The time period of a satellite is given by Kepler's Third Law: \[ T \propto \sqrt{r^3} \] where \( T \) is the time period and \( r \) is the distance from the center of the Earth. For two satellites, we can write the ratio of their time periods as: \[ \frac{T_1}{T_2} = \left( \frac{r_1}{r_2} \right)^{3/2} \] Let \( r_1 = 2.5R \) and \( r_2 = 7.5R \). Substituting these values into the equation: \[ \frac{T_1}{T_2} = \left( \frac{2.5R}{7.5R} \right)^{3/2} = \left( \frac{1}{3} \right)^{3/2} = \frac{1}{9} \]
Thus, the ratio of the time periods is \( \frac{1}{9} \).