C IV 5806 A in Wolf-Rayet stars

Details C IV 5806 A in Wolf-Rayet stars C IV 5806 A in Wolf-Rayet stars

Oct 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988pasp..100.1269u&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 100, Oct. 1988, p. 1269-1272.

Astronomy and Astrophysics

Astronomy

Carbon, Light Emission, Spectral Line Width, Stellar Spectra, Wolf-Rayet Stars, Abundance, Electron Density (Concentration), Electron Energy, Photoionization

Scientific paper

It is shown that the observed differences between the equivalent widths of the C IV λ5806 line in WC and WN stars can be understood using the fractional populations of the levels of the C atom predicted using a simple theory and the solar value for N(C)/N(H). The dominant factor causing the difference in line strength between WC and WN types is the electron temperature. The electron density is a second significant factor. The line-emitting regions (LERs) of WN stars seem to have lower density than the LERs of WC spectra.

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