Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978mnras.182..559w&link_type=abstract
Monthly Notices of the Royal Astronomical Society, vol. 182, Mar. 1978, p. 559-594. Research supported by the Science Research
Astronomy and Astrophysics
Astronomy
102
Abundance, Satellite Observation, Spectral Line Width, Stellar Spectra, Ultraviolet Spectra, Wolf-Rayet Stars, Carbon, Helium, Nitrogen, Nuclear Fusion, Sky Surveys (Astronomy), Spaceborne Astronomy, Spectral Energy Distribution, Td-1 Satellite
Scientific paper
Based on data from the S2/68 sky survey experiment of the ERSO TD-1 satellite, the ultraviolet spectra of nine Wolf-Rayet (WR) stars are presented. The equivalent widths of emission lines present in WN and WC stars are given. The data are combined with ground-based observations and analyzed for continuum energy distributions and line strengths. The flux distributions, corrected for interstellar extinction, are compared with those predicted by model atmosphere computations to yield color temperatures and Zanstra temperatures calculated from the intensity of the He II 1640 wavelength line. The results, about 30,000 K, are lower than previously expected. The observed helium, nitrogen, and carbon lines, occurring in the ultraviolet and visible spectra of one WC and three WN stars are analyzed to determine the abundances of these species. It seems that the carbon abundance controls the gross spectral characteristics of WN and WC stars. The evolutionary status of WR stars is outlined by comparing the results with the products of thermonuclear burning. It is found that WR stars are in the helium-burning phase with WC stars more evolved than WN stars.
Willis Alan J.
Wilson Raymond
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