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Neutrino Emissions in All Flavors up to the Pre-bounce of Massive Stars and the Possibility of Their Detections

Kato, Chinami and Nagakura, Hiroki and Furusawa, Shun and Takahashi, Koh and Umeda, Hideyuki and Yoshida, Takashi and Ishidoshiro, Koji and Yamada, Shoichi (2017) Neutrino Emissions in All Flavors up to the Pre-bounce of Massive Stars and the Possibility of Their Detections. Astrophysical Journal, 848 (1). Art. No. 48. ISSN 1538-4357. http://resolver.caltech.edu/CaltechAUTHORS:20171011-142153794

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Abstract

This paper is a sequel to our 2015 paper, Kato et al., which calculated the luminosities and spectra of electron-type anti-neutrinos (ν[overbar]_e) from the progenitors of core-collapse supernovae. Expecting that the capability to detect electron-type neutrinos (ν_e) will increase dramatically with the emergence of liquid-argon detectors such as DUNE, we broaden the scope in this study to include all flavors of neutrinos emitted from the pre-bounce phase. We pick up three progenitor models of electron capture supernovae (ECSNe) and iron-core collapse supernovae (FeCCSNe). We find that the number luminosities reach ~10^(57) s^(–1) and ~10^(53) s^(–1) at maximum for ν_e and ν[overbar]_e, respectively. We also estimate the numbers of detection events at terrestrial neutrino detectors including DUNE, taking flavor oscillations into account and assuming the distance to the progenitors to be 200 pc. It is demonstrated that ν[overbar]_e from the ECSN progenitor will be undetected at almost all detectors, whereas we will be able to observe ≳15,900 ν_e at DUNE for the inverted mass hierarchy. From the FeCCSN progenitors, the number of ν[overbar]_e events will be largest for JUNO, 200–900 ν[overbar]_e, depending on the mass hierarchy, whereas the number of ν_e events at DUNE is ≳2100 for the inverted mass hierarchy. These results imply that the detection of ν[overbar]_e is useful to distinguish progenitors of FeCCSNe from those of ECSNe, while ν_e will provide us with detailed information on the collapse phase regardless of the type and mass of the progenitor.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aa8b72DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aa8b72/metaPublisherArticle
https://arxiv.org/abs/1704.05480arXivDiscussion Paper
ORCID:
AuthorORCID
Kato, Chinami0000-0003-4213-0076
Nagakura, Hiroki0000-0002-7205-6367
Ishidoshiro, Koji0000-0001-9271-2301
Yamada, Shoichi0000-0002-2166-5605
Additional Information:© 2017 The American Astronomical Society. Received 2017 April 18; revised 2017 September 6; accepted 2017 September 7; published 2017 October 10. We are grateful to Dr. Tachibana for providing us with the table of nuclear weak interaction rates and to Dr. Beacom for his useful advice. This work is partly supported by Grants-in-Aid for Scientific Research from the Ministry of Education, Culture, Sports, Science and Technology of Japan (Nos. 24244036, 24103006, 26104007, 26400220, 26400271), and the HPCI Strategic Program of Japanese MEXT. H.N. and S.F. are supported by the Japan Society for the Promotion of Science Postdoctoral Fellowships for Research Abroad. Some numerical calculations were carried out on the PC cluster at the Center for Computational Astrophysics, National Astronomical Observatory of Japan. K.T. is supported by Overseas Research Fellowships of the Japan Society for the Promotion of Science (JSPS).
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funders:
Funding AgencyGrant Number
Ministry of Education, Culture, Sports, Science and Technology (MEXT)24244036
Ministry of Education, Culture, Sports, Science and Technology (MEXT)24103006
Ministry of Education, Culture, Sports, Science and Technology (MEXT)26104007
Ministry of Education, Culture, Sports, Science and Technology (MEXT)26400220
Ministry of Education, Culture, Sports, Science and Technology (MEXT)26400271
Subject Keywords:neutrinos – stars: evolution – stars: massive – supernovae: general
Record Number:CaltechAUTHORS:20171011-142153794
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20171011-142153794
Official Citation:Chinami Kato et al 2017 ApJ 848 48
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:82290
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:11 Oct 2017 21:38
Last Modified:11 Oct 2017 21:38

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