Model atmospheres for rotating B stars

Details Model atmospheres for rotating B stars Model atmospheres for rotating B stars

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apjs...77..541c&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 77, Dec. 1991, p. 541-606.

Statistics

Computation

52

B Stars, Stellar Atmospheres, Stellar Models, Stellar Rotation, Computational Astrophysics, Early Stars, Stellar Interiors

Scientific paper

The results of extensive model atmosphere calculations applicable to rotating early-type stars are presented. While the results largely conform with those of earlier work, it is clear that the effects of rotation on the structure of the interior are likely to play as large a role in determining the emergent spectra of rotating stars as the rotational effects of the atmosphere. For lines that tend to weaken with decreasing temperature, rotation will cause the line to appear similar in strength to that of later type stars. The reverse is true for lines that increase in strength with decreasing temperature. Polarization of the UV Balmer continuum is shown to persist to much later spectral types than might be expected on the basis of ionization studies alone. In addition, it is shown that rotation behaves like a spatial filter for sharp absorption lines resulting in the enhancement of the degree of polarization in the wings of these lines. It is suggested that the effect could be quite pronounced in the FUV of the Balmer continuum complicating the interpretation of the behavior of the polarization found in the spectra of Be stars.

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