Appearance of neutronization peak and decaying supernova neutrinos

Abstract

Nonradiative neutrino decay, which is not satisfactorily constrained, possibly and significantly changes the detected neutrino signal from galactic supernova explosions. We focus on the appearance of a sharp peak due to a neutronization burst in the time profile; this phenomenon would occur if the original ν_e, produced at the neutrinosphere and becoming ν_{2,3} at the stellar surface, decays into a lighter antineutrino state such as \barν_{1,2} coupled to \barν_e. This is due to the fact that the signature of the neutronization burst is common to all numerical simulations. Therefore, the appearance of a neutronization peak in the \barν_e signal, if it were detected, would clearly indicate the nonstandard properties of neutrinos. Using a newly developed formulation that includes flavor conversions inside the supernova envelope and neutrino decay during propagation in a vacuum, we calculate the expected neutrino signal at the detectors; the lifetimes of three modes τ_{12}, τ_{13}, and τ_{23} are taken to be free parameters. We further introduce simple quantities, which represent a peak sharpness of time profile and spectral hardness, and investigate the parameter dependence of these quantities. As the result, it is found that they are quite dependent on the relevant parameters, but it would be quite difficult to distinguish models using the signal obtained by the Super-Kamiokande detector; the future megaton-class detectors would have sufficient sensitivity. We also compare the neutrino decay model with another mechanism, i.e., resonant spin-flavor conversion, which also may give the appearance of a neutronization peak, and conclude that these two independent mechanisms give a different signal and one can be distinguished from the other.