सिद्धान्तशिरोमणि: गणिताध्याय (भास्कराचार्य - ग्रहगणित, मध्यमाधिकार व स्पष्टाधिकार सटीक)

433 daily motions namely 48′-46″, what will it be for an arbitrary Dṛk-kṣepa ?" We have (D × 48′-46″) / 3438 . Converting 48¾ / 3438 ie. 195 / 13752 ie. 65 / 4584 into a continued fraction, this will be equal to 1/(70+) 1/(1+) 1/(1+) 1/(10+) 1/3 of which a very approximate convergent is 1/71 as taken by Bhāskara. If the radius be taken to be 120, the coefficient of D will be 48¾ / 120 = 195 / 480 = 13 / 32 = 1/(2+) 1/(2+) 1/6 = 2/5 very approximately. Latter half of verse 13 and first half of verse 14. An easy method to compute the parallax in longitude and latitude. Taking the Dṛk-ṣepa of the Moon as well as the Sun to be the Hsine of the meridian zenith-distance of the Vitribha and the H cosine of its meridian zenith-distance as the Vitribha-Sanku, the parallaxes in latitude and longitude could be got from them respectively. Comm. Parallax in longitude is computed from the Vitribha-Sanku, whereas parallax in latitude is computed from the Dṛk-kṣepa or the Hsine of the zenith-distance of the Vitribha. Thus for both the purpose the Vitribha's position is important, whose zenith-distance and altitude give respectively the parallax in latitude and longitude. Since in practice it is a little cumbrous to obtain the Vitribha's altitude and zenith-distance, an approximate procedure is suggested. Obtaining the declination or the Sphuṭa-krānti of the Moon taking him to coincide with the Vitribha by the method described in verse 3 of the Graha-cchāyādhikāra, and using the formula z+δ=ϕ, the meridian zenith-distance of the Vitribha can be got. This may be assumed to be the Dṛk-ṣepa approximately. The 55