Pre-supernova Alert System for Super-Kamiokande

被引：2

作者：

Machado, L. N. ^{[1
,2
]}

Abe, K. ^{[3
,4
]}

Hayato, Y. ^{[3
,4
]}

Hiraide, K. ^{[3
,4
]}

Ieki, K. ^{[3
]}

Ikeda, M. ^{[3
,4
]}

Kameda, J. ^{[3
,4
]}

Kanemura, Y. ^{[3
]}

Kaneshima, R. ^{[3
]}

Kashiwagi, Y. ^{[3
]}

Kataoka, Y. ^{[3
,4
]}

Miki, S. ^{[3
]}

Mine, S. ^{[3
]}

Miura, M. ^{[3
]}

Moriyama, S. ^{[3
,4
]}

Nakano, Y. ^{[3
]}

Nakahata, M. ^{[3
,4
]}

Nakayama, S. ^{[3
,4
]}

Noguchi, Y. ^{[3
]}

Okamoto, K. ^{[3
]}

Sato, K. ^{[3
]}

Sekiya, H. ^{[3
,4
]}

Shiba, H. ^{[3
]}

Shimizu, K. ^{[3
]}

Shiozawa, M. ^{[3
,4
]}

Sonoda, Y. ^{[3
]}

Suzuki, Y. ^{[3
]}

Takeda, A. ^{[3
,4
]}

Takemoto, Y. ^{[3
,4
]}

Takenaka, A. ^{[3
]}

Tanaka, H. ^{[3
,4
]}

Watanabe, S. ^{[3
]}

Yano, T. ^{[3
]}

de Perio, P. ^{[4
]}

Martens, K. ^{[4
]}

Vagins, M. R. ^{[4
,5
]}

Bian, J. ^{[5
]}

Griskevich, N. J. ^{[5
]}

Kropp, W. R. ^{[5
]}

Locke, S. ^{[5
]}

Smy, M. B. ^{[4
,5
]}

Sobel, H. W. ^{[4
,5
]}

Takhistov, V ^{[4
,5
]}

Yankelevich, A. ^{[5
]}

Han, S. ^{[6
]}

Kajita, T. ^{[4
,6
]}

Okumura, K. ^{[4
,6
]}

Tashiro, T. ^{[6
]}

Tomiya, T. ^{[6
]}

Wang, X. ^{[6
]}

机构：

[1] Ist Nazl Fis Nucl, Dipartimento Fis, Sez Napoli, I-80126 Naples, Italy

[2] Univ Napoli, I-80126 Naples, Italy

[3] Univ Tokyo, Inst Cosm Ray Res, Kamioka Observ, Gifu, Akita 5061205, Japan

[4] Univ Tokyo, Univ Tokyo Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan

[5] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA

[6] Univ Tokyo, Res Ctr Cosm Neutrinos, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan

[7] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan

[8] Univ Autonoma Madrid, Dept Theoret Phys, E-28049 Madrid, Spain

[9] British Columbia Inst Technol, Dept Phys, Burnaby, BC V5G 3H2, Canada

[10] TRIUMF, 4004 Wesbrook Mall, Vancouver, BC V6T 2A3, Canada

[11] Boston Univ, Dept Phys, Boston, MA 02215 USA

[12] Calif State Univ Dominguez Hills, Dept Phys, Carson, CA 90747 USA

[13] Chonnam Natl Univ, Inst Universe & Elementary Particles, Gwangju 61186, South Korea

[14] Duke Univ, Dept Phys, Durham, NC 27708 USA

[15] Ecole Polytech, Lab Leprince Ringuet, IN2P3 CNRS, F-91120 Palaiseau, France

[16] Junior Coll, Fukuoka Inst Technol, Fukuoka 8110295, Japan

[17] Gifu Univ, Dept Phys, Gifu 5011193, Japan

[18] Gwangju Inst Sci & Technol, GIST Coll, Gwangju 500712, South Korea

[19] Univ Hawaii, Dept Phys & Astron, Honolulu, HI 96822 USA

[20] ICISE, Inst Interdisciplinary Res Sci & Educ, Quy Nhon 55121, Vietnam

[21] Inst for Basic Sci Korea, Daejeon, South Korea

[22] Imperial Coll London, Dept Phys, London SW7 2AZ, England

[23] Ist Nazl Fis Nucl, Dipartimento Interuniv Fis, Sez Bari, I-70125 Bari, Italy

