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Astron. Astrophys. 319, 867-880 (1997)


Table of Contents
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Search for forced oscillations in binaries

I. The eclipsing and spectroscopic binary V 436 Persei [FORMULA] 1 Persei * **

P. Harmanec 1, P. Hadrava 1, S. Yang 2, D. Holmgren 1, P. North 3, P. Koubský 1, J. Kubát 1 and E. Poretti 4

1 Astronomický ústav Akademie v d eské republiky, 251 65 Ond ejov, Czech Republic (hec(had, david, koubsky, kubat)@sunstel.asu.cas.cz)
2 Department of Physics and Astronomy, University of Victoria, P.O. Box 3055, Victoria, B.C., V8W 3P6, Canada (yang@uvastro.phys.uvic.ca)
3 Institut d'Astronomie de l'Université de Lausanne, CH-1290 Chavannes-des-Bois, Switzerland (Pierre.North@obs.unige.ch)
4 Osservatorio Astronomico, Via E. Bianchi 46, I-22055 Merate (CO), Italy (poretti@merate.mi.astro.it)

Received 20 May 1996 / Accepted 21 August 1996

Abstract

Outline of a project aimed at testing the presence of rapid line-profile variations in the atmospheres of hot components of close binaries is presented and its first results are described. An analysis of new electronic spectra of the eclipsing binary V436 Per from three observatories and of photoelectric observations, obtained earlier by several authors, leads to a unique determination of all basic physical elements of this interesting object. The first practical application of a new method of spectral disentangling allowed us to obtain, for the first time, individual accurate line profiles of both binary components and to derive their rotational velocities and orbital radial-velocity curves. We also detected absorption sub-features travelling from blue to red accross the He I  6678 line profile, in a series of six spectra taken during one night. At least one of the components of V436 Per is, therefore, a new hot line-profile variable.

Key words: stars: binaries: eclipsing – stars: binaries: spectroscopic – stars: fundamental parameters – stars: oscillations – stars: individual: V436 Per 1 Per

* This research is based on spectra from the Dominion Astrophysical, Ond ejov, and Haute Provence Observatories
** Table 3 is only available in electronic form at CDS via anonymous ftp 130.79.128.5 or via http:/cdsweb.u-strasbg.fr/Abstract.html

Send offprint requests to: P. Harmanec

© European Southern Observatory (ESO) 1997

Online publication: July 3, 1998

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