सिद्धान्तशिरोमणि: गणिताध्याय (भास्कराचार्य - ग्रहगणित, मध्यमाधिकार व स्पष्टाधिकार सटीक)

centric conjunction and which does not show an apparent conjunction when there is a geocentric conjunction. In other words parallax in latitude plays a very important part in solar eclipses. Also ☉ D being the parallax in longitude, the moment of apparent conjunction might be preceded or followed by a geocentric conjunction according as the Sun lies along VA or AV. Thus having determined the exact moment of apparent conjunction using the magnitude of ☉ D, then we have to rectify the latitude using the magnitude of VB. If that rectified latitude of β falls short of R+r where R is the angular radius of the Sun and r that of the Moon, then there will be a solar eclipse. It will be noted that when the Sun coincides with V at the moment of conjunction, there is no parallax in longitude ☉ D being zero (Fig. 92) in that position. Also there will be no parallax in latitude when the Ecliptic assumes the position of a vertical circle passing through the zenith, the Drik-lambana then being entirely along the Ecliptic. In this case the Vitribhalagna V will coincide with Z and (4 H sin V ☉) / R which is termed the Madhyamalambana is now entirely along the Ecliptic and as such it is the Sphutalambana in this case. We have said above that when V coincides with Z, the Madhyamalambana is zero at Z, and that the maximum is equal to 4 nādīs on the horizon. In between Z and the horizon it has the formula (4 H sin V ☉) / R . Noting further that in this case when the H cosine of the zenith-distance of V ie. the Śanku of V is R, the entire lambana is along the Ecliptic, the nāti being zero, and the Madhyamalambana is itself the Sphuta- lambana, and again when V does not coincide with Z, H cos ZV is no longer R but has assumed Kōti-Rūpa ie. the form of a H cosine, as well as the Sphuta-lambana also, which assumes Kōti-Rūpa ie. of the form ☉ D of Fig. 92, where ☉ C is the Madhyamalambana, ☉ D is the