By means of self-consistent three-dimensional ( 3D ) magnetohydrodynamics ( MHD ) numerical simulations , we analyze magnetized solar-like stellar winds and their dependence on the plasma- \beta parameter ( the ratio between thermal and magnetic energy densities ) .
This is the first study to perform such analysis solving the fully ideal 3D MHD equations .
We adopt in our simulations a heating parameter described by \gamma , 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 \sim 1000 km s ^ { -1 } at r \sim 20 ~ { } r _ { 0 } and a maximum temperature of \sim 6 \times 10 ^ { 6 } K at r \sim 6 ~ { } r _ { 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 \sim 45 ^ { o } 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 \gamma , we show that the key parameter in determining the wind velocity profile is the \beta -parameter at the coronal base .
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 .
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 \gamma in our results and we show that it is also important in determining the wind structure .