  Based on the new findings on the turbulent dynamo in \citet{XL16}, we examine
the magnetic field amplification in the context of supernova remnants. Due to
the strong ion-neutral collisional damping in the weakly-ionized interstellar
medium, the dynamo in the preshock turbulence remains in the damping kinematic
regime, which leads to {\it a linear-in-time growth of the magnetic field
strength}. The resultant magnetic field structure enables effective diffusion
upstream and shock acceleration of cosmic rays to energies above the "knee".
Differently, the nonlinear dynamo in the postshock turbulence leads to {\it a
linear-in-time growth of the magnetic energy} due to the turbulent magnetic
diffusion. Given a weak initial field strength in the postshock region, the
magnetic field saturates at a significant distance from the shock front as a
result of the inefficiency of the nonlinear dynamo. This result is in a good
agreement with existing numerical simulations and well explains the X-ray spots
detected far behind the shock front.
