Observational and theoretical mass-loss rates of O stars in the Magellanic Clouds

Details Observational and theoretical mass-loss rates of O stars in the Magellanic Clouds Observational and theoretical mass-loss rates of O stars in the Magellanic Clouds

Nov 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...334..626l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 334, Nov. 15, 1988, p. 626-638.

Astronomy and Astrophysics

Astrophysics

21

Magellanic Clouds, O Stars, Stellar Luminosity, Stellar Mass Ejection, Stellar Winds, Emission Spectra, H Alpha Line, Metallicity, Stellar Evolution, Ultraviolet Spectra

Scientific paper

The stellar-wind properties of 26 luminous O stars in the Magellanic Clouds are investigated. Observational mass-loss rates (MLRs) are derived from the H-alpha emission in these stars. It is found that MLRs derived from H-alpha and from UV resonance lines agree if the velocity law and carbon- and nitrogen-ionization fractions of the wind are the same as in comparable Galactic stars and if the canonical abundances for the Clouds are adopted. Theoretical and observational MLRs disagree if the stellar parameters associated with a given spectral type are identical in the Galaxy and in the Magellanic Clouds. Due to the extreme sensitivity of a line-driven wind to the stellar luminosity, the MLRs derived theoretically are strongly dependent on the adopted spectral-type/T(eff) calibration. If the T(eff) of SMC stars is hotter by about 10 percent than in Galactic stars of identical spectral type, theoretical and observational MLRs agree.

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