Other
Scientific paper
Jan 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983sao..reptq....d&link_type=abstract
Semiannual Progress Report, 1 Apr. - 30 Sep. 1982 Smithsonian Astrophysical Observatory, Cambridge, MA.
Other
Chromosphere, Cool Stars, Giant Stars, Late Stars, Line Spectra, Radiant Cooling, Stellar Winds, Supergiant Stars, Absorption Spectra, Calcium, Ionization, Magnesium, Stellar Envelopes, Stellar Models
Scientific paper
The formation of spectral lines in expanding spherical atmospheres was determined in a physically realistic way, taking into account multilevel atomic processes, partial frequency redistribution, and other non-LTE transfer effects that affect the formation of optically thick lines. The formation of MgII and Ca II circumstellar absorption lines in late type giants and supergiants is investigated. The radiative cooling rate as a function of density and temperature was calculated from the results of plane parallel chromospheric models and these results were used to approximate the radiative cooling in an extended wind. The run of temperature was calculated along with the density and velocity profiles. The most important prediction of these models is that a warm zone in the wind must exist as a result of the wave heating. Within this zone, the Ca II and Mg II atoms can be ionized to Ca III and Mg III, so that the gas is transparent in the resonance transitions.
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