EDP Sciences
Free access
Volume 405, Number 3, July III 2003
Page(s) 1087 - 1093
Section Stellar atmospheres
DOI http://dx.doi.org/10.1051/0004-6361:20030725

A&A 405, 1087-1093 (2003)
DOI: 10.1051/0004-6361:20030725

Basic physical properties of the close binary V497 Cep in the open cluster NGC 7160

K. Yakut1, A. E. Tarasov2, 3, C. Ibanoglu1, P. Harmanec4, 5, B. Kalomeni1, D. E. Holmgren6, 7, H. Bozic8 and P. Eenens9

1  University of Ege, Faculty of Science, Department of Astronomy and Space Sciences, 35100 Bornova, Izmir, Turkey
2  Crimean Astrophysical Observatory, 98409 Nauchny, Crimea, Ukraine
3  Isaac Newton Institute of Chile, Crimean Branch, 98409 Nauchny, Crimea, Ukraine
4  Astronomical Institute of the Charles University, V Holesovickách 2, 180 00 Praha 8, Czech Republic
5  Astronomical Institute of the Academy of Sciences, 251 65 Ondrejov, Czech Republic
6  SMART Technologies, Inc., Bay 8, 1460 - 28 Street NE, Calgary, Alberta, T2A 7W6, Canada
7  Dominion Astrophysical Observatory, Canada
8  Hvar Observatory, Faculty of Geodesy, Zagreb University, Kaciceva 26, 10000 Zagreb, Croatia
9  Departamento de Astronomia, Universidad de Guanajuato, Apartado 144, 36000 Guanajuato, GTO, Mexico

(Received 28 March 2003 / Accepted 6 May 2003)

New light and radial-velocity curves of $\!$, a binary in the open cluster NGC 7160, were obtained and the linear ephemeris of the system was refined to ${\rm HJD \, (Min\, I)} =
(2\,446 \,299.1596\pm0.0064) + (1\fd2028287\pm0\fd0000015) \times
E$ . The first light and radial-velocity curve solutions allowed us to derive the basic physical properties of this astrophysically important binary. It was found that the observed light variation of consists of a strong ellipticity effect and a small contribution from grazing eclipses. A comparison of masses and radii of with theoretical evolutionary tracks indicates that both binary components are very close to the zero-age main sequence. A comparison of disentangled line profiles of the He I 6678 line with synthetic, rotationally broadened line profiles indicates that the rotation of both stars is synchronized with the orbital revolution as expected. This finding increases the credibility of our solutions. We find $E(B-V)=0\fm39$. The distance to the cluster NGC 7160 was found to be about 760 ( $\pm$ 100) pc which agrees well with other available estimates.

Key words: stars: binaries: eclipsing -- stars: binaries: spectroscopic -- stars: individual: -- Galaxy: open clusters and associations: individual: NGC 7160

Offprint request: K. Yakut, yakut@astronomy.sci.ege.edu.tr

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