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A system of binary stars of masses \( m_{A} \) and \( m_{B} \) are moving in circular orbits of radii \( r_{A} \) and \( r_{B} \) respectively. If \( T_{A} \) and \( T_{B} \) are the times periods of masses \( m_{A} \) and \( m_{B} \) respectively then,
[IIT-JEE 2006]
(a) \( \frac{T_{A}}{T_{B}}=\left(\frac{r_{A}}{r_{B}}\right)^{3 / 2} \)
(b) \( T_{A}T_{B} \) (if \( r_{A}r_{B} \) )
(c) \( T_{A}T_{B} \) (if \( \left.m_{A}m_{B}\right) \)
(d) \( T_{A}=T_{B} \)
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