A radiative ionization and thermal equilibrium model for the wind from P Cygni

Details A radiative ionization and thermal equilibrium model for the wind from P Cygni A radiative ionization and thermal equilibrium model for the wind from P Cygni

Dec 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985mnras.217..867d&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 217, Dec. 15, 1985, p. 867-893.

Statistics

Computation

42

Astronomical Models, Gas Ionization, Radiative Transfer, Stellar Mass Ejection, Stellar Winds, Thermodynamic Equilibrium, Balmer Series, Helium, Statistical Analysis, Wind Profiles

Scientific paper

The radial variation of the temperature and ionization equilibrium in the wind from the bright star P Cygni is calculated for a range of mass loss rates and velocity laws. The calculations were performed within the framework of a numerical model of the statistical and thermal equilibria at a number of radii spanning the wind, taking into account the radiative transfer effects. The ionization balance of the most abundant heavy elements in the model is included in the calculations. A list of the elements is given in an appendix. The boundary between the stellar core and the wind is identified by the radial point R radius R, at which the continuum radiation field becomes optically thin. It is shown that the ionization of ground state hydrogen and helium in P Cygni is maintained primarily by photoionization of the n=2 levels in the diluting stellar radiation field. Photoionization is in turn responsible for the strong dependence of hydrogen and helium on the local wind temperature. Estimates of the ionization balance outside a radius of about 10 were near neutrality. A detailed description is given of the computation procedures which were used to derive the wind temperature profiles.

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