Three-dimensional numerical simulations of magnetized winds of solar-like stars

Abstract

By means of self-consistent three-dimensional magnetohydrodynamics (MHD) numerical simulations, we analyze magnetized solar-like stellar winds and their dependence on the plasma-β parameter (the ratio between thermal and magnetic energy densities). This is the first study to perform such analysis solving the fully ideal three-dimensional MHD equations. We adopt in our simulations a heating parameter described by γ, which is responsible for the thermal acceleration of the wind. We analyze winds with polar magnetic field intensities ranging from 1 to 20 G. We show that the wind structure presents characteristics that are similar to the solar coronal wind. The steady-state magnetic field topology for all cases is similar, presenting a configuration of helmet streamer-type, with zones of closed field lines and open field lines coexisting. Higher magnetic field intensities lead to faster and hotter winds. For the maximum magnetic intensity simulated of 20 G and solar coronal base density, the wind velocity reaches values of 1000 km s-1 at r 20r 0 and a maximum temperature of 6 × 106 K at r 6r 0. The increase of the field intensity generates a larger "dead zone" in the wind, i.e., the closed loops that inhibit matter to escape from latitudes lower than 45°extend farther away from the star. The Lorentz force leads naturally to a latitude-dependent wind. We show that by increasing the density and maintaining B 0 = 20 G the system recover back to slower and cooler winds. For a fixed γ, we show that the key parameter in determining the wind velocity profile is the β-parameter at the coronal base. Therefore, there is a group of magnetized flows that would present the same terminal velocity despite its thermal and magnetic energy densities, as long as the plasma-β parameter is the same. This degeneracy, however, can be removed if we compare other physical parameters of the wind, such as the mass-loss rate. We analyze the influence of γ in our results and we show that it is also important in determining the wind structure. © 2009. The American Astronomical Society.