Testing tidal theory for evolved stars by using red-giant binaries observed by Kepler

TL;DR

This study tests tidal theories in evolved stars using Kepler-observed red-giant binaries, confirming that equilibrium tide dissipation dominates over dynamical tide dissipation during the red-giant phase, impacting stellar evolution models.

Contribution

It applies equilibrium-tide formalism to a comprehensive Kepler red-giant binary sample, confirming the dominance of equilibrium tide dissipation and refining understanding of stellar evolution.

Findings

Equilibrium tide dissipation explains observed binary characteristics.

Dynamical tide dissipation is weak during the red-giant phase.

Eccentricity is not a reliable indicator of evolutionary state.

Abstract

Tidal interaction governs the redistribution of angular momentum in close binary stars and planetary systems and determines the systems evolution towards the possible equilibrium state. Turbulent friction acting on the equilibrium tide in the convective envelope of low-mass stars is known to have a strong impact on this exchange of angular momentum in binaries. Moreover, theoretical modelling in recent literature as well as presented in this paper suggests that the dissipation of the dynamical tide, constituted of tidal inertial waves propagating in the convective envelope, is weak compared to the dissipation of the equilibrium tide during the red-giant phase. This prediction is confirmed when we apply the equilibrium-tide formalism developed by Zahn (1977), Verbunt & Phinney (1995), and Remus, Mathis & Zahn (2012) onto the sample of all known red-giant binaries observed by the NASA Kepler mission. Moreover, the observations are adequately explained by only invoking the equilibrium tide dissipation. Such ensemble analysis also benefits from the seismic characterisation of the oscillating components and surface rotation rates. Through asteroseismology, previous claims of the eccentricity as an evolutionary state diagnostic are discarded. This result is important for our understanding of the evolution of multiple star and planetary systems during advanced stages of stellar evolution.