that the distance from a SN is 10 kpc, which is close to the distance from the Galactic center. The event rate for other distances is easily transformed using the relation $d^2N_i/dE_e dt \propto d^{-2}$. We assumed that the detection efficiency is unity when $E_e$ is larger than $E_{th} = 5$ MeV and otherwise zero supposing the third phase of the SK experiment (SK-III) [@ta08]. We consider the antineutrino-proton reaction $$p + \bar{\nu}_e \rightarrow n + e^+.
%p + \bar{\nu}_e &\rightarrow& n + e^+
%e^- + \nu_e (\bar{\nu}_e) &\rightarrow& e^- + \nu_e (\bar{\nu}_e) \\
%e^- + \nu_{\mu,\tau} (\bar{\nu}_{\mu,\tau}) &\rightarrow&
%e^- + \nu_{\mu,\tau} (\bar{\nu}_{\mu,\tau}) \\
%^{16}{\rm O} + \nu_e &\rightarrow& ^{16}{\rm F} + e^- \\
%^{16}{\rm O} + \bar{\nu}_e &\rightarrow& ^{16}{\rm N} + e^+ \quad ,$$ The reaction rate is adopted from [@sv03].

Results
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Effective squared masses
------------------------

It should be useful to know the dependence of effective squared masses on the density when one evaluates the conversion probabilities of neutrinos and antineutrinos through the RSF and MSW resonances. We will compare the results between the cases of $Y_e = 0.49$ and 0.51. We used the density profile of the 15 $M_\odot$ presupernova and the magnetic field of $B_0 = 