The stellar wind of an O8.5 I(f) star in M 31

Details The stellar wind of an O8.5 I(f) star in M 31 The stellar wind of an O8.5 I(f) star in M 31

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...295..136h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 295, no. 1, p. 136-146

Astronomy and Astrophysics

Astrophysics

19

Abundance, Early Stars, Line Spectra, Stellar Mass Ejection, Stellar Winds, Ultraviolet Spectra, Data Reduction, Faint Object Camera, Hubble Space Telescope, Light Scattering, Magellanic Clouds, Radiation Pressure

Scientific paper

We rediscuss the UV spectrum of OB 78#231, an O8.5 I(f) star in the Andromeda galaxy M 31, which has been obtained with the Faint Object Spectrograph on the Hubble Space Telescope by Hutchings et al. (1992). The spectrum has been re-extracted with better knowledge of background, calibration, and scattered light. The empirical analysis of the stellar wind lines results in a terminal velocity and mass loss rate similar to those typically found in comparable galactic objects. Furthermore, a comparison with an FOS spectrum of an O7 supergiant in the Small Magellanic Cloud and IUE spectra of galactic objects implies a metallicity close to galactic counterparts. These results are confirmed quantitatively by spectrum synthesis calculations using a theoretical description of O-star winds.

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