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Reconstruction of Cherenkov image bymultiple telescopes of LHAASO-WFCTA

Radiation Detection Technology and Methods 2022年第4期6卷 544-557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 j.T.Cai zhe Cao zhen Cao j.Chang j.F.Chang E.S.Chen Liang Chen Liang Chen Long Chen M.j.Chen M.L.Chen Q.H.Chen S.H.Chen S.z.Chen T.L.Chen Y.Chen H.L.Cheng N.Cheng Y.D.Cheng S.W.Cui X.H.Cui Y.D.Cui B.D’Ettorre Piazzoli B.z.Dai H.L.Dai z.G.Dai Danzengluobu Ddella Volpe K.K.Duan j.H.Fan Y.z.Fan z.X.Fan j.Fang K.Fang C.F.Feng L.Feng S.H.Feng X.T.Feng Y.L.Feng B.Gao C.D.Gao L.Q.Gao Q.Gao W.Gao W.K.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 S.L.He X.B.He Y.He M.Heller Y.K.Hor C.Hou X.Hou H.B.Hu Q.Hu S.Hu S.C.Hu X.j.Hu D.H.Huang W.H.Huang X.T.Huang X.Y.Huang Y.Huang z.C.Huang X.L.ji H.Y.jia K.jia K.jiang z.j.jiang M.jin M.M.Kang T.Ke D.Kuleshov K.Levochkin B.B.Li Cheng Li Cong Li F.Li H.B.Li H.C.Li H.Y.Li j.Li jian Li jie Li K.Li WLLi XRLi Xin Li Xin Li YzLi 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 W.j.Long R.Lu Q.Luo H.K.Lv B.Q.Ma L.L.Ma X.H.Ma j.R.Mao A.Masood z.Min W.Mitthumsiri Y.C.Nan z.W.Ou B.Y.Pang P.Pattarakijwanich z.Y.Pei M.Y.Qi Y.Q.Qi B.Q.Qiao j.j.Qin D.Ruffolo A.Sáiz C.Y.Shao 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.Wang R.N.Wang W.Wang X.G.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 X.F.Wu Y.S.Wu S.Q.Xi j.Xia j.j.Xia G.M.Xiang D.X.Xiao G.Xiao G.G.Xin Y.L.Xin Y.Xing z.Xiong D.L.Xu R.X.Xu L.Xue D.H.yan j.z.yan C.W.yang F.F.yang H.W.yang j.Y.yang L.L.yang M.j.yang R.z.yang S.B.yang Y.H.Yao z.G.Yao Y.M.Ye L.Q.Yin N.Yin X.H.You z.Y.You Y.H.Yu Q.Yuan H.Yue H.D.zeng T.X.zeng W.zeng z.K.zeng M.zha X.X.zhai B.B.zhang F.zhang H.M.zhang H.Y.zhang j.L.zhang L.X.zhang Li zhang Lu zhang P.F.zhang P.P.zhang R.zhang S.B.zhang S.R.zhang S. Key Laboratory of Particle Astrophyics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina Dublin Institute for Advanced Studies 31 Fitzwilliam Place2DublinIreland Max-Planck-Institut for Nuclear Physics P.O.Box 10398069029 HeidelbergGermany State Key Laboratory of Particle Detection and Electronics BeijingChina University of Science and Technology of China Hefei 230026AnhuiChina School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina College of Physics Sichuan UniversityChengdu 610065SichuanChina School of Astronomy and Space Science Nanjing UniversityNanjing 210023JiangsuChina Center for Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina Key Laboratory of Dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China Hebei Normal University Shijiazhuang 050024HebeiChina School of Physics and Astronomy(zhuhai)&Sino-French Institute of Nuclear Engineering and Technology(zhuhai) Sun Yat-sen UniversityZhuhai 519000China School of Physics(Guangzhou) Sun Yat-sen UniversityGuangzhou 510275GuangdongChina Dipartimento di Fisica dell’Universitàdi Napoli“Federico II” Complesso Universitario di Monte Sant’Angelovia Cinthia80126 NapoliItaly School of Physics and Astronomy Yunnan UniversityKunming 650091YunnanChina Département de Physique Nucléaire et Corpusculaire Facultéde SciencesUniversitéde Genève

