KamLAND SENSITIVITY TO NEUTRINOS FROM PRE-SUPERNOVA STARS
Name
Asakura-2016-KamLAND SENSITIVITY.pdf
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646.81 KB
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Author(s)
Winslow, Lindley
Date Issued
February 2016
Journal
The Astrophysical Journal
Publisher
IOP Publishing
Citation
Asakura, K., A. Gando, Y. Gando, T. Hachiya, S. Hayashida, H. Ikeda, K. Inoue, et al. “KamLAND SENSITIVITY TO NEUTRINOS FROM PRE-SUPERNOVA STARS.” The Astrophysical Journal 818, no. 1 (February 10, 2016): 91. © 2016 The American Astronomical Society
Version
Final published version
Abstract
In the late stages of nuclear burning for massive stars (M > 8 M[subscript ⊙]), the production of neutrino–antineutrino pairs through various processes becomes the dominant stellar cooling mechanism. As the star evolves, the energy of these neutrinos increases and in the days preceding the supernova a significant fraction of emitted electron anti-neutrinos exceeds the energy threshold for inverse beta decay on free hydrogen. This is the golden channel for liquid scintillator detectors because the coincidence signature allows for significant reductions in background signals. We find that the kiloton-scale liquid scintillator detector KamLAND can detect these pre-supernova neutrinos from a star with a mass of 25 M[subscript ⊙] at a distance less than 690 pc with 3σ significance before the supernova. This limit is dependent on the neutrino mass ordering and background levels. KamLAND takes data continuously and can provide a supernova alert to the community.
MIT Department
Massachusetts Institute of Technology. Department of Physics
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Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.
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DOI of Published Version
https://doi.org/10.3847/0004-637x/818/1/91
