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Title: Observing Supernova Neutrino Light Curves with Super-Kamiokande. III. Extraction of Mass and Radius of Neutron Stars from Synthetic Data
Authors: Suwa, Yudai
Harada, Akira
Harada, Masayuki
Koshio, Yusuke
Mori, Masamitsu
Nakanishi, Fumi
Nakazato, Ken’ichiro
Sumiyoshi, Kohsuke
Wendell, Roger A.
Author's alias: 諏訪, 雄大
Keywords: Supernova neutrinos
Neutrino astronomy
Neutrino telescopes
Core-collapse supernovae
Neutron stars
Issue Date: 20-Jul-2022
Publisher: American Astronomical Society
Journal title: The Astrophysical Journal
Volume: 934
Issue: 1
Thesis number: 15
Abstract: Neutrinos are guaranteed to be observable from the next Galactic supernova (SN). Optical light and gravitational waves are also observable, but may be difficult to observe if the location of the SN in the Galaxy or the details of the explosion are unsuitable. The key to observing the next SN is to first use neutrinos to understand various physical quantities and then link them to other signals. In this paper, we present Monte Carlo sampling calculations of neutrino events from Galactic SN explosions observed with Super-Kamiokande. The analytical solution of neutrino emission, which represents the long-term evolution of the neutrino light curve from SNe, is used as a theoretical template. It gives the event rate and event spectrum through inverse beta decay interactions with explicit model parameter dependence. Parameter estimation is performed on these simulated sample data by fitting least squares using the analytical solution. The results show that the mass, radius, and total energy of a remnant neutron star produced by an SN can be determined with an accuracy of ∼ 0.1 M⊙, ∼1 km, and ∼ 10⁵¹ erg, respectively, for a Galactic SN at 8 kpc.
Rights: © 2022. The Author(s). Published by the American Astronomical Society
Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
URI: http://hdl.handle.net/2433/286091
DOI(Published Version): 10.3847/1538-4357/ac795e
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