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Journal of Physics: Conference Series 2019年第1期1423卷

作者： Zhao, Jiankun Xiong, Chao Yan, Wenxun Ge, Liangquan School of Nuclear Science and Engineering East China University of Technology Nanchang 330013 China College of Applied Nuclear Technology and Automation Engineering Chengdu University of Technology Chengdu 610059 China Fundamental Science on Radioactive Geology and Exploration Technology Laboratory East China Institute of Technology Nanchang Jiangxi 330013 China School of Nuclear Science and Engineering East China University of Technology Nanchang 330013 China Fundamental Science on Radioactive Geology and Exploration Technology Laboratory East China Institute of Technology Nanchang Jiangxi 330013 China School of Nuclear Science and Engineering East China University of Technology Nanchang 330013 China College of Applied Nuclear Technology and Automation Engineering Chengdu University of Technology Chengdu 610059 China

As “banded structure” is a vexed question in orbital Gamma spectroscopy data inversion. In this paper, a new method to level the lunar global data of average atomic number by the fiducial-value in the stable composition circle is proposed. In order to verify the accuracy, the existing moon-sampling rock data as the “standard sample” and fast neutron data are also presented. The slope of the positive fit curve is 1.875 and the correlation coefficient is 0.72. And some geological characteristics, such as the structural boundaries and internal features of the Antarctic Aiken Basin, can identify obviously.

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Constraining the Cosmic-ray Energy Based on Observations of Nearby Galaxy Clusters by LHAASO

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arXiv 2025年

作者： Cao, Zhen Aharonian, F. Bai, Y.X. Bao, Y.W. Bastieri, D. Bi, X.J. Bi, Y.J. Bian, W. Bukevich, A.V. Cai, C.M. Cao, W.Y. Cao, Zhe Chang, J. Chang, J.F. Chen, A.M. Chen, E.S. Chen, H.X. Chen, Liang Chen, Long Chen, M.J. Chen, M.L. Chen, Q.H. Chen, S. Chen, S.H. Chen, S.Z. Chen, T.L. Chen, X.B. Chen, X.J. Chen, Y. Cheng, N. Cheng, Y.D. Chu, M.C. Cui, M.Y. Cui, S.W. Cui, X.H. Cui, Y.D. Dai, B.Z. Dai, H.L. Dai, Z.G. Danzengluobu Diao, Y.X. Dong, X.Q. Duan, K.K. Fan, J.H. Fan, Y.Z. Fang, J. Fang, J.H. Fang, K. Feng, C.F. Feng, H. Feng, L. Feng, S.H. Feng, X.T. Feng, Y. Feng, Y.L. Gabici, S. Gao, B. Gao, C.D. Gao, Q. Gao, W. Gao, W.K. Ge, M.M. Ge, T.T. Geng, L.S. Giacinti, G. Gong, G.H. Gou, Q.B. Gu, M.H. Guo, F.L. Guo, J. Guo, X.L. Guo, Y.Q. Guo, Y.Y. Han, Y.A. Hannuksela, O.A. Hasan, M. He, H.H. He, H.N. He, J.Y. He, X.Y. He, Y. Hernández-Cadena, S. Hor, Y.K. Hou, B.W. Hou, C. Hou, X. Hu, H.B. Hu, S.C. Huang, C. Huang, D.H. Huang, J.J. Huang, T.Q. Huang, W.J. Huang, X.T. Huang, X.Y. Huang, Y. Huang, Y.Y. Ji, X.L. Jia, H.Y. Jia, K. Jiang, H.B. Jiang, K. Jiang, X.W. Jiang, Z.J. Jin, M. Kaci, S. Kang, M.M. Karpikov, I. Khangulyan, D. Kuleshov, D. Kurinov, K. Li, B.B. Li, Cheng Li, Cong Li, D. Li, F. Li, H.B. Li, H.C. Li, Jian Li, Jie Li, K. Li, L. Li, R.L. Li, S.D. Li, T.Y. Li, W.L. Li, X.R. Li, Xin Li, Y.Z. Li, Zhe Li, Zhuo Liang, E.W. Liang, Y.F. Lin, S.J. Liu, B. Liu, C. Liu, D. Liu, D.B. Liu, H. Liu, H.D. Liu, J. Liu, J.L. Liu, J.R. Liu, M.Y. Liu, R.Y. Liu, S.M. Liu, W. Liu, X. Liu, Y. Liu, Y. Liu, Y.N. Lou, Y.Q. Luo, Q. Luo, Y. Lv, H.K. Ma, B.Q. Ma, L.L. Ma, X.H. Mao, J.R. Min, Z. Mitthumsiri, W. Mou, G.B. Mu, H.J. Nan, Y.C. Neronov, A. Ng, K.C.Y. Ni, M.Y. Nie, L. Ou, L.J. Pattarakijwanich, P. Pei, Z.Y. Qi, J.C. Key Laboratory of Particle Experimental Physics Division Computing Center Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China University of Chinese Academy of Sciences Beijing100049 China TIANFU Cosmic Ray Research Center Sichuan Chengdu China University of Science and Technology of China Anhui Hefei230026 China Yerevan State University 1 Alek Manukyan Street Yerevan0025 Armenia Max-Planck-Institut for Nuclear Physics P.O. Box 103980 Heidelberg69029 Germany Tsung-Dao Lee Institute School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Center for Astrophysics Guangzhou University Guangdong Guangzhou510006 China Institute for Nuclear Research of Russian Academy of Sciences Moscow117312 Russia School of Physical Science and Technology School of Information Science and Technology Southwest Jiaotong University Sichuan Chengdu610031 China State Key Laboratory of Particle Detection and Electronics China Key Laboratory of Dark Matter and Space Astronomy Key Laboratory of Radio Astronomy Purple Mountain Observatory Chinese Academy of Sciences Jiangsu Nanjing210023 China Research Center for Astronomical Computing Zhejiang Laboratory Zhejiang Hangzhou311121 China Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China School of Physics and Astronomy Yunnan University Yunnan Kunming650091 China Key Laboratory of Cosmic Rays Tibet University Ministry of Education Tibet Lhasa850000 China School of Astronomy and Space Science Nanjing University Jiangsu Nanjing210023 China Department of Physics The Chinese University of Hong Kong New Territories Shatin Hong Kong Hebei Normal University Hebei Shijiazhuang050024 China Key Laboratory of Radio Astronomy and Technology National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Sun Yat-sen University Guangdong Zhuhai519000 China Sun Yat-sen University Guangdong Guangzhou510275

