Yakut, K.Aerts, C.Morel, T.2019-10-272019-10-2720071432-07461432-0746https://doi.org/10.1051/0004-6361:20065506https://hdl.handle.net/11454/39642Aims. Our goal was to improve the fundamental parameters of the massive close double-lined eclipsing B2.5V+B2.5V binary CV Velorum. Methods. We gathered new high-resolution echelle 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. Results. We obtained the following values for the physical parameters: M-1 = 6.066(74) M-circle dot, M-2 = 5.972(70) M-circle dot, R-1 = 4.126(24) R-circle dot, R-2 = 3.908(27) R-circle dot, logL(1) = 3.20(5) L-circle dot, and logL(2) = 3.14(5) L-circle dot. 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.en10.1051/0004-6361:20065506info:eu-repo/semantics/openAccessstars : early-typestars : oscillationsstars : binaries : eclipsingstars : fundamental parametersstars : evolutionstars : individual : CV VelorumArticle4672647655WOS:000246424900028Q1Q1