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

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The apparent latitude of the Moon is equal to the
algebraic sum of his geocentric latitude and the parallax
in latitude. From this apparent latitude are to be calcu-
lated the Sthiti-khanda and Marda-khanda of the solar
eclipse (by the method described in the chapter on lunar
eclipse, taking the eclipsing body or grāhaka to be the
Moon and the eclipsed or Grāhya to be the Sun).
Comm. The geocentric parallax of the Moon has a
double effect on the occurence of a solar eclipse as men-
tioned before. If the parallax be resolved along the
Ecliptic and along a secondary to the Ecliptic, we have
respectively the parallax in longitude and that in latitude.
The parallax in longitude makes the apparent moment of
conjunction at a given place, differ from the moment of
the geocentric conjunction, whereas the parallax in latitude
makes the magnitude of apparent latitude of the Moon at
the place of observation differ from that of the geocentric.
The apparent latitude is equal to the sum or difference
of the geocentric latitude and the parallax in latitude.
Having got the apparent latitude, the computation of the
Sthiti and Marda-khandas could be done according to the
method described in the chapter on lunar eclipse.
For a point C on the surface of the Earth, a solar
eclipse occurs if the latitude of the Moon be less than MD
Fig. 100