  We investigate the influence of magnetic field amplification on the
core-collapse supernovae in highly magnetized progenitors through
three-dimensional simulations. By considering rotating models, we observe a
strong correlation between the exponential growth of the magnetic field in the
gain region and the initiation of shock revival, with a faster onset compared
to the non-rotating model. We highlight that the mean magnetic field
experiences exponential amplification as a result of $\alpha$-effect in the
dynamo process, which works efficiently with the increasing kinetic helicity of
the turbulence within the gain region. Our findings indicate that the
significant amplification of the mean magnetic fields leads to the development
of locally intense turbulent magnetic fields, particularly in the vicinity of
the poles, thereby promoting the revival of the shock by neutrino heating.
