TY - JOUR
T1 - Observing Supernova Neutrino Light Curves with Super-Kamiokande. II. Impact of the Nuclear Equation of State
AU - Nakazato, Ken'Ichiro
AU - Nakanishi, Fumi
AU - Harada, Masayuki
AU - Koshio, Yusuke
AU - Suwa, Yudai
AU - Sumiyoshi, Kohsuke
AU - Harada, Akira
AU - Mori, Masamitsu
AU - Wendell, Roger A.
N1 - Funding Information:
This work is supported by Grant-in-Aid for Scientific Research (15K05093, 16K17665, 17H02864, 19K03837, 20H00174, 20H01904, 20H01905, and 20K03973) and Grant-in-Aid for Scientific Research on Innovative Areas (17H06357, 17H06365, 18H04586, 18H05437, 19H05802, 19H05811, and 20H04747) from the Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan. This work was partially carried out by the joint research program of the Institute for Cosmic Ray Research (ICRR), The University of Tokyo. For providing high-performance computing resources, Research Center for Nuclear Physics in Osaka University, Yukawa Institute of Theoretical Physics in Kyoto University, Center for Computational Astrophysics in National Astronomical Observatory of Japan, Computing Research Center in KEK, JLDG on SINET4 of NII, Information Technology Center in Nagoya University, and Information Technology Center in University of Tokyo are acknowledged. This work was partly supported by MEXT as “Program for Promoting Researches on the Supercomputer Fugaku” (Toward a unified view of the universe: from large scale structures to planets).
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/1/1
Y1 - 2022/1/1
N2 - The late-time evolution of the neutrino event rate from supernovae is evaluated for Super-Kamiokande using simulated results of proto-neutron star (PNS) cooling. In the present work, we extend the result of Suwa et al., who studied the dependence of the neutrino event rate on the PNS mass, but focus on the impact of the nuclear equation of state (EOS). We find that the neutrino event rate depends on both the high-density and low-density EOS, where the former determines the radius of the PNS and the latter affects its surface temperature. Based on the present evaluation of the neutrino event rate, we propose a new analysis method to extract the time variability of the neutrino average energy taking into account the statistical error in the observation.
AB - The late-time evolution of the neutrino event rate from supernovae is evaluated for Super-Kamiokande using simulated results of proto-neutron star (PNS) cooling. In the present work, we extend the result of Suwa et al., who studied the dependence of the neutrino event rate on the PNS mass, but focus on the impact of the nuclear equation of state (EOS). We find that the neutrino event rate depends on both the high-density and low-density EOS, where the former determines the radius of the PNS and the latter affects its surface temperature. Based on the present evaluation of the neutrino event rate, we propose a new analysis method to extract the time variability of the neutrino average energy taking into account the statistical error in the observation.
UR - http://www.scopus.com/inward/record.url?scp=85125853292&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85125853292&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ac3ae2
DO - 10.3847/1538-4357/ac3ae2
M3 - Article
AN - SCOPUS:85125853292
SN - 0004-637X
VL - 925
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 98
ER -