Abstract
Fast stellar winds of young massive stars and supernovae play an essential role in the evolution of the interstellar medium in the Milky Way. They dominate the dynamics of the active starforming regions in starburst galaxies and in particularly their non-thermal radiation. The non-thermal emission from starburst galaxies NGC 253, M82, NGC 1068 was detected from radio to gamma-rays. To model the observed radiation, one needs to know the complex structure of the flows and magnetic fields in the starforming regions. In this work a 2.5D magnetohydrodynamic (MHD) simulation (i.e., we consider 3D vector fields, but assume a 2D axisymmetric geometry) of the interaction between a stellar wind and a supernova remnant shock wave is carried out using the MHD module of the code PLUTO. The structure of the flows in the collision region is obtained taking into account the magnetic fields of the rotating source stars. We present the profiles of the bulk plasma velocity, density and magnetic field in the collision region. The amplification of regular magnetic fields in such systems is studied.
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