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-β parameter. By solving the fully ideal 3D MHD equations, we show that the plasma-β 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-β parameter is the same.
- Publication:
-
Cosmic Magnetic Fields: From Planets, to Stars and Galaxies
- Pub Date:
- April 2009
- DOI:
- 10.1017/S1743921309030932
- arXiv:
- arXiv:0901.1118
- Bibcode:
- 2009IAUS..259..415V
- Keywords:
-
- Stars: coronae;
- stars: late-type;
- stars: magnetic fields;
- stars: mass loss;
- Astrophysics - Solar and Stellar Astrophysics
- E-Print:
- 2 pages, 4 figures, Proceedings of the IAU Symposium 259, "Cosmic Magnetic Fields: From Planets, to Stars and Galaxies", November 2008