Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985nascp2358...57g&link_type=abstract
In NASA. Goddard Space Flight Center The Origin of Nonradiative Heating/Momentum in Hot Stars p 57-61 (SEE N85-17755 08-88)
Astronomy and Astrophysics
Astronomy
Absorption Spectra, Beryllium, Resonance Lines, Stars, Stellar Models, Stellar Spectra, Stellar Winds, Iue, Line Spectra, Radial Velocity, Ultraviolet Astronomy, Ultraviolet Radiation
Scientific paper
The stars omega Ori (B2 IIIe), 66 Oph (B2 IVe), and 59 Cyg (B1.5 IVe) are discussed. The extent to which the narrow absorption components in these Be stars differs from narrow components in the O stars and gamma Cas is explored. Any models or mechanisms for the formation of narrow absorption features in the UV resonance lines of Be star spectra must account for the presence of multiple narrow absorption features which are variable in number, radial velocity, and strength. Models predicting a high and low density structure to the stellar wind caused by instabilities in a flow driven by radiation pressure or by variable mass loss may be more successful in describing the behavior of winds in early Be stars. These models appear to be capable of producing single absorption components in the velocity range observed for O stars and very early Be stars.
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