Journal
ASTROPHYSICAL JOURNAL
Volume 719, Issue 1, Pages 28-44Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/719/1/28
Keywords
magnetohydrodynamics (MHD); stars: evolution; stars: interiors; stars: magnetic field; Sun: rotation
Categories
Funding
- Natural Sciences and Engineering Research Council of Canada
Ask authors/readers for more resources
The model of magnetic braking of solar rotation considered by Charbonneau & MacGregor has been modified so that it is able to reproduce for the first time the rotational evolution of both the fastest and slowest rotators among solar-type stars in open clusters of different ages, without coming into conflict with other observational constraints, such as the time evolution of the atmospheric Li abundance in solar twins and the thinness of the solar tachocline. This new model assumes that rotation-driven turbulent diffusion, which is thought to amplify the viscosity and magnetic diffusivity in stellar radiative zones, is strongly anisotropic with the horizontal components of the transport coefficients strongly dominating over those in the vertical direction. Also taken into account is the poloidal field decay that helps to confine the width of the tachocline at the solar age. The model's properties are investigated by numerically solving the azimuthal components of the coupled momentum and magnetic induction equations in two dimensions using a finite element method.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available