सिद्धान्तदर्पण (महामहोपाध्याय सामन्त चन्द्रशेखर सिंह - नग्न-नेत्र खगोल वेध एवं गणित महाकोश)

Introduction xxxv
Now, take 1/10 of the Sun's equation and
mutiply by the first Moon's motion, dividing by its
mean motion. Add the result to the 3rd Moon, when
the Sun's equation is subtractive, and subtract from
it when the Sun's equation is additive. After this,
the other corrections (such as Bhujantara), common
to all the planets, are to be applied before the
Moon's place becomes apparent.¹
On a cursory view, the amount of Tungantara
inequality appears double of that of evection. But
if we take the Moon's greatest equation of centre
into account, the apparent discrepancy vanishes.
For, the amount of the greatest equation of the
Moon is 6° 18′, and the maximum evection 1° 20′
making the total of 7° 38′. Chandrasekhara has 5° 1′
as the greatest equation and 2° 40′ as the greatest
Tungantara, making the total of 7° 41′. The other
inequalities discovered by Chandrasekhara are
about the same as those in use in English
astronomy.
The astronomical constants adopted by our
India astronomers open up a large field for enquiry.
It is not my purpose to discuss their bearings upon
the antiquity of Indian astronomy. But I cannot but
remark that it is often reiterated in season and out
of season than substantiated, that the Indian
astronomers borrowed largely from Greek
astronomy. As far as I am aware, this assertion is
based upon (1) the identity of certain Sanskrit and
Greek astronomical terms, (2) the fact of Garga
praising the Yavanas for their proficiency in

1. It should be noted here that the last-named inequality
   (Digamsa) is also applied to the Moon's node in the
   above-mentioned manner (S.D. VIII, 33).