The Effect of Convection on Solar-type Pulsations

I shall provide an overview of our current understanding of modelling energy exchange between stellar convection and acoustic oscillations in stars supporting solar-type pulsations. Stellar calculations, adopting a 1D, non-local, time-dependent convection model, are calibrated against seismic observations and 3D-simulation results. These stellar models are tested against data from the Sun and from Kepler main-sequence stars. This provides insight into the physical processes that determine energy transport in the outer stellar layers leading to more accurate calculations of pulsation frequencies and their damping rates, as well as to more realistic predictions of oscillation amplitude ratios and phases.