3D hydrodynamic simulations of massive main-sequence stars. III. The effect of radiation pressure and diffusion leading to a 1D equilibrium model

• Published in: arXiv.org
• Main Authors: Mao, Huaqing, Woodward, Paul, Falk Herwig, Denissenkov, Pavel A, Blouin, Simon, Thompson, William, McDermott, Benjamin
• Format: Paper
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 09.08.2024
• Subjects: Convection; Diffusion effects; Diffusion rate; Entrainment; Gravity waves; Heating rate; Main sequence stars; Pressure effects; Radiation; Radiation effects; Radiation pressure; Simulation; Stellar evolution; Thermal diffusion; Three dimensional models; Time
• ISSN: 2331-8422

We present 3-D hydrodynamical simulations of core convection with a stably stratified envelope of a \unit{25}{\Msun} star in the early phase of the main-sequence. We use the explicit gas-dynamics code \code{PPMstar} which tracks two fluids and includes radiation pressure and radiative diffusion. Multiple series of simulations with different luminosities and radiative thermal conductivities are presented. The entrainment rate at the convective boundary, internal gravity waves in and above the boundary region, and the approach to dynamical equilibrium shortly after a few convective turnovers are investigated. We perform very long simulations on \(896^3\) grids accelerated by luminosity boost factors \(1000\), \(3162\) and \(10000\). In these simulations the growing penetrative convection reduces the initially unrealistically large entrainment. This reduction is enabled by a spatial separation that develops between the entropy gradient and the composition gradient. The convective boundary moves outward much more slowly at the end of these simulations. Finally, we present a 1-D method to predict the extent and character of penetrative convection beyond the Schwarzschild bounxdary. The 1-D model is based on a spherically-averaged reduced entropy equation that takes the turbulent dissipation as input from the 3-D hydrodynamic simulation and takes buoyancy and all other energy sources and sinks into account. This 1-D method is intended to be ultimately deployed in 1-D stellar evolution calculations and is based on the properties of penetrative convection in our simulations carried forward through the local thermal timescale.