Rapid variability in O star winds

Details Rapid variability in O star winds Rapid variability in O star winds

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.281b.145h&link_type=abstract

In ESA, Proceedings of the Celebratory Symposium on a Decade of UV Astronomy with the IUE Satellite, Volume 2 p 145-149 (SEE N89

Astronomy and Astrophysics

Astronomy

36

Iue, O Stars, Spaceborne Astronomy, Stellar Winds, Ultraviolet Astronomy, Ultraviolet Spectra, Variability, Terminal Velocity, Ultraviolet Absorption, Wind Velocity

Scientific paper

Rapid, systematic changes in the absorption parts of the P-Cygni profiles of the resonance lines of Si IV, C IV and N V in four O stars are reported. Two types of variability are found: (1) in the form of the discrete absorption components, which appear episodically at low (but supersonic) velocity in the P-Cygni profiles and accelerate through the profile. The recurrence timescale varies approximately with stellar rotation period. The acceleration differs from star to star and, for a given star, from episode to episode, and (2) significant (10 pct) changes in the velocity of the steep edge of the saturated P-Cygni profiles, which are correlated with the discrete component behavior in the unsaturated Si IV line. This implies that the steep edge cannot be a good measure of the terminal velocity of the wind. An alternative determination of the maximum bulk velocity is proposed. It is suggested that both types of variability are typical for all early-type stars. The magnitude of the effect varies, however, from star to star as well as for a given star.

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