Details

Autor(en) / Beteiligte

• Schmid, V. S.
• Tkachenko, A.
• Aerts, C.
• Degroote, P.
• Bloemen, S.
• Murphy, S. J.
• Van Reeth, T.
• Pápics, P. I.
• Bedding, T. R.
• Keen, M. A.
• Prša, A.
• Menu, J.
• Debosscher, J.
• Hrudková, M.
• De Smedt, K.
• Lombaert, R.
• Németh, P.

Titel

KIC 10080943: An eccentric binary system containing two pressure- and gravity-mode hybrid pulsators

Ist Teil von

• Astronomy and astrophysics (Berlin), 2015-12, Vol.584, p.A35

Ort / Verlag

EDP Sciences

Erscheinungsjahr

2015

Link zum Volltext

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• Context. γ Doradus and δ Scuti pulsators cover the transition region between low mass and massive main-sequence stars, and as such, are critical for testing stellar models. When they reside in binary systems, we can combine two independent methods to derive critical information, such as precise fundamental parameters to aid asteroseismic modelling. In the Kepler light curve of KIC 10080943, clear signatures of gravity- and pressure-mode pulsations have been found. Ground-based spectroscopy revealed this target to be a double-lined binary system. Aims. We present the analysis of four years of Kepler photometry and high-resolution spectroscopy to derive observational constraints with which to evaluate theoretical predictions of the stellar structure and evolution for intermediate-mass stars. Methods. We used the method of spectral disentangling to determine atmospheric parameters for both components and derive the orbital elements. With phoebe, we modelled the ellipsoidal variation and reflection signal of the binary in the light curve and used classical Fourier techniques to analyse the pulsation modes. Results. We show that the eccentric binary system KIC 10080943 contains two hybrid pulsators with masses M1 = 2.0 ± 0.1 M⊙ and M2 = 1.9 ± 0.1 M⊙, with radii R1 = 2.9 ± 0.1 R⊙ and R2 = 2.1 ± 0.2 R⊙. We detect rotational splitting in the g and p modes for both stars and use them to determine a first rough estimate of the core-to-surface rotation rates for the two components, which will be improved by future detailed seismic modelling.