supernova neutrinos, it might mean that the shock wave reaches H-resonance ( ∼ 1000 g / cm $^{3}$) very early after core bounce. Then, we would expect that this kind of supernova explosion exhibits a strong shock wave effect in the direction of observer. Moreover, assume that we could know viewing angle from the axis of a supernova in optical and radio observations. If the viewing angle is small and the influence of the shock wave is seen very early, this supernova has strong shock like a narrow beaming jet along the axis of supernova explosion. Therefore, we would expect that this supernova explodes in the mechanism associated with the jet formation [66–72]. If the viewing angle is large and the influence of the shock is seen very early, we would expect that this supernova has a rather wide jet and may be close to the spherical symmetric explosion. On the other hand, if the influence of the shock wave is seen in the supernova neutrinos at relatively later time, and the viewing angle is small, we would expect that this explosion is also close to the spherical symmetry without jet. Therefore, we would expect that this supernova explodes in the mechanism without a jet. Details of the influence of neutrino oscillation on jet explosion are discussed in [73]. Recently, oxygen emission-line profiles from supernovae are observed, which could be a signature of an aspheric explosion [74]. We would study the asphericity of the supernova explosions more in detail from such an optical observation and simultaneous detection of the supernova neutrinos. The flavor-exchange effects by the neutrino self-interactions might also be important because of their huge flux immediately after the emission out of the proto-neutron star (e.g., [75, 76]). This could change initial neutrino spectrum from what we assumed here. We investigated the neutrino signal to study the effect of the shock wave propagation as well as the dependence on unknown neutrino oscillation parameters of mass hierarchy and θ$_{13}$ by carrying out numerical calculations of the neutrino event number using the simulation result of a supernova explosion. We followed adiabatic collapse of iron core, core bounce, and the shock wave propagation in the stellar envelope for a long time ( ≳ 10 s) using general relativistic hydrodynamical code and realistic density profile. Then, we could calculate detailed time evolution of the event number rate and spectra of the supernova neutrinos. IV. CONCLUSION 21