Volume 503, Number 3, September I 2009
|Page(s)||873 - 881|
|Section||Stellar structure and evolution|
|Published online||29 April 2009|
The triple system HIP 96515: a low-mass eclipsing binary with a DB white dwarf companion*
LAEX-CAB (INTA-CSIC); Postal address: LAEFF, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain e-mail: firstname.lastname@example.org
2 Depto. de Física, Universidade Federal de Minas Gerais, C.P.702, 30161-970 – Belo Horizonte, MG, Brazil
3 Laboratório Nacional de Astrofísica/MCT, Rua Estados Unidos 154, 37504-364 Itajubá, Brazil
4 Département de Physique, Université de Montréal, C.P. 6128, Succ. Centre-Ville, Montréal, Québec H3C 3J7, Canada
5 European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei Muenchen, Germany
6 European Southern Observatory, Alonso de Cordova 3107, Casilla 19, Santiago, Chile
7 Laboratoire d'Astrophysique, Observatoire de Grenoble, BP 53, 38041 Grenoble, Cedex 9, France
8 Instituto de Astrofísica de Canarias, C Vía Láctea, s/n, E38205 - La Laguna (Tenerife), Spain
Accepted: 27 January 2009
Context. HIP 96515 A is a double-lined spectroscopic binary included in the SACY catalog as a potential young star. It has a visual companion (CCDM 19371-5134 B, HIP 96515 B) at 86. If bound to the primary, the optical and infrared colors of this wide companion are consistent with those of a white dwarf.
Aims. We attempt to characterize the system HIP 96515 A&B by studying each of its components.
Methods. We analyzed spectroscopic and photometric observations of HIP 96515 A and its visual companion, HIP 96515 B. To confirm the system as a common proper-motion pair, we analyzed the astrometry of the components using high-angular resolution infrared observations obtained within a time span of two years, and archival astrometry.
Results. The high-resolution optical spectrum of HIP 96515 A was used to derive a mass ratio, , close to 0.9. The optical lightcurve of HIP 96515 A shows periodic variations with Porbital = 2.3456 days, revealing that HIP 96515 A is an eclipsing binary with preliminary orbital parameters of i = ± , and M1 = 0.59 ± 0.03 and M2 = 0.54 ± 0.03 , for the primary and secondary, respectively, at an estimated distance of 42 ± 3 pc. This is a new eclipsing binary with component masses below 0.6 . Multi-epoch observations of HIP 96515 A&B show that the system is a common proper-motion pair. The optical spectrum of HIP 96515 B is consistent with a pure helium atmosphere (DB) white dwarf. The comparison with evolutionary cooling sequence models provides = 19 126 ± 195 K, = 8.08, = 0.6, and a distance of ~46 pc. The estimated WD cooling age is ~100 Myr and the total age of the object (including the main-sequence phase) is ~400 Myr. Finally, if HIP 96515 A&B are coeval, and assuming a common age of ~400 Myr, the comparison of the masses of the eclipsing binary members with evolutionary tracks shows that they are underestimated by ~15% and 10%, for the primary and secondary, respectively.
Key words: stars: white dwarfs / stars: binaries: eclipsing / stars: individual: HIP 96515
© ESO, 2009
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