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Convection in stellar models

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Abstract

Convection has two main effects of interest to stellar modelers: It changes the stratification compared to a radiative or conductive region, and it mixes the matter efficiently. This was recognized early on, and a rudimentary description of convection was soon worked out—this is the familiar mixing length formulation. This paper will compare and contrast this much used formulation with results from realistic 3D simulations of interacting convection and radiation in the surface layers of stars. Due to space limitations, this review will be concerned with convective envelopes, only.

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  1. R. Trampedach

    Present address: JILA, University of Colorado, 440 UCB, Boulder, CO, 80309, USA

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  1. Research School of Astronomy and Astrophysics, Mt. Stromlo Observatory, Cotter Road, Weston, ACT 2611, Australia

    R. Trampedach

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Trampedach, R. Convection in stellar models. Astrophys Space Sci 328, 213–219 (2010). https://doi.org/10.1007/s10509-010-0329-7

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