\times  64 $ & $ 2.8^{\circ} $ & 125 & & & 569 & 2500 & 1.3 & 2,0 & 0.05\
\[tab:models\]

Result
======

As summarized in Table 1, all the computed models including nine 3D models and fifteen 2D models exhibit shock revival, leading to the possibility of explosion. Before going into detail how the explosion dynamics and stochasticity are different in 2D and 3D, we briefly outline the hydrodynamics features taking model 3D-H-1 as an example.

The top panel of Figure \[fig1\] shows the blast morphology of model 3D-H-1 at $t_{\rm pb} = 230$ ms (postbounce) when the revived shock is reaching an angle-averaged radius of 400 km (e.g., red dashed line in the right panel of Figure. \[fig2\]). As seen from the side wall panels, a bipolar explosion is obtained for this model. The bottom left panel (red regions) shows that the ratio of the residency timescale to the neutrino heating timescale (e.g., Equations (6) and (7) in @takiwaki12) exceeds unity behind the shock, which presents evidence that the shock revival is driven by the neutrino-heating mechanism. The bottom right panel of Figure \[fig1\] depicts spacial distribution of the net neutrino heating rate at $t_{\rm pb} = 