Step 1: Apply Stefan–Boltzmann law.
For a blackbody,
\[
P = \sigma A T^4 = \sigma (4\pi R^2) T^4
\]
Given \(P_1 = P_2 = 1\, \text{kW}\),
\[
R_1^2 T_1^4 = R_2^2 T_2^4
\]
\[
\frac{R_1}{R_2} = \left(\frac{T_2}{T_1}\right)^{-2} = \left(\frac{2000}{1000}\right)^{-2} = \frac{1}{4}^2 = 0.0625
\]
Step 2: Conclusion.
Hence, the ratio of radii \(R_1 / R_2 = 0.0625\).

At a particular temperature T, Planck's energy density of black body radiation in terms of frequency is \(\rho_T(\nu) = 8 \times 10^{-18} \text{ J/m}^3 \text{ Hz}^{-1}\) at \(\nu = 3 \times 10^{14}\) Hz. Then Planck's energy density \(\rho_T(\lambda)\) at the corresponding wavelength (\(\lambda\)) has the value \rule{1cm}{0.15mm} \(\times 10^2 \text{ J/m}^4\). (in integer)
[Speed of light \(c = 3 \times 10^8\) m/s]
(Note: The unit for \(\rho_T(\nu)\) in the original problem was given as J/m³, which is dimensionally incorrect for a spectral density. The correct unit J/(m³·Hz) or J·s/m³ is used here for the solution.)