Volume 429, Number 2, January II 2005
|Page(s)||631 - 643|
|Section||Stellar structure and evolution|
|Published online||17 December 2004|
The β Cephei variable in the eclipsing binary HD 92024*
I. Determination of the orbit
Royal Observatory of Belgium, Ringlaan 3, 1180 Brussels, Belgium e-mail: email@example.com
2 OBSS/WE, Vrije Universiteit Brussel, Pleinlaan 2, 1050 Brussels, Belgium
3 Department of Physics, University of Zagreb, Bijenička 32, 10000 Zagreb, Croatia
4 Institut d'Astrophysique et de Géophysique, Université de Liège, 17 Allée du 6 Août, 4000 Liège, Belgium
5 European Southern Observatory, Casilla 19001, Alonso de Cordova 3107, Vitacura, Santiago, Chile
6 Faculty of Electrical Engineering and Computing, Department of Applied Physics, University of Zagreb, Unska 3, 10000 Zagreb, Croatia
Accepted: 28 August 2004
HD 92024 is a member of the open cluster ; it is the only eclipsing binary system with a component known in the southern hemisphere. This paper presents the first spectroscopic analysis of the single-lined binary and provides an orbital analysis based on recent high-resolution spectroscopy and photometry. A procedure to derive orbital elements with minimal influence of the pulsational line-profile variations on the radial velocities is applied, and we find the stellar masses to be and respectively, and radii of , . The temperatures are K and K. The surface gravity values of and indicate that the binary consists of an evolved early B-type primary and a late-B main sequence companion. The resulting distance kpc and systemic velocity -16 km s-1 confirm cluster membership. Theoretical stellar models indicate an age of Myr, somewhat higher than the literature value for the brightest members of .
Key words: stars: binaries: eclipsing / stars: binaries: spectroscopic / stars: early-type / techniques: spectroscopic
© ESO, 2005
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