Expected oscillation parameters for red giants from dynamical masses and radii

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.