Neutrino physics with JUNO

被引：948

作者：

An, Fengpeng ^{[1
]}

An, Guangpeng ^{[2
]}

An, Qi ^{[3
]}

Antonelli, Vito ^{[4
,5
]}

Baussan, Eric ^{[6
]}

Beacom, John ^{[7
,8
]}

Bezrukov, Leonid ^{[9
]}

Blyth, Simon ^{[10
]}

Brugnera, Riccardo ^{[11
,12
]}

Avanzini, Margherita Buizza ^{[13
]}

Busto, Jose ^{[14
]}

Cabrera, Anatael ^{[15
]}

Cai, Hao ^{[16
]}

Cai, Xiao ^{[2
]}

Cammi, Antonio ^{[17
,18
]}

Cao, Guofu ^{[2
]}

Cao, Jun ^{[2
]}

Chang, Yun ^{[19
]}

Chen, Shaomin ^{[20
]}

Chen, Shenjian ^{[21
]}

Chen, Yixue ^{[22
]}

Chiesa, Davide ^{[17
,23
]}

Clemenza, Massimiliano ^{[17
,23
]}

Clerbaux, Barbara ^{[24
]}

Conrad, Janet ^{[25
]}

D'Angelo, Davide ^{[4
,5
]}

De Kerret, Herve ^{[15
]}

Deng, Zhi ^{[20
]}

Deng, Ziyan ^{[2
]}

Ding, Yayun ^{[2
]}

Djurcic, Zelimir ^{[26
]}

Dornic, Damien ^{[14
]}

Dracos, Marcos ^{[6
]}

Drapier, Olivier ^{[13
]}

Dusini, Stefano ^{[12
]}

Dye, Stephen ^{[27
]}

Enqvist, Timo ^{[28
]}

Fan, Donghua ^{[29
]}

Fang, Jian ^{[2
]}

Favart, Laurent ^{[24
]}

Ford, Richard ^{[4
,5
]}

Goeger-Neff, Marianne ^{[30
]}

Gan, Haonan ^{[31
]}

Garfagnini, Alberto ^{[11
,12
]}

Giammarchi, Marco ^{[4
,5
]}

Gonchar, Maxim ^{[32
]}

Gong, Guanghua ^{[20
]}

Gong, Hui ^{[20
]}

Gonin, Michel ^{[13
]}

Grassi, Marco ^{[2
]}

机构：

[1] E China Univ Sci & Technol, Shanghai 200237, Peoples R China

[2] Inst High Energy Phys, Beijing 100039, Peoples R China

[3] Univ Sci & Technol China, Hefei 230026, Peoples R China

[4] Ist Nazl Fis Nucl, Sez Milano, Via Celoria 16, I-20133 Milan, Italy

[5] Univ Milan, Dipartimento Fis, Milan, Italy

[6] Univ Strasbourg, CNRS, IN2P3, Inst Pluridisciplinaire Hubert Curien, Strasbourg, France

[7] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA

[8] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA

[9] Russian Acad Sci, Inst Nucl Res, Moscow 117312, Russia

[10] Natl Taiwan Univ, Dept Phys, Taipei, Taiwan

[11] Univ Padua, Dipartimento Fis & Astron, Padua, Italy

[12] Ist Nazl Fis Nucl, Sez Padova, Padua, Italy

[13] Ecole Polytech, Leprince Ringuet Lab, Palaiseau, France

[14] Ctr Phys Particules Marseille, Marseille, France

[15] CEA, Astroparticle Phys Lab, CNRS, Observ Paris, Paris, France

[16] Wuhan Univ, Wuhan 430072, Peoples R China

[17] Ist Nazl Fis Nucl, Sez Milano, Via Celoria 16, I-20133 Milan, Italy

[18] Politecn Milan, Dept Energy, CeSNEF Enrico Fermi Ctr Nucl Studies, I-20133 Milan, Italy

[19] Natl United Univ, Miaoli 36003, Taiwan

[20] Tsinghua Univ, Beijing 100084, Peoples R China

[21] Nanjing Univ, Nanjing 210008, Jiangsu, Peoples R China

[22] North China Elect Power Univ, Beijing, Peoples R China

[23] Univ Milano Bicocca, Dept Phys, Milan, Italy

[24] Univ Libre Bruxelles, Brussels, Belgium

[25] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[26] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA

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

[28] Univ Oulu, Oulu Southern Inst, Pyhasalmi, Finland

[29] Wuyi Univ, Jiangmen, Peoples R China

[30] Tech Univ Munich, Garching, Germany

[31] Chinese Acad Geol Sci, Inst Hydrogeol & Environm Geol, Shijiazhuang, Peoples R China

[32] Joint Inst Nucl Res, Dubna, Russia

[33] Forschungszentrum Julich, Cent Inst Engn Elect & Analyt Elect Syst ZEA 2, D-52425 Julich, Germany

