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Supernova neutrinos are crucially important to probe the final phases ofmassive star evolution. As is well known from observations of SN1987A,neutrinos provide information on the physical conditions responsible forneutron star formation and on the supernova explosion mechanism. However, thereis still no complete understanding of the long-term evolution of neutrinoemission in supernova explosions, although there are a number of modernsimulations of neutrino radiation hydrodynamics, which study neutrino emissionat times less than one second after the bounce. In the present work wesystematically calculate the number of neutrinos that can be observed inSuper-Kamiokande over periods longer than ten seconds using the database ofNakazato et al. (2013) anticipating that neutrinos from a Galactic supernovacan be detected for several tens of seconds. We find that for a supernova at adistance of 10 kpc, neutrinos remain observable for longer than 30 s for alow-mass neutron star ($1.20M_\odot$ gravitational mass) and even longer than100 s for a high-mass neutron star ($2.05M_\odot$). These scenarios are muchlonger than the observations of SN1987A and longer than the duration ofexisting numerical simulations. We propose a new analysis method based on thecumulative neutrino event distribution as a function of reverse time from thelast observed event, as a useful probe of the neutron star mass. Our resultdemonstrates the importance of complete modeling of neutrino light curves inorder to extract physical quantities essential for understanding supernovaexplosion mechanisms, such as the mass and radius of the resulting neutronstar.

Observing Supernova Neutrino Light Curves with Super-Kamiokande: Expected Event Number over 10 s