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

361
for, as mentioned before, the daily motions of the Moon
and the Sun are ready computed for every day. Also the
advantage in using this formula is that besides the fact
that we need to deal only with small quantities instead of
the big numbers of Yojanas, the true value for the day of
eclipse is got by using the true daily motions. Using the
mean daily motions, however, we have for the mean
diameter, ²/₁₅ m₁ — ⁵/₁₂ s₁ = ²/₁₅ × 790′–35″ — ⁵/₁₂ × 59′–8″
= 105 ⅔ — 24 ⅔ = 81 very approximately.
Note (3) In obtaining a convergent for (s − e)/Ks , since
the values of s and Ks are parameters s/Ks is got alright,
where e/Ks is more exaggerated as the value of the hori-
zontal solar parallax. By this term the result is increased
to an extent of 3′ out of which 1′ is mitigated by the fact
that we have to take the earth's atmosphere also into