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We present three-dimensional global numerical simulations of the cosmic-ray(CR) driven dynamo in barred galaxies. We study the evolution of theinterstellar medium of the barred galaxy in the presence of non-axisymmetriccomponent of the potential, i.e., the bar. The magnetohydrodynamical dynamo isdriven by CRs, which are continuously supplied to the disk by supernova (SN)remnants. No magnetic field is present at the beginning of simulations butone-tenth of SN explosions is a source of a small-scale randomly orienteddipolar magnetic field. In all models we assume that 10% of 10^51 erg SNkinetic energy output is converted into CR energy. To compare our resultsdirectly with the observed properties of galaxies, we construct realistic mapsof polarized radio emission. The main result is that the CR-driven dynamo canamplify weak magnetic fields up to a few {\mu}G within a few Gyr in barredgalaxies. The obtained e-folding time is equal to 300 Myr and the magneticfield reaches equipartition at time t ~ 4.0 Gyr. Initially, the completelyrandom magnetic field evolves into large-scale structures. An even(quadrupole-type) configuration of the magnetic field with respect to thegalactic plane can be observed. Additionally, the modeled magnetic fieldconfiguration resembles maps of the polarized intensity observed in barredgalaxies. Polarization vectors are distributed along the bar and between spiralarms. Moreover, the drift of magnetic arms with respect to the spiral patternin the gas density distribution is observed during the entire simulation time.

Global simulations of the magnetic field evolution under the influence of the cosmic-ray-driven dynamo