KamLAND SENSITIVITY TO NEUTRINOS FROM PRE-SUPERNOVA STARS
| Autor: | B. K. Fujikawa, A. Gando, S. Obara, T. O'Donnell, John G. Learned, Yu. Efremenko, M. Koga, M. Sakai, Sanshiro Enomoto, J. Shirai, Ken-Ichi Fushimi, S. Ishio, B. E. Berger, Sei Yoshida, M. P. Decowski, K. Ueshima, K. Nakamura, D. Motoki, T. Oura, H. Tachibana, S. Matsuno, T. Ishikawa, B. D. Xu, S. Matsuda, A. Kozlov, H. J. Karwowski, Kunio Inoue, Werner Tornow, A. Piepke, Y. Shirahata, T. Hachiya, D. M. Markoff, K. Tamae, K. Asakura, H. Ikeda, Koji Ishidoshiro, Y. Takemoto, I. Shimizu, T. I. Banks, A. Suzuki, Lindley Winslow, J. Maricic, T. Mitsui, J. A. Detwiler, S. Hayashida, Hideki Watanabe, Y. Gando |
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| Přispěvatelé: | IoP (FNWI), Gravitation and Astroparticle Physics Amsterdam, GRAPPA (ITFA, IoP, FNWI), Faculty of Science, Other Research IHEF (IoP, FNWI) |
| Rok vydání: | 2016 |
| Předmět: |
Semileptonic decay
Physics - Instrumentation and Detectors Physics::Instrumentation and Detectors Astrophysics::High Energy Astrophysical Phenomena FOS: Physical sciences Astrophysics Electron Astronomy & Astrophysics 01 natural sciences Atomic High Energy Physics - Experiment High Energy Physics - Experiment (hep-ex) Particle and Plasma Physics 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics Nuclear 010303 astronomy & astrophysics physics.ins-det Astrophysics::Galaxy Astrophysics Physics High Energy Astrophysical Phenomena (astro-ph.HE) astro-ph.HE 010308 nuclear & particles physics hep-ex neutrinos Molecular Astronomy and Astrophysics Instrumentation and Detectors (physics.ins-det) Stars Supernova Space and Planetary Science Inverse beta decay High Energy Physics::Experiment Neutrino Astrophysics - High Energy Astrophysical Phenomena general [supernovae] Astronomical and Space Sciences Physical Chemistry (incl. Structural) |
| Zdroj: | The Astrophysical Journal, vol 818, iss 1 Astrophysical Journal, 818(1):91. IOP Publishing Ltd. |
| ISSN: | 0004-637X |
| Popis: | In the late stages of nuclear burning for massive stars ($M>8~M_{\sun}$), 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 $25~M_{\sun}$ at a distance less than 690~pc with 3$\sigma$ 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. Comment: 19 pages, 6 figures, 1 table |
| Databáze: | OpenAIRE |
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