The β Cephei variable in the eclipsing binary HD 92024. I. Determination of the orbit

Details The β Cephei variable in the eclipsing binary HD 92024. I. Determination of the orbit The β Cephei variable in the eclipsing binary HD 92024. I. Determination of the orbit

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005a%26a...429..631f&link_type=abstract

Astronomy and Astrophysics, v.429, p.631-643 (2005)

Astronomy and Astrophysics

Astrophysics

12

Stars: Binaries: Eclipsing, Stars: Binaries: Spectroscopic, Stars: Early-Type, Techniques: Spectroscopic

Scientific paper

HD 92024 is a member of the open cluster NGC 3293; it is the only eclipsing binary system with a β Cephei 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&sun; and 3.0±0.5 M&sun; respectively, and radii of 8.4±0.8 R&sun;, 2.1±0.4 R&sun;. The temperatures are 25 500±500 K and 12 500±1000 K. The surface gravity values of log g= 3.77±0.08 and 4.27±0.18 indicate that the binary consists of an evolved early B-type primary and a late-B main sequence companion. The resulting distance 2.8±0.3 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 NGC 3293.
Based on observations made with ESO Telescopes at the La Silla Observatory, Chile, under programmes 66.D-0297, 67.D-0023, 68.D-028, and with the Strömgren Automatic Telescope, La Silla.

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