Step 1: Entropy change of the body.
The body is heated from temperature \(T\) to \(2T\) at constant pressure. \[ \Delta S_{\text{body}} = C_p \ln{\frac{2T}{T}} = C_p \ln{2} \]
Step 2: Entropy change of the reservoir.
The heat lost by the reservoir is equal to the heat gained by the body. \[ Q = C_p (2T - T) = C_p T \] The reservoir temperature remains constant at \(2T\), so its entropy change is: \[ \Delta S_{\text{res}} = -\frac{Q}{T_{\text{res}}} = -\frac{C_p T}{2T} = -\frac{C_p}{2} \]
Step 3: Total entropy change.
\[ \Delta S_{\text{total}} = \Delta S_{\text{body}} + \Delta S_{\text{res}} \] \[ \Rightarrow \frac{\Delta S_{\text{total}}}{C_p} = \ln{2} - \frac{1}{2} = 0.693 - 0.5 = 0.193 \]
Step 4: Conclusion.
Hence, the total change in entropy of the system and reservoir in units of \(C_p\) is \(0.19\).

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.)