Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990rmxaa..20...85k&link_type=abstract
Revista Mexicana de Astronomia y Astrofisica, Vol. 20, No. 2, p. 85 - 112
Astronomy and Astrophysics
Astronomy
15
Wolf-Rayet Stars: Uv Spectra, Wolf-Rayet Stars: Element Abundances, Wolf-Rayet Stars: Stellar Rotation
Scientific paper
The results of a detailed line-identification study of the IUE(1100-1900 A) spectrum of the Wolf-Rayet star HD 193077 (WR 138) is presented. The emission line spectrum is shown to be dominated by Fe V+Fe VI lines below 1500 A. The interstellar-line spectrum contains a large variety of atomic and ionic species, ranging from C I to Si IV and C IV, and CO. Interstellar features displaced by approximately -45 km s-1 are associated with the strong lines arising from the ionized species. The measurable photospheric absorption line spectrum contains lines primarily from Fe V, Fe IV, N IV, N III, C III, Ni IV, Si III, Si II, with an increase in full widhts at continuun intensity (FWCI) with decreasing ionization potential. This progression ranges from values of FWCI of 250 km s-1 for the highest ionization lines, through 800 km s-1 for the lowest ionization lines in the UV to approximately 1500 km s-1 for hydrogen, and is consistent with a rapidly rotating star. It is pointed out that the photospheric lines originating in the polar region will suffer from limb darkening effects which makes them weaker than would be observed in a non-rotating star of equivalent temperature and gravity, thus providing evidence, though not conclusive, that the emission-line and the photospheric-line spectra arise in the same star.
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