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मध्यज्यावर्गविश्लिष्टम् दृक्क्षेपः शेषतः पदम् । तत्त्रिज्यावर्गविश्लेषान् मूलम् शङ्कुः स दृग्गतिः॥
Subtract the square from the Madhajyá: the square-root of the remainder is ([1] nearly equal to) the drikshepa or the sine of the zenith-distance of the nonagesimal (or the sine of the latitude of the zenith). The square-root of the difference between the squares of the drikshepa and the radius is the Śanku or the sine of the altitude of the nonagesimal. This sine is called the drịggati. [1. For, the square-root of the remainder multiplied by the radius and divided by the cosine of the ecliptical part intercepted between the nonagesimal and the culminating point becomes the exact drịkshepa or the sine of the latitude of the Zenith. B. D.]
english translation
नताम्शबाहुकोटिज्ये +अस्फुटे दृक्क्षेपदृग्गती । एकज्यार्धगतश् छेदो लब्धम् दृग्गतिजीवया॥
(Or) the sine and cosine of the zenith-distance (of the culminating point of the Ecliptic,) are the rough drịkshepa and drịggati (respectively.) Dividing the square of the sine of one sign (or 30°) by the drịggati (above found,) the quantity obtained is called the chheda or the divisor.
english translation
मध्यलग्नार्कविश्लेषज्या छेदेन विभाजिता। रवीन्द्वोर् लम्बनम् ज्ञेयम् प्राक्पश्चाद् घटिकादिकम्॥
The sine of the difference between the place of the Sun and the nonagesimal divided by the chheda gives the Moon's parallax in longitude from the Sun reduced to (sávana) Ghaṭikás, whether the Sun be east or west (of the nonagesimal.[2]) [2. All Hindu astronomers suppose that every planet daily traverses 12000 yojanas nearly in its orbit and as the part of a planet's orbit intercepted between the sensible and rational horizon is equal to the earth's semi-diameter (or 800 yojanas which = 1 / 15 th of 12000) therefore, the extreme or horizontal parallax of a planet is thought to be equal to 1 / 15 part of its diurnal motion: thus the Moon's horizontal parallax is 52′ 42″ nearly and the Sun's 3′ 56″ and hence the horizontal parallax of the Moon from the Sun is = (52′ 42″) − (3′ 56″) = 48′ 46″. And four Ghaṭikás in which the Moon describes 48′ 46″ from the Sun is the horizontal parallax in time. Now, let l {\displaystyle l} = the latitude of a planet (the Sun or Moon), d {\displaystyle d} = the difference between the places of the planet and the nonagesimal, a {\displaystyle a} = the altitude of the nonagesimal, p {\displaystyle p} = the horizontal parallax, x {\displaystyle x} = the parallax in longitude, y {\displaystyle y} = the parallax in latitude. Then we have the equation, x = p sin a . sin ( d + x ) R . cos l ± y {\displaystyle x=p{\frac {\sin {a.}\sin {(d+x)}}{R.\cos {l\pm y}}}} which is common in astronomy.]
english translation
मध्यलग्नाधिके भानौ तिथ्यन्तात् प्रविशोधयेत् । धनम् ऊने +असकृत् कर्म यावत् सर्वम् स्थिरीभवेत्॥
Subtract the parallax in time (just found) from the end of the true time of conjunction if the place of the Sun be beyond that of the nonagesimal; but if it be within, add the parallax. At this applied time of conjunction find again the parallax in time and with it apply the end of the true time of conjunction and repeat the same process of calculation until you have the same parallax and the applied time of conjunction in every repetition. (The parallax lastly found is the exact parallax in time and the time of the conjunction is the middle of the solar eclipse.)
english translation
दृक्क्षेपः शीततिग्माम्श्वोर् मध्यभुक्त्यन्तराहतः। तिथिघ्नत्रिज्यया भक्तो लब्धम् सावनतिर् भवेत् ॥
Multiply the drịkshepa (or the sine of the zenith-distance of the nonagesimal) by the mean diurnal motion of the Moon from the Sun, and divide the product by fifteen times the radius: the quotient is the parallax in latitude of the Moon from the Bun.
english translation