Introduction One of main scientiﬁc goals of the Large High Altitude Air Shower Observatory(LHAASO)is to accurately measure the energy spectra of different cosmic ray compositions around the‘knee’*** Wide Field-of-View(FoV)Cherenkov Telescope Array(WFCTA),which is one of the main detectors of LHAASO and has 18 telescopes,is built to achieve this *** telescopes are put together and point to connected directions for a larger *** Telescopes are deployed spatially as close as possible,but due to their own size,the distance between two adjacent telescopes is about 10 ***,the Cherenkov lateral distribution and the parallax between the two telescopes should be considered in the event building process for images crossing over the boundaries of FoVs of the *** event building method for Cherenkov images measured by multiple telescopes of WFCTA is *** performance of the shower measurements using the combined images is evaluated by comparing with showers that are fully contained by a virtual telescope in *** and conclusion It is proved that the developed event building process can help to increase the FoV of WFCTA by 30%while maintaining the same reconstruction quality,compared to the separate telescope reconstruction method.

关键词： method directions conclusion

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LHAASO-KM2A detector simulation using Geant4

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Radiation Detection Technology and Methods 2024年第3期8卷 1437-1447页

作者： zhen Cao F.Aharonian Q.An Axikegu Y.X.Bai Y.W.Bao D.Bastieri X.j.Bi Y.j.Bi j.T.Cai Q.Cao W.Y.Cao zhe Cao j.Chang j.F.Chang A.M.Chen E.S.Chen Liang Chen Lin Chen Long Chen M.j.Chen M.L.Chen Q.H.Chen S.H.Chen S.z.Chen T.L.Chen Y.Chen N.Cheng Y.D.Cheng M.Y.Cui S.W.Cui X.H.Cui Y.D.Cui B.z.Dai H.L.Dai z.G.Dai Danzengluobu X.Q.Dong K.K.Duan j.H.Fan Y.z.Fan j.Fang K.Fang C.F.Feng L.Feng S.H.Feng X.T.Feng Y.L.Feng S.Gabici B.Gao C.D.Gao L.Q.Gao Q.Gao W.Gao W.K.Gao M.M.Ge L.S.Geng G.Giacinti G.H.Gong Q.B.Gou M.H.Gu F.L.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han H.H.He H.N.He j.Y.He X.B.He Y.He Y.K.Hor B.W.Hou C.Hou X.Hou H.B.Hu Q.Hu S.C.Hu D.H.Huang T.Q.Huang W.j.Huang X.T.Huang X.Y.Huang Y.Huang z.C.Huang X.L.ji H.Y.jia K.jia K.jiang X.W.jiang z.j.jiang M.jin M.M.Kang T.Ke D.Kuleshov K.Kurinov B.B.Li Cheng Li Cong Li D.Li F.Li H.B.Li H.C.Li H.Y.Li j.Li jian Li jie Li K.Li W.L.Li W.L.Li X.R.Li Xin 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.Y.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.Liu Y.N.Liu R.Lu Q.Luo H.K.Lv B.Q.Ma L.L.Ma X.H.Ma j.R.Mao z.Min W.Mitthumsiri H.j.Mu Y.C.Nan A.Neronov z.W.Ou B.Y.Pang P.Pattarakijwanich z.Y.Pei M.Y.Qi Y.Q.Qi B.Q.Qiao j.j.Qin D.Ruffolo A.Sáiz D.Semikoz C.Y.Shao L.Shao O.Shchegolev X.D.Sheng F.W.Shu H.C.Song Yu.V.Stenkin V.Stepanov Y.Su Q.N.Sun X.N.Sun z.B.Sun P.H.T.Tam Q.W.Tang z.B.Tang W.W.Tian C.Wang C.B.Wang G.W.Wang H.G.Wang H.H.Wang j.C.Wang K.Wang L.P.Wang L.Y.Wang P.H.Wang R.Wang W.Wang X.G.Wang X.Y.Wang Y.Wang Y.D.Wang Y.j.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 X.F.Wu Y.S.Wu S.Q.Xi j.Xia j.j.Xia G.M.Xiang D.X.Xiao G.Xiao G.G.Xin Y.L.Xin Y.Xing z.Xiong D.L.Xu R.F.Xu R.X.Xu W.L.Xu L.Xue D.H.yan j.z.yan T.yan C.W.yang F.yang F.F.yang H.W.yang j.Y.yang L.L.yang M.j.yang R.z.yang S.B.yang Y.H.Yao z.G.Yao Y.M.Ye L.Q.Yin N.Yin X.H.You z.Y.You Y.H.Yu Q.Yuan H.Yue H.D.zeng T.X.zeng W.zeng M.zha B.B.zhang F.zhang H.M.zhang H.Y.zhang j.L.zhang L.X.zhang Li zhang P.F.zhang P.P.zhang R.zhang S.B.zh Key Laboratory of Particle Astrophysics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing100049China University of Chinese Academy of Sciences Beijing100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina Dublin Institute for Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-Planck-Institute for Nuclear Physics 69029Heidelberg103980Germany State Key Laboratory of Particle Detection and Electronics BeijingChina University of Science and Technology of China Hefei230026AnhuiChina School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu610031SichuanChina School of Astronomy and Space Science Nanjing UniversityNanjing210023JiangsuChina Center for Astrophysics Guangzhou UniversityGuangzhou510006GuangdongChina Hebei Normal University Shijiazhuang050024HebeiChina Key Laboratory of Dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of Physics and Astronomy(zhuhai)&School of Physics(Guangzhou)&Sino-French Institute of Nuclear Engineering and Technology(zhuhai) Sun Yat-sen UniversityGuangzhouZhuhai 510275519000GuangdongChina School of Physics and Astronomy Yunnan UniversityKunming 650091YunnanChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237ShandongChina APC UniversitéParis CitéCNRS/IN2P3CEA/IRFUObservatoire de ParisParis 11975205France Department of Engineering Phys

