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Diffusive shock acceleration (DSA) of cosmic rays in collisionless shocks
strongly depends on parameters of the turbulent magnetic field that allows
the shock to form. Mechanisms of production of this field are still notunderstood, but recent observations suggest that interstellar magnetic
fields may be strongly amplified in SNR shocks. While a completedescription of magnetic turbulence generation is only possible with
particle-in-cell (PIC) simulations (which are limited due to computational
costliness), nonlinear Monte Carlo simulations of DSA can approximate the
process and provide more realistic estimates of magnetic field strengththan current analytic solutions. Presented in the poster are models
describing the self-consistent amplification to very high values of
magnetic field by cosmic rays in interstellar shocks.
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