Influence of star formation on galactic magnetic fields in a model with vertical structure

E. Mikhailov - V. Pushkarev

Faculty of Physics, Lomonosov Moscow State University, Leninskie Gory, Moscow 119991, Russia

Abstract
The evolution of large-scale galactic magnetic fields in case of active processes, such as active star formation, supernovae explosions, outflows from stars and other processes that change the interstellar turbulence is studied. Previous studies used the no-z approximation which has been developed for thin galaxy discs. In order to consider the z-structure of a magnetic field and to identify how the star formation vary vertical properties of the field, a model has been developed that takes into account the z-dependence of the magnetic field. The influence of active star formation is described with random fluctuations of model coefficients because they exist for a quite small time; their distribution can be assumed with probability laws. Basic properties of the magnetic field evolution for different spatial densities of star formation regions are characterized. The case when the star formation depends on the time through damping of its activity is also discussed. Tables 1, Figs 4, Refs 13.