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