IUE observations of pulsating stars: Atmospheric structure, shock waves and stellar winds

Details IUE observations of pulsating stars: Atmospheric structure, shock waves and stellar winds IUE observations of pulsating stars: Atmospheric structure, shock waves and stellar winds

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.281a..29w&link_type=abstract

In ESA, A Decade of UV Astronomy with the IUE Satellite, Volume 1 p 29-40 (SEE N89-10682 01-89)

Astronomy and Astrophysics

Astronomy

8

Iue, Shock Waves, Spaceborne Astronomy, Stellar Atmospheres, Stellar Mass Ejection, Stellar Winds, Ultraviolet Astronomy, Variable Stars, Pulses, Stellar Models

Scientific paper

Pulsating stars studied by IUE, including Miras and semiregular long period variables, Cepheids, RR Lyrae stars, delta Scuti stars, Beta Cep stars, Be stars, hot subdwarfs (PG1159 stars), and pulsating white dwarfs are discussed. The interpretation of IUE observations of obviously pulsating stars in terms of static model atmospheres, models applicable to similar but nonpulsating stars, or models applicable to stars with different pulsation properties is always fundamentally wrong. The atmospheric temperature, density, and velocity structure of a star is very much altered by the presence of radial (or large amplitude nonradial) pulsation, and the structure depends strongly on the pulsation period and on the efficiency of mechanisms driving a stellar wind. For the well-studied radially pulsating stars (Beta Cep variables, Cepheids of all types, and long period variables) IUE observations are all at least qualitatively consistent with the predictions of models and analytic theory based on the assumption that pulsation is the dominant factor.

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