EDP Sciences
Free access
Volume 440, Number 1, September II 2005
Page(s) 249 - 260
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20053009

A&A 440, 249-260 (2005)
DOI: 10.1051/0004-6361:20053009

The orbit of the close spectroscopic binary $\varepsilon\,$Lup and the intrinsic variability of its early B-type components

K. Uytterhoeven1, 2, P. Harmanec2, 3, J. H. Telting4 and C. Aerts1, 5

1  Institute of Astronomy, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, 3001 Leuven, Belgium
    e-mail: katrienu@sunstel.asu.cas.cz
2  Astronomical Institute, Academy of Sciences, Fricova 298, 251 65 Ondrejov, Czech Republic
3  Astronomical Institute of the Charles University, V Holesovickách 2, 180 00 Praha 8, Czech Republic
4  Nordic Optical Telescope, Apartado de Correos 474, 38700 Santa Cruz de La Palma, Spain
5  Department of Astrophysics, University of Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands

(Received 7 March 2005 / Accepted 5 May 2005)

We subjected 106 new high-resolution spectra of the double-lined spectroscopic close binary $\varepsilon\,$Lup, obtained in a time-span of 17 days from two different observatories, to a detailed study of orbital and intrinsic variations. We derived accurate values of the orbital parameters. We refined the sidereal orbital period to $4\fd55970$ days and the eccentricity to e=0.277. By adding old radial velocities, we discovered the presence of apsidal motion with a period of the rotation of apses of about 430 years. Such a value agrees with theoretical expectations. Additional data is needed to confirm and refine this value. Our dataset did not allow us to derive the orbit of the third body, which is known to orbit the close system in ~64 years. We present the secondary of $\varepsilon\,$Lup as a new $\beta$ Cephei variable, while the primary is a $\beta$ Cephei suspect. A first detailed analysis of line-profile variations of both primary and secondary led to detection of one pulsation frequency near 10.36 c d-1 in the variability of the secondary, while no clear periodicity was found in the primary, although low-amplitude periodicities are still suspected. The limited accuracy and extent of our dataset did not allow any further analysis, such as mode-identification.

Key words: stars: binaries: spectroscopic -- stars: binaries: close -- stars: oscillations -- line: profiles -- stars: individual: $\varepsilon\,$Lup

SIMBAD Objects

© ESO 2005