Galaxy clusters act as reservoirs of high-energy cosmic rays (CRs). As CRs propagate through the intracluster medium, they generate diffuse γ-rays detectable by arrays such as LHAASO. These γ-rays result from proton-proton (pp) collisions of very high-energy cosmic rays (VHECRs) or inverse Compton (IC) scattering of positron-electron pairs created by pγ interactions of ultra-high-energy cosmic rays (UHECRs). We analyzed diffuse γ-ray emission from the Coma, Perseus, and Virgo clusters using LHAASO data. Diffuse emission was modeled as a disk of radius R500 for each cluster while accounting for point sources. No significant diffuse emission was detected, yielding 95% confidence level (C.L.) upper limits on the γ-ray flux: for WCDA (1–25 TeV) and KM2A (>25 TeV), less than (49.4, 13.7, 54.0) and (1.34, 1.14, 0.40) ×10−14 ph cm−2 s−1 for Coma, Perseus, and Virgo, respectively. The γ-ray upper limits can be used to derive model-independent constraints on the integral energy of CRp above 10 TeV (corresponding to the LHAASO observational range > 1 TeV under the pp scenario) to be less than (1.96, 0.59, 0.08) × 1061 erg. The absence of detectable annuli/ring-like structures, indicative of cluster accretion or merging shocks, imposes further constraints on models in which the UHECRs are accelerated in the merging shocks of galaxy clusters. Copyright © 2025, The Authors. All rights reserved.

关键词： Cosmic rays

Calibration of the air shower energy scale of the water and air Cherenkov techniques in the LHAASO experiment

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Physical Review D 2021年第6期104卷 062007-062007页

