(b) From Kepler’s third law of planetary motion
$\ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ T^{2} \propto R^{3}$
$Given,\ \ \ \ {\ R}_{1} = R,\ \ R_{2} = 5R$
$\therefore\ \ \ \ \ \ \ \ \ \ \ \frac{T_{1}^{2}}{T_{2}^{2}} = \frac{R^{3}}{(5R)^{3}}$
$\Longrightarrow \ \ \ \ \ \ \ \ \frac{T_{1}}{T_{2}} = \frac{1}{(5)^{3/2}}\ \ $
$\ \ \ \ \ \ \ \ \ \ \ \ \ \ \ T_{2} = 5^{3/2}T_{1}$
$\therefore\ \ \ \ \ \ \ \ \ \ \ T_{2} = 5^{\frac{3}{2}}T\ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \left\lbrack \therefore T_{1} = T \right\rbrack$