K+K-π+π-π0 final states are studied using a sample of 14×106 ψ(2S) decays collected with the Beijing Spectrometer (BESII) at the Beijing Electron-Positron Collider. The branching fractions of ψ(2S) decays to K+K-π+π-π0, ωK+K-, ωf0(1710), K*(892)0K-π+π0+c. c., K*(892)+K-π+π-+c.c., K*(892)+K-ρ0+c.c. and K*(892)0K-ρ++c.c. are determined. The first two agree with previous measurements, and the last five are first measurements.

M. Ablikim;J. Z. Bai;Y. Ban;J. G. Bian;X. Cai;H. F. Chen;H. S. Chen;H. X. Chen;J. C. Chen;Jin Chen;Y. B. Chen;S. P. Chi;Y. P. Chu;X. Z. Cui;Y. S. Dai;L. Y. Diao;Z. Y. Deng;Q. F. Dong;S. X. Du;J. Fang;双世 房;C. D. Fu;C. S. Gao;Y. N. Gao;S. D. Gu;Y. T. Gu;Y. N. Guo;Y. Q. Guo;Z. J. Guo;F. A. Harris;K. L. He;M. He;Y. K. Heng;H. M. Hu;T. Hu;G. S. Huang;X. T. Huang;X. B. Ji;X. S. Jiang;X. Y. Jiang;J. B. Jiao;D. P. Jin;S. Jin;Yi Jin;Y. F. Lai;钢 李;海波 李;H. H. Li;J. Li;R. Y. Li;S. M. Li;W. D. Li;W. G. Li;X. L. Li;X. N. Li;X. Q. Li;Y. L. Li;Y. F. Liang;H. B. Liao;B. J. Liu;C. X. Liu;F. Liu;Fang Liu;H. H. Liu;H. M. Liu;J. Liu;J. B. Liu;觉平 刘;Q. Liu;R. G. Liu;Z. A. Liu;Y. C. Lou;F. Lu;G. R. Lu;J. G. Lu;C. L. Luo;凤才 马;H. L. Ma;L. L. Ma;Q. M. Ma;X. B. Ma;Z. P. Mao;X. H. Mo;J. Nie;S. L. Olsen;H. P. Peng;R. G. Ping;N. D. Qi;H. Qin;J. F. Qiu;Z. Y. Ren;建国 陈;L. Y. Shan;L. Shang;C. P. Shen;D. L. Shen;肖雁 沈;H. Y. Sheng;H. S. Sun;J. F. Sun;S. S. Sun;Y. Z. Sun;Z. J. Sun;Z. Q. Tan;X. Tang;G. L. Tong;G. S. Varner;D. Y. Wang;L. Wang;L. L. Wang;L. S. Wang;萌 王;平 王;P. L. Wang;W. F. Wang;贻芳 王;Z. Wang;志勇 汪;Zhe Wang;Zheng Wang;C. L. Wei;D. H. Wei;N. Wu;X. M. Xia;X. X. Xie;G. F. Xu;X. P. Xu;Y. Xu;M. L. Yan;H. X. Yang;Y. X. Yang;铭汉 叶;Y. X. Ye;Z. Y. Yi;G. W. Yu;长征 苑;J. M. Yuan;Y. Yuan;S. L. Zang;Y. Zeng;Yu Zeng;B. X. Zhang;B. Y. Zhang;C. C. Zhang;D. H. Zhang;洪起 张;H. Y. Zhang;J. W. Zhang;J. Y. Zhang;S. H. Zhang;X. M. Zhang;X. Y. Zhang;Yiyun Zhang;Z. P. Zhang;D. X. Zhao;J. W. Zhao;M. G. Zhao;P. P. Zhao;W. R. Zhao;Z. G. Zhao;汉青 郑;J. P. Zheng;Z. P. Zheng;L. Zhou;N. F. Zhou;K. J. Zhu;Q. M. Zhu;Y. C. Zhu;Y. S. Zhu;Yingchun Zhu;Z. A. Zhu;B. A. Zhuang;X. A. Zhuang;冰松 邹

