Ultraviolet and optical spectroscopy of a B supergiant star in M 31

Details Ultraviolet and optical spectroscopy of a B supergiant star in M 31 Ultraviolet and optical spectroscopy of a B supergiant star in M 31

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...292..213b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 292, no. 1, p. 213-220

Astronomy and Astrophysics

Astronomy

19

B Stars, Spectrum Analysis, Stellar Color, Stellar Models, Stellar Winds, Supergiant Stars, Ultraviolet Spectra, Visible Spectrum, Abundance, H Alpha Line, H Gamma Line, Hubble Space Telescope, Ultraviolet Astronomy

Scientific paper

We present and discuss the UV spectrum of the supergiant star in NGC206-277 in M 31, obtained with the Faint Object Spectrograph (FOS) on Hubble Space Telescope (HST). An optical blue spectrum taken at Kitt Peak National Observatory (KPNO) is also shown. From the optical and UV line spectra we classify the star B1.5Ia. We fit the continuum far-UV flux distribution, deriving Teff = 20,000 K, and with this temperature we find log g = 2.5 by comparing the Hgamma line and He I lines with predictions from Non-Local Thermodynamic Equilibrium (NLTE) models. We analyze the stellar UV wind line profiles with the SEI method and derive a terminal velocity of upsiloninfinity approximately equal to 700 km/s. We fit the Halpha emission line obtained at the WHT with a newly developed (by H.J.G.L.M.L.) code similar to the SEI method for UV lines, and derive dm/dt = 1.3 +/- 0.5 10-6 solar mass/yr. We find that the P Cygni profiles of the M 31 star have slightly weaker and narrower absorptions, and no emission component. We correct our previously published mass-loss estimate for an O star (NGC206-231) in the same association. The correct value is dm/dt approximately equals 10-6 solar mass/yr, assuming solar abundances.

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