作者： F. Aharonian Q. An Axikegu L. X. Bai Y. X. Bai Y. W. Bao D. Bastieri X. J. Bi Y. J. Bi H. Cai J. T. Cai Zhen Cao Zhe Cao J. Chang J. F. Chang B. M. Chen E. S. Chen J. Chen Liang Chen Long Chen M. J. Chen M. L. Chen Q. H. Chen S. H. Chen S. Z. Chen T. L. Chen X. L. Chen Y. Chen N. Cheng Y. D. Cheng S. W. Cui X. H. Cui Y. D. Cui B. Z. Dai H. L. Dai Z. G. Dai Danzengluobu D. della Volpe B. D’Ettorre Piazzoli X. J. Dong K. K. Duan J. H. Fan Y. Z. Fan Z. X. Fan J. Fang K. Fang C. F. Feng L. Feng S. H. Feng Y. L. Feng B. Gao C. D. Gao L. Q. Gao Q. Gao W. Gao M. M. Ge L. S. Geng G. H. Gong Q. B. Gou M. H. Gu F. L. Guo J. G. Guo X. L. Guo Y. Q. Guo Y. Y. Guo Y. A. Han H. H. He H. N. He J. C. He S. L. He X. B. He Y. He M. Heller Y. K. Hor C. Hou H. B. Hu S. Hu S. C. Hu X. J. Hu D. H. Huang Q. L. Huang W. H. Huang X. T. Huang X. Y. Huang Z. C. Huang F. Ji X. L. Ji H. Y. Jia K. Jiang Z. J. Jiang C. Jin T. Ke D. Kuleshov K. Levochkin B. B. Li Cong Li Cheng Li F. Li H. B. Li H. C. Li H. Y. Li J. Li K. Li W. L. Li Xin Li X. R. Li Y. Li Y. Z. Li Zhe Li Zhuo Li E. W. Liang Y. F. Liang S. J. Lin B. Liu C. Liu D. Liu H. Liu H. D. Liu J. Liu J. L. Liu J. S. Liu J. Y. Liu M. Y. Liu R. Y. Liu S. M. Liu W. Liu Y. Liu Y. N. Liu Z. X. Liu W. J. Long R. Lu H. K. Lv B. Q. Ma L. L. Ma X. H. Ma J. R. Mao A. Masood Z. Min W. Mitthumsiri T. Montaruli Y. C. Nan B. Y. Pang P. Pattarakijwanich Z. Y. Pei M. Y. Qi Y. Q. Qi B. Q. Qiao J. J. Qin D. Ruffolo V. Rulev A. Sáiz L. Shao O. Shchegolev X. D. Sheng J. Y. Shi H. C. Song Yu. V. Stenkin V. Stepanov Y. Su Q. N. Sun X. N. Sun Z. B. Sun P. H. T. Tam Z. B. Tang W. W. Tian B. D. Wang C. Wang H. Wang H. G. Wang J. C. Wang J. S. Wang L. P. Wang L. Y. Wang R. N. Wang W. Wang X. G. Wang X. J. Wang X. Y. Wang Y. Wang Y. D. Wang Y. J. Wang Y. P. Wang Z. H. Wang Z. X. Wang Zhen Wang Zheng Wang D. M. Wei J. J. Wei Y. J. Wei T. Wen C. Y. Wu H. R. Wu S. Wu W. X. Wu X. F. Wu S. Q. Xi J. Xia J. J. Xia G. M. Xiang D. X. Xiao G. Xiao H. B. Xiao G. G. Xin Y. L. Xin Y. Xing D. L. Xu R. X. Xu L. Xue D. H. Yan J. Z. Dublin Institute for Advanced Studies 31 Fitzwilliam Place 2 Dublin Ireland Max-Planck-Institut for Nuclear Physics P.O. Box 103980 69029 Heidelberg Germany State Key Laboratory of Particle Detection and Electronics China University of Science and Technology of China 230026 Hefei Anhui China School of Physical Science and Technology & School of Information Science and Technology Southwest Jiaotong University 610031 Chengdu Sichuan China College of Physics Sichuan University 610065 Chengdu Sichuan China Key Laboratory of Particle Astrophysics & Experimental Physics Division & Computing Center Institute of High Energy Physics Chinese Academy of Sciences 100049 Beijing China TIANFU Cosmic Ray Research Center Chengdu Sichuan China School of Astronomy and Space Science Nanjing University 210023 Nanjing Jiangsu China Center for Astrophysics Guangzhou University 510006 Guangzhou Guangdong China University of Chinese Academy of Sciences 100049 Beijing China School of Physics and Technology Wuhan University 430072 Wuhan Hubei China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences 210023 Nanjing Jiangsu China Hebei Normal University 050024 Shijiazhuang Hebei China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences 200030 Shanghai China Key Laboratory of Cosmic Rays (Tibet University) Ministry of Education 850000 Lhasa Tibet China National Astronomical Observatories Chinese Academy of Sciences 100101 Beijing China School of Physics and Astronomy & School of Physics (Guangzhou) Sun Yat-sen University 519082 Zhuhai Guangdong China School of Physics and Astronomy Yunnan University 650091 Kunming Yunnan China Département de Physique Nucléaire et Corpusculaire Faculté de Sciences Université de Genève 24 Quai Ernest Ansermet 1211 Geneva Switzerland Dipartimento di Fisica dell’Università di Napoli “Federico II” Complesso Universitario di Mo