[24] Univ Politecn Ban, I-70125 Bari, Italy

[25] Ist Nazl Fis Nucl, Dipartimento Fis, I-35131 Padua, Italy

[26] Univ Padua, I-35131 Padua, Italy

[27] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy

[28] Univ Roma La Sapienza, I-100185 Rome, Italy

[29] Int Lab Astrophys Neutrino & Cosmol Expt, Kashiwa, Chiba 2778582, Japan

[30] Keio Univ, Dept Phys, Yokohama, Kanagawa 2238522, Japan

[31] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan

[32] Kings Coll London, Dept Phys, London WC2R 2LS, England

[33] Kobe Univ, Dept Phys, Kobe, Hyogo 6578501, Japan

[34] Kyoto Univ, Dept Phys, Kyoto, Kyoto 6068502, Japan

[35] Univ Liverpool, Dept Phys, Liverpool L69 7ZE, Merseyside, England

[36] Miyagi Univ Educ, Dept Phys, Sendai, Miyagi 9800845, Japan

[37] Nagoya Univ, Inst Space Earth Environm Res, Nagoya, Aichi 4648602, Japan

[38] Nagoya Univ, Kobayashi Maskawa Inst Origin Particles & Univers, Nagoya, Aichi 4648602, Japan

[39] Natl Ctr Nucl Res, PL-02093 Warsaw, Poland

[40] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA

[41] Okayama Univ, Dept Phys, Okayama 7008530, Japan

[42] Univ Oxford, Dept Phys, Oxford OX1 3PU, England

[43] Harwell Oxford, Rutherford Appleton Lab, STFC, Warrington OX11 0QX, Cheshire, England

[44] Daresbury Lab, Warrington OX11 0QX, Cheshire, England

[45] Harwell, Rutherford Appleton Lab, STFC, Didcot OX11 0QX, Oxon, England

[46] Seoul Natl Univ, Dept Phys, Seoul 151742, South Korea

[47] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England

[48] Shizuoka Univ Welf, Dept Informat Social Welf, Shizuoka 4258611, Japan

[49] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea

[50] Tohoku Univ, Fac Sci, Dept Phys, Sendai, Miyagi 9808578, Japan

来源：

ASTROPHYSICAL JOURNAL | 2022年 / 935卷 / 01期

基金：

英国科学技术设施理事会; 新加坡国家研究基金会; 中国国家自然科学基金; 美国国家科学基金会; 日本学术振兴会; 加拿大自然科学与工程研究理事会;

关键词：

NEUTRINO BURST; STARS; SENSITIVITY; EVOLUTION; DETECTOR; TRIGGER; GIANTS; WIND; MASS;

D O I：

10.3847/1538-4357/ac7f9c

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In 2020, the Super-Kamiokande (SK) experiment moved to a new stage (SK-Gd) in which gadolinium (Gd) sulfate octahydrate was added to the water in the detector, enhancing the efficiency to detect thermal neutrons and consequently improving the sensitivity to low energy electron anti-neutrinos from inverse beta decay (IBD) interactions. SK-Gd has the potential to provide early alerts of incipient core-collapse supernovae through detection of electron anti-neutrinos from thermal and nuclear processes responsible for the cooling of massive stars before the gravitational collapse of their cores. These pre-supernova neutrinos emitted during the silicon burning phase can exceed the energy threshold for IBD reactions. We present the sensitivity of SK-Gd to pre-supernova stars and the techniques used for the development of a pre-supernova alarm based on the detection of these neutrinos in SK, as well as prospects for future SK-Gd phases with higher concentrations of Gd. For the current SK-Gd phase, high-confidence alerts for Betelgeuse could be issued up to 9 hr in advance of the core collapse itself.

引用

页数：14

共 50 条

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