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Modelling the binary F-type g-mode pulsator KIC10080943
Valentina Schmid (Institute for Astronomy, KU Leuven)
Pulsating binary stars are ideal targets for testing the theory of stellar structure and evolution. Fundamental parameters can be derived from binary modelling to high precision 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, which contains two gravity and pressure hybrid pulsators. A detailed observational study has provided fundamental and seismic parameters for both components. In our study, we have used the stellar evolution code MESA and the seismic code GYRE, to compare theoretical properties to the observed mean period spacing and position in the Hertzsprung-Russell diagram. Additional constraints imposed by the binarity, are the mass ratio, equal age and composition. We present here the first consistent seismic modelling of a binary F-type g-mode pulsator. Our best models have masses below the values estimated from binarity, which is a consequence of the low observed mean g-mode period spacing. We find that strength of overshooting and turbulent diffusion can be well constrained by the equal-age requirement for the two stars. However, we find no significant difference for different shapes of the overshooting. Furthermore, when we aim to explain the morphology of the period spacing pattern, we lose the agreement with the binary parameters. Our models present a fruitful starting point for more detailed studies, which also take the tidal interactions into account.