Stratification in WR envelopes as seen in HeII lines

Details Stratification in WR envelopes as seen in HeII lines Stratification in WR envelopes as seen in HeII lines

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...282..529n&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 282, no. 2, p. 529-534

Astronomy and Astrophysics

Astrophysics

11

Helium, Line Spectra, Stellar Envelopes, Stratification, Wolf-Rayet Stars, Optical Thickness, Spectral Line Width, Velocity Distribution

Scientific paper

Using literature data on lines widths we show that the HeII emission lines originate in different regions of the Wolf-Rayet (WR) envelope. It is concluded that because of variations of lines widths within one series of an ion the Ionization Potential vs. Full Width at Half Maximum (FWHM) velocity diagrams can not be used for quantitative analysis of WR stars. Another physical quantity such as line optical depth should be used. For simplicity we use nu (principal quantum number of upper level) or EP - excitation energy of the upper level in (u-1) transition. The correlation is strongest with nu, indicating the importance of optical depth effects on the line formation region. The velocity run in the envelopes of 5 Wolf-Rayet stars HD 4004, 191765, 192163, 193928, 50896 is discussed on the basis of the He II (n-3), (n-4) and (n-5) series emissions lines widths on the nu or EP vs. FWHM velocity graphs.

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