121 Neglecting the motion of the Sun's apogee and assuming that the Rsines vary uniformly, we have Rsin' Rsin Therefore, TRUE DAILY MOTION OF THE MOON S' Sm F (current Rsine-difference) xm 225 approx. (current Rsine-difference) > mxr₁ 225× 80 approx. Hence the above rule. Since the Sun's true daily motion has been obtained here with the help of the Rsines (jivā), therefore it is generally called jivābhukti.. A rule for finding the true daily motion (called jivabhukti) of the Moon: 15-17. (When the Moon is in the odd quadrant) subtract the part of the bahu due to her mean anomaly lying in the elementary are corresponding to the current Rsine-difference (antyajivādhanus- khanda) from the daily motion of the (Moon's) mean anomaly; (when the Moon is) in the even quadrant, subtract the remain- der obtained by subtracting that (part) from 225. Then take (as many) Rsine-differences in the reverse order, (if the Moon is) in the odd quadrant, or in the serial order, if the Moon is in the even quadrant, as correspond to (the above residue of) the motion of the (Moon's) mean anomaly (literally, the mean daily motion of the moon diminished by that of its apogee). (To the sum of those Rsine-differences) add the Rsine- differences (phala) corresponding to the arcs (of the daily motion of the Moon's mean anomaly which lie) in the first and last elementary arcs which are to be determined by proportion with the Rsine-differences (corresponding to those elementary arcs). Then calculate the (Moon's) equation of the centre (phala) co- rresponding to that (i.e., multiply that by the Moon's tabulated epicycle and divide by 80). The (Moon's) mean daily motion, when diminished or increased by that equation (according as the ¹ The assumption that the Rsines vary uniformly is false.
