  We investigate the structure of magnetic field amplified by turbulent
velocity fluctuations, in the framework of the kinematic Kazantsev-Kraichnan
model. We consider Kolmogorov distribution of velocity fluctuations, and assume
that both Reynolds number and magnetic Reynolds number are very large. We
present the full numerical solution of the model for the spectra and the growth
rates of magnetic fluctuations. We consider astrophysically relevant limits of
large and small magnetic Prandtl numbers, and address both helical and
nonhelical cases.
