Coronal radiative losses refer to the energy that is radiated away by the solar corona, which is the outermost layer of the Sun's atmosphere. The corona is extremely hot, with temperatures reaching millions of degrees Celsius, and it emits energy primarily in the form of X-rays and ultraviolet radiation. In astrophysics, particularly in the study of stellar atmospheres, radiative losses occur when hot plasma (such as that found in the corona) cools by emitting photons.
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