- 

 u rity of Surya or of Chandra. Chandra, from the 

 " west, approaches from the earth's shadow, which on 

 " entering, he is obscured. For the instant of the puri- 

 *' nima, from the half sum of the chandramana and the 

 f tamoliptamana subtract the vicshepa, the remainder is 

 " the cftchanna. If the ch'channa is greater * than the 

 " grahyamarui, the eclipse will be total ; and if less, the 

 " eclipse will be proportion-ably less. The grahya and 

 " grahaca deduct and also add ; square the difference 

 " and the sum severally ; subtract the square of the 

 " vicshepa from each of those squares, and the square 

 " root of each remainder multiply by sixty ; divide 

 (< each product by the difference of the gati of Surya 



* Or, when the cb'cbanna and grabyamana are equal, the eclipse 

 Wjotal, 



S 4 



