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Title: KamLAND Sensitivity to Neutrinos from Pre-Supernova Stars

Abstract

In the late stages of nuclear burning for massive stars (M > 8 M ⊙), the production of neutrino-antineutrino pairs through various processes becomes the dominant stellar cooling mechanism. Furthermore, 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. Here, 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 ⊙ 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.

Authors:
; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; more »; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; « less
Publication Date:
Research Org.:
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC), Nuclear Physics (NP) (SC-26); Nuclear Science Division
Contributing Org.:
The KamLAND Collaboration
OSTI Identifier:
1379082
Alternate Identifier(s):
OSTI ID: 1469138
Report Number(s):
LBNL-1004322
Journal ID: ISSN 1538-4357; ark:/13030/qt8gq4z5tf
Grant/Contract Number:  
AC02-05CH11231; FG03-00ER41138; FG02-01ER41166
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 818; Journal Issue: 1; Journal ID: ISSN 1538-4357
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; neutrinos; supernovae: general

Citation Formats

Asakura, K., Gando, A., Gando, Y., Hachiya, T., Hayashida, S., Ikeda, H., Inoue, K., Ishidoshiro, K., Ishikawa, T., Ishio, S., Koga, M., Matsuda, S., Mitsui, T., Motoki, D., Nakamura, K., Obara, S., Oura, T., Shimizu, I., Shirahata, Y., Shirai, J., Suzuki, A., Tachibana, H., Tamae, K., Ueshima, K., Watanabe, H., Xu, B. D., Kozlov, A., Takemoto, Y., Yoshida, S., Fushimi, K., Piepke, A., Banks, T. I., Berger, B. E., Fujikawa, B. K., O’Donnell, T., Learned, J. G., Maricic, J., Matsuno, S., Sakai, M., Winslow, L. A., Efremenko, Y., Karwowski, H. J., Markoff, D. M., Tornow, W., Detwiler, J. A., Enomoto, S., and Decowski, M. P. KamLAND Sensitivity to Neutrinos from Pre-Supernova Stars. United States: N. p., 2016. Web. doi:10.3847/0004-637X/818/1/91.
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Asakura, K., Gando, A., Gando, Y., Hachiya, T., Hayashida, S., Ikeda, H., Inoue, K., Ishidoshiro, K., Ishikawa, T., Ishio, S., Koga, M., Matsuda, S., Mitsui, T., Motoki, D., Nakamura, K., Obara, S., Oura, T., Shimizu, I., Shirahata, Y., Shirai, J., Suzuki, A., Tachibana, H., Tamae, K., Ueshima, K., Watanabe, H., Xu, B. D., Kozlov, A., Takemoto, Y., Yoshida, S., Fushimi, K., Piepke, A., Banks, T. I., Berger, B. E., Fujikawa, B. K., O’Donnell, T., Learned, J. G., Maricic, J., Matsuno, S., Sakai, M., Winslow, L. A., Efremenko, Y., Karwowski, H. J., Markoff, D. M., Tornow, W., Detwiler, J. A., Enomoto, S., & Decowski, M. P. KamLAND Sensitivity to Neutrinos from Pre-Supernova Stars. United States. doi:10.3847/0004-637X/818/1/91.
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Asakura, K., Gando, A., Gando, Y., Hachiya, T., Hayashida, S., Ikeda, H., Inoue, K., Ishidoshiro, K., Ishikawa, T., Ishio, S., Koga, M., Matsuda, S., Mitsui, T., Motoki, D., Nakamura, K., Obara, S., Oura, T., Shimizu, I., Shirahata, Y., Shirai, J., Suzuki, A., Tachibana, H., Tamae, K., Ueshima, K., Watanabe, H., Xu, B. D., Kozlov, A., Takemoto, Y., Yoshida, S., Fushimi, K., Piepke, A., Banks, T. I., Berger, B. E., Fujikawa, B. K., O’Donnell, T., Learned, J. G., Maricic, J., Matsuno, S., Sakai, M., Winslow, L. A., Efremenko, Y., Karwowski, H. J., Markoff, D. M., Tornow, W., Detwiler, J. A., Enomoto, S., and Decowski, M. P. Wed . "KamLAND Sensitivity to Neutrinos from Pre-Supernova Stars". United States. doi:10.3847/0004-637X/818/1/91. https://www.osti.gov/servlets/purl/1379082.
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@article{osti_1379082,
title = {KamLAND Sensitivity to Neutrinos from Pre-Supernova Stars},
author = {Asakura, K. and Gando, A. and Gando, Y. and Hachiya, T. and Hayashida, S. and Ikeda, H. and Inoue, K. and Ishidoshiro, K. and Ishikawa, T. and Ishio, S. and Koga, M. and Matsuda, S. and Mitsui, T. and Motoki, D. and Nakamura, K. and Obara, S. and Oura, T. and Shimizu, I. and Shirahata, Y. and Shirai, J. and Suzuki, A. and Tachibana, H. and Tamae, K. and Ueshima, K. and Watanabe, H. and Xu, B. D. and Kozlov, A. and Takemoto, Y. and Yoshida, S. and Fushimi, K. and Piepke, A. and Banks, T. I. and Berger, B. E. and Fujikawa, B. K. and O’Donnell, T. and Learned, J. G. and Maricic, J. and Matsuno, S. and Sakai, M. and Winslow, L. A. and Efremenko, Y. and Karwowski, H. J. and Markoff, D. M. and Tornow, W. and Detwiler, J. A. and Enomoto, S. and Decowski, M. P.},
abstractNote = {In the late stages of nuclear burning for massive stars (M > 8 M⊙), the production of neutrino-antineutrino pairs through various processes becomes the dominant stellar cooling mechanism. Furthermore, 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. Here, 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⊙ 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.},
doi = {10.3847/0004-637X/818/1/91},
journal = {The Astrophysical Journal (Online)},
number = 1,
volume = 818,
place = {United States},
year = {2016},
month = {2}
}
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DOI:  10.3847/0004-637X/818/1/91
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Cited by: 13 works
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Figures / Tables:

Figure 1 Figure 1: Time evolution of the $\bar{v}_e$ luminosity of pre-SN just before collapse(Odrzywolek & Heger 2010) and of SN after collapse(Nakazato et al. 2013). Note the timescale of the horizontal axis, which is linear after the collapse but logarithmic before collapse.
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