Abstract

Eclipsing systems are essential objects for understanding the properties of stars and stellar systems. Eclipsing systems with pulsating components are furthermore advantageous because they provide accurate constraints on the component properties, as well as a complementary method for pulsation mode determination, crucial for precise asteroseismology. The outcome of space missions aiming at delivering high-accuracy light curves for many thousands of stars in search of planetary systems has also generated new insights in the field of variable stars and revived the interest of binary systems in general. The detection of eclipsing systems with pulsating components has particularly benefitted from this, and progress in this field is growing fast. In this review, we showcase some of the recent results obtained from studies of eclipsing systems with pulsating components based on data acquired by the space missions Kepler or TESS. We consider different system configurations including semi-detached eclipsing binaries in (near-)circular orbits, a (near-)circular and non-synchronized eclipsing binary with a chemically peculiar component, eclipsing binaries showing the heartbeat phenomenon, as well as detached, eccentric double-lined systems. All display one or more pulsating component(s). Among the great variety of known classes of pulsating stars, we discuss unevolved or slightly evolved pulsators of spectral type B, A or F and red giants with solar-like oscillations. Some systems exhibit additional phenomena such as tidal effects, angular momentum transfer, (occasional) mass transfer between the components and/or magnetic activity. How these phenomena and the orbital changes affect the different types of pulsations excited in one or more components, offers a new window of opportunity to better understand the physics of pulsations.

Highlights

  • Eclipsing systems are essential objects for understanding the properties of stars and stellar systems in general

  • The discrepancy is due to a combination of (i) the presence of pulsations that are commensurate with the orbital period and (ii) the precision of the Kepler data illustrating the need for improved limb darkening coefficients and albedo’s

  • Since the equilibrium tide of a close binary system with a circular orbit leads to equidistant frequency splitting of an excited mode by the orbital frequency according to theoretical predictions [46,47,48], the frequency multiplets in the p-mode region can be interpreted as tidally split p modes, similar to the conclusion of Guo et al [49] during the pulsation study of KIC 9851944

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Summary

Introduction

Eclipsing systems are essential objects for understanding the properties of stars and stellar systems in general. Eclipsing binary (EB) systems with pulsating components are advantageous because they provide accurate constraints on the component properties, as well as a complementary method for pulsation mode determination (during the eclipses), crucial for precise asteroseismology. They may undergo a series of phenomena which are due to the (possibly strong) gravitational forces acting on the components, which in turn can influence the stellar pulsations. To maintain the focus on the kinds of interactions that can occur between the gravitational forces in the systems on the one hand and the pulsations of their constituents on the other hand, we restricted our article selection to EB systems with either a main-sequence or slightly evolved pulsating component of spectral type B, A or F, or with a pulsating red giant star

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