Far-ultraviolet Spectroscopy of O+O Binaries in the Magellanic Clouds

Details Far-ultraviolet Spectroscopy of O+O Binaries in the Magellanic Clouds Far-ultraviolet Spectroscopy of O+O Binaries in the Magellanic Clouds

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.0304s&link_type=abstract

American Astronomical Society Meeting 210, #03.04; Bulletin of the American Astronomical Society, Vol. 39, p.98

Astronomy and Astrophysics

Astronomy

Scientific paper

We report FUSE observations in 2006 of three O-type, double-lined spectroscopic binaries in the Magellanic Clouds. Their binary nature was discovered only in the past several years. The systems have very short periods (1.4 - 2.25 days), represent rare, young evolutionary stages of massive stars and binaries, and provide a unique glimpse at some of the most massive systems that form in dense clusters of massive stars. The systems are: LH54-425 in the LMC (O3IIIf + O6V, P=2.25 days, 100+50 M¤), J053441-693139 in the LMC (O2-3If + O6V, P=1.4 days, 41+27 M¤), and Hodge 53-47 in the SMC (O6V + O4-5IIIf, P=2.2 days, 24+14 M¤, where the O4 star appears to be less massive than the O6 star). These represent some of the most massive binaries known. Their short periods indicates that wind interaction and mass transfer are likely important factors in their evolution. The spectra provide quantitative and systematic studies of phase-dependent stellar wind properties, wind collision effects in O+O binaries at lower metallicities, improved radial velocity curves, and FUV spectrophotometric changes as a function of orbital phase.

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