of Planetarg Corejunctions 191 also circles through the two planets, meeting the ecliptic in x and y * than, in order to find Mawe ascertain the values of 88 and M४; and, in like manner, to ind Mowe absertain the values of ou' and Mr. Now at he Fig . equator, of in a right sphere, the cireles NS and Ps would coincide, and the distance as disappeat: hen, the rpount of 88" b¢jing dependent upon the latitude (desc) at the observer . NPthe process by which it is calculated is called the “f Opera.
- ion for }ntitude ' (84age-
auna, Or else aasaa drea', ba). Again, it P and Py were the same point, or in the eclip tie and equator coincided, PS and Ps would coincide, and E M3would disppear : hence the process of calculation of Ms is called the operation for ecliptic-roviption (nynod¢l« c te:(ty, or Oria aga72 dalkalerman). •O. The latter of the two processes, although stated after the other in the text, is the one first ex plained by the commentary we wil also, as in the eace of th defeclion (note to iv, 24-25), give to it our first attention The point 8, to which the planet is referred by a cicle passing through the pole P, is skyled by the commentary uygya¢grchd, "f the planet's longi kude a5 8orrected for ecliptic-deviation,” and the distance Mg, which it is desired to ascertain is called cyaajkfbs 6be correction, in minutes for ecliptic-te viation. Instead, however, of finding M8, the process taught in the text finds Mtthe corresponding distance on the circle of dnily revolution, DF, of the point M—which is then sourned equal to M.A. The proportion upon which the rule, aB stated in verse 10is ultimate }y founded, is --Venkateswaran raman (सम्भाषणम्) ०६:५८, ३ दिसम्बर २०१८ (UTC)}, --...- R : sin MSt : : MS ; Mt the triangle MSt, which is always very small, being treated as if it were a plane triangle, right-angled at t. But now also, as the latitude Ms is always a small quantity, the angle PSPy may be treated as if equal to PMP(not drawn in bhe figure) ; and this angle is, as was shown in con: