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We investigate magnetized solar-like stellar winds by means ofself-consistent three-dimensional (3D) magnetohydrodynamics (MHD) numericalsimulations. We analyze winds with different magnetic field intensities anddensities as to explore the dependence on the plasma-beta parameter. By solvingthe fully ideal 3D MHD equations, we show that the plasma-beta parameter is thecrucial parameter in the configuration of the steady-state wind. Therefore,there is a group of magnetized flows that would present the same terminalvelocity despite of its thermal and magnetic energy densities, as long as theplasma-beta parameter is the same.

Numerical Simulations of Magnetized Winds of Solar-Like Stars