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

Neutrino-driven massive stellar explosions in 3D fostered by magnetic fields via turbulent $\alpha$-effect