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

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fying that r is in the western hemisphere and is brought
into view for clarity).
Fig. 96 Fig. 97
Verse 11 and first half of verse 12. Then the sum
of ZV and the latitude of V assuming V to be the Moon,
or the difference of the above two, as the case may be,
according as both of them are north or of opposite
directions, gives the arc whose Hsine is the Dṛk-kṣepa
of the Moon, The Dṛk-kṣepas of the Sun and the Moon
multiplied respectively by 1/15th of their daily motions and
divided by the radius R (equal to 3438′) are the parallaxes
of the Sun and the Moon in latitude. The sum or
difference of these parallaxes according as they are of
opposite or the same direction, is the true parallax in
latitude in the context of a solar eclipse.
Comm. The true parallax in latitude sought above is
the relative parallax of the Sun and the Moon in latitude.
Suppose in fig. 92, VB is the parallax in latitude pertain-
ing to the Sun and VB′ that pertaining to the Moon; then
BB′ is the relative parallax, the difference being taken in
this case because both are of the same direction.
Parallax in latitude namely CD in fig. 92, we saw
equal to VB which is equal to (4H / R) sin ZV, In other words