Observations of structure in the stellar wind of HD 152408

Details Observations of structure in the stellar wind of HD 152408 Observations of structure in the stellar wind of HD 152408

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.221...67p&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 221, no. 1-2, p. 67-76

Physics

1

Giant Stars, O Stars, Solar Wind Velocity, Stellar Mass, Stellar Physics, Stellar Structure, Stellar Winds, Ultraviolet Spectra, Variability, Balmer Series, H Alpha Line, H Beta Line, Photosphere, Spectroscopy, Stellar Luminosity

Scientific paper

We report on the presence of substantial, low-velocity stellar wind structure in the extreme O supergiant HD 152408, based on optical spectroscopic time-series observations. Systematic variations in the form of migrating optical depth enhancements occur in the absorption trough of the He I lamda 5876 P Cygni profile. These variations start deep in the stellar wind, slowly accelerate bluewards to greater than 0.5 upsiloninfinity over approximately 1-2 days, and recur at intervals of about 1 day. Sympathetic variations are apparent in the Balmer emission lines. The observations provide constraints on the stability of the low-velocity stellar wind regime, and indicate the presence of large-amplitude perturbations at great depths in the outflow.

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