पञ्चसिद्धान्तिका (आचार्य वराहमिहिर - सूर्य, रोमक, पौलिश, वासिष्ठ एवं पितामह सिद्धान्त)

196 PAÑCASIDDHĀNTIKĀ maximum equation of the centre, given as 143', also is an indicator, agreeing as it does with Ptolemy's. Though the Moon's maximum equation of the centre given is 296', and Ptolemy's is 301', and thus there appears to be a difference, we are not sure that the given quantity is 296', on account of the extremely corrupt nature of the text in the concerned part. There are also lacunae in the computations intended by the author, which are to be supplied from the siddhāntas dealt with already or known otherwise. The method of computing the true Sun and Moon given here is an improvement on the Pauliśa. Only the solar eclipse is dealt with here. The lunar eclipse is omitted probably because it is not different from that of either the Pauliśa and Vāsiṣṭha given, or the Saura to be given. In contrast with the primitive method of the Pauliśa, the Romaka method of computation of the solar eclipse is far advanced, and almost the same as that of the later siddhāntas like the Āryabhaṭīya or the Saura. For instance, the parallax in latitude is correctly sought to be computed by using sine ZDN, though the ZDN itself is approximate, being got by combining the latitude of the place and the declination of the nonagesimal. Only the method given for correcting the declination for the nonagesimal to compensate for the Moon being situated on its own orbit instead of the ecliptic, is wrong, as commonly seen in works of authors prior to Bhāskarācārya II. Making the parallax in latitude and the Moon's true angular diameter depend on the Moon's true motion, and the Sun's true angular diameter on the Sun's true motion, is in accordance with the later siddhāntas, though giving the respective mean diameters as 34' and 30' is very rough. The first contact, middle, and last contact, as also the directions of the points of contact, are intended to be taken from the Vāsiṣṭha-Pauliśa, not being given here. The omission of the total or annular phases does not matter, since they cannot be got correctly by the rough methods given. Further, let us not mind the omission of the successive approximation to be done in the computation of the circumstances, though necessary as shown. (This may be because it is not found in the original or easily understood to be necessary). But it will certainly be better to use in the computation the parallax-corrected latitude of the new moon corrected for parallax, instead of that of the uncorrected new moon as given by the text, the former being generally nearer the time of the thing computed. We do not know why the author has not said so. Inspite of all this, the Romaka is interesting as being comparatively more ancient, and forming a link between the earlier and the later Siddhāntas. [इति पञ्चसिद्धान्तिकायां वराहमिहिरविरचितायां रोमकसिद्धान्तेऽर्कग्रहणमष्टमोऽध्यायः ||]¹

1. Col. A. रोमकसिद्धान्तेऽर्कग्रहणमष्टमष्टमोध्यायः; B.C.D. इति रोमकसिद्धान्तेऽर्कग्रहणमष्टमोऽध्यायः Thus ends Chapter Eight entitled ‘Romaka-Siddhānta: Solar Eclipse’ in the Pañcasiddhāntikā composed by Varāhamihira