Two gravitaionally bound stars with equal masses m, separated by a distance d, revolve about their cneter of mass in circular orbites. Show that the period is proportional to d^3/2 and find the proportionality constant.(adsbygoogle = window.adsbygoogle || []).push({});

I know that in this case, F = mv^2/r and that F=Gm^2/d^2.

But where do I go from here??

Thanks for any help!

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# Deriving Kepler's Third Law

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