The radiated power \( P \) of a body is governed by the Stefan-Boltzmann law, which states that:
\[
P = \sigma A T^4,
\]
where \( P \) is the power radiated, \( A \) is the surface area, \( T \) is the absolute temperature, and \( \sigma \) is the Stefan-Boltzmann constant.
For spherical bodies, the surface area \( A \) is proportional to \( R^2 \), where \( R \) is the radius. Therefore, the ratio of radiated powers \( P_1 : P_2 \) is:
\[
\frac{P_1}{P_2} = \frac{R_1^2 T_1^4}{R_2^2 T_2^4}.
\]
Thus, the ratio of the radiated powers depends on both the radii and the temperatures of the bodies.