KM2A is one of the main sub-arrays of LHAASO,working on gamma ray astronomy and cosmic ray physics at energies above 10 *** simulation is the important foundation for estimating detector performance and data *** is a big challenge to simulate the KM2A detector in the framework of Geant4 due to the need to track numerous photons from a large number of detector units(>6000)with large altitude difference(30)and huge coverage(1.3).In this paper,the design of the KM2A simulation code G4KM2A based on Geant4 is *** process of G4KM2A is optimized mainly in memory consumption to avoid memory *** simplifications are used to significantly speed up the execution of *** running time is reduced by at least 30 times compared to full detector *** particle distributions and the core/angle resolution comparison between simulation and experimental data of the full KM2A array are also presented,which show good agreement.

关键词： LHAASO KM2A Simulation GEANT4

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由超拍电子伏特加速器产生的超高能伽马射线气泡

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Science Bulletin 2024年第4期69卷 449-457页

作者： LHAASO Collaboration zhen Cao Chuandong Gao Cong Li Ruo-Yu Liu Ruizhi yang 不详 Key Laboratory of Particle Astrophyics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China University of Science and Technology of China Hefei 230026China

We report the detection of aγ-ray bubble spanning at least 100deg2 in ultra-high energy(UHE)up to a few PeV in the direction of the star-forming region Cygnus X,implying the presence super PeVatron(s)accelerating protons to at least 10 PeV.A log-parabola form with the photon indexΓ(E)=(2.71±0.02)+(0.11±0.02)×log10(E/10 TeV)is found fitting the gamma-ray energy spectrum of the bubble *** sources,“hot spots”correlated with very massive molecular clouds,and a quasi-spherical amorphousγ-ray emitter with a sharp central brightening are observed in the *** the core of~0.5°,spatially associating with a region containing massive OB association(Cygnus OB2)and a microquasar(Cygnus X-3),as well as previously reported multi-TeV sources,an enhanced concentration of UHEγ-rays is observed with 2 photons at energies above 1 *** general feature of the bubble,the morphology,and the energy spectrum,are reasonably reproduced by the assumption of a particle accelerator in the core,continuously injecting protons into the ambient medium.

关键词： Cosmic rays γ-rays Interstellar medium Star cluster

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Evidence for particle acceleration approaching PeV energies in the W51 complex

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Science Bulletin 2024年第18期69卷 2833-2841页