Physical Review D - Particles, Fields, Gravitation and Cosmology

2006

A partial wave analysis is presented of J/ψ→φπ ⁺π^- and φK⁺K^- from a sample of 58M J/ψ events in the BES II detector. The f₀(980) is observed clearly in both sets of data, and parameters of the Flatté formula are determined accurately: M=965±8(stat)±6(syst)MeV/c², g₁=165±10±15MeV/c², g₂/g ₁=4.21±0.25±0.21. The φππ data also exhibit a strong ππ peak centred at M=1335MeV/c². It may be fitted with f₂(1270) and a dominant 0⁺ signal made from f ₀(1370) interfering with a smaller f₀(1500) component. There is evidence that the f₀(1370) signal is resonant, from interference with f₂(1270). There is also a state in ππ with M=1790_-30⁺⁴⁰MeV/c² and Γ=270 _-30⁺⁶⁰MeV/c²; spin 0 is preferred over spin 2. This state, f₀(1790), is distinct from f₀(1710). The φKK̄ data contain a strong peak due to f₂′(1525). A shoulder on its upper side may be fitted by interference between f ₀(1500) and f₀(1710).

M. Ablikim;J. Z. Bai;Y. Ban;J. G. Bian;D. V. Bugg;X. Cai;J. F. Chang;H. F. Chen;H. S. Chen;H. X. Chen;J. C. Chen;Jin Chen;Jun Chen;M. L. Chen;Y. B. Chen;S. P. Chi;Y. P. Chu;X. Z. Cui;H. L. Dai;Y. S. Dai;Z. Y. Deng;燎原 董;Q. F. Dong;S. X. Du;Z. Z. Du;J. Fang;双世 房;C. D. Fu;H. Y. Fu;C. S. Gao;Y. N. Gao;M. Y. Gong;W. X. Gong;S. D. Gu;Y. N. Guo;Y. Q. Guo;Z. J. Guo;F. A. Harris;K. L. He;M. He;X. He;Y. K. Heng;H. M. Hu;T. Hu;G. S. Huang;X. P. Huang;X. T. Huang;X. B. Ji;C. H. Jiang;X. S. Jiang;D. P. Jin;S. Jin;Y. Jin;Yi Jin;Y. F. Lai;F. Li;G. Li;H. H. Li;J. Li;J. C. Li;Q. J. Li;R. Y. Li;S. M. Li;卫东 李;W. G. Li;晓磊 李;X. Q. Li;Y. L. Li;Y. F. Liang;H. B. Liao;C. X. Liu;F. Liu;Fang Liu;H. H. Liu;H. M. Liu;J. Liu;J. B. Liu;觉平 刘;R. G. Liu;Z. A. Liu;Z. X. Liu;F. Lu;G. R. Lu;H. J. Lu;J. G. Lu;C. L. Luo;L. X. Luo;X. L. Luo;凤才 马;H. L. Ma;J. M. Ma;L. L. Ma;Q. M. Ma;X. B. Ma;X. Y. Ma;Z. P. Mao;X. H. Mo;J. Nie;Z. D. Nie;S. L. Olsen;H. P. Peng;N. D. Qi;C. D. Qian;H. Qin;J. F. Qiu;Z. Y. Ren;建国 陈;L. Y. Shan;L. Shang;D. L. Shen;肖雁 沈;H. Y. Sheng;F. Shi;X. Shi;H. S. Sun;J. F. Sun;S. S. Sun;Y. Z. Sun;Z. J. Sun;X. Tang;N. Tao;Y. R. Tian;G. L. Tong;G. S. Varner;D. Y. Wang;J. Z. Wang;K. Wang;L. Wang;L. S. Wang;萌 王;平 王;P. L. Wang;S. Z. Wang;W. F. Wang;贻芳 王;政 王;Z. Y. Wang;Zhe Wang;Zheng Wang;C. L. Wei;D. H. Wei;Y. M. Wu;X. M. Xia;X. X. Xie;B. Xin;G. F. Xu;H. Xu;S. T. Xue;M. L. Yan;F. Yang;H. X. Yang;J. Yang;Y. X. Yang;M. Ye;铭汉 叶;Y. X. Ye;L. H. Yi;Z. Y. Yi;C. S. Yu;G. W. Yu;长征 苑;J. M. Yuan;Y. Yuan;S. L. Zang;Y. Zeng;Yu Zeng;B. X. Zhang;B. Y. Zhang;C. C. Zhang;D. H. Zhang;H. Y. Zhang;J. Zhang;J. W. Zhang;J. Y. Zhang;Q. J. Zhang;S. Q. Zhang;X. M. Zhang;X. Y. Zhang;Y. Y. Zhang;Yiyun Zhang;Z. P. Zhang;Z. Q. Zhang;D. X. Zhao;J. B. Zhao;J. W. Zhao;M. G. Zhao;P. P. Zhao;W. R. Zhao;X. J. Zhao;Y. B. Zhao;政国 赵;汉青 郑;J. P. Zheng;L. S. Zheng;Z. P. Zheng;X. C. Zhong;B. Q. Zhou;G. M. Zhou;L. Zhou;N. F. Zhou;K. J. Zhu;Q. M. Zhu;Y. C. Zhu;Y. S. Zhu;Yingchun Zhu;Z. A. Zhu;B. A. Zhuang;X. A. Zhuang;冰松 邹

Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics

2005-2-10

Using 2.25 × 10⁸, J/ψ events collected with the BESIII detector at the BEPCII storage rings, we observe for the first time the process J/ψ → pp¯a₀(980), a₀(980) → π⁰η with a significance of 6.5σ (3.2σ including systematic uncertainties). The product branching fraction of J/ψ → pp¯a₀ (980) → pp¯ π⁰η is measured to be (6.8 ± 1.2 ± 1.3) × 10^-5, where the first error is statistical and the second is systematic. This measurement provides information on the a₀ production near threshold coupling to pp and improves the understanding of the dynamics of J/ψ decays to four-body processes.

M. Ablikim;M. N. Achasov;X. C. Ai;O. Albayrak;M. Albrecht;D. J. Ambrose;F. F. An;Q. An;J. Z. Bai;R. Baldini Ferroli;Y. Ban;D. W. Bennett;J. V. Bennett;M. Bertani;D. Bettoni;J. M. Bian;F. Bianchi;E. Boger;O. Bondarenko;I. Boyko;S. Braun;R. A. Briere;浩 蔡;和生 陈;旭荣 陈;燎原 董;双世 房;立波 郭;性涛 黄;钢 李;海波 李;卫东 李;晓磊 李;觉平 刘;前 刘;凤才 马;加伦 平;建国 陈;肖雁 沈;洁琬 孙;昌建 唐;萌 王;贻芳 王;振军 肖;铭汉 叶;长征 苑;宏浩 张;政国 赵;阳恒 郑;冰松 邹

Physical Review D - Particles, Fields, Gravitation and Cosmology

2014-9-26

Based on 5.8 × 10⁷ J/ψ events detected in BESII, the branching fractions of J/ψ → φη and φη′ are measured for different η and η decay modes. The results are significantly higher than previous measurements. An upper limit on B(J/ψ → φη⁰) is also obtained.

