Modeling rotating stars in two dimensions

Abstract

In this lecture I present the way stars can be modeled in two dimensions and especially the fluid flows that are driven by rotation. I discuss some of the various ways of taking into account turbulence and conclude this contribution by a short presentation of some of the first results obtained with the ESTER code on the modeling of interferometrically observed fast rotating early-type stars.

16 pages, 2 fig. to appear in Proceedings of the Evry Schatzman School 2012 of PNPS and CNRS/INSU on the "Role and mechanisms of angular momentum transport during the formation and early evolution of stars", Eds. P.Hennebelle & C.Charbonnel

References in corpus (9)

• Acoustic oscillations of rapidly rotating polytropic stars. II. Effects of the Coriolis and centrifugal accelerations
• Resolving Vega and the inclination controversy with CHARA/MIRC
• Self-consistent 2D models of fast rotating early-type star
• The dynamics of the radiative envelope of rapidly rotating stars. I. A spherical Boussinesq model
• Pulsations of rapidly rotating stars: I. The ACOR numerical code
• Mode visibilities in rapidly rotating stars
• Gravity Darkening in Binary Stars
• On the dynamics of radiative zones in rotating stars
• Matching the Spectral Energy Distribution and p Mode Oscillation Frequencies of the Rapidly Rotating Delta Scuti Star ? Ophiuchi with a 2D Rotating Stellar Model