Neutrino flavor conversion in supernova 1987A

By using detailed models of the progenitor we show that the non-adiabatic solution of the solar-neutrino problem by the Mikheyev-Smirnov-Wolfenstein mechanism is compatible with the possible observation of neutronization ${\nu }_e$ from SN 1987A in its wide range of the mixing parameters at Δ$m^2$≳${10}^{\mathrm{-}6}$ ${\mathrm{eV}}^2$. We also argue that, under the assumption of hierarchy of neutrino masses, our consistency solution favors the ${\nu }_e$–heaviest-flavor-neutrino mixing as the cause of the solar-neutrino deficit.