The Wide Field-of-View Cherenkov Telescope Array (WFCTA) and the Water Cherenkov Detector Array (WCDA) of LHAASO are designed to work in combination for measuring the energy spectra of the cosmic ray species over a very wide energy range from a few TeV to 10 PeV. The energy calibration can be achieved with a proven technique of measuring the westward shift of the Moon shadow cast by galactic cosmic rays due to the geomagnetic field. This deflection angle Δ is inversely proportional to the cosmic ray rigidity. The precise measurement of the shifts by WCDA allows us to calibrate its energy scale for energies as high as 35 TeV. Through a set of commonly triggered events, the energy scales can be propagated to WFCTA. The energies of the events can be derived both by WCDA-1 and WFCTA with the median energies 23.4±0.1±1.3 TeV and (21.9±0.1 TeV), respectively, which are consistent within uncertainties. In addition, the propagation of the energy scale is also validated by the Moon shadow based on the same data selection criteria of the commonly triggered events. This paper reports, for the first time, an observational measurement of the absolute energy scale of the primary cosmic rays generating showers observed by air Cherenkov telescopes.

关键词： Cosmic ray composition & spectra

Achieving High Hetero-Deformation Induced (HDI) Strengthening and Hardening in Brass by Dual Heterostructures

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SSRN

SSRN 2020年

作者： Fang, X.T. Li, Z.K. Wang, Y.F. Ruiz, M. Ma, X.L. Wang, H.Y. Zhu, Y. Schoell, R. Zheng, C. Kaoumi, D. Zhu, Y.T. Department of Materials Science and Engineering North Carolina State University RaleighNC27695 United States Key Laboratory for Anisotropy and Texture of Materials of Ministry of Education Northeastern University Shenyang110819 China School of Aeronautics and Astronautics Sichuan University Chengdu610065 China Department of Materials Science and Engineering Texas A&M University College StationTX77840 United States Department of Mechanical and Aerospace Engineering North Carolina State University RaleighNC27695 United States Department of Nuclear Engineering North Carolina State University RaleighNC27695 United States Science and Technology on Thermostructural Composite Materials Laboratory Northwestern Polytechnical University Xi’an710072 China Nano and Heterogeneous Structural Materials Center Nanjing University of Science and Technology Nanjing210094 China

Heterostructured materials have a superior combination of strength and ductility, due to their ability to produce hetero-deform induced (HDI) strengthening and hardening. Therefore, achieving high HDI strengthening and hardening is a goal for designing heterostructures. Here we report a dual heterostructure in brass that includes heterogeneous lamella and gradient structures, fabricated by rolling, partial annealing and rotationally accelerated shot peening (RASP). Extraordinary HDI strengthening and hardening were achieved by the dual heterostructures, which led to a more superior combination of strength and ductility, than the single heterostructures. This finding presents a new pathway to designing heterostructures in metallic materials. © 2020, The Authors. All rights reserved.

关键词： Deformation

Effectiveness of Fiber Bragg Grating monitoring in the centrifugal model test of soil slope under rainfall conditions

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Journal of Mountain Science 2017年第5期14卷 936-947页

作者： LI Long-qi JU Neng-pan GUO Yong-xing State Key Laboratory of Geohazard Prevention and Geoenvironment Protection Chengdu University of Technology Chengdu 610059 China College of Environment and Civil Engineering Chengdu University of Technology Chengdu 610059 China School of Machinery and Automation Wuhan University of Science and Technology Wuhan 430081 China

Centrifugal model testsare playing an increasingly importantrolein investigating slope characteristics under rainfall conditions. However, conventional electronic transducers usually fail during centrifugal model tests because of the impacts of limitedtest space, high centrifugal force, and presence of water, with the result that limited valid data is obtained. In this study, Fiber Bragg Grating(FBG) sensing technology is employed in the design and development of displacement gauge, an anchor force gauge and an anti-slide pile moment gauge for use on centrifugal model slopes with and without a retaining structure. The two model slopes were installed and monitored at a centrifugal acceleration of 100 g. The test results show that the sensors developed succeed in capturing the deformation and retaining structure mechanical response of the model slopes during and after rainfall. The deformation curvefor the slope without retaining structure shows a steepresponse that turns gradualfor the slope with retaining structure. Importantly, for the slope with the retaining structure, results suggest that more attention be paid to increase of anchor force and antislide pile moment during rainfall. This study verifies the effectiveness of FBG sensing technology in centrifuge research and presents a new and innovative method for slope model testing under rainfall conditions.

