described. We adopted the time evolution of the density profile calculated using the adiabatic explosion model in [@kk08]. The energy spectra of the neutrinos and the neutrino oscillation parameters are also written in this section. In Sec. III we describe the relation of the effective squared mass with the density and the conversion probabilities due to the RSF conversion and the MSW effect. Based on the obtained characteristics, the dependence of the neutrino spectra and expected neutrino signals on the electron fraction, magnetic field, and the neutrino oscillation parameters is shown. In Sec. IV we discuss the time evolution of the SN neutrino signal and constraints on the neutrino oscillation parameters and magnetic moment. We also discuss the relations of assumed magnetic field and the density profile in the deep region of the SN ejecta. Finally, in Sec. V we summarize this study.

Model
=====

Supernova explosion model
-------------------------

![\[fig:sn-density\] The density distribution of the SN ejecta at $t$ = 0, 0.5, 1, 2, 3, 4, 5, 6, 7, 8, 9, and 10 s. The progenitor is 15 $M_\odot$ presupernova star [@ww95]. The shock propagation is calculated in [@kk08]. ](f1.eps){width="8.5cm"}

In order to study the time evolution of the neutrino 