M. Ablikim;J. Z. Bai;Y. Ban;J. G. Bian;X. Cai;J. F. Chang;H. F. Chen;H. S. Chen;H. X. Chen;J. C. Chen;Jin Chen;Jun Chen;M. L. Chen;Y. B. Chen;S. P. Chi;Y. P. Chu;X. Z. Cui;H. L. Dai;Y. S. Dai;Z. Y. Deng;燎原 董;Q. F. Dong;S. X. Du;Z. Z. Du;J. Fang;双世 房;C. D. Fu;H. Y. Fu;C. S. Gao;Y. N. Gao;M. Y. Gong;W. X. Gong;S. D. Gu;Y. N. Guo;Y. Q. Guo;Z. J. Guo;F. A. Harris;K. L. He;M. He;X. He;Y. K. Heng;H. M. Hu;T. Hu;G. S. Huang;X. P. Huang;X. T. Huang;X. B. Ji;C. H. Jiang;X. S. Jiang;D. P. Jin;S. Jin;Y. Jin;Yi Jin;Y. F. Lai;F. Li;钢 李;H. H. Li;J. Li;J. C. Li;Q. J. Li;R. Y. Li;S. M. Li;卫东 李;W. G. Li;X. L. Li;X. Q. Li;Y. L. Li;Y. F. Liang;H. B. Liao;C. X. Liu;F. Liu;Fang Liu;H. H. Liu;H. M. Liu;J. Liu;J. B. Liu;觉平 刘;R. G. Liu;Z. A. Liu;Z. X. Liu;F. Lu;G. R. Lu;H. J. Lu;J. G. Lu;C. L. Luo;L. X. Luo;X. L. Luo;凤才 马;H. L. Ma;J. M. Ma;L. L. Ma;Q. M. Ma;X. B. Ma;X. Y. Ma;Z. P. Mao;X. H. Mo;J. Nie;Z. D. Nie;S. L. Olsen;H. P. Peng;N. D. Qi;C. D. Qian;H. Qin;J. F. Qiu;Z. Y. Ren;建国 陈;L. Y. Shan;L. Shang;D. L. Shen;肖雁 沈;H. Y. Sheng;F. Shi;X. Shi;H. S. Sun;J. F. Sun;S. S. Sun;Y. Z. Sun;Z. J. Sun;X. Tang;N. Tao;Y. R. Tian;G. L. Tong;G. S. Varner;D. Y. Wang;J. Z. Wang;K. Wang;L. Wang;L. S. Wang;萌 王;平 王;P. L. Wang;S. Z. Wang;W. F. Wang;贻芳 王;政 王;志勇 汪;Zhe Wang;Zheng Wang;C. L. Wei;D. H. Wei;N. Wu;Y. M. Wu;X. M. Xia;X. X. Xie;B. Xin;G. F. Xu;H. Xu;S. T. Xue;M. L. Yan;F. Yang;H. X. Yang;J. Yang;Y. X. Yang;M. Ye;铭汉 叶;Y. X. Ye;L. H. Yi;Z. Y. Yi;C. S. Yu;G. W. Yu;长征 苑;J. M. Yuan;Y. Yuan;S. L. Zang;Y. Zeng;Yu Zeng;B. X. Zhang;B. Y. Zhang;C. C. Zhang;D. H. Zhang;H. Y. Zhang;J. Zhang;J. W. Zhang;J. Y. Zhang;Q. J. Zhang;S. Q. Zhang;X. M. Zhang;X. Y. Zhang;Y. Y. Zhang;Yiyun Zhang;Z. P. Zhang;晴 张;D. X. Zhao;J. B. Zhao;J. W. Zhao;M. G. Zhao;P. P. Zhao;W. R. Zhao;X. J. Zhao;Y. B. Zhao;Z. G. Zhao;汉青 郑;J. P. Zheng;L. S. Zheng;Z. P. Zheng;X. C. Zhong;B. Q. Zhou;G. M. Zhou;L. Zhou;N. F. Zhou;K. J. Zhu;Q. M. Zhu;Y. C. Zhu;Y. S. Zhu;Yingchun Zhu;Z. A. Zhu;B. A. Zhuang;X. A. Zhuang;冰松 邹

