Datensatz

Zusammenfassung

Stellar masses and radii of stars with stochastic (solar-like) oscillations can be derived using asteroseismic scaling relations. Here, we predict the asteroseismic observables using the dynamical masses and radii from red-giants in eclipsing binary systems. We show that the predicted frequency of maximum oscillation power (ν_max) is generally lower than the observed one, while the predicted large frequency separation (Δν) is in most cases larger than the observed value. This shows that both the scaling relations for Δν and ν_max used with solar references contribute to the observed differences between dynamical and asteroseismically determined masses and radii.