[Chapter on Eclipses] Laghumanasam

Multiply by six squared, which is thirty-six. For Mars, multiply the sine of the base original: "bhujajya", the sine of the planet's angular distance from the node by twelve. For Mercury, multiply by sixteen; for Jupiter, by nine; for Venus, by sixteen; and for Saturn, also by sixteen. Thus, the sine of the base, expressed in degrees and multiplied by its respective multiplier, becomes the minutes of latitude term: "vikshepa-kalipta" — the celestial latitude measured in arc-minutes. For the Moon, these values are already considered corrected. However, for Mars and the others, one must multiply those minutes of latitude by their respective corrected diameters and divide by their own "shighra-cheda" term: "shighra-cheda" — a divisor related to the planet's distance from Earth. The result obtained will be the clear (corrected) minutes of latitude. This means they become "sphuta" (accurate). According to the rules of addition and subtraction for North and South: if the "padona-bhuja" a specific trigonometric component is positive, the latitude is South; if it is negative, the latitude is North. In this manner, one should calculate the latitude. || 6 || 7 ||

Now, to determine the occurrence or non-occurrence of an eclipse, he says: "The difference between two latitudes..." For the two celestial bodies whose eclipse is being examined, if their latitudes are in the same direction, take the difference between them. If they are in different directions, take the sum of the latitudes. That is the "vimbantara"—the distance in minutes between the centers of the two disks. When this distance is less than the "manardha-yoga" (the sum of the two semi-diameters), an intersection occurs, meaning an eclipse will take place. If the distance between the centers is greater than the sum of the semi-diameters, there will be no eclipse. In both solar and lunar eclipses, the Moon's latitude itself constitutes the distance between the centers, because the Sun and the Earth's shadow have no latitude. However, in a solar eclipse, the "corrected latitude" (adjusted for parallax) must be used. || 8 ||

Now, he describes the calculation of the time of parallax term: "lambana" — solar parallax in time, crucial for predicting the exact moment of a solar eclipse for the sake of correcting the moment of conjunction in a solar eclipse: "Subtract the Sun..." If the conjunction of the Sun and Moon occurs before midday, subtract the previously calculated hours of conjunction from the measure of half the day. If the conjunction occurs after midday, add the hours of conjunction to the measure of half the day. This gives the hours from sunrise to the end of the lunar day. This applies if the conjunction is during the day. If it is at night, subtract half the day from the hours of conjunction; the remainder will be the hours of the night passed or remaining. Having thus determined the time of the end of the lunar day, find the rising sign for that moment, subtract the corrected Sun from that rising sign, and multiply the remaining signs by five. Multiply the degrees by ten, divide by sixty, and add them to the place of the signs. [The hours in the place of the signs...

1. Variant reading: "...less than the Sun..."