FUSE Observations of the Stellar Winds of Two O7 Supergiants in the Magellanic Clouds

Details FUSE Observations of the Stellar Winds of Two O7 Supergiants in the Magellanic Clouds FUSE Observations of the Stellar Winds of Two O7 Supergiants in the Magellanic Clouds

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...195.0623f&link_type=abstract

American Astronomical Society, 195th AAS Meeting, #06.23; Bulletin of the American Astronomical Society, Vol. 31, p.1377

Astronomy and Astrophysics

Astronomy

Scientific paper

The main goal of the FUSE hot-star program is to characterize the stellar winds of a large sample of early-type stars in the Galaxy, LMC, and SMC in order to study mass loss as a function of metallicity. As the first step in this program, we compare the stellar wind features observed in FUSE spectra of Sk -67o111, an O7 Ib(f) star in the LMC, with those of Sk 80 = AV 232, an O7 Iaf+ star in the SMC. These features include the resonance doublets of S iv λ λ 1063, 1073, P v λ λ 1118, 1128 (which is blended with the excited transitions of Si iv λ λ 1122, 1128), and O vi λ λ 1032, 1038. These ionic species sample a wider range of temperatures and provide a more comprehensive indication of the ionization balance at different locations in the wind than the diagnostics found in the IUE/HST wavebands. Consequently, they revive the possibility of using resonance lines to determine accurate mass-loss rates. The FUSE observations of Sk -67o111 and Sk 80 reveal striking differences in the strength and morphology of the O vi wind profile, and confirm that stars in the SMC have smaller outflow velocities than their counterparts in the LMC. This work is supported by NASA contract NAS5-32985.

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