The LMC Eclipsing Binary HV2241: Fundamental Properties and Evolution

Details The LMC Eclipsing Binary HV2241: Fundamental Properties and Evolution The LMC Eclipsing Binary HV2241: Fundamental Properties and Evolution

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...202.0806b&link_type=abstract

American Astronomical Society Meeting 202, #08.06; Bulletin of the American Astronomical Society, Vol. 35, p.708

Astronomy and Astrophysics

Astronomy

Scientific paper

We are investigating the LMC eclipsing binary HV 2241 as part of a larger project directed toward the determination of the physical properties of LMC stars and the distance to the LMC. HV 2241 is a semi-detached system, consisting of an ˜O7 III primary component and an ˜B0 III secondary (filling its Roche equipotential surface) in a 4.34 d orbit. The datasets being analyzed consist of previously published CCD photometry (Strömgren u, Cousins Ic, and V), HST/FOS 110-480 nm spectrophotometry, and newly acquired 400-530 nm echelle spectroscopy using the Blanco 4-meter telescope at CTIO. Preliminary values for the temperature ratios of the components, the stellar radii and masses, and the inclination of the stars' orbits are used to model the system with the Wilson-Devinney eclipsing binary code. Analyses of the spectrophotometry yield surface temperatures of the stars and the amount of interstellar reddening. The resulting stellar properties for the primary star (radius, temperature, and mass) are compared with stellar evolution models for consistency. The distance to HV 2241 is computed from a knowledge of the stars' radii and temperatures as well as the amount of reddening.
We gratefully acknowledge financial support from the NASA - Delaware Valley Space Grant consortium, and from the National Science Foundation through HST grant GO-06683. We are grateful for the skilled assistance of the CTIO staff during our January 2000 observing run.

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