Ultraviolet spectroscopy of mass loss from late B-type supergiants

Details Ultraviolet spectroscopy of mass loss from late B-type supergiants Ultraviolet spectroscopy of mass loss from late B-type supergiants

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986iraj...17..256b&link_type=abstract

Irish Astronomical Journal (ISSN 0021-1052), vol. 17, March 1986, p. 256-263.

Astronomy and Astrophysics

Astronomy

1

B Stars, Late Stars, Stellar Mass Ejection, Supergiant Stars, Ultraviolet Spectroscopy, Absorption Spectra, Iue, Resonance Lines, Stellar Models, Stellar Winds

Scientific paper

Underhill and Fahey (1984) proposed a model in which the discrete absorption components of supergiants are due to parcels of material ejected from local spots above the photospheres of hot stars; this model is presently compared with recent UV observations of Beta Ori, which has exhibited optical and UV variability, and with observations of HD 199478 and HD 21291, which exhibit blue-shifted absorption components. The model considered is found to be able to explain in principle the longevity of the discrete absorption components.

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