Entropy in adiabatic regions of convection simulations

TL;DR

This paper demonstrates that the entropy in the deep, adiabatic layers of stellar convection simulations can be described by a simple function of gravity and effective temperature, aiding in better stellar model calibration.

Contribution

It introduces a straightforward relation for entropy in adiabatic regions of convection simulations, improving the calibration process for stellar models.

Findings

Entropy can be expressed as a simple function of g and log T_eff.

This relation offers a potential method for calibrating stellar models.

The approach simplifies the connection between 3D simulations and 1D models.

Abstract

One of the largest sources of uncertainty in stellar models is caused by the treatment of convection in stellar envelopes. One dimensional stellar models often make use of the mixing length or equivalent approximations to describe convection, all of which depend on various free parameters. There have been attempts to rectify this by using 3D radiative-hydrodynamic simulations of stellar convection, and in trying to extract an equivalent mixing length from the simulations. In this paper we show that the entropy of the deeper, adiabatic layers in these simulations can be expressed as a simple function of og g and log T_{eff} which holds potential for calibrating stellar models in a simple and more general manner.