Physical Review D - Particles, Fields, Gravitation and Cosmology

2005-2

M. Ablikim;J. Z. Bai;Y. Ban;J. G. Bian;X. Cai;J. F. Chang;H. F. Chen;H. S. Chen;H. X. Chen;J. C. Chen;Jin Chen;Jun Chen;M. L. Chen;Y. B. Chen;S. P. Chi;Y. P. Chu;X. Z. Cui;H. L. Dai;Y. S. Dai;Z. Y. Deng;燎原 董;Q. F. Dong;S. X. Du;Z. Z. Du;J. Fang;双世 房;C. D. Fu;H. Y. Fu;C. S. Gao;Y. N. Gao;M. Y. Gong;W. X. Gong;S. D. Gu;Y. N. Guo;Y. Q. Guo;Z. J. Guo;F. A. Harris;K. L. He;M. He;X. He;Y. K. Heng;H. M. Hu;T. Hu;G. S. Huang;X. P. Huang;X. T. Huang;X. B. Ji;C. H. Jiang;X. S. Jiang;D. P. Jin;S. Jin;Y. Jin;Yi Jin;Y. F. Lai;F. Li;钢 李;H. H. Li;J. Li;J. C. Li;Q. J. Li;R. Y. Li;S. M. Li;卫东 李;W. G. Li;晓磊 李;X. Q. Li;Y. L. Li;Y. F. Liang;H. B. Liao;C. X. Liu;F. Liu;Fang Liu;H. H. Liu;H. M. Liu;J. Liu;J. B. Liu;觉平 刘;R. G. Liu;Z. A. Liu;Z. X. Liu;F. Lu;G. R. Lu;H. J. Lu;J. G. Lu;C. L. Luo;L. X. Luo;X. L. Luo;凤才 马;H. L. Ma;J. M. Ma;L. L. Ma;Q. M. Ma;X. B. Ma;X. Y. Ma;Z. P. Mao;X. H. Mo;J. Nie;Z. D. Nie;S. L. Olsen;H. P. Peng;N. D. Qi;C. D. Qian;H. Qin;J. F. Qiu;Z. Y. Ren;建国 陈;L. Y. Shan;L. Shang;D. L. Shen;肖雁 沈;H. Y. Sheng;F. Shi;X. Shi;H. S. Sun;J. F. Sun;S. S. Sun;Y. Z. Sun;Z. J. Sun;X. Tang;N. Tao;Y. R. Tian;G. L. Tong;G. S. Varner;D. Y. Wang;J. Z. Wang;K. Wang;L. Wang;L. S. Wang;M. Wang;P. Wang;P. L. Wang;S. Z. Wang;W. F. Wang;贻芳 王;Z. Wang;Z. Y. Wang;Zhe Wang;Zheng Wang;C. L. Wei;D. H. Wei;N. Wu;Y. M. Wu;X. M. Xia;X. X. Xie;B. Xin;G. F. Xu;H. Xu;S. T. Xue;M. L. Yan;F. Yang;H. X. Yang;J. Yang;Y. X. Yang;M. Ye;M. H. Ye;Y. X. Ye;L. H. Yi;Z. Y. Yi;C. S. Yu;G. W. Yu;长征 苑;J. M. Yuan;Y. Yuan;S. L. Zang;Y. Zeng;Yu Zeng;B. X. Zhang;B. Y. Zhang;C. C. Zhang;D. H. Zhang;H. Y. Zhang;J. Zhang;J. W. Zhang;J. Y. Zhang;Q. J. Zhang;S. Q. Zhang;X. M. Zhang;X. Y. Zhang;Y. Y. Zhang;Yiyun Zhang;Z. P. Zhang;晴 张;D. X. Zhao;J. B. Zhao;J. W. Zhao;M. G. Zhao;P. P. Zhao;W. R. Zhao;X. J. Zhao;Y. B. Zhao;Z. G. Zhao;汉青 郑;J. P. Zheng;L. S. Zheng;Z. P. Zheng;X. C. Zhong;B. Q. Zhou;G. M. Zhou;L. Zhou;N. F. Zhou;K. J. Zhu;Q. M. Zhu;Y. C. Zhu;Y. S. Zhu;Yingchun Zhu;Z. A. Zhu;B. A. Zhuang;X. A. Zhuang;冰松 邹

Physical Review D - Particles, Fields, Gravitation and Cosmology

2005-1

To investigate the nature of the φ(3770) resonance and to measure the cross section for e⁺e^-→DD, a cross-section scan data sample, distributed among 41 center-of-mass energy points from 3.73 to 3.89 GeV, was taken with the BESIII detector operated at the BEPCII collider in the year 2010. By analyzing the large angle Bhabha scattering events, we measure the integrated luminosity of the data sample at each center-of-mass energy point. The total integrated luminosity of the data sample is 76:16ϵ0:04±0:61 pb^-1, where the first uncertainty is statistical and the second systematic.

M. Ablikim;M. N. Achasov;S. Ahmed;M. Albrecht;M. Alekseev;A. Amoroso;F. F. An;Q. An;Y. Bai;O. Bakina;R. Baldini Ferroli;Y. Ban;K. Begzsuren;D. W. Bennett;J. V. Bennett;N. Berger;M. Bertani;D. Bettoni;F. Bianchi;E. Boger;I. Boyko;R. A. Briere;浩 蔡;X. Cai;和生 陈;旭荣 陈;燎原 董;双世 房;立波 郭;性涛 黄;钢 李;海波 李;卫东 李;晓磊 李;前 刘;加伦 平;建国 陈;肖雁 沈;洁琬 孙;昌建 唐;贻芳 王;志勇 汪;振军 肖;铭汉 叶;长征 苑;宏浩 张;尧 张;政国 赵;阳恒 郑;冰松 邹

Chinese Physics C

2018-5

It describes the feasibility and realization of using embedded Linux in DAQ readout system of high energy physics experiment. The first part, the hardware and software framework is introduced. And then emphasis is placed on the key technologies during the system realization. The development is based on the VME bus and vme_universe driver. Finally, the test result is presented: the readout system can work well in Embedded Linux OS.

