Step 1: For the isothermal expansion (A → B).
\[ W_1 = nRT \ln{\frac{V_2}{V_1}} = RT \ln{4} \] \[ Q_1 = W_1 = RT \ln{4} \]
Step 2: For the isochoric heating (B → C).
Since volume is constant, \(Q_2 = nC_V (T_2 - T_1)\). For an ideal gas: \[ \frac{P_2}{T_2} = \frac{P_1}{T_1} \] At the end of isothermal expansion, \(P_B = \frac{P}{4}\). After heating at constant volume, final pressure \(P_C = P\). \[ \Rightarrow \frac{T_2}{T_1} = \frac{P_C}{P_B} = \frac{P}{P/4} = 4 \] For a monatomic gas, \(C_V = \frac{3R}{2}\). \[ Q_2 = nC_V (T_2 - T_1) = \frac{3R}{2} (4T - T) = \frac{9RT}{2} \]
Step 3: Total heat transfer.
\[ Q_{\text{total}} = Q_1 + Q_2 = RT \ln{4} + \frac{9RT}{2} \] \[ \frac{Q_{\text{total}}}{RT} = \ln{4} + 4.5 = 1.386 + 4.5 = 5.886 \]
Step 4: Conclusion.
Hence, the total heat transfer in the process in units of \(RT\) is \(5.89\).

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.)