$\Delta m^2_{ij}$ as follows: $$\begin{aligned}
\Delta m^2_{21} &=& 7.6 \times 10^{-5} {\rm eV^2} \quad {\rm and} \\
|\Delta m^2_{31}| &=& 2.5 \times 10^{-3} {\rm eV^2}. \nonumber\end{aligned}$$ The mixing angles are taken as $$\sin^22\theta_{12} = 0.87 \quad {\rm and} \quad
\sin^22\theta_{23} = 1.$$ The mass hierarchy, i.e., the sign of $\Delta m^2_{31}$, and the mixing angle $\sin^22\theta_{13}$ are taken as parameters. We consider both of normal and inverted mass hierarchies. For the mixing angle $\sin^22\theta_{13}$, we consider $\sin^22\theta_{13} = 0.04$ (adiabatic MSW-H case) and $1 \times 10^{-6}$ (nonadiabatic MSW-H case). The former value corresponds to adiabatic conversion at the MSW-H resonance in the presupernova density profile. The latter value corresponds to nonadiabatic at the MSW-H resonance.

We assume that the transition magnetic moment of neutrinos $\mu_{\alpha \beta}$ does not depend on flavors. We set $\mu_{\alpha \beta} = 1 \times 10^{-12} \mu_B$ commonly. This value is the same as that adopted in [@as03a; @as03b; @as03c]. Since the effect of neutrino magnetic moment appears in the form of $\mu_{\alpha \beta}B$, small magnetic moment with strong magnetic field may bring about a similar effect to the case of large magnetic moment with weak magnetic field.

Detection of neutrino signals
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We evaluate the event 