Linking 1D Stellar Evolution to 3D Hydrodynamical Simulations

TL;DR

This paper investigates convective boundary mixing in massive stellar models using the GENEVA code, providing initial insights that inform future 3D hydrodynamical simulations and impact understanding of stellar phenomena.

Contribution

It offers the first analysis of convective boundary properties in massive stars, highlighting differences in boundary stiffness that influence mixing processes.

Findings

Lower boundaries are 'stiffer' than upper boundaries based on the bulk Richardson number.

Reduced convective boundary mixing is expected at lower boundaries.

Implications for flame propagation and nova onset are discussed.

Abstract

In this contribution we present initial results of a study on convective boundary mixing (CBM) in massive stellar models using the GENEVA stellar evolution code. Before undertaking costly 3D hydrodynamic simulations, it is important to study the general properties of convective boundaries, such as the: composition jump; pressure gradient; and `stiffness'. Models for a 15Mo star were computed. We found that for convective shells above the core, the lower (in radius or mass) boundaries are `stiffer' according to the bulk Richardson number than the relative upper (Schwarzschild) boundaries. Thus, we expect reduced CBM at the lower boundaries in comparison to the upper. This has implications on flame front propagation and the onset of novae.