Volume 446, Number 2, February I 2006
|Page(s)||583 - 589|
|Section||Stellar structure and evolution|
|Published online||13 January 2006|
The new orbital elements and properties of Persei
Astronomical Institute of the Charles University, V Holešovič kách 2, 180 00 Praha 8, Czech Republic e-mail: [liba;hec]@sirrah.troja.mff.cuni.cz
2 Astronomical Institute, Academy of Sciences of the Czech Republic, Fričova 298, 251 65 Ondřejov, Czech Republic e-mail: [libich;hec;had;koubsky;skoda;slechta;katrienu]@sunstel.asu.cas.cz
3 Astronomical Institute, Academy of Sciences of the Czech Republic, Boční II/1401a, 141 31 Praha 4, Czech Republic e-mail: firstname.lastname@example.org
4 Dept. of Physics and Astronomy, University of Victoria, PO Box 3055, Victoria, B.C., V8W 3P6 Canada e-mail: email@example.com
5 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, 3001 Leuven, Belgium e-mail: [conny;katrienu]@ster.kuleuven.be
6 Department of Astrophysics, “Radboud University Nijmegen”, PO Box 9010, 6500 GL Nijmegen, The Netherlands
7 Royal Observatory of Belgium, Ringlaan 3, 1180 Brussel, Belgium e-mail: peter@ksb–orb.oma.be
8 Observatoire de la Côte d'Azur Département GEMINI, UMR 6203, 06304 Nice Cedex 4, France e-mail: mathias@obs–nice.fr
Accepted: 18 July 2005
A detailed analysis of a large collection of electronic spectra from three observatories, together with radial velocities published earlier, were used to derive a new ephemeris and improved orbital elements for the ε Per binary. Observations covering a time interval of about 37 000 days (101.3 years) can be reconciled with a constant orbital period of 1406916000004. The high orbital eccentricity of 0.5550.009 was also confirmed. New spectral observations confirm that there is a periodic variation of the systemic velocity. Together with new evidence from astrometric observations (also analyzed here), they confirm the existence of a third body in the system with an orbital period of about 9600 days (26.3 years), rather than 4156 days, as reported earlier. Application of the disentangling technique to the Hα spectra with good ratios did not allow detection of spectral lines of either the secondary or tertiary components. For plausible inclinations between 30° and 90°, the observed mass function implies a mass of the secondary , if a primary mass is adopted of 13.52.0 . Attempts to detect the third body via interferometric observations should continue in spite of this first negative result.
Key words: stars: early-type / stars: binaries: spectroscopic
© ESO, 2006
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