关键词： Fiber Bragg Grating sensing technology Centrifugal model test Soil slope Rainfall conditions Slope displacement

Determination of responses of liquid xenon to low energy electron and nuclear recoils using the PandaX-II detector

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arXiv 2021年

作者： Yan, Binbin Abdukerim, Abdusalam Chen, Wei Chen, Xun Chen, Yunhua Cheng, Chen Cui, Xiangyi Fan, Yingjie Fang, Deqing Fu, Changbo Fu, Mengting Geng, Lisheng Giboni, Karl Gu, Linhui Guo, Xuyuan Han, Ke He, Changda Huang, Di Huang, Peiyao Huang, Yan Huang, Yanlin Huang, Zhou Ji, Xiangdong Ju, Yonglin Li, Shuaijie Liu, Jianglai Lei, Zhuoqun Ma, Wenbo Ma, Yugang Mao, Yajun Meng, Yue Ni, Kaixiang Ning, Jinhua Ning, Xuyang Ren, Xiangxiang Shang, Changsong Si, Lin Shen, Guofang Tan, Andi Wang, Anqing Wang, Hongwei Wang, Meng Wang, Qiuhong Wang, Siguang Wang, Wei Wang, Xiuli Wang, Zhou Wu, Mengmeng Wu, Shiyong Wu, Weihao Xia, Jingkai Xiao, Mengjiao Xie, Pengwei Yan, Rui Yang, Jijun Yang, Yong Yu, Chunxu Yuan, Jumin Yuan, Ying Yue, Jianfeng Zeng, Xinning Zhang, Dan Zhang, Tao Zhao, Li Zheng, Qibin Zhou, Jifang Zhou, Ning Zhou, Xiaopeng School of Physics and Astronomy Shanghai Jiao Tong University MOE Key Laboratory for Particle Astrophysics and Cosmology Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai200240 China Shanghai Institute of Applied Physics Chinese Academy of Sciences Shanghai201800 China Institute of Modern Physics Fudan University Shanghai200433 China Shanghai Jiao Tong University Sichuan Research Institute Chengdu610213 China Yalong River Hydropower Development Company Ltd. 288 Shuanglin Road Chengdu610051 China School of Physics Sun Yat-Sen University Guangzhou510275 China Tsung-Dao Lee Institute Shanghai200240 China School of Physics Nankai University Tianjin300071 China Institute of Modern Physics Fudan University Shanghai200433 China School of Physics Peking University Beijing100871 China School of Physics Beihang University Beijing100191 China International Research Center for Nuclei and Particles in the Cosmos Beijing Key Laboratory of Advanced Nuclear Materials and Physics Beihang University Beijing100191 China School of Medical Instrument and Food Engineering University of Shanghai for Science and Technology Shanghai200093 China Department of Physics University of Maryland College ParkMD20742 United States School of Mechanical Engineering Shanghai Jiao Tong University Shanghai200240 China Shandong University Jinan250100 China Shanghai Advanced Research Institute Chinese Academy of Sciences Shanghai201210 China Center for High Energy Physics Peking University Beijing100871 China

We report a systematic determination of the responses of PandaX-II, a dual phase xenon time projection chamber detector, to low energy recoils. The electron recoil (ER) and nuclear recoil (NR) responses are calibrated, respectively, with injected tritiated methane or 220Rn source, and with 241Am-Be neutron source, within an energy range from 1 − 25 keV (ER) and 4 − 80 keV (NR), under the two drift fields of 400 and 317 V/cm. An empirical model is used to fit the light yield and charge yield for both types of recoils. The best fit models can well describe the calibration data. The systematic uncertainties of the fitted models are obtained via statistical comparison against the data. Copyright © 2021, The Authors. All rights reserved.

