Reference : The early-type close binary CV Velorum revisited
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
The early-type close binary CV Velorum revisited
Yakut, K. [Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, 3001 Leuven, Belgium; Department of Astronomy and Space Sciences, Ege University, 35100 Ä°zmir, Turkey]
Aerts, C. mailto [Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, 3001 Leuven, Belgium ; Department of Astrophysics, University of Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands]
Morel, Thierry [Katholieke Universiteit Leuven, Departement Natuurkunde en Sterrenkunde, Instituut voor Sterrenkunde, Celestijnenlaan 200D, 3001 Leuven, Belgium > > > >]
Astronomy and Astrophysics
EDP Sciences
Yes (verified by ORBi)
Les Ulis
[en] stars: early-type ; stars: oscillations ; stars: binaries: eclipsing ; stars: fundamental ; parameters ; stars: evolution ; stars: individual: CV Velorum
[en] Aims:Our goal was to improve the fundamental parameters of the massive close double-lined eclipsing B2.5V+B2.5V binary CV Velorum. <BR />Methods: We gathered new high-resolution échelle spectroscopy on 13 almost consecutive nights covering 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. <BR />Results: We obtained the following values for the physical parameters: M[SUB]1[/SUB] = 6.066(74)~M_ȯ, M[SUB]2[/SUB] = 5.972(70)~M_ȯ, R[SUB]1[/SUB] = 4.126(24)~R_ȯ, R[SUB]2[/SUB] = 3.908(27)~R_ȯ, log L[SUB]1[/SUB] = 3.20(5)~L_ȯ, and log L[SUB]2[/SUB] = 3.14(5)~L_ȯ. 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. 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. Based on spectroscopic observations gathered with the CORALIE spectrograph mounted on the 1.2 m Euler telescope at La Silla, Chile.

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