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

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sidereal measure of the same time we have to take A and
not A'.
Verse 12. Sāvana measure alone is to be employed while
finding the gnomonic shadow ie. while the zenith-distance
of the planet is to be computed, because the arc of the
diurnal circle of the planet indicates only Sāvana measure.
Suppose the Udayalagna falls short of the current lagna,
then the Bhōgyakāla ie. the remaining rising time of the
Rāśi in which the planet is situated added to the elapsed
time of the Rāśi of the current lagna together with the
sum of the rising times of the Rāśis in between gives the
difference of the Udayalagna of the planet and the current
lagna.
Comm. (Ref. fig. 111). Let p be the planet's place
on the Ecliptic at the moment in question when the lagna
is L (or the foot of the latitude of the planet
in case it is not on the ecliptic). Let PA be
the remainder of the Rāśi in which the
planet is situated. Then the time of rising
of the arc PA is here termed Bhōgyakāla.
Let DL be the arc of the Rāśi in which the
current lagna L is situated, which has arisen.
The time of rising of this arc DL is called
Bhuktakāla. The times of risings of the
Rāśis in between namely AB, BC, CD are
called Madhyōdayās. The sum of the rising times of
PA, AB, BC, CD, DL gives the time in between the rise
of P and that of L which is the time that has elapsed after
the planet has arisen upto the current Lagna ie. the rising
time of L.
Verse 13. The method of computing the gnomonic
shadow of the planet or what is the same the zenith-
distance of the planet, as per the method of computing
that of the Sun (extended to the case of the planet) after