关键词： Calibration

Electron-Ion Collider in China

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arXiv 2021年

作者： Anderle, Daniele P. Bertone, Valerio Cao, Xu Chang, Lei Chang, Ningbo Chen, Gu Chen, Xurong Chen, Zhuojun Cui, Zhufang Dai, Lingyun Deng, Weitian Ding, Minghui Feng, Xu Gong, Chang Gui, Longcheng Guo, Feng-Kun Han, Chengdong He, Jun Hou, Tie-Jiun Huang, Hongxia Huang, Yin Kumerički, Krešimir Kaptari, L.P. Li, Demin Li, Hengne Li, Minxiang Li, Xueqian Liang, Yutie Liang, Zuotang Liu, Chen Liu, Chuan Liu, Guoming Liu, Jie Liu, Liuming Liu, Xiang Liu, Tianbo Luo, Xiaofeng Lyu, Zhun Ma, Boqiang Ma, Fu Ma, Jianping Ma, Yugang Mao, Lijun Mezrag, Cédric Moutarde, Hervé Ping, Jialun Qin, Sixue Ren, Hang Roberts, Craig D. Rojo, Juan Shen, Guodong Shi, Chao Song, Qintao Sun, Hao Sznajder, Pawel Wang, Enke Wang, Fan Wang, Qian Wang, Rong Wang, Ruiru Wang, Taofeng Wang, Wei Wang, Xiaoyu Wang, Xiaoyun Wu, Jiajun Wu, Xinggang Xia, Lei Xiao, Bowen Xiao, Guoqing Xie, Ju-Jun Xie, Yaping H., Xing H., Xu N., Xu S., Xu M., Yan W., Yan W., Yan X., Yan J., Yang Y.-B., Yang Z., Yang D., Yao P., Yin C.-P., Yuan W., Zhan J., Zhang J., Zhang P., Zhang C.-H., Chang Z., Zhang H., Zhao K.-T., Chao Q., Zhao Y., Zhao Z., Zhao L., Zheng J., Zhou X., Zhou X., Zhou B., Zou L., Zou Guangdong Provincial Key Laboratory of Nuclear Science Institute of Quantum Matter South China Normal University Guangzhou510006 China IRFU CEA Université Paris-Saclay Gif-sur-YvetteF-91191 France Institute of Modern Physics Chinese Academy of Sciences Lanzhou730000 China University of Chinese Academy of Sciences Beijing100049 China Nankai University Tianjin300071 China Xinyang Normal University Xinyang464000 China School of Physics and Materials Science Guangzhou University Guangzhou510006 China Hunan University Changsha410082 China Nanjing University Nanjing210093 China Huazhong University of Science and Technology Wuhan430074 China Fondazione Bruno Kessler Villa Tambosi Strada delle Tabarelle 286 VillazzanoTNI-38123 Italy School of Physics Peking University Beijing100871 China Hunan Normal University Changsha410081 China Institute of Theoretical Physics Chinese Academy of Sciences Beijing100190 China Nanjing normal university Nanjing210023 China Department of Physics College of Sciences Northeastern University Shenyang110819 China Southwest Jiaotong University Chengdu610000 China Department of Physics Faculty of Science University of Zagreb Bijenička c. 32 Zagreb10000 Croatia Bogoliubov Laboratory of Theoretical Physics Joint Institute for Nuclear Research Dubna141980 Russia School of Physics and Microelectronics Zhengzhou University Zhengzhou450001 China Lanzhou university Lanzhou730000 China Shandong University Qingdao266237 China Institute of Particle Physics Central China Normal University Wuhan430079 China School of Physics Southeast University Nanjing211189 China Institute of Modern Physics Fudan University Shanghai200433 China Shanghai Institute of Applied Physics Chinese Academy of Sciences Shanghai201800 China Department of Physics Chongqing University Chongqing401331 China Department of Physics and Astronomy Vrije Universiteit Amsterdam De Boelelaan 1081 Amsterdam1081HV Netherlands Nik

Lepton scattering is an established ideal tool for studying inner structure of small particles such as nucleons as well as nuclei. As a future high energy nuclear physics project, an Electron-ion collider in China (EicC) has been proposed. It will be constructed based on an upgraded heavy-ion accelerator, High Intensity heavy-ion Accelerator Facility (HIAF) which is currently under construction, together with a new electron ring. The proposed collider will provide highly polarized electrons (with a polarization of ∼80%) and protons (with a polarization of ∼70%) with variable center of mass energies from 15 to 20 GeV and the luminosity of (2-3) × 1033 cm−2 s−1. Polarized deuterons and Helium-3, as well as unpolarized ion beams from Carbon to Uranium, will be also available at the EicC. The main foci of the EicC will be precision measurements of the structure of the nucleon in the sea quark region, including 3D tomography of nucleon;the partonic structure of nuclei and the parton interaction with the nuclear environment;the exotic states, especially those with heavy flavor quark contents. In addition, issues fundamental to understanding the origin of mass could be addressed by measurements of heavy quarkonia near-threshold production at the EicC. In order to achieve the above-mentioned physics goals, a hermetical detector system will be constructed with cutting-edge technologies. This document is the result of collective contributions and valuable inputs from experts across the globe. The EicC physics program complements the ongoing scientific programs at the Jefferson Laboratory and the future EIC project in the United States. The success of this project will also advance both nuclear and particle physics as well as accelerator and detector technology in China. © 2021, CC BY.

