( 28 ) 7° 2 It will be seen from the above that Chandrasekhara has practically assumed the sidereal periods of the sun and the moon, as given in the Sírya-Siddhants, but has materially advanced upon it as regards the periods of the other planets. Having re- gard to the comparatively slow motion of Jupiter and of Saturn, and the nature of the instruments used, it would have been a surprise if closer approximation to their true periods were made. Let us now compare the mean inclinations of the orbita of the planets to the ecliptic. Eng. Ast. Súrya-3. Siromani. Darpara Mercury* 7o O 8" 5° 25' Venus* 3 23 35 2 46 3 6 3 23 Mars 1 51 2 Jupiter 1 18 41 Saturn 2 29. 40 Moon 5 8 48 4 304 305 9. Obliquity of 28 27 24 0 24 0 28 30 the Ecliptic) On account of the difference in the planetary theories and in the method of calculation between modern astronomy and our Siddhántas, the eccentricities of the planetary orbits cannot be compared with advantage. But as they make no difference in the case of the sun and the moon, their greatest equations aro. given here for comparison, . The inclination given in the Siddhántas is redoved to the geocentrio system. The general reador may be reminded that the inclinations are alli subject to variation and that the old Siddhanta values were not so far wide of the truth, as they appear from the table. Digitized by Google