作者： LHAASO Collaboration zhen Cao F.Aharonian Axikegu Y.X.Bai Y.W.Bao D.Bastieri X.j.Bi Y.j.Bi W.Bian A.V.Bukevich Q.Cao W.Y.Cao zhe Cao j.Chang j.F.Chang A.M.Chen E.S.Chen H.X.Chen Liang Chen Lin Chen Long Chen M.j.Chen M.L.Chen Q.H.Chen S.Chen S.H.Chen S.z.Chen T.L.Chen Y.Chen N.Cheng Y.D.Cheng M.Y.Cui S.W.Cui X.H.Cui Y.D.Cui B.z.Dai H.L.Dai z.G.Dai Danzengluobu X.Q.Dong K.K.Duan j.H.Fan Y.z.Fan j.Fang j.H.Fang K.Fang C.F.Feng H.Feng L.Feng S.H.Feng X.T.Feng Y.Feng Y.L.Feng S.Gabici B.Gao C.D.Gao Q.Gao W.Gao W.K.Gao M.M.Ge L.S.Geng G.Giacinti G.H.Gong Q.B.Gou M.H.Gu F.L.Guo X.L.Guo Y.Q.Guo Y.Y.Guo Y.A.Han M.Hasan H.H.He H.N.He j.Y.He Y.He Y.K.Hor B.W.Hou C.Hou X.Hou H.B.Hu Q.Hu S.C.Hu D.H.Huang T.Q.Huang W.j.Huang X.T.Huang X.Y.Huang Y.Huang X.L.ji H.Y.jia K.jia K.jiang X.W.jiang z.j.jiang M.jin M.M.Kang I.Karpikov D.Kuleshov K.Kurinov B.B.Li C.M.Li Cheng Li Cong Li D.Li F.Li H.B.Li H.C.Li jian Li jie Li K.Li S.D.Li W.L.Li W.L.Li X.R.Li Xin Li Y.z.Li zhe Li zhuo Li E.W.Liang Y.F.Liang S.j.Lin B.Liu C.Liu D.Liu D.B.Liu H.Liu H.D.Liu j.Liu j.L.Liu M.Y.Liu R.Y.Liu S.M.Liu W.Liu Y.Liu Y.N.Liu Q.Luo Y.Luo H.K.Lv B.Q.Ma L.L.Ma X.H.Ma j.R.Mao z.Min W.Mitthumsiri H.j.Mu Y.C.Nan A.Neronov L.j.Ou P.Pattarakijwanich z.Y.Pei j.C.Qi M.Y.Qi B.Q.Qiao j.j.Qin A.Raza D.Ruffolo A.Sáiz M.Saeed D.Semikoz L.Shao O.Shchegolev X.D.Sheng F.W.Shu H.C.Song Yu.V.Stenkin V.Stepanov Y.Su D.X.Sun Q.N.Sun X.N.Sun z.B.Sun j.Takata P.H.T.Tam Q.W.Tang R.Tang z.B.Tang W.W.Tian C.Wang C.B.Wang G.W.Wang H.G.Wang H.H.Wang j.C.Wang Kai Wang Kai Wang L.P.Wang L.Y.Wang P.H.Wang R.Wang W.Wang X.G.Wang X.Y.Wang Y.Wang Y.D.Wang Y.j.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 Q.W.Wu S.Wu X.F.Wu Y.S.Wu S.Q.Xi j.Xia G.M.Xiang D.X.Xiao G.Xiao Y.L.Xin Y.Xing D.R.Xiong z.Xiong D.L.Xu R.F.Xu R.X.Xu W.L.Xu L.Xue D.H.yan j.z.yan T.yan C.W.yang C.Y.yang F.yang F.F.yang L.L.yang M.j.yang R.z.yang W.X.yang Y.H.Yao z.G.Yao L.Q.Yin N.Yin X.H.You z.Y.You Y.H.Yu Q.Yuan H.Yue H.D.zeng T.X.zeng W.zeng M.zha B.B.zhang F.zhang H.zhang 不详 Key Laboratory of Particle Astrophysics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduChina Dublin Institute for Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-Planck-Institut for Nuclear Physics P.O.Box 103980Heidelberg 69029Germany School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Center for Astrophysics Guangzhou UniversityGuangzhou 510006China Tsung-Dao Lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China Institute for Nuclear Research of Russian Academy of Sciences Moscow 117312Russia Hebei Normal University Shijiazhuang 050024China University of Science and Technology of China Hefei 230026China State Key Laboratory of Particle Detection and Electronics China Key Laboratory of Dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Research Center for Astronomical Computing Zhejiang LaboratoryHangzhou 311121China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China School of Physics and Astronomy Yunnan UniversityKunming 650091China Key Laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of Physics and Astronomy(zhuhai)&School of Physics(Guangzhou)&Sino-French Institute of Nuclear Engineering and Technology(zhuhai) Sun Yat-sen UniversityZhuhai 519000&Guangzhou 510275GuangdongChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China APC UniversitéParis Cité

