Constraints for models of Be stars derived from UV and IRAS observations

Details Constraints for models of Be stars derived from UV and IRAS observations Constraints for models of Be stars derived from UV and IRAS observations

Aug 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...182...80l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 182, no. 1, Aug. 1987, p. 80-90. ZWO-supported research.

Astronomy and Astrophysics

Astronomy

56

B Stars, Infrared Spectra, Stellar Mass Ejection, Stellar Models, Ultraviolet Spectra, Infrared Astronomy Satellite, Stellar Atmospheres, Stellar Envelopes, Stellar Spectra

Scientific paper

The observations of UV line profiles and IR excess of 10 Be stars are interpreted quantitatively in order to derive constraints for models of Be stars. Two models are considered: a disc model in which the UV lines are formed in the high velocity polar region and the IR excess is formed in the high density equatorial disc, and a circumstellar shell model where the UV lines are formed in a spherically symmetric wind and the IR excess is formed in a circumstellar shell which surrounds the wind region. The UV and IR observations can be explained by both models. The results of the studies of the polarization and the Balmer emission profiles in Be stars, strongly support the disc model and do not agree with the circumstellar shell model. The large contrast in mass flux and density between the polar region and the disc region cannot be explained by radiation driven winds of rapidly rotating stars. Some other mechanism which enhances the mass loss in the equatorial region is required.

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