3D stellar atmospheres for stellar structure models and asteroseismology

TL;DR

This paper reviews the use of 3D numerical simulations of stellar surface convection to improve understanding of stellar atmospheres, their role in stellar structure models, and their application in helio- and asteroseismology.

Contribution

It analyzes the principles, requirements, and uncertainties of 3D stellar atmosphere models and discusses their integration into stellar structure and evolution theories.

Findings

Comparison of solar surface simulations from different teams.

Discussion of uncertainties in 3D stellar atmosphere modeling.

Assessment of 3D models in reducing stellar modeling uncertainties.

Abstract

Convection is the most important physical process that determines the structure of the envelopes of cool stars. It influences the surface radiation flux and the shape of observed spectral line profiles and is responsible for both generating and damping solar-like oscillations, among others. 3D numerical simulations of stellar surface convection have developed into a powerful tool to model and analyse the physical mechanisms operating at the surface of cool stars. This review discusses the main principles of 3D stellar atmospheres used for such applications. The requirements from stellar structure and evolution theory to use them as boundary conditions are analysed as well as the capabilities of using helio- and asteroseismology to reduce modelling uncertainties and probing the consistency and accuracy of 3D stellar atmospheres as part of this process. Simulations for the solar surface made by different teams are compared and some issues concerning the uncertainties of this modelling approach are discussed.