Alfvén Wave-driven Supernova Explosion

We investigate the role of Alfvén waves in the core-collapse supernova (SN) explosion. We assume that Alfvén waves are generated by convections inside a proto-neutron star (PNS) and emitted from its surface. Then these waves propagate outwards and dissipate via nonlinear processes and heat up matter around a stalled prompt shock. To quantitatively assess the importance of this process for revival of the stalled shock, we perform 1D time-dependent hydrodynamical simulations, taking into account the heating via the dissipation of Alfvén waves. We show that the shock revival occurs if the surface field strength is larger than ∼ 2×1015G and if the amplitude of velocity fluctuation at the PNS surface is larger than ∼ 20% of the local sound speed. Interestingly, the Alfvén 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 Alfvén waves as long as they are larger than the threshold values given above. It should be emphasized that Alfvén waves can produce SN explosions even without rotation if a PNS has strong magnetic fields of the magnetar scale. Subject headings: MHD – supernovae:general – waves