Figure 14: Panel (a) shows explosion energies (red line) versus input neutrino luminosities ( ), where green and blue lines show contributions from kinetic and thermal energy, respectively. Panel (b) shows the mass of protoneutron star ( ) and the explosion timescales ( ) as a function of . is estimated as the enclosed mass exceeding and as the time scale when the mass ejection rate at 100 km drops down to in our 2D simulations (from [248]).