Pulsational characteristics of mass accreting stars in close binary systems

Eclipsing binaries with pulsating components constitute a unique subclass of binary systems, combining insights from both orbital dynamics and stellar pulsations. These systems have recently given rise to the emerging field of tidal asteroseismology. While pulsations in single stars are relatively well understood, their counterparts in binary systems pose new challenges. In particular, the effects of binarity—especially mass transfer—on the oscillation properties of stellar components remain largely unexplored. This is especially true for stars that gain mass during their evolution. Eclipsing binaries serve as crucial benchmarks for testing stellar evolution theory, offering precise stellar parameters that enable accurate age estimates and reconstruction of evolutionary histories.In this context, we present results from studies of a 10Ms Cephei-type pulsator in a binary system, focusing on the asteroseismic properties of mass-accreting models. We investigate how mass accretion modifies the internal structure, including changes in the density and sound speed profiles, and how these changes influence the pulsation spectrum. Our models reveal systematic deviations in both g- and p-mode frequencies compared to single-star counterparts, highlighting the sensitivity of stellar oscillations to past binary interactions. These findings provide a new perspective on asteroseismology in binary systems and emphasize the need to account for mass transfer history when interpreting pulsation spectra.