Volume 592, August 2016
|Number of page(s)||15|
|Section||Stellar structure and evolution|
|Published online||09 August 2016|
Asteroseismic modelling of the two F-type hybrid pulsators KIC 10080943A and KIC 10080943B
1 Institute for Astronomy, KU Leuven Celestijnenlaan 200D 3001 Leuven Belgium
2 Department of Astrophysics/IMAPP, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands
Received: 31 March 2016
Accepted: 22 May 2016
Context. Pulsating binary stars are ideal targets for testing the theory of stellar structure and evolution. Fundamental parameters can be derived to high precision from binary modelling and provide crucial constraints for seismic modelling. High-order gravity modes are sensitive to the conditions near the convective core and therefore allow for a determination of parameters describing interior physics, especially the convective-core overshooting parameter. KIC 10080943 is a binary system that contains two gravity- and pressure-mode hybrid pulsators. A detailed observational study has provided fundamental and seismic parameters for both components.
Aims. We aim to find a model that is able to predict the observed g-mode period spacings and stellar parameters of both components of KIC 10080943.
Methods. By calculating model grids with the stellar evolution code MESA and the seismic code GYRE, we can compare theoretical properties to the observed mean period spacing and position in the Hertzsprung-Russell diagram.
Results. The masses of our best models are somewhat below the values estimated from binarity, which is a consequence of the low observed mean g-mode period spacing. We find that the amount of core overshooting and diffusive mixing can be well constrained by the equal-age requirement for the two stars, however, we find no significant difference for different shapes of core overshooting. The measured rotation rates are within the limit of validity for the first-order perturbation approximation. We can find a good fit by using the traditional approximation for the pulsations, when taking slightly younger models with a higher asymptotic period spacing. This is because the zonal modes experience a slight shift due to the Coriolis force, which the first-order perturbation approximation ignores.
Key words: stars: individual: KIC 10080943 / binaries: spectroscopic / stars: oscillations / stars: evolution
© ESO, 2016
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