The time taken by a body to revolve around another body is related to its distance from the body around which it is revolving by Kepler's third law of planetary motion.

Assuming a constant distance between the two bodies, the square of the period of orbit is directly proportional to the cube of the distance between them. Or if we represent the period of orbit as t and the distance between them as d, we have t^2 = k* d^3

=> t = k*d^(3/2)

Once we know the value of k, we can easily calculate the time period of revolution for any distance between the two bodies.

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