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Issue A&A
Volume 429, Number 2, January II 2005
Page(s) 631 - 643
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20041527



A&A 429, 631-643 (2005)
DOI: 10.1051/0004-6361:20041527

The $\beta$ Cephei variable in the eclipsing binary HD 92024

I. Determination of the orbit
L. M. Freyhammer1, 2, H. Hensberge1, C. Sterken2, K. Pavlovski3, A. Smette4, 5 and S. Ilijic6

1  Royal Observatory of Belgium, Ringlaan 3, 1180 Brussels, Belgium
    e-mail: lfreyham@vub.ac.be
2  OBSS/WE, Vrije Universiteit Brussel, Pleinlaan 2, 1050 Brussels, Belgium
3  Department of Physics, University of Zagreb, Bijenicka 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

(Received 24 June 2004 / Accepted 28 August 2004)

Abstract
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 $15.0^{+3.0}_{-4.0}~M_\odot$ and $3.0\pm0.5~M_\odot$ respectively, and radii of $8.4\pm0.8~R_\odot$, $2.1\pm0.4~R_\odot$. The temperatures are $25\,500\pm500$ K and $12\,500\pm1000$ K. The surface gravity values of $\log g= 3.77\pm0.08$ and $4.27\pm0.18$ indicate that the binary consists of an evolved early B-type primary and a late-B main sequence companion. The resulting distance $2.8\pm0.3$ kpc and systemic velocity -16 km s -1 confirm cluster membership. Theoretical stellar models indicate an age of 10-13 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

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