Xiao Lu Ji;Mei Ye;Ke Jun Zhu;Xiao Nan Li;贻芳 王

Hedianzixue Yu Tance Jishu/Nuclear Electronics and Detection Technology

2010-1

Using e+e- annihilation data corresponding to an integrated luminosity of 3.19 fb-1 collected at a center-of-mass energy of 4.178 GeV with the BESIII detector, we measure the absolute branching fractions BDs+→ηe+νe=(2.323±0.063stat±0.063syst)% and BDs+→η′e+νe=(0.824±0.073stat±0.027syst)% via a tagged analysis technique, where one Ds is fully reconstructed in a hadronic mode. Combining these measurements with previous BESIII measurements of BD+→η(′)e+νe, the η-η′ mixing angle in the quark flavor basis is determined to be φP=(40.1±2.1stat±0.7syst)°. From the first measurements of the dynamics of Ds+→η(′)e+νe decays, the products of the hadronic form factors f+η(′)(0) and the Cabibbo-Kobayashi-Maskawa matrix element |Vcs| are determined with different form factor parametrizations. For the two-parameter series expansion, the results are f+η(0)|Vcs|=0.4455±0.0053stat±0.0044syst and f+η′(0)|Vcs|=0.477±0.049stat±0.011syst.

M. Ablikim;M. N. Achasov;S. Ahmed;M. Albrecht;M. Alekseev;A. Amoroso;F. F. An;琪 安;J. Z. Bai;Y. Bai;O. Bakina;R. Baldini Ferroli;Y. Ban;K. Begzsuren;D. W. Bennett;J. V. Bennett;N. Berger;M. Bertani;D. Bettoni;F. Bianchi;E. Boger;I. Boyko;R. A. Briere;H. Cai;X. Cai;A. Calcaterra;G. F. Cao;旭荣 陈;燎原 董;双世 房;立波 郭;性涛 黄;海波 李;卫东 李;晓磊 李;翔 刘;加伦 平;建国 陈;肖雁 沈;洁琬 孙;昌建 唐;贻芳 王;振军 肖;铭汉 叶;长征 苑;宏浩 张;尧 张;政国 赵;阳恒 郑;冰松 邹

Physical Review Letters

2019-3-25

The Jiangmen Underground Neutrino Observatory (JUNO), a 20 kton multi-purpose 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 3-4σ 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 sin²θ₁₂, Δm₂₁², and | Δm_ee² 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 ∼5000 inverse-beta-decay events and ∼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 ∼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 θ₂₃ mixing angle. Detection of the ⁷Be and ⁸B 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 eV² < Δm₄₁² < 10^-2 eV² and a sufficiently large mixing angle θ₁₄ 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⁺ + ν 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.

