पृष्ठम्:लघुभास्करीयम्.djvu/१४१

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68 A rule relating to the determination of the magnitude and direction of the alka-ular0 : 15-16. Multiply the Rsine of the (local) latitude by the Rversed-sine of the 15us between the times of (the beginning , piddle, or end of) the eclipse and the middle of the might or day1, and divide by the radius (.८.,3438') : (the result is the Rsine of the nk50-20alu710). The direction of the result (i.e., nk90 ulamu) is (determined) in the following manner : (If the eclipsed body, at the time of the first or last contact is) in the eastern half of the celestial sphere, the directions of the aks0-0alamu for the eastern and western halves of the disc (of the eclipsed body) (.e., of the sharsa-and m20k90-0alam41 in the case of the Moon and nice uerऽa in the case of the Sum) are 10rth and south (respectively); (if the eclipsed body is) in the western half of the celestial sphere, (they are to be taken) reversely.* “The usus between the times of (the beginning, middle, or end of) the eclipse and the middle of the might or day are the ८sus of the hour angle* of the eclipsed body for that time. Thus the rule given in the text is egua valent to the following formula :

3438 3 We where H is the hour angle of the eclipsed body, and # the latitude of the local place. This formula, as pointed out by me in the Maha-Bhaskary0 is inaccu rate. For details see my motes on MBi, v. 42-44 . s Night when the eclipse is lunar and day when the eclipse is solar . Measured east or west of the local meridian