Description
A high-temperature core called a proto-neutron star(PNS) is formed after a core-collapse supernova explosion. The PNS cools down by emitting neutrinos and becomes neutron-rich. It is important to understand neutrino emission of the cooling phase because it only depends on the environment of PNS, such as density, temperature, and composition. It would have smaller uncertainties than the earlier phase, typically one second after the onset of the explosion, which is affected by many physical processes.
In this poster, we report the most updated estimation of supernova neutrino events observable by Super-Kamiokande in the late phase of the PNS cooling using the various PNS model changing mass and the nuclear equation of state.
| Collaboration | nuLC Collaboration |
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Primary author
Fumi Nakanishi
(Okayama University)