[34] Shanghai Jiao Tong Univ, Shanghai 200030, Peoples R China

[35] Beijing Normal Univ, Beijing 100875, Peoples R China

[36] Univ Hamburg, Inst Expt Phys, Hamburg, Germany

[37] China Inst Atom Energy, Beijing, Peoples R China

[38] Shandong Univ, Jinan 250100, Peoples R China

[39] Harbin Inst Technol, Harbin 150006, Peoples R China

[40] Yerevan Phys Inst, Yerevan 375036, Armenia

[41] Inst High Energy Phys, Vienna, Austria

[42] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

[43] Dongguan Univ Technol, Dongguan, Peoples R China

[44] Univ Tubingen, Inst Phys, Morgenstelle 14, Tubingen, Germany

[45] Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic

[46] Chongqing Univ, Chongqing 630044, Peoples R China

[47] Sun Yat Sen Univ, Guangzhou 510275, Guangdong, Peoples R China

[48] Natl Chiao Tung Univ, Inst Phys, Hsinchu, Taiwan

[49] Univ Illinois, Dept Phys, Urbana, IL USA

[50] Univ Houston, Dept Phys, Houston, TX USA

来源：

JOURNAL OF PHYSICS G-NUCLEAR AND PARTICLE PHYSICS | 2016年 / 43卷 / 03期

基金：

中国国家自然科学基金; 美国国家科学基金会;

关键词：

reactor neutrino experiments; large scintillator detectors; neutrino physics; neutrino astronomy; CORE-COLLAPSE; DARK-MATTER; CHEMICAL-COMPOSITION; SUPERNOVA SHOCK; NUCLEON DECAY; MASSIVE STARS; FISSION-PRODUCTS; MAGNETIC-MOMENT; LEPTON-NUMBER; GEO-NEUTRINOS;

D O I：

10.1088/0954-3899/43/3/030401

中图分类号：

O57 [原子核物理学、高能物理学];

学科分类号：

070202 ;

摘要：

The Jiangmen Underground Neutrino Observatory (JUNO), a 20 kton multipurpose underground liquid scintillator detector, was proposed with the determination of the neutrino mass hierarchy (MH) as a primary physics goal. The excellent energy resolution and the large fiducial volume anticipated for the JUNO detector offer exciting opportunities for addressing many important topics in neutrino and astro-particle physics. In this document, we present the physics motivations and the anticipated performance of the JUNO detector for various proposed measurements. Following an introduction summarizing the current status and open issues in neutrino physics, we discuss how the detection of antineutrinos generated by a cluster of nuclear power plants allows the determination of the neutrino MH at a 3-4 sigma significance with six years of running of JUNO. The measurement of antineutrino spectrum with excellent energy resolution will also lead to the precise determination of the neutrino oscillation parameters sin(2) theta(12), Delta m(21)(2), and vertical bar Delta m(ee)(2)vertical bar to an accuracy of better than 1%, which will play a crucial role in the future unitarity test of the MNSP matrix. The JUNO detector is capable of observing not only antineutrinos from the power plants, but also neutrinos/antineutrinos from terrestrial and extra-terrestrial sources, including supernova burst neutrinos, diffuse supernova neutrino background, geoneutrinos, atmospheric neutrinos, and solar neutrinos. As a result of JUNO's large size, excellent energy resolution, and vertex reconstruction capability, interesting new data on these topics can be collected. For example, a neutrino burst from a typical core-collapse supernova at a distance of 10 kpc would lead to similar to 5000 inverse-beta-decay events and similar to 2000 all-flavor neutrino-proton ES events in JUNO, which are of crucial importance for understanding the mechanism of supernova explosion and for exploring novel phenomena such as collective neutrino oscillations. Detection of neutrinos from all past core-collapse supernova explosions in the visible universe with JUNO would further provide valuable information on the cosmic star-formation rate and the average core-collapse neutrino energy spectrum. Antineutrinos originating from the radioactive decay of uranium and thorium in the Earth can be detected in JUNO with a rate of similar to 400 events per year, significantly improving the statistics of existing geoneutrino event samples. Atmospheric neutrino events collected in JUNO can provide independent inputs for determining the MH and the octant of the theta(23) mixing angle. Detection of the Be-7 and B-8 solar neutrino events at JUNO would shed new light on the solar metallicity problem and examine the transition region between the vacuum and matter dominated neutrino oscillations. Regarding light sterile neutrino topics, sterile neutrinos with 10-(5) eV(2) < Delta m(41)(2) < 10(-2) and a sufficiently large mixing angle theta(14) could be identified through a precise measurement of the reactor antineutrino energy spectrum. Meanwhile, JUNO can also provide us excellent opportunities to test the eV-scale sterile neutrino hypothesis, using either the radioactive neutrino sources or a cyclotron-produced neutrino beam. The JUNO detector is also sensitive to several other beyondthe-standard-model physics. Examples include the search for proton decay via the p -> K++ <(v)over bar> decay channel, search for neutrinos resulting from dark-matter annihilation in the Sun, search for violation of Lorentz invariance via the sidereal modulation of the reactor neutrino event rate, and search for the effects of non-standard interactions. The proposed construction of the JUNO detector will provide a unique facility to address many outstanding crucial questions in particle and astrophysics in a timely and cost-effective fashion. It holds the great potential for further advancing our quest to understanding the fundamental properties of neutrinos, one of the building blocks of our Universe.

引用

页数：188

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