EDP Sciences
Free Access
Volume 440, Number 1, September II 2005
Page(s) L9 - L12
Section Letters
DOI https://doi.org/10.1051/0004-6361:200500156

A&A 440, L9-L12 (2005)
DOI: 10.1051/0004-6361:200500156


Stellar evolution with rotation and magnetic fields

IV. The solar rotation profile
P. Eggenberger, A. Maeder and G. Meynet

Observatoire de Genève, 51 chemin de Maillettes, 1290 Sauverny, Switzerland
    e-mail: Patrick.Eggenberger@obs.unige.ch

(Received 2 June 2005 / Accepted 16 July 2005)

We examine the generation of a magnetic field in a solar-like star and its effects on the internal distribution of the angular velocity. We suggest that the evolution of a rotating star with magnetic fields leads to an equilibrium value of the differential rotation. This equilibrium is determined by the magnetic coupling, which favours a constant rotation profile, and meridional circulation which tends to build differential rotation. The global equilibrium stage is close to solid body rotation between about 0.7 and 0.2 $R_{\odot}$, in good agreement with helioseismic measurements.

Key words: stars: rotation -- stars: magnetic fields -- stars: evolution

© ESO 2005