The Universal System of Astronomy, Part Two

Siddhānta-tattva-viveka A famous 17th-century astronomical treatise by Kamalākara

From the given position, the surface of the base of the observation site should be known. Then, by the Rule of Three traiśāśika; a mathematical proportion where the fourth term is found from three known values, the result is obtained in one place. According to the method stated here:

The sine jyā original: sijyā/jyā, by the power of the calculation and divided by the result, becomes the cosine koṭi. That very sine is the result of the multiplication... divided by the sine, it proceeds as the form of the sine of the colatitude lamba-jyā; the sine of the angle of the celestial equator above the horizon. It is calculated by the difference of the radius trijyā, and the product of the cosine koṭi and the sine, divided by the radius, is subtracted from the result.

In this case, the sine is greater than the position... and the errors of the past are avoided. Here, the declination krānti; the angular distance of a celestial body north or south of the celestial equator is measured as described.

The sine of the maximum declination parama-krānti-jyā is 92193 original: paramakrāntijyā ९२१९३. Its square varga is 948150. Divided by the square of the radius trijyā, 15919, the square root mūla is 2712.25. From this, the earth-sine kubhjyā; a specific sine value used in calculating the sun's rising and setting is 935.

In this context, for the sake of the greater half, if more than a sixth is added, an eclipse grahaṇa may occur... The sine is established first... the maximum result... the measurement in fingers aṅgula; a traditional unit of measurement is 4.