The total energy being radiated (the area under the curve) increases rapidly as the temperature increases (Stefan–Boltzmann Law).The intensity (or flux) at all wavelengths increases as the temperature of the blackbody increases.As the temperature of the blackbody increases, the peak wavelength decreases (Wien’s Law).The spectral profile (or curve) at a specific temperature corresponds to a specific peak wavelength, and vice versa.The blackbody radiation curves have quite a complex shape (described by Planck’s Law).Stefan–Boltzmann Law, which relates the total energy emitted (E) to the absolute temperature (T). Conversely, as the temperature of the body increases, the wavelength at the emission peak decreases.ģ. Wien’s Displacement Law, which states that the frequency of the peak of the emission (f max) increases linearly with absolute temperature (T). Planck’s Law of blackbody radiation, a formula to determine the spectral energy density of the emission at each wavelength (E λ) at a particular absolute temperature (T).Ģ. The characteristics of blackbody radiation can be described in terms of several laws:ġ. Blackbody radiation curves at several different temperatures.
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