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A planet is revolving round the sum. Its distance from the sun at Apogee is \( r_{A} \) and that at Perigee is \( r_{p} \). The mass of planet and sun is \( m \) and \( M \) respectively, \( v_{A} \) and \( v_{P} \) is the velocity of planet at Apogee and Perigee respectively and \( T \) is the time period of revolution of planet round the sun.
(a) \( T^{2}=\frac{\pi^{2}}{2 G m}\left(r_{A}+r_{P}\right)^{2} \)
(b) \( T^{2}=\frac{\pi^{2}}{2 G M}\left(r_{A}+r_{P}\right)^{3} \)
(c) \( v_{\mathrm{A}} \mathrm{r}_{\mathrm{A}}=\mathrm{v}_{\mathrm{P}} \mathrm{r}_{\mathrm{P}} \)
(d) \( v_{A}v_{P}, r_{A}r_{P} \)
(1) \( a, b, c \) (2) \( a, b, d \) (3) \( b, c, d \) (4) all
\( \mathrm{W} \)
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