Dynamics of Turbulent Convection and Convective Overshoot in a Moderate Mass Star

TL;DR

This study uses 3D radiative hydrodynamic simulations to explore convection and overshoot in a 1.47 solar mass star, revealing complex surface granulation, a significant radius increase, and a two-layer overshoot region impacting stellar models.

Contribution

First detailed 3D simulation of convection and overshoot in a moderate mass star, showing new insights into the overshoot layer structure and its effects on stellar modeling.

Findings

Surface granulation spans 2-12 Mm with organized clusters.

Convective downdrafts reach speeds over 20 km/s and penetrate the radiative zone.

The overshoot region consists of an adiabatic extension and a deeper subadiabatic layer.

Abstract

Continued progress in observational stellar astrophysics requires a deep understanding of the underlying convection dynamics. We present results of realistic 3D radiative hydrodynamic simulations of the outer layers of a moderate mass star (1.47 Msun), including the full convection zone, the overshoot region, and the top layers of the radiative zone. The simulation results show that the surface granulation has a broad range of scales, from 2 to 12 Mm, and that large granules are organized in well-defined clusters, consisting of several granules. Comparison of the mean structure profiles from 3D simulations with the corresponding 1D standard stellar model shows an increase of the stellar radius by ~800 km, as well as significant changes in the thermodynamic structure and turbulent properties of the ionization zones. Convective downdrafts in the intergranular lanes between granulation clusters reach speeds of more than 20 km/s, penetrate through the whole convection zone, hit the radiative zone, and form a 8 Mm thick overshoot layer. Contrary to semi-empirical overshooting models, our results show that the 3D dynamic overshoot region consists of two layers: a nearly adiabatic extension of the convection zone and a deeper layer of enhanced subadiabatic stratification. This layer is formed because of heating caused by the braking of the overshooting convective plumes. This effect has to be taken into account in stellar modeling and the interpretation of asteroseismology data. In particular, we demonstrate that the 3D model can qualitatively explain deviations from the standard solar model found by helioseismology.