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

398 Vikṣepa or the celestial latitude of the Moon M₂ R₂ is to be drawn along this Valanasūtra M₂ V. With R₂ as centre and radius p drawn the Rāhu-Bimba. Fig. 89 Depiction of Fig. 88, keeping the Moon fixed The slight flaw in this figure is that ML₁ L₃ implied as the path of the Moon is taken to be parallel to the ecliptic R₁ R₂ R₃ the path of the eclipsing body the Grāhakamārga, in as much as latitudes are drawn perpendi- cular to ML₁ L₃. This figure depicts a total eclipse of the Moon. If M coincides with R₂ at the middle moment of the eclipse, then the eclipse is called central. The duration of a central eclipse will be on the average the time that the Moon's disc takes to cross the diameter of the Rāhu-Bimba with its relative velocity. Hence the mean duration of a central eclipse is Average diameter of Rāhu + Average diameter of the Moon ────────────────────────────────────────────────────────── Relative velocity of the Moon with respect to the shadow = [(81+64) × 24] / [790′-35″ — 59′-8″] hrs = 145/732 × 24 = 290/61 = 4 hrs–45 minutes approximately.