Dynamical Asteroseismology: towards improving the theories of stellar structure and (tidal) evolution

Abstract

Abstract. The potential of the dynamical asteroseismology, the research area that builds upon the synergies between the asteroseismology and binary stars research fields, is discussed in this manuscript. We touch upon the following topics: i) the mass discrepancy observed in intermediate-to high-mass main-sequence and evolved binaries as well as in the low mass systems that are still in the pre-main sequence phase of their evolution; ii) the rotationally induced mixing in high-mass stars, in particular how the most recent theoretical predictions and spectroscopic findings compare to the results of asteroseismic investigations; iii) internal gravity waves and their potential role in the evolution of binary star systems and surface nitrogen enrichment in high-mass stars; iv) the tidal evolution theory, in particular how its predictions of spin-orbit synchronisation and orbital circularisation compare to the present-day high-quality observations; v) the tidally-induced pulsations and their role in the angular momentum transport within binary star systems; vi) the scaling relations between fundamental and seismic properties of stars across the entire HR-diagram.

Physical properties and CNO abundances for high-mass stars in four main-sequence detached eclipsing binaries: V478 Cyg, AH Cep, V453 Cyg and V578 Mon

“…The mass discrepancy for high-mass stars in binary systems is now a well-determined effect, which points to short-comings in modern evolutionary models. The inclusion of some extra mixing into the models allows to minimise the discrepancy between the dynamical and evolutionary masses of stars but, as stressed by Tkachenko (2017), the high overshooting values appear to be inconsistent with asteroseismological values known for single stars of similar masses. As already stressed in Sect.…”