14 Surya-Siddhija 2. These diameters, each multiplied by the true motion, and divided by the mean motion, of its own planet, give the corrected (sphuta) diameters. If that of the sun be multiplied by the number of the Sun's revolutions in an Age, and divided by that of the On'g • 8. 0; if it be multiplied by the moon's orbit (ackshi, and divided by the Sun's orbit, the result will be its diameter upon the moon's orbit : all these, divided by fifteen, give the measures of the diameters in minutes The absolute value of 1.hs diameters of the sun and noon being stated in yojanas, it is required to find their apparent values, in minuteR of age. In order to this, they are projected upon the moon's orbit, or upon a circle escribed about Bhe earth at the moon's mean distance, of which circle-sine९ 824,000+ 21,8(0= 15—one minute is equivalent to fifteen yojanas. £he method of the process will be made clear by the nexed figure (Fig. 18). Let E be the earth's place, EM OF En the mern tistance of Fig. 18.
the moon, and Es the mean listnnce of the sun, Let U equal the sun's diameter, 8500s. But now let the sun be at the greater distance ES': the part of bia man orbib which his disk will cost will no longer be ऽ'], but a less quantity, fu, and r will be to 'U, or 'J', as ES to ES. But the text is not willing to acknowledge here , any more than in the second chapter, an actual inequality in the distance of the sun from the earth at different time, even bhough that inequality be most unequiv००७lly implied in the processes it prescribes : so, instead of calculating ES" as well as ES , which the method of epieyclex affords fall facilities for doing, it substitutes, for the ratio of Es to ES, the inverse ratio of the daily motion at १be mean distance IE8 to that at the true distance E3. The ratios, however, are not precisely equal. The are an (Fig. A, P. 76of the eccentric circle is supposed to be traversed by the Sun or goo with a aniform velocity. Tft, then, the motion at any given point, as . were