[Chapter on Miscellaneous Topics] Laghumanasa

The corrected divisororiginal: "śīghraccheda" - a mathematical value used in calculating planetary positions is obtained by adjusting the total radiusoriginal: "tri-jyā". This is what is meant: For the five planets starting with Mars, one should separately place the slow-correctedoriginal: "manda-sphuṭa" - the position after the first equation of center position, subtract it from its own fast-apexoriginal: "śīghrocca" - the point of highest velocity, similar to an epicycle's center, and calculate the sineoriginal: "bhujajyā" and cosineoriginal: "koṭijyā" as before. Having placed these together, take the sine again, divide it by three, and always add the result to the previously calculated mean diameter; this becomes the true diameter. Again, taking that true diameter separately, one should adjust it by the entire fast-cosine. If the cosine is negative, subtract it; if positive, add it. That becomes the true fast-divisor.

Next, convert the fast-sine into minutes of arc, divide by the fast-divisor, and take the resulting degrees. Divide the remainder by sixty and then by that same divisor to get the minutes. Keeping the divisor safe, place those fast-degrees together and apply them as a correction (addition or subtraction) to the slow-corrected planet. If the sine is negative, subtract; if positive, add. That results in the true planetThe final longitude of the planet. This is how the true positions of Mars, Mercury, Jupiter, Venus, and Saturn should be calculated.

Now, he describes the assumption of the "fast-apexes" for Mars and the others: "The stars..." etc. The "star-planets" are the five planets starting with Mars. Among them, for whichever planet is desired, the faster of the two—the planet's own mean motion or the Sun's mean motion—is its fast-apex, and the other is the mean position. Thus, for Mars, Jupiter, and Saturn, the Sun's mean motion is the fast-apex, and their own mean motion is the "mean." For Mercury and Venus, their own mean motion is the fast-apex, and the Sun's mean motion is the "mean." This is the established rule. For Mercury and Venus, having assigned the Sun's mean motion as their own mean motion, one should calculate the slow-corrected and fast-corrected positions. || 6 ||

Subtract the fast-correction divided by twelve from the diameter.
Multiply the remainder by the difference in motions, divide by the divisor,
and subtract from the fast-velocity to get the [planet's] true velocity. || 7 ||

Now he describes the calculation of the true velocity for Mars and the others: "The diameter..." etc. Divide the planet's fast-sine-correction by twelve. Subtract the result from the true diameter. Multiply the remainder by the difference between the planet's slow-corrected velocity and the fast-apex velocity. Divide this by the fast-divisor. Subtract the result from the fast-apex velocity. The remainder is the true velocity of the planet. If the correction to be subtracted is greater than the velocity, then subtract the fast-velocity from that correction; the remainder is the planet's retrograde velocityoriginal: "vakra-bhukti" - when a planet appears to move backward in the sky. || 7 ||

Now begins the Chapter on Miscellaneous Topics.

The moon's velocity-degrees multiplied by the cosine of the moon's anomaly
and divided by eleven, are the multipliers for the sine and cosine
of the distance between the Sun and Moon divided by five, respectively. || 1 ||