In this paper, we study how the shock wave propagation and the neutrino oscillation pa- rameters affect the supernova neutrinos. We calculate neutrino oscillations of the supernova neutrinos by using supernova simulation result in adiabatic explosion model. In our model, we calculate all processes of core collapse, bounce, and shock propagation continuously in a unified manner. In order to clarify detailed dependence of the result on the neutrino oscilla- tion parameters and the shock wave, we calculate survival probabilities, energy spectra, and the event rates of three flavors of supernova neutrinos to be detected with SK and SNO. In Sec. II, we introduce our numerical method. In Sec. III, we show time evolution of the survival probability and energy spectra of the supernova neutrinos. We also study the event rates. We analyze the dependence of these neutrino signals on neutrino oscillation parameters and the shock effect. We discuss the ratio of high- to low-energy neutrino events which will be detected by SK and SNO. We discuss the difference of the expected supernova neutrinos using both parameterized density and the density obtained by the simulations of supernova explosion in Sec. III E. We also discuss other effects of supernova explosions and supernova neutrinos which should affect the time evolution of the neutrino signal. Finally, we conclude our paper in Sec. IV. In order to obtain the detailed density profile in a supernova explosion and to examine the MSW effect on supernova neutrinos, we use one dimensional simulation result of the supernova. We model the supernova explosion using an implicit Lagrangian code for general relativistic spherical hydrodynamics [47]. The numerical tables of Shen’s relativistic equation of state (EOS) [48] and Timmes’s EOS [49] are adopted for the high and low density matters in this code, respectively. We adopt the presupernova model of a 15 M ⊙ star provided by Woosley and Weaver (WW95) [50] as the initial condition. We use the distribution of the electron fraction Y$_{e}$ in WW95. We perform calculations of all processes throughout the core collapse, bounce, and shock propagation continuously by adiabatic collapse with fixed electron fraction to follow the shock wave for a long time scale ( > 10 s) and a wide density range, consistently [51]. We thus succeeded in the calculation of the propagation of the II. NUMERICAL METHOD A. Supernova Model 5