[ 32 ] first of the second quadrature, Call the moon thus corrected, the third moon, Mg. Now, take To of the sun's equation and multiply 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 Bhujántara), common to all the planets, are to be applied before the moon's place becomes apparent.* On a cursory view, the amount of Tungántara inequality appears double of that of evection. But if we take the moon's greatest equation of centre into account, the apparent discre pancy 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 equa- tion, and 2° 40' as the greatest Tungántara, 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 Indian astrono mers 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 oftener re-iterated in season and out of season than substantiated, that the Indian Astrono mers borrowed largely from Greek astronomy. As far as I am Aware, this assertion is based upon (1) the identity of certain ,
- It should be noted here that the last-named inequality (Digausa) is
also applied to the moon's node in the above-mentioned meanor (VIII, 33). Digitized by Google
