Models for stellar coronae - Thin coronae with radiative forces

Details Models for stellar coronae - Thin coronae with radiative forces Models for stellar coronae - Thin coronae with radiative forces

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...185..247h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 185, no. 1-2, Oct. 1987, p. 247-252.

Astronomy and Astrophysics

Astrophysics

Hot Stars, Radiative Transfer, Stellar Coronas, Stellar Mass Ejection, Stellar Models, B Stars, Mass Flow Rate, O Stars, Supergiant Stars, Velocity Distribution

Scientific paper

Models are calculated for small coronae heated by saw tooth waves with radiative forces acting in the cool region above the corona. The radiative forces are introduced in a parameterized form. The mass loss rates obtained in the models are orders of magnitude lower than the mass loss rates observed in OB supergiants. Attempts to produce models with higher mass loss rates failed. It is not known whether the difficulty is numerical or physical. Given the large difference between the mass loss rate produced in these models and the observed mass loss rates in OB supergiants, it seems likely that these models do not exist at the observed mass loss rates. The results illustrate the main properties of small coronal models with radiative forces. For a given mechanical heating the mass loss up to a limit is almost independent of the radiative forces. Beyond that limit the solution suddenly disappears and the small corona is blown away by the radiative forces. Then presumably a Castor, Abbott, and Klein solution would be formed. This would provide a mechanism for establishing that solution in a star. The models have a two stage velocity distribution which cannot be represented by the parameterized velocity distribution used in interpreting the ultraviolet and infrared observations.

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