Stellar winds from hot stars in the Magellanic Clouds

Details Stellar winds from hot stars in the Magellanic Clouds Stellar winds from hot stars in the Magellanic Clouds

Jun 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...293..407g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 293, June 15, 1985, p. 407-413.

Astronomy and Astrophysics

Astronomy

73

Hot Stars, Magellanic Clouds, Stellar Winds, Ultraviolet Astronomy, B Stars, Iue, O Stars, Spectral Line Width, Stellar Mass Ejection, Terminal Velocity

Scientific paper

O and B stars in the LMC and SMC have been observed with the IUE in order to compare their winds and mass loss rates with those of their galactic counterparts. It is found that while the wind terminal velocities are generally about 20 percent lower than in galactic stars of the same spectral type, it is not clear that the mass loss rates are significantly lower. This conclusion differs from the conclusions of other studies, and the reasons are discussed. The most important reason is that a less luminous set of stars with new spectral types determined from slit spectra is being examined. The discussion of stellar winds rests heavily on a comparison of relevant wind parameters observed in O stars using both high and low dispersion IUE spectra.

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