To solve the problem of calculating the energy radiated per minute by a black body of surface area \ (200 \, \text {cm}^2\) maintained at \ (127^\circ C\), we will use Stefan-Boltzmann Law, which states that the power radiated by a black body is given by: \ [ P = \sigma A T^4 \] where: - \ (P\) is the power (energy per second) in watts (J/s The power radiated by a black body is given by the Stefan-Boltzmann law, which states that the power \ ( P \) radiated by a black body is proportional to the fourth power of its temperature \ ( T \) and its surface area \ ( A \). If the temperature of the black body is now changed so that it radiates maximum energy at wavelength 3/4λ0, the power radiated by it becomes nP . Thus, the radiated power per unit area as a function of wavelength is: Power per unit area is P = dE/2dtdA P = d E / 2 d t d A, where dA d A is the area of the small hole: The cylinder is the black body and the hemisphere is where the hole radiates to. , power radiated. Black-body, or thermal, radiation is continuous: it radiates at all wavelengths. In contrast, a white body is one with a "rough surface that reflects all incident rays completely and uniformly in all directions. The temperature of a black body is an ideal substance which can emit and absorb all frequencies of light. Similar questions Q. [1] The radiation was not predicted by previous models which assumed that once electromagnetic radiation is inside the event horizon, it cannot escape. For an ideal absorber/emitter or black body, the Stefan–Boltzmann law states that the total energy radiated per unit surface area per unit time (also known as the radiant exitance) is directly proportional to the fourth power of the black body's temperature, T: In Wien’s displacement law, it is the ratio of the temperature of a black body and the wavelength at which it emits the light.

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