Entropy in adiabatic regions of convection simulations

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.

arXiv commentAccepted for publication in ApJ Letters

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• The Radius and Entropy of a Magnetized, Rotating Fully-convective Star: Analysis With Depth-dependent Mixing Length Theories
• Key Issues Review: Numerical studies of turbulence in stars
• Improved calibration of the radii of cool stars based on 3D simulations of convection: implications for the solar model
• Stellar evolution models with entropy-calibrated mixing-length parameter: application to red giants
• The impact of the transport of chemicals and electronic screening on helioseismic and neutrino observations in solar models
• Simulating the outer layers of rapidly rotating stars