EDP Sciences
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Volume 404, Number 2, June III 2003
Page(s) 611 - 620
Section Stellar atmospheres
DOI http://dx.doi.org/10.1051/0004-6361:20030489

A&A 404, 611-620 (2003)
DOI: 10.1051/0004-6361:20030489

Spectroscopic and photometric observations of the short-period RS CVn-type star ER Vulpeculae

D. P. Kjurkchieva1, D. V. Marchev1 and S. Zola2, 3

1  Department of Physics, Shoumen University, 9700 Shoumen, Bulgaria and Isaac Newton Institute of Chile, Bulgarian Branch
    e-mail: d.kyurkchieva@shu-bg.net; d.marchev@shu-bg.net
2  Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244 Cracow, Poland
3  Mt. Suhora Observatory of the Pedagogical University, ul. Podchorazych 2, 30-084 Cracow, Poland

(Received 10 September 2002 / Accepted 25 March 2003)

Spectroscopic observations around the H $_{\alpha}$ line and BVR photometry of the eclipsing, short-period, RS CVn-type star ER Vul are presented. The solutions of new radial velocity and light curves yielded the following masses and radii of the components: $M_{\rm 1}=1.16$ $M_{\odot}$, $M_{\rm 2}=1.05$ $M_{\odot}$, $R_{\rm 1}=1.25$ $R_{\odot}$, $R_{\rm 2}=1.12$ $R_{\odot}$. The equatorial velocities corresponding to the measured rotational broadenings of the spectral lines are: $V_{\rm
eq}^{\rm 1}=90$  km s -1 and $V_{\rm eq}^{\rm 2}=80$ km s -1. Their ratio is just equal to the ratio of the stellar radii. We detected excess emission in the H $_{\alpha}$ and CaI 6494 lines that changes during the orbital cycle. Our spectral data show the presence of absorbing matter around the mass center of the system.

Key words: stars: activity -- binaries: eclipsing -- binaries: spectroscopic -- stars: chromospheres -- stars: individual: ER Vul -- stars: starspots

Offprint request: S. Zola, zola@astro1.as.wsp.krakow.pl

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