Detectability of Late-time Supernova Neutrinos with Fallback Accretion onto Protoneutron star

Abstract

We investigate the late-time neutrino emission powered by fallback mass accretion onto proto-neutron star (PNS), using neutrino radiation-hydrodynamic simulations with full Boltzmann neutrino transport. We follow the time evolution of accretion flow onto PNS until the system reaches a steady state. A standing shock wave is commonly formed in the accretion flow, whereas the shock radius varies depending on mass accretion rate and PNS mass. A sharp increase in temperature emerges in the vicinity of PNS ($\sim 10$ km), which characterizes neutrino emission. Both neutrino luminosity and average energy become higher with increasing mass accretion rate and PNS mass. The mean energy of emitted neutrinos is in the range of $10\lesssim\epsilon\lesssim20\,\mathrm{MeV}$, which is higher than that estimated from PNS cooling models ($\lesssim10\,\mathrm{MeV}$). Assuming a distance to core-collapse supernova of $10\,\mathrm{kpc}$, we quantify neutrino event rates for Super-Kamiokande (Super-K) and DUNE. The estimated detection rates are well above the background, and their energy-dependent features are qualitatively different from those expected from PNS cooling models. Another notable feature is that the neutrino emission is strongly flavor dependent, exhibiting that the neutrino event rate hinges on the neutrino oscillation model. We estimate them in the case with adiabatic Mikheev-Smirnov-Wolfenstein model, and show that the normal- and inverted mass hierarchy offer the large number of neutrino detection in Super-K and DUNE, respectively. Hence the simultaneous observation with Super-K and DUNE of the fallback neutrinos will provide a strong constraint on neutrino mass hierarchy.