We perform hydrodynamic supernova simulations in spherical symmetry for over 100 single stars of solar metallicity to explore the progenitor-explosion and progenitor-remnant connections established by the neutrino-driven mechanism .
We use an approximative treatment of neutrino transport and replace the high-density interior of the neutron star ( NS ) by an inner boundary condition based on an analytic proto-NS core-cooling model , whose free parameters are chosen such that explosion energy , nickel production , and energy release by the compact remnant of progenitors around 20 M _ { \odot } are compatible with Supernova 1987A .
Thus we are able to simulate the accretion phase , initiation of the explosion , subsequent neutrino-driven wind phase for 15–20 s , and the further evolution of the blast wave for hours to days until fallback is completed .
Our results challenge long-standing paradigms .
We find that remnant mass , launch time , and properties of the explosion depend strongly on the stellar structure and exhibit large variability even in narrow intervals of the progenitors ’ zero-age-main-sequence mass .
While all progenitors with masses below \sim 15 M _ { \odot } yield NSs , black hole ( BH ) as well as NS formation is possible for more massive stars , where partial loss of the hydrogen envelope leads to weak reverse shocks and weak fallback .
Our NS baryonic masses of \sim 1.2–2.0 M _ { \odot } and BH masses > 6 M _ { \odot } are compatible with a possible lack of low-mass BHs in the empirical distribution .
Neutrino heating accounts for SN energies between some 10 ^ { 50 } erg and \sim 2 \times 10 ^ { 51 } erg , but can hardly explain more energetic explosions and nickel masses higher than 0.1–0.2 M _ { \odot } .
These seem to require an alternative SN mechanism .