The early-type close binary CV Velorum revisited

Abstract

Our goal was to improve the fundamental parameters of the massive close double-lined eclipsing B2.5V+B2.5V binary CV Velorum.We gathered new high-resolution echelle spectroscopy on 13 almost consecutive nights covering essentially two orbits. We computed a simultaneous solution to all the available high-quality radial-velocity and light data with the latest version of the Wilson-Deviney code. We obtained the following values for the physical parameters: $M_1=6.066(74)M_{\odot }$, $M_2=5.972(70)M_{\odot }$, $R_1=4.126(24)R_{\odot }$, $R_2=3.908(27)R_{\odot }$, $\log L_1=3.20(5)L_{\odot }$, and $\log L_2=3.14(5)L_{\odot }$. The quoted errors contain a realistic estimate of systematic uncertainties mainly stemming from the effective temperature estimation. We derived abundances for both components and found them to be compatible with those of B stars in the solar neighbourhood. We discovered low-amplitude periodic line-profile variations with the orbital frequency for both components. Their interpretation requires new data with a longer time span. The primary rotates subsynchronously while the secondary's $v\sin i$ and radius are compatible with synchronous rotation. Finally, we provide an update of the empirical mass-luminosity relation for main-sequence B stars which can be used for statistical predictions of masses or luminosities.

11 pages, 7 figures, accepted for publication in Astronomy & Astrophysics

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• The nature of the eccentric doubled-lined eclipsing binary system KIC 2306740 with Kepler space photometry
• Quantitative spectroscopy of close binary stars