关键词： Polarization

Calibration of the air shower energy scale of the water and air cherenkov techniques in the LHAASO experiment

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arXiv 2021年

作者： Aharonian, F. An, Q. Axikegu Bai, L.X. Bai, Y.X. Bao, Y.W. Bastieri, D. Bi, X.J. Bi, Y.J. Cai, H. Cai, J.T. Cao, Z. Cao, Z. Chang, J. Chang, J.F. Chang, X.C. Chen, B.M. Chen, J. Chen, L. Chen, L. Chen, L. Chen, M.J. Chen, M.L. Chen, Q.H. Chen, S.H. Chen, S.Z. Chen, T.L. Chen, X.L. Chen, Y. Cheng, N. Cheng, Y.D. Cui, S.W. Cui, X.H. Cui, Y.D. Dai, B.Z. Dai, H.L. Dai, Z.G. Danzengluobu della Volpe, D. D'Ettorre Piazzoli, B. Dong, X.J. Fan, J.H. Fan, Y.Z. Fan, Z.X. Fang, J. Fang, K. Feng, C.F. Feng, L. Feng, S.H. Feng, Y.L. Gao, B. Gao, C.D. Gao, Q. Gao, W. Ge, M.M. Geng, L.S. Gong, G.H. Gou, Q.B. Gu, M.H. Guo, J.G. Guo, X.L. Guo, Y.Q. Guo, Y.Y. Han, Y.A. He, H.H. He, H.N. He, J.C. He, S.L. He, X.B. He, Y. Heller, M. Hor, Y.K. Hou, C. Hou, X. Hu, H.B. Hu, S. Hu, S.C. Hu, X.J. Huang, D.H. Huang, Q.L. Huang, W.H. Huang, X.T. Huang, Z.C. Ji, F. Ji, X.L. Jia, H.Y. Jiang, K. Jiang, Z.J. Jin, C. Kuleshov, D. Levochkin, K. Li, B.B. Li, C. Li, C. Li, F. Li, H.B. Li, H.C. Li, H.Y. Li, J. Li, K. Li, W.L. Li, X. Li, X. Li, X.R. Li, Y. Li, Y.Z. Li, Z. Li, Z. Liang, E.W. Liang, Y.F. Lin, S.J. Liu, B. Liu, C. Liu, D. Liu, H. Liu, H.D. Liu, J. Liu, J.L. Liu, J.S. Liu, J.Y. Liu, M.Y. Liu, R.Y. Liu, S.M. Liu, W. Liu, Y.N. Liu, Z.X. Long, W.J. Lu, R. Lv, H.K. Ma, B.Q. Ma, Lingling Ma, X.H. Mao, J.R. Masood, A. Mitthumsiri, W. Montaruli, T. Nan, Y.C. Pang, B.Y. Pattarakijwanich, P. Pei, Z.Y. Qi, M.Y. Ruffolo, D. Rulev, V. Sáiz, A. Shao, L. Shchegolev, O. Sheng, X.D. Shi, J.R. Song, H.C. Stenkin, Yu.V Stepanov, V. Sun, Q.N. Sun, X.N. Sun, Z.B. Tam, P.H.T. Tang, Z.B. Tian, W.W. Wang, B.D. Wang, C. Wang, H. Wang, H.G. Wang, J.C. Wang, J.S. Wang, L.P. Wang, L.Y. Wang, R.N. Wang, W. Wang, W. Wang, X.G. Wang, X.J. Wang, X.Y. Wang, Y.D. Wang, Y.J. Key Laboratory of Particle Astrophyics Experimental Physics Division Computing Center Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China University of Chinese Academy of Sciences Beijing100049 China TIANFU Cosmic Ray Research Center ChengduSichuan China State Key Laboratory of Particle Detection and Electronics China University of Science and Technology of China Hefei Anhui230026 China Department of Engineering Physics Tsinghua University Beijing100084 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China National Space Science Center Chinese Academy of Sciences Beijing100190 China School of Physics Peking University Beijing100871 China Center for Astrophysics Guangzhou University GuangzhouGuangdong510006 China Sun Yat-sen University ZhuhaiGuangdong519082 China School of Physical Science and Technology Guangxi University Nanning Guangxi530004 China Hebei Normal University Shijiazhuang Hebei050024 China School of Physics and Microelectronics Zhengzhou University ZhengzhouHenan450001 China School of Astronomy and Space Science Nanjing University NanjingJiangsu210023 China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences NanjingJiangsu210023 China Institute of Frontier and Interdisciplinary Science Shandong University QingdaoShandong266237 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Tsung-Dao Lee Institute School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China School of Physical Science and Technology School of Information Science and Technology Southwest Jiaotong University ChengduSichuan610031 China College of Physics Sichuan University ChengduSichuan610065 China Key Laboratory of Cosmic Rays Tibet University Ministry of Education Lhasa Tibet850000 China School of Phy

