KamLAND SENSITIVITY TO NEUTRINOS FROM PRE-SUPERNOVA STARS

The KamLAND Collaboration

doi:10.3847/0004-637X/818/1/91

KamLAND SENSITIVITY TO NEUTRINOS FROM PRE-SUPERNOVA STARS

The KamLAND Collaboration

Research output: Contribution to journal › Article › peer-review

45 Scopus citations

Abstract

In the late stages of nuclear burning for massive stars (M > 8 M_ȯ), 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_ȯ 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.

Original language	English (US)
Article number	91
Journal	Astrophysical Journal
Volume	818
Issue number	1
DOIs	https://doi.org/10.3847/0004-637X/818/1/91
State	Published - Feb 10 2016
Externally published	Yes

Keywords

neutrinos
supernovae: general

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/0004-637X/818/1/91

Cite this

@article{4fd13db51d4447dc89a00df8f2545311,

title = "KamLAND SENSITIVITY TO NEUTRINOS FROM PRE-SUPERNOVA STARS",

abstract = "In the late stages of nuclear burning for massive stars (M > 8 Mȯ), 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 Mȯ 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.",

keywords = "neutrinos, supernovae: general",

author = "{The KamLAND Collaboration} and K. Asakura and A. Gando and Y. Gando and T. Hachiya and S. Hayashida and H. Ikeda and K. Inoue and K. Ishidoshiro and T. Ishikawa and S. Ishio and M. Koga and S. Matsuda and T. Mitsui and D. Motoki and K. Nakamura and S. Obara and T. Oura and I. Shimizu and Y. Shirahata and J. Shirai and A. Suzuki and H. Tachibana and K. Tamae and K. Ueshima and H. Watanabe and Xu, {B. D.} and A. Kozlov and Y. Takemoto and S. Yoshida and K. Fushimi and A. Piepke and Banks, {T. I.} and Berger, {B. E.} and Fujikawa, {B. K.} and T. O'Donnell and Learned, {J. G.} and J. Maricic and S. Matsuno and M. Sakai and Winslow, {L. A.} and Y. Efremenko and Karwowski, {H. J.} and Markoff, {D. M.} and W. Tornow and Detwiler, {J. A.} and S. Enomoto and Decowski, {M. P.}",

year = "2016",

month = feb,

day = "10",

doi = "10.3847/0004-637X/818/1/91",

language = "English (US)",

volume = "818",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing Ltd.",

number = "1",

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TY - JOUR

T1 - KamLAND SENSITIVITY TO NEUTRINOS FROM PRE-SUPERNOVA STARS

AU - The KamLAND Collaboration

AU - Asakura, K.

AU - Gando, A.

AU - Gando, Y.

AU - Hachiya, T.

AU - Hayashida, S.

AU - Ikeda, H.

AU - Inoue, K.

AU - Ishidoshiro, K.

AU - Ishikawa, T.

AU - Ishio, S.

AU - Koga, M.

AU - Matsuda, S.

AU - Mitsui, T.

AU - Motoki, D.

AU - Nakamura, K.

AU - Obara, S.

AU - Oura, T.

AU - Shimizu, I.

AU - Shirahata, Y.

AU - Shirai, J.

AU - Suzuki, A.

AU - Tachibana, H.

AU - Tamae, K.

AU - Ueshima, K.

AU - Watanabe, H.

AU - Xu, B. D.

AU - Kozlov, A.

AU - Takemoto, Y.

AU - Yoshida, S.

AU - Fushimi, K.

AU - Piepke, A.

AU - Banks, T. I.

AU - Berger, B. E.

AU - Fujikawa, B. K.

AU - O'Donnell, T.

AU - Learned, J. G.

AU - Maricic, J.

AU - Matsuno, S.

AU - Sakai, M.

AU - Winslow, L. A.

AU - Efremenko, Y.

AU - Karwowski, H. J.

AU - Markoff, D. M.

AU - Tornow, W.

AU - Detwiler, J. A.

AU - Enomoto, S.

AU - Decowski, M. P.

PY - 2016/2/10

Y1 - 2016/2/10

N2 - In the late stages of nuclear burning for massive stars (M > 8 Mȯ), 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 Mȯ 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.

AB - In the late stages of nuclear burning for massive stars (M > 8 Mȯ), 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 Mȯ 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.

KW - neutrinos

KW - supernovae: general

UR - http://www.scopus.com/inward/record.url?scp=84959441280&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84959441280&partnerID=8YFLogxK

U2 - 10.3847/0004-637X/818/1/91

DO - 10.3847/0004-637X/818/1/91

M3 - Article

AN - SCOPUS:84959441280

SN - 0004-637X

VL - 818

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

M1 - 91

ER -

KamLAND SENSITIVITY TO NEUTRINOS FROM PRE-SUPERNOVA STARS

Abstract

Keywords

ASJC Scopus subject areas

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