Modeling Radial Velocities and Eclipse Photometry of the Kepler Target KIC 4054905: an Oscillating Red Giant in an Eclipsing Binary

TL;DR

This paper investigates the accuracy of asteroseismic relations for red giants by analyzing an eclipsing binary system with a red giant component, comparing dynamical and seismic measurements.

Contribution

It demonstrates a method to test asteroseismic mass and radius estimates using eclipsing binary systems with red giants.

Findings

Identified 16 suitable eclipsing binary systems with red giants.

Illustrated the approach on one system to compare dynamical and seismic parameters.

Highlights the importance of calibrating seismic relations for red giants.

Abstract

Asteroseismology is a powerful tool to measure the fundamental properties of stars and probe their interiors. This is particularly efficient for red giants because their modes are well detectable and give information on their deep layers. However, the seismic relations used to infer the mass and radius of a star have been calibrated on the Sun. Therefore, it is crucial to assess their accuracy for red giants which are not perfectly homologous to it. We study eclipsing binaries with a giant component to test their validity. We identified 16 systems for which we intend to compare the dynamical masses and radii obtained by combined photometry and spectroscopy to the values obtained from asteroseismology. In the present work, we illustrate our approach on a system from our sample.