Improvements to stellar structure models, based on a grid of 3D convection simulations. II. Calibrating the mixing-length formulation

TL;DR

This paper calibrates the mixing-length parameter in stellar models using 3D hydrodynamics simulations, revealing how it varies across different stellar types and evolutionary stages, improving the accuracy of stellar structure modeling.

Contribution

It provides a detailed calibration of the mixing-length parameter against 3D simulations for a range of stellar types, enhancing stellar evolution models.

Findings

The mixing-length parameter varies from 1.6 to 2.05 across the stellar grid.

The Sun's mixing-length parameter is on the typical plateau, showing little evolution.

Stars on the giant branch follow tracks of nearly constant mixing-length parameter.

Abstract

We perform a calibration of the mixing length of convection in stellar structure models against realistic 3D radiation-coupled hydrodynamics (RHD) simulations of convection in stellar surface layers, determining the adiabat deep in convective stellar envelopes. The mixing-length parameter $\alpha$ is calibrated by matching averages of the 3D simulations to 1D stellar envelope models, ensuring identical atomic physics in the two cases. This is done for a previously published grid of solar-metallicity convection simulations, covering from 4200 K to 6900 K on the main sequence, and 4300-5000 K for giants with logg=2.2. Our calibration results in an $\alpha$ varying from 1.6 for the warmest dwarf, which is just cool enough to admit a convective envelope, and up to 2.05 for the coolest dwarfs in our grid. In between these is a triangular plateau of $\alpha$ ~ 1.76. The Sun is located on this plateau and has seen little change during its evolution so far. When stars ascend the giant branch, they largely do so along tracks of constant $\alpha$, with $\alpha$ decreasing with increasing mass.