  We investigate the role of Alfven waves in the core-collapse supernova (SN)
explosion. We assume that Alfven waves are generated by convections inside a
proto-neutron star (PNS) and emitted from its surface. Then these waves
propagate outwards, dissipate via nonlinear processes, and heat up matter
around a stalled prompt shock. To quantitatively assess the importance of this
process for the revival of the stalled shock, we perform 1D time-dependent
hydrodynamical simulations, taking into account the heating via the dissipation
of Alfven waves that propagate radially outwards along open flux tubes. We show
that the shock revival occurs if the surface field strength is larger than
~2e15 G and if the amplitude of velocity fluctuation at the PNS surface is
larger than 20% of the local sound speed. Interestingly, the Alfven wave
mechanism is self-regulating in the sense that the explosion energy is not very
sensitive to the surface field strength and initial amplitude of Alfven waves
as long as they are larger than the threshold values given above.
