3D Hydrodynamical Simulations of Stellar Convection for Helio- and Asteroseismology
Abstract
Hydrodynamical simulations of stellar convection are an essential theoretical tool for gaining insight into the physics of mixing and heat transport by convection, and also into the interaction of convection with pulsation. They are particularly useful for obtaining an accurate description of the structure of the superadiabatic layer, which is important to explain the observed frequencies of $p$-modes in solar-like oscillating stars. The simulations can also be used to probe analytical models of excitation and damping of modes, and thus explain their amplitudes, and eventually the physical completeness of such models. This presentation discussed general challenges of such 3D hydrodynamical simulations developed for helio- and asteroseismology; it summarized some recent results in this field for the Sun, and which are also relevant to other lower main-sequence stars.
- Publication:
-
Stars and their Variability Observed from Space
- Pub Date:
- 2020
- Bibcode:
- 2020svos.conf..209K
- Keywords:
-
- convection;
- hydrodynamics;
- asteroseismology;
- turbulence;
- methods: numerical