Connection between nonradial pulsations and stellar winds in massive stars. IV. Atmospheric structure and mass loss from pulsation with speculative application to B and Be stars

Journal Article · Wed Jan 01 04:00:00 EST 1986 · Publ. Astron. Soc. Pac.; (United States)

DOI:https://doi.org/10.1086/131716· OSTI ID:5556786

Willson, L A

Pulsation produces alterations in the density structure of a stellar atmosphere, and it drives or enhances mass loss. A summary is provided of some very general results which were obtained on the basis of an analysis of models calculated by Bowen (1985) for the atmospheres of radially pulsating cool stars. It is pointed out that four parameters are needed to characterize the structure of the atmosphere of a pulsating star, if simplifying assumptions are made regarding isothermal conditions with respect to shocks and the global temperature distribution. Some possible implications of the nonradial pulsations observed in B and Be stars for the structure of their atmospheres are discussed. Attention is given to the stellar wind, and applications to B and Be stars. 9 references.

• Research Organization: Iowa State Univ. of Science and Technology, Ames
• OSTI ID: 5556786
• Journal Information: Publ. Astron. Soc. Pac.; (United States), Journal Name: Publ. Astron. Soc. Pac.; (United States) Vol. 98; ISSN PASPA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
DATA
INFORMATION
MASS
MATHEMATICAL MODELS
NUMERICAL DATA
PULSATIONS
RADIATION PRESSURE
STARS
STELLAR ACTIVITY
STELLAR ATMOSPHERES
STELLAR FLARES
STELLAR WINDS
SUPERMASSIVE STARS
THEORETICAL DATA