Dr. Anya Samadi
For stars located in the overlap region of the γ Dor and the δ Scuti instability strips, we expect to find both low- (g) and high-frequency (p) pulsation modes. The hybrid pulsators provide information from the surface ( p modes) as well as from the near-core regions (g modes). When such a pulsator is part of an eclipsing binary (and/or a double-lined spectroscopic binary), the situation becomes even more favorable for a deep analysis: by means of light curve (spectrum) modeling of the system’s properties, one can obtain model-independent and (more) accurately determined fundamental stellar parameters (than in the case of single stars), therefore more reliable constraints for stellar models. Additionally, the information derived from a detailed pulsation study (i.e. νmax, ∆ν and individ- ual pulsation frequencies) can be associated to fundamental stellar parameters like the mean stellar density ρ (e.g. Suárez 2014). These two independent approaches (a light curve analysis and its associated binary modeling to determine the component properties and the complementary frequency analysis of the residual light curve) allow to revisit the stellar evolution models, in connection with the asteroseismic modeling.