The WO stars. I - Helium in the optical spectrum of Sand 4

Details The WO stars. I - Helium in the optical spectrum of Sand 4 The WO stars. I - Helium in the optical spectrum of Sand 4

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...265..563p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 265, no. 2, p. 563-569.

Astronomy and Astrophysics

Astrophysics

16

Helium, Stellar Spectra, Visible Spectrum, Wolf-Rayet Stars, Emission Spectra, Line Spectra, Stellar Atmospheres, Stellar Winds

Scientific paper

We present here the results of the analysis performed on intermediate resolution optical spectra of the WR star Sand 4 (WR 102) which is the most extreme of the small WO subgroup. We performed a detailed analysis of the main emission features in order to obtain reliable line identifications and to derive the physical conditions of the star's atmosphere. He II is the main contributor to the 468 nm and 654 nm emissions. The very high ionization O VIII 606.4-6.8 nm doublet is present with a narrower emission, suggesting line formation in deeper atmospheric layers. We conclude that Sand 4 is a highly evolved object, surely more evolved than a WCE star, but the transition from WC to WO appears to be fairly smooth.

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