A double star in a system of two stars of masses m and 2m, rotating about their centre of mass only under their mutual gravitational attraction. If r is the separation between these two stars then their time period of rotation about their centre of mass will be proportional to-
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(a, d)
r 2 = 
= 
= 
= 
T 2 ∝ r 3/2 , T 2 ∝ m –1/2
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