Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...221...78g&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 221, no. 1, Aug. 1989, p. 78-88.
Astronomy and Astrophysics
Astronomy
120
O Stars, Resonance Lines, Stellar Winds, Terminal Velocity, Ultraviolet Astronomy, Astronomical Catalogs, Line Spectra, Stellar Envelopes, Stellar Mass Ejection, Thermodynamic Equilibrium
Scientific paper
The SEI method (Lamers et al., 1987) is used to obtain P Cygni profiles of the UV resonance lines of C IV, N V, and S IV and of the subordinate UV lines of N IV and C III observed in the spectra of 27 O-type stars. Theoretical profiles which include the turbulence effects agree well with the observations, and they can account for the deep absorption troughs, the shape of the violet absorption wings, and the wavelength of the emission peak. The resulting terminal velocities of the stellar winds are found to be systematically lower by about 400 km/s than previous estimates obtained using the Sobolev approximation (Castor and Lamers, 1979), suggesting that the narrow absorption components, observed in the UV resonance lines of O and B stars, reach the terminal velocity of the winds.
Groenewegen Martin A. T.
Lamers Henny J. G. L. M.
Pauldrach Adalbert W. A.
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