Model calculations for photospheres and envelopes - Applications to 'classical' Be stars

Details Model calculations for photospheres and envelopes - Applications to 'classical' Be stars Model calculations for photospheres and envelopes - Applications to 'classical' Be stars

Feb 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...191..348h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 191, no. 2, Feb. 1988, p. 348-358.

Astronomy and Astrophysics

Astrophysics

20

B Stars, H Ii Regions, Photosphere, Stellar Envelopes, H Lines, Hydrogen, Stellar Models, Stellar Spectra

Scientific paper

Spherical NLTE model photospheres surrounded by envelopes are calculated in order to interpret the hydrogen spectra of 'classical' Be stars. Both parts are assumed to be in radiative equilibrium. With these models, the existence of extended compact H II-regions around B stars can be understood as a consequence of photoionization by Balmer continuum photons, bound-bound collisions, large optical depths in the hydrogen lines, and high photon densities in the optically thin continua. Consideration is given to the interaction between the photosphere and the envelope and the dependencies of spectral features on the free model parameters. Observed spectra and statistical results can be understood in terms of these models.

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