Volume 563, March 2014
|Number of page(s)||17|
|Section||Stellar structure and evolution|
|Published online||07 March 2014|
1 INAF – Osservatorio astronomico di Roma, via Frascati 33, 00040 Monteporzio C., Italy
2 Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany
3 Institut d’Astrophysique et Géophysique Université de Liège, Allée du 6 Aôut, 4000 Liège, Belgium
4 Korea Astronomy and Space Science Institute, 305-348 Daejeon, Korea
5 Erciyes University, Science Faculty, Astronomy and Space Sci. Dept., 38039 Kayseri, Turkey
6 Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA
7 Center for Exoplanets and Habitable Worlds, The Pennsylvania State University, University Park, PA 16802, USA
8 Department of Astronomy & Space Sciences, University of Ege, 35100 İzmir, Turkey
9 Instituut for Sterrenkunde, K.U. Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium
10 Center for High Angular Resolution Astronomy and Department of Physics and Astronomy, Georgia State University, PO Box 5060, Atlanta GA 30302-5060, USA
11 Astrophysics Group, Keele University, Staffordshire ST5 5BG, UK
Received: 18 October 2013
Accepted: 12 January 2014
Analysis of eclipsing binaries containing non-radial pulsators allows i) combining two different and independent sources of information on the internal structure and evolutionary status of the components and ii) studying the effects of tidal forces on pulsations. KIC 3858884 is a bright Kepler target whose light curve shows deep eclipses, complex pulsation patterns with pulsation frequencies typical of δ Sct, and a highly eccentric orbit. We present the result of the analysis of Kepler photometry and of high resolution phase-resolved spectroscopy. Spectroscopy yielded both the radial velocity curves and, after spectral disentangling, the primary-component effective temperature and metallicity, and line-of-sight projected rotational velocities. The Kepler light curve was analyzed with an iterative procedure that was devised to disentangle eclipses from pulsations and takes the visibility of the pulsating star into account during eclipses. The search for the best set of binary parameters was performed by combining the synthetic light curve models with a genetic minimization algorithm, which yielded a robust and accurate determination of the system parameters. The binary components have very similar masses (1.88 and 1.86 M⊙) and effective temperatures (6800 and 6600 K), but different radii (3.45 and 3.05 R⊙). The comparison with the theoretical models showed a somewhat different evolutionary status of the components and the need to introduce overshooting in the models. The pulsation analysis indicates the hybrid nature of the pulsating (secondary) component, where the corresponding high order g-modes might be excited by an intrinsic mechanism or by tidal forces.
Key words: binaries: eclipsing / binaries: spectroscopic / stars: fundamental parameters / stars: interiors / stars: oscillations / stars: individual: KIC 3858884
Full Table B.1 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/563/A59
Appendices are available in electronic form at http://www.aanda.org
© ESO, 2014
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