Carbon and nitrogen lines in the spectra of Wolf-Rayet stars

Details Carbon and nitrogen lines in the spectra of Wolf-Rayet stars Carbon and nitrogen lines in the spectra of Wolf-Rayet stars

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apjs...67..187b&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 67, June 1988, p. 187-223. NASA-NSERC-supported research.

Astronomy and Astrophysics

Astrophysics

32

Carbon, Nitrogen, Stellar Spectra, Wolf-Rayet Stars, Radiative Transfer, Stellar Atmospheres

Scientific paper

Predictions of 29 energy ratios involving emission lines of He II, C II, C III, C IV, N III, N IV, and N V are presented. Comparison of observed energy ratios with the predicted energy ratios shows that WC spectra can be understood in terms of solar composition, T* = 2.5 × 104K, 5×104 ≤ Te ≤ 105K, and Ne ≈ 1010cm-3, while WN spectra imply solar composition, T* = 2.5×104K, 105 ≤ Te ≤ 2×105K, 109 ≤ Ne ≤1010cm-3. The line-emitting regions have volumes of the order of 1041 - 1044cm3. The line-emitting regions may be in the form of thin disks having radii of the order of 1015cm. It is noted that Population I Wolf-Rayet stars may be young objects still surrounded by remnant natal disks, while Population II Wolf-Rayet stars may be surrounded by disks generated by their red giant parents.

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