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A planet of mass \( \mathrm{m} \) is moving in an elliptical orbit about the sun (mass of sun \( =\mathrm{M} \) ). The maximum and minimum distances of the planet from the sun are \( r_{1} \) and \( r_{2} \) respectively. The period of revolution of the planet will be proportional to :
(1) \( r_{1}^{3 / 2} \)
(2) \( \mathrm{r}_{2}^{3 / 2} \)
(3) \( \left(r_{1}-r_{2}\right)^{3 / 2} \)
(4) \( \left(r_{1}+r_{2}\right)^{3 / 2} \)
\( \mathrm{P} \)
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