K is for ... Kepler's 3rd Law

T 2 = R 3

The above equation was formulated in 1619 by the German mathematician and astronomer Johannes Kepler (1571-1630). It expresses the mathematical relationship of all celestial orbits. Basically, it states that the square of the time of one orbital period (T2) is equal to the cube of its average orbital radius (R3).

So an orbital duration of 365.25 days gives a distance of 9.2956e+7 miles from the sun.

And there you have it.