Numerical Simulations of Magnetized Winds of Solar-Like Stars
Abstract
We investigate magnetized solar-like stellar winds by means of self-consistent three-dimensional (3D) magnetohydrodynamics (MHD) numerical simulations. We analyze winds with different magnetic field intensities and densities as to explore the dependence on the plasma-beta parameter. By solving the fully ideal 3D MHD equations, we show that the plasma-beta parameter is the crucial parameter in the configuration of the steady-state wind. Therefore, there is a group of magnetized flows that would present the same terminal velocity despite of its thermal and magnetic energy densities, as long as the plasma-beta parameter is the same.
Keywords
Cite
@article{arxiv.0901.1118,
title = {Numerical Simulations of Magnetized Winds of Solar-Like Stars},
author = {A. A. Vidotto and M. Opher and V. Jatenco-Pereira and T. I. Gombosi},
journal= {arXiv preprint arXiv:0901.1118},
year = {2009}
}
Comments
2 pages, 4 figures, Proceedings of the IAU Symposium 259, "Cosmic Magnetic Fields: From Planets, to Stars and Galaxies", November 2008