Theγ-ray emission from the W51 complex is widely acknowledged to be attributed to the interaction between the cosmic rays(CRs)accelerated by the shock of supernova remnant(SNR)W51C and the dense molecular clouds in the adjacent star-forming region,***,the maximum acceleration capability of W51C for CRs remains *** on observations conducted with the Large High Altitude Air Shower Observatory(LHAASO),we report a significant detection ofγrays emanating from the W51 complex,with energies from 2 to 200 *** LHAASO measurements,for the first time,extend theγ-ray emission from the W51 complex beyond 100 TeV and reveal a significant spectrum bending at tens of *** combining the"π^(0)-decay bump"featured data from Fermi-LAT,the broadbandγ-ray spectrum of the W51 region can be well-characterized by a simple pp-collision *** observed spectral bending feature suggests an exponential cutoff at~400 TeV or a power-law break at~200 TeV in the CR proton spectrum,most likely providing the first evidence of SNRs serving as CR accelerators approaching the PeV ***,two young star clusters within W51B could also be theoretically viable to produce the most energeticγrays observed by *** findings strongly support the presence of extreme CR accelerators within the W51 complex and provide new insights into the origin of Galactic CRs.

关键词： UHE c-ray Cosmic rays SNR W51C Star clusters

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High-energy-density lithium manganese iron phosphate for lithium-ion batteries: Progresses, challenges, and prospects

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journal of Energy Chemistry 2025年第1期100卷 1-17页

作者： Bokun zhang Xiaoyun Wang Shuai Wang yan Li Libo Chen Handong jiao zhijing Yu jiguo Tu State Key Laboratory of Advanced Metallurgy University of Science and Technology Beijing Research Institute for Intelligent Wearable Systems The Hong Kong Polytechnic University Institute of Advanced Structure Technology Beijing Institute of Technology

The soaring demand for smart portable electronics and electric vehicles is propelling the advancements in high-energy–density lithium-ion *** manganese iron phosphate (LiMnxFe1-xPO4) has garnered significant attention as a promising positive electrode material for lithium-ion batteries due to its advantages of low cost,high safety,long cycle life,high voltage,good high-temperature performance,and high energy *** LiMnxFe1-xPO4has made significant breakthroughs in the past few decades,there are still facing great challenges in poor electronic conductivity and Li-ion diffusion,manganese dissolution affecting battery cycling performance,as well as low tap *** review systematically summarizes the reaction mechanisms,various synthesis methods,and electrochemical properties of LiMnxFe1-xPO4to analyze reaction processes accurately and guide material ***,the main challenges currently faced are concluded,and the corresponding various modification strategies are discussed to enhance the reaction kinetics and electrochemical performance of LiMnxFe1-xPO4,including multi-scale particle regulation,heteroatom doping,surface coating,as well as microscopic morphology ***,in view of the current research challenges faced by intrinsic reaction processes,kinetics,and energy storage applications,the promising research directions are *** importantly,it is expected to provide key insights into the development of high-performance and stable LiMnxFe1-xPO4materials,to achieve practical energy storage requirements.

关键词： Lithium manganese iron phosphate High energy density Lithium-ion batteries Reaction mechanism Tap density

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Deciphering Water Oxidation Catalysts: The Dominant Role of Surface Chemistry over Reconstruction Degree in Activity Promotion

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NANO-MICRO LETTERS 2025年第1期17卷 1-15页

作者： An, Li Li, jianyi Sun, Yuanmiao zhu, jiamin Seow, justin zhu Yeow zhang, Hong zhang, Nan Xi, Pinxian Xu, zhichuan j. yan, Chun-Hua Lanzhou Univ Frontiers Sci Ctr Rare Isotopes Key Lab Nonferrous Met Chem & Resources Utilizat G State Key Lab Appl Organ ChemColl Chem & Chem Eng Lanzhou 730000 Peoples R China Nanyang Technol Univ Sch Mat Sci & Engn Singapore 639798 Singapore Chinese Acad Sci Fac Mat Sci & Energy Engn Shenzhen Inst Adv Technol Inst Technol Carbon Neutral Shenzhen 518055 Peoples R China Yunnan Univ Natl Ctr Int Res Photoelect & Energy Mat Electron Microscopy Ctr Sch Mat & EnergyKey Lab Electromagnet Mat & Devic Kunming 650091 Peoples R China Baotou Res Inst Rare Earths