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We present self-consistent, axisymmetric core-collapse supernova simulationsperformed with the Prometheus-Vertex code for 18 pre-supernova models in therange of 11-28 solar masses, including progenitors recently investigated byother groups. All models develop explosions, but depending on the progenitorstructure, they can be divided into two classes. With a steep density declineat the Si/Si-O interface, the arrival of this interface at the shock frontleads to a sudden drop of the mass-accretion rate, triggering a rapid approachto explosion. With a more gradually decreasing accretion rate, it takes longerfor the neutrino heating to overcome the accretion ram pressure and explosionsset in later. Early explosions are facilitated by high mass-accretion ratesafter bounce and correspondingly high neutrino luminosities combined with apronounced drop of the accretion rate and ram pressure at the Si/Si-Ointerface. Because of rapidly shrinking neutron star radii and receding shockfronts after the passage through their maxima, our models exhibit shortadvection time scales, which favor the efficient growth of the standingaccretion-shock instability. The latter plays a supportive role at least forthe initiation of the re-expansion of the stalled shock before runaway. Takinginto account the effects of turbulent pressure in the gain layer, we derive ageneralized condition for the critical neutrino luminosity that captures theexplosion behavior of all models very well. We validate the robustness of ourfindings by testing the influence of stochasticity, numerical resolution, andapproximations in some aspects of the microphysics.

Progenitor-dependent Explosion Dynamics in Self-consistent, Axisymmetric Simulations of Neutrino-driven Core-collapse Supernovae