848 str५-Siddhdata gives us, as the moon's latitude at the moment of opposition, 16 25*S. Nowthen, by iv. 10-11, seui-diameter of eclipseu body (84 41"+2, . of eclipsing body (ly 80’-2), 17’ 23 5’ 18 their sun , lelue moon's latitude 02 8” 10 25 * Anount of greatest obscuration (yrika) 46 12 and since this mount is greater than the liumcter of the eclipsed body , it is evidumb thnt tre eclipse is a total one. 'his is a list unfortunate result for the Hindu calculation to yield for, in point of fact, the "clipse in question is only a partial onc, olbscuring alsout four-fifths of the dinmeter of the noon's disk. The source of tho error lie mainly in the nuishcenment. t। ] ntively to the Sun and moon, of the moon's node, until the conRequent fulke value found for 1he Moon's latituate. The latter quentity actually annount, at the time of opposition , ko 85 42 + nor than twice {he value given it !y he Hindu processes An it will be seen, on yearing to the table on p, 148, that the elative erok in the place of the moon's node, having been accumulating fo¥ Reven confuries, is now about 3, and so reclugue, by TrUr® Lhan hnlt, the true distance of the moon from he note . We have tried whether the and uision of the correction of the ho would betwer tho result, but that is not the case: the orror of position is still (see the table) nearly 2", and the udon's latitude is increased only to 24° 11, so that the eclipse still appears to le total. It is evidently high time that a new correction of biju be applied by the Hindu astronOnners to their elements, at least to sch ५s enter into the calculation of eclipses. VIII. I'o find the duration of the eclipse, and of total obscuration, and the lines of contact, inmmersion, encrgence, and separation. Diameter n the splipsing body, the slaadow Do. 'clipsed body, the moon, 90° 30” 34 41 90 80" 84 41 Bu। Ind diference . 125 11 Eu-819 2nd half-difference (CM MR CN, Pig, p1, p. 152), 62 8b ASruares of do. 849A deduct ejuare of latitude 269 38 49 27 83 724 89 remain Kyuure roots of retuainders (GA and CB), 880 0 25 485 21 ap" In order to reduce these quantities to time, we need [rst to ascertain
