Abstract
This chapter defines principles associated with a black body. They are necessary to know to understand solar and terrestrial radiation as well as infrared thermometry, discussed in a subsequent chapter. Kirchhoff's principle of radiation, which defines a black body, is derived. An example of a black body is illustrated. The Stefan–Boltzmann law, which gives the temperature of a black body, is given. The spectrum of a black body, which requires knowledge of Wien's displacement law, is discussed. The temperature of the earth and sun is calculated, assuming that they are black bodies. Solar and terrestrial radiation are compared. The equation for the heat budget at the surface of the earth is given, which includes the term of solar radiation. Solar radiation is further examined by presenting the equation for the radiation balance. Terms associated with this equation are defined, including albedo. Appendices give biographies of Kirchhoff, Stefan, Boltzmann, and Wien.
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