| Issue |
A&A
Volume 368, Number 3, March IV 2001
|
|
|---|---|---|
| Page(s) | 932 - 938 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361:20010047 | |
| Published online | 15 March 2001 | |
Accretion disk in the binary system V367 Cygni*
1
Astronomical Observatory of the Jagiellonian University, ul. Orla 171, 30-244 Cracow, Poland
2
Mt. Suhora Observatory of the Pedagogical University, ul. Podchorążych 2, 30-084 Cracow, Poland
3
N. Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland
Corresponding author: S. Zoła, sfzola@cyf-kr.edu.pl
Received:
4
April
2000
Accepted:
2
January
2001
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 
, almost
completely filling the secondary component's Roche lobe.
Mass is transferred from the less massive (
) to the more massive
(
) star at a high rate of 5-7 10-5} M_{\odot/yr.
Key words: binaries: eclipsing, accretion disks, individual: V367 Cyg
© ESO, 2001
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