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Abstract

The true position of the Earth’s shadow is said to be the sum of the true position of the Sun and a half-circle (180 degrees). Having determined the position of the Moon and the [Earth’s] shadow either at sunrise or at sunset, whichever is closer [to the conjunction], the time of their conjunction may be determined. If [the longitude of] the Moon is greater then the conjunction is over, and if it is less then it is yet to occur. Their difference [in longitude] multiplied by 60 and divided by their difference in daily motion [gives] the time for conjunction (the yogakāla) expressed in ghatīs etc. that has already elapsed or is yet to elapse respectively.

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Correspondence to K. Ramasubramanian .

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Ramasubramanian, K., Sriram, M. (2011). Lunar eclipse. In: Tantrasaṅgraha of Nīlakaṇṭha Somayājī. Sources and Studies in the History of Mathematics and Physical Sciences. Springer, London. https://doi.org/10.1007/978-0-85729-036-6_4

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