Results
We present the preliminary results from a temporal evolution of velocity, density and magnetic field.
For velocity, we show the t = 0 curve representing the stationary wind. As the simulation evolves, without any acceleration mechanism, the velocity of the particles becomes negative near the star surface (inward movement) due to gravitation. For example, in one year curve the velocity is negative in the region r/r0 < 5, and for upper layers the velocity still remains positive as in the initial curve. We see also that the velocity peak decreases with time.
In the density profile evolution, we can observe the formation of shock waves propagating outward for r/r0 > 10 in accordance with the velocity profiles.
The magnetic field does not changes during the simulations.
So, in order to maintain the observed flux it is necessary an acceleration mechanism acting uninterruptedly.
Future simulations will take into account some acceleration mechanisms (thermal, magnetic, etc.).