Fengpeng An;Guangpeng An;琪 安;Vito Antonelli;Eric Baussan;John Beacom;Leonid Bezrukov;Simon Blyth;Riccardo Brugnera;Margherita Buizza Avanzini;Jose Busto;Anatael Cabrera;浩 蔡;Xiao Cai;Antonio Cammi;Guofu Cao;俊 曹;Yun Chang;Shaomin Chen;Shenjian Chen;义学 陈;Davide Chiesa;Massimiliano Clemenza;Barbara Clerbaux;Janet Conrad;Davide D'Angelo;Hervé De Kerret;Zhi Deng;Ziyan Deng;Yayun Ding;Zelimir Djurcic;Damien Dornic;Marcos Dracos;Olivier Drapier;Stefano Dusini;Stephen Dye;Timo Enqvist;Donghua Fan;Jian Fang;Laurent Favart;Richard Ford;Marianne Göger-Neff;Haonan Gan;Alberto Garfagnini;Marco Giammarchi;Maxim Gonchar;Guanghua Gong;Hui Gong;Michel Gonin;Marco Grassi;Christian Grewing;Mengyun Guan;Vic Guarino;Gang Guo;Wanlei Guo;Xin Heng Guo;Caren Hagner;Ran Han;Miao He;Yuekun Heng;Yee Hsiung;Jun Hu;Shouyang Hu;Tao Hu;Hanxiong Huang;性涛 黄;Lei Huo;Ara Ioannisian;Manfred Jeitler;Xiangdong Ji;Xiaoshan Jiang;Cécile Jollet;Li Kang;Michael Karagounis;Narine Kazarian;Zinovy Krumshteyn;Andre Kruth;Pasi Kuusiniemi;Tobias Lachenmaier;Rupert Leitner;Chao Li;Jiaxing Li;卫东 李;Weiguo Li;晓梅 李;Xiaonan Li;Yi Li;Yufeng Li;Zhi Bing Li;Hao Liang;Guey Lin Lin;Tao Lin;Yen Hsun Lin;Jiajie Ling;Ivano Lippi;Dawei Liu;Hongbang Liu;Hu Liu;江来 刘;Jianli Liu;Jinchang Liu;前 刘;Shubin Liu;Shulin Liu;Paolo Lombardi;Yongbing Long;Haoqi Lu;Jiashu Lu;Jingbin Lu;Junguang Lu;Bayarto Lubsandorzhiev;Livia Ludhova;Shu Luo;Vladimir Lyashuk;Randolph Möllenberg;Xubo Ma;Fabio Mantovani;Yajun Mao;Stefano M. Mari;William F. McDonough;Guang Meng;Anselmo Meregaglia;Emanuela Meroni;Mauro Mezzetto;Lino Miramonti;Thomas Mueller;Dmitry Naumov;Lothar Oberauer;Juan Pedro Ochoa-Ricoux;Alexander Olshevskiy;Fausto Ortica;Alessandro Paoloni;Haiping Peng;Jen Chieh Peng;Ezio Previtali;Ming Qi;Sen Qian;Xin Qian;Yongzhong Qian;Zhonghua Qin;Georg Raffelt;Gioacchino Ranucci;Barbara Ricci;Markus Robens;Aldo Romani;Xiangdong Ruan;Xichao Ruan;Giuseppe Salamanna;Mike Shaevitz;Valery Sinev;Chiara Sirignano;Monica Sisti;Oleg Smirnov;Michael Soiron;Achim Stahl;Luca Stanco;Jochen Steinmann;Xilei Sun;洁琬 孙;Dmitriy Taichenachev;Jian Tang;Igor Tkachev;Wladyslaw Trzaska;Stefan Van Waasen;Cristina Volpe;Vit Vorobel;Lucia Votano;Chung Hsiang Wang;立国 王;Hao Wang;Meng Wang;Ruiguang Wang;Siguang Wang;Wei Wang;Yi Wang;贻芳 王;Zhe Wang;政 王;Zhigang Wang;Zhimin Wang;Wei Wei;Liangjian Wen;Christopher Wiebusch;Björn Wonsak;Qun Wu;Claudia Elisabeth Wulz;Michael Wurm;Yufei Xi;Dongmei Xia;Yuguang Xie;Zhi Zhong Xing;Jilei Xu;Baojun Yan;Changgen Yang;朝文 杨;Guang Yang;Lei Yang;Yifan Yang;Yu Yao;Ugur Yegin;Frédéric Yermia;Zhengyun You;Boxiang Yu;Chunxu Yu;Zeyuan Yu;Sandra Zavatarelli;Liang Zhan;Chao Zhang;宏浩 张;Jiawen Zhang;Jingbo Zhang;Qingmin Zhang;Yu Mei Zhang;Zhenyu Zhang;Zhenghua Zhao;阳恒 郑;Weili Zhong;Guorong Zhou;Jing Zhou;Li Zhou;Rong Zhou;Shun Zhou;Wenxiong Zhou;Xiang Zhou;Yeling Zhou;宇峰 周;Jiaheng Zou

Journal of Physics G: Nuclear and Particle Physics

2016-2-10

We have carefully examined, in both analytical and numerical ways, how small the terrestrial matter effects can be in a given medium-baseline reactor antineutrino oscillation experiment like JUNO or RENO-50. Taking the forthcoming JUNO experiment as an example, we show that the inclusion of terrestrial matter effects may reduce the sensitivity of the neutrino mass ordering measurement by Δ ² _MO≃ 0:6, and a neglect of such effects may shift the best-fit values of the avor mixing angle θ12 and the neutrino mass-squared di-erence θ21 by about 1αto 2α in the future data analysis. In addition, a preliminary estimate indicates that a 2α sensitivity of establishing the terrestrial matter effects can be achieved for about 10 years of data taking at JUNO with the help of a suitable near detector implementation.

Yu Feng Li;贻芳 王;Zhi Zhong Xing

Chinese Physics C

2016-9