Physical processes leading to surface inhomogeneities: the case of rotation
Michel Rieutord
TL;DR
This paper explores the physical mechanisms behind surface inhomogeneities in rotating stars, focusing on gravity darkening, and presents a detailed derivation of the omega-model for early-type stars, also discussing effects in convective and binary stars.
Contribution
It provides a comprehensive derivation of the omega-model for gravity darkening in early-type stars and discusses extensions to convective and binary star systems.
Findings
Derivation of the omega-model for gravity darkening
Analysis of gravity darkening in convective envelope stars
Discussion of gravity darkening in binary systems
Abstract
In this lecture I discuss the bulk surface heterogeneity of rotating stars, namely gravity darkening. I especially detail the derivation of the omega-model of Espinosa Lara & Rieutord (2011), which gives the gravity darkening in early-type stars. I also discuss the problem of deriving gravity darkening in stars owning a convective envelope and in those that are members of a binary system.
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