Stochastic excitation of acoustic modes in stars

TL;DR

This paper reviews models of stochastic excitation of solar-like oscillations in stars, highlighting how turbulence, stratification, and metallicity influence mode excitation and how seismic data inform stellar convection properties.

Contribution

It provides a comprehensive comparison of theoretical models for stochastic excitation, emphasizing the impact of convection modeling and stellar parameters on mode excitation rates.

Findings

Mode excitation rates depend on turbulent convection modeling.

Seismic data can infer properties of stellar turbulent convection.

Stratification and metallicity significantly influence oscillation excitation.

Abstract

For more than ten years, solar-like oscillations have been detected and frequencies measured for a growing number of stars with various characteristics (e.g. different evolutionary stages, effective temperatures, gravities, metal abundances ...). Excitation of such oscillations is attributed to turbulent convection and takes place in the uppermost part of the convective envelope. Since the pioneering work of Goldreich & Keely (1977), more sophisticated theoretical models of stochastic excitation were developed, which differ from each other both by the way turbulent convection is modeled and by the assumed sources of excitation. We review here these different models and their underlying approximations and assumptions. We emphasize how the computed mode excitation rates crucially depend on the way turbulent convection is described but also on the stratification and the metal abundance of the upper layers of the star. In turn we will show how the seismic measurements collected so far allow us to infer properties of turbulent convection in stars.