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Fostered by the possibilities of multi-dimensional computational modeling, inparticular the advent of three-dimensional (3D) simulations, our understandingof the neutrino-driven explosion mechanism of core-collapse supernovae (SNe)has experienced remarkable progress over the past decade. Firstself-consistent, first-principle models have shown successful explosions in 3D,and even failed cases may be cured by moderate changes of the microphysicsinside the neutron star (NS), better grid resolution, or more detailedprogenitor conditions at the onset of core collapse, in particular large-scaleperturbations in the convective Si and O burning shells. 3D simulations havealso achieved to follow neutrino-driven explosions continuously from theinitiation of the blast wave, through the shock breakout from the progenitorsurface, into the radioactively powered evolution of the SN, and towards thefree expansion phase of the emerging remnant. Here we present results from suchsimulations, which form the basis for direct comparisons with observations ofSNe and SN remnants in order to derive constraints on the still disputedexplosion mechanism. It is shown that predictions based on hydrodynamicinstabilities and mixing processes associated with neutrino-driven explosionsyield good agreement with measured NS kicks, light-curve properties of SN1987A, and asymmetries of iron and 44Ti distributions observed in SN 1987A andCassiopeia A.

Spatial distribution of radionuclides in 3D models of SN 1987A and Cas A