Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26as...79..359g&link_type=abstract
Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 79, no. 3, Sept. 1989, p. 359-383.
Astronomy and Astrophysics
Astronomy
143
Line Shape, O Stars, Stellar Spectra, Stellar Winds, Ultraviolet Astronomy, Astronomical Catalogs, Interstellar Matter, Iue, Line Spectra, Terminal Velocity, Turbulent Flow
Scientific paper
The theoretical UV P Cygni profiles of the UV resonance lines for C IV, N V, Si IV, C III, and N IV of 26 O-type stars and one B star were calculated using the SEI method described by Lamers et al. (1987), taking into account the effects of turbulence in the wind, limb darkening, photospheric lines, and interstellar Ly alpha. The results were compared with profiles observed with the IUE satellite. The profile fits were found to be very accurate, showing significant improvement over previously obtained fits with the Sobolev (1958) method. The SEI method and the line fitting analysis are described and the results are presented in terms of the column densities and distributions of absorbing atoms, and the velocity laws.
Groenewegen Martin A. T.
Lamers Henny J. G. L. M.
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