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

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and then the elongation has to increase as the Uccha
gained over the Sun, the initial conjunction was the
modern Superior conjunction. The other position of the
Uccha when again the elongation i'e. the equation is Zero
must be therefore the Inferior conjunction. Also at the
motion of Superior conjunction, the planet must be having
the maximum daily motion, as it is clear from a heliocen-
tric figure that at that point the relative motion of the
planet with respect to a geocentric observer is the sum of
the velocities of the planet and the earth. Hence this
Uccha is spoken of as the Śīghroccha also because the
Uccha being a geocentrically moving point having helio-
centric angular motion, its velocity is always greater than
that of its planet namely the Sun. The word Uccha is
applied because at the Superior conjunction the planet is
farthest or highest from the earth. The excess of the
longitude of this Uccha over the longitude of the planet ie.
the Sun is known as the Śīghrakendra or anomaly as it is
said in the verse under commentary ‘चलोच्चं ग्रहोनं भवेत्
शीघ्रकेन्द्रम्’. Thus in the case of Mercury and Venus, the
Śīghraphala came to be discovered first. This being dis-
covered, formulated as will be shortly shown, and applied
to the mean Sun as the planet, still it was found that there
was a difference between the computed position and the
observed position. Such differences were tabulated. By
analogy from the case of the Sun and the Moon, it was
thought that there should be also a Mandoccha here also,
so that the point indicated by the position of the mean
planet after being corrected by the equation where the
above tabulated difference was zero, was identified as the
Mandoccha. From the H Sine of the maximum difference
taken as the radius of the Manda epicycle, its circumference
was then computed.
In the case of the superior planets, we have already
said that the geocentric sidereal periods accord with their
heliocentric ones. Calculating the mean position of the
planet and finding its difference from the observed true