Physics
Scientific paper
Nov 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...250..709a&link_type=abstract
Astrophysical Journal, Part 1, vol. 250, Nov. 15, 1981, p. 709-718.
Physics
24
Chromosphere, Solar Atmosphere, Solar Physics, Solar Wind, Stellar Coronas, Energy Dissipation, Ion Production Rates, Solar Radiation, Solar Temperature, Stellar Models, Stellar Structure
Scientific paper
An attempt is made to provide an updated explanation of the essential structure features of the solar atmosphere based, where possible, on the constraints imposed by the physics of the solar plasma. The chromospheric temperature plateaus are identified with plasma properties determined by the degree of ionization of hydrogen. This is possible because the energy loss is solely by radiation and the nature of the radiation loss changes rather discontinuously as the degree of ionization increases. The ionization conditions are discussed in relation to other stars. In the case of the transition region and the corona, the plasma is essentially fully ionized and, in addition, the role of radiation enters somewhat indirectly.
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