The Wide Field-of-View Cherenkov Telescope Array (WFCTA) and the Water Cherenkov Detector Arrays (WCDA) of LHAASO are designed to work in combination for measuring the energy spectra of various cosmic ray species over a very wide energy range from a few TeV to 10 PeV. The energy calibration of WCDA can be achieved with a proven technique of measuring the westward shift of the Moon shadow of galactic cosmic rays due to the geomagnetic field. This deflection angle ∆ is inversely proportional to the energy of the cosmic rays. The precise measurements of the shifts by WCDA allows us to calibrate its energy scale for energies as high as 35 TeV. The energy scale measured by WCDA can be used to cross calibrate the energy reconstructed by WFCTA, which spans the whole energy range up to 10 PeV. In this work, we will demonstrate the feasibility of the method using the data collected from April 2019 to January 2020 by the WFCTA array and WCDA-1 detector, the first of the three water Cherenkov ponds, already commissioned at LHAASO site. © 2021, CC BY.

关键词： Cosmic rays

A MODIFIED SCATTERING MODEL OF ROW WHEAT AT X- BAND

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A MODIFIED SCATTERING MODEL OF ROW WHEAT AT X- BAND

IEEE International Geoscience and Remote Sensing Symposium

作者： Lei He Yuxia Li Wenyi Hu Hongping Shu Ling Tong School of software Engineering Chengdu University of Information Technology Chengdu Sichuan China School of Automation Engineering University of Electronic Science and Technology of China. College of Cyber Security Chengdu University of Technology

Cereal crops, contrary to natural vegetation, have the different characteristics for their regular planting. Further, the random assumption of the radiative transfer theory is not suitable for cereal canopy. The paper aimed to present a modified scattering model of row wheat at X-band (center frequency 3.2GHz). The modified scattering model considered both the surface scattering of soil and the volume scattering of wheat canopy. In different wheat growth stage, the weights of the two kinds of scattering phenomenon were set up based on an empirical growth model because of their visible area. A series of data including wheat growth parameters and backscatter coefficients, related to the interaction, were collected for the analyses of the model. The research results showed the model could better reflect the scattering phenomenon of regulate planting, which is helpful to agriculture remote sensing fields.

关键词： Scattering Backscatter Soil Agriculture Vegetation mapping Mathematical model Analytical models

Utilizing competitions between optical parametric amplifications and dissipations to manipulate photon transport

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Physical Review A 2019年第2期100卷 023826-023826页

作者： Cong-Hua Yan W. Z. Jia Xin-Hong Jia Hao Yuan Yong Li Haidong Yuan College of Physics and Electronic Engineering Sichuan Normal University Chengdu 610068 China Department of Mechanical and Automation Engineering The Chinese University of Hong Kong Shatin Hong Kong School of Physical Science and Technology Southwest Jiaotong University Chengdu 610031 China School of Physics and Materials Science Anhui University Hefei 230023 China Beijing Computational Science Research Center Beijing 100094 China Synergetic Innovation Center for Quantum Effects and Applications Hunan Normal University Changsha 410081 China

Dissipations in the waveguide-cavity systems destroy quantum interference between the incident signal photons and the cavity photons linearly and, thus, usually limit the manipulation of the photon transport. Here, we adopt a four-mode microring cavity including both second-order (χ(2)) and third-order (χ(3)) nonlinearities side coupled to two different waveguides to manipulate photon transport against dissipative effects. The results show that the incident signal photons can be amplified due to the optical parametric amplification (OPA) originated from χ(3) nonlinearities. Owing to the coherent interference between cavity photons with different frequencies, the transmission spectra of the signal field are split into two amplified peaks. The transmission intensities are not always linearly reduced by increasing the dissipations but determined by the competition between the OPA and the dissipations. It means that we can utilize the OPA process to overcome the dissipative effects to manipulate photon transport and, thus, control the transmission intensities of the incident signal photon from Tc=0 to Tc>100%. This competition can also be used to convert the signal field to the idler field with amplified efficiencies.

关键词： Nonlinear optics Optical coherence Optical microcavities Waveguides