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  1. All black bodies heated to a given temperature emit thermal radiation. The radiation energy per unit time from a black body is proportional to the fourth power of the absolute temperature and can be expressed with Stefan-Boltzmann Law as q = σ T4 A (1) where q= heat transfer per unit time (W) σ= 5.6703 10-8 (W/m2K4) - TheStefan-Boltzmann Constant
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    The absolute temperature of an object emitting thermal radiation is inversely proportional to the peak wavelength of its spectrum and directly proportional to the peak frequency of its spectrum. T ∝1/λ max T ∝ fmax
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