| Issue |
A&A
Volume 472, Number 2, September III 2007
|
|
|---|---|---|
| Page(s) | 587 - 598 | |
| Section | Stellar atmospheres | |
| DOI | https://doi.org/10.1051/0004-6361:20067015 | |
| Published online | 09 July 2007 | |
Multiwavelength optical observations of chromospherically active binary systems*,**
V. FF UMa (2RE J0933+624): a system with orbital period variation
1
Departamento de Astrofísica, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, 28040 Madrid, Spain e-mail: mcz@astrax.fis.ucm.es
2
Department of Astronomy, University of Florida, Gainesville, FL 32611, USA
Received:
22
December
2006
Accepted:
31
May
2007
Context.This is the fifth paper in a series aimed at studying the chromospheres of active binary systems using several optical spectroscopic indicators to obtain or improve orbital solution and fundamental stellar parameters.
Aims.We present here the study of FF UMa (2RE J0933+624), a recently discovered, X-ray/EUV selected, active binary with strong Hα emission. The objectives of this work are, to find orbital solutions and define stellar parameters from precise radial velocities and carry out an extensive study of the optical indicators of chromospheric activity.
Methods.We obtained high resolution echelle spectroscopic observations during five observing runs from 1998 to 2004. We found radial velocities by cross correlation with radial velocity standard stars to achieve the best orbital solution. We also measured rotational velocity by cross-correlation techniques and have studied the kinematic by galactic space-velocity components (U, V, W) and Eggen criteria. Finally, we have determined the chromospheric contribution in optical spectroscopic indicators, from Ca ii H & K to Ca ii IRT lines, using the spectral subtraction technique.
Results.We have found that this system presents an orbital period variation,
higher than previously detected in other RS CVn systems. We determined
an improved orbital solution, finding a circular orbit with a
period of 3.274 days. We derived the stellar parameters, confirming
the subgiant nature of the primary component (MP = 1.67
and 
) and
obtained rotational velocities (
), of
km s-1 and
km s-1 for the primary and secondary
components respectively.
From our kinematic study, we can deduce its membership to
the Castor moving group.
Finally, the activity study has given us a
better understanding of the possible mechanisms that
produce the orbital period variation.
Key words: stars: activity / stars: binaries: spectroscopic / stars: chromospheres / stars: late-type
Based on observations collected with the 2.2 m telescope at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto (Almería, Spain), operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC); with the Nordic Optical Telescope (NOT), operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway and Sweden, in the Spanish Observatorio del Roque de Los Muchachos of the Instituto de Astrofísica de Canarias; with the 2.1 m Otto Struve Telescope at McDonald Observatory of the University of Texas at Austin (USA) and with Hobby-Eberly Telescope, which is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universität München, and Georg-August-Universität Göttingen.
© ESO, 2007
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