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

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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
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