Forum Springer Astron. Astrophys.
Forum Whats New Search Orders

Astron. Astrophys. 317, 823-831 (1997)

Table of Contents
Available formats: HTML | PDF | (gzipped) PostScript

The strongly constrained interacting binary BY Crucis *

K. Daems ** 1, C. Waelkens 1 and M. Mayor 2

1 Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200B, B-3001 Heverlee, Belgium
2 Geneva Observatory, 51 Chemin des Maillettes, CH-1290 Sauverny, Switzerland

Received 26 April 1996 / Accepted 13 June 1996


We discuss spectroscopic and photometric observations (UV to IR) of BY Crucis, a new bright member of the interacting binaries of the W Serpentis class. The orbital period is 106.4 days, and the mass function amounts to 5.92  [FORMULA]. The primary is an early-F supergiant which fills its Roche lobe; the massive secondary is hidden inside a thick accretion disk, which is probably the dominant light source in the ultraviolet. The observed variations in the photometric lightcurves are caused mainly by ellipsoidal variations. It is unlikely that an eclipse occurs.

A particularly interesting circumstance is that BY Cru is a probable member of a visual multiple system which contains another evolved star. This circumstance enables us to estimate with some accuracy the age of the interacting binary and the initial mass of the primary. The history of this binary is then much more constrained than for the other W Serpentis stars. Also taking into account the fact that the binary has avoided Case C Roche lobe overflow, we determine upper and lower bounds for the initial and present masses of both components, and conclude that mass transfer has only been moderately non-conservative.

Key words: binaries: close – circumstellar matter – stars: evolution – stars: individual: BY Cru

* Based on observations obtained at the European Southern Observatory, La Silla, Chile; and at the Swiss Telescope, La Silla, Chile
** Research Assistant of the Belgian National Fund for Scientific Research

Send offprint requests to: K. Daems, Leuven

© European Southern Observatory (ESO) 1997

Online publication: July 8, 1998