Step 1: Understanding the Problem:
The question asks for the fundamental physical law of radiation heat transfer that relates the total emissive power of a blackbody to its absolute temperature raised to the fourth power.
Step 2: Key Formula or Approach:
The Stefan-Boltzmann law describes the total thermal energy radiated by a blackbody per unit surface area per unit time.
The mathematical relationship is given as:
\[ E = \sigma T^4 \]
where $E$ represents the total emissive power ($\text{W/m}^2$), $T$ represents the absolute temperature ($\text{K}$), and $\sigma$ represents the Stefan-Boltzmann constant ($\sigma \approx 5.67 \times 10^{-8} \text{ W/m}^2\text{K}^4$).
Step 3: Detailed Explanation:
• Stefan-Boltzmann Law: Explains that the total radiative energy emitted by a blackbody is proportional to the fourth power of its absolute temperature ($T^4$).
• Newton's Law of Cooling: Governs convective heat transfer, stating that the rate of heat loss from a body is proportional to the temperature difference between the body and its environment ($\Delta T$).
• Fick's Second Law: Governs non-steady-state mass diffusion, predicting how concentration fields change over time.
• Planck's Law: Describes the spectral distribution of electromagnetic radiation emitted by a blackbody in thermal equilibrium, rather than the integrated total emissive power.
Step 4: Final Answer:
Therefore, the Stefan-Boltzmann Law is the correct law relating emissive power to the fourth power of temperature.