Accretion disk in the binary system V367 Cygni

Free access article

Issue		A&A Volume 368, Number 3, March IV 2001


Page(s)		932 - 938
Section		Formation, structure and evolution of stars
DOI		http://dx.doi.org/10.1051/0004-6361:20010047

A&A 368, 932-938 (2001)
DOI: 10.1051/0004-6361:20010047

Accretion disk in the binary system V367 Cygni

S. Zola^{1, 2} and W. Ogloza^{2, 3}

¹ Astronomical Observatory of the Jagiellonian University, ul. Orla 171, 30-244 Cracow, Poland
² Mt. Suhora Observatory of the Pedagogical University, ul. Podchorazych 2, 30-084 Cracow, Poland
³ N. Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland

(Received 4 April 2000/ Accepted 2 January 2001 )

Abstract
New photoelectric observations of the interacting binary V367 Cyg were made during two consecutive seasons, 1996 and 1997, using the two-channel photometer at Mt. Suhora Observatory. The BVRI light curves are analyzed and system parameters are derived for two alternative models: with and without an accretion disk. A contact configuration is obtained for the no-disk model. The semidetached model, with a disk around the invisible component gives a better fit and, in addition, explains most of the observed features of V367 Cyg. The disk in V367 Cyg has a radius of about $R_{\rm d}=23 R_{\odot}$ , almost completely filling the secondary component's Roche lobe. Mass is transferred from the less massive ( $3.3 M_{\odot}$ ) to the more massive ( $4.0 M_{\odot}$ ) star at a high rate of 5-7 10-5} M_{\odot/yr.

Key words: binaries: eclipsing, accretion disks, individual: V367 Cyg

Offprint request: S. Zola, sfzola@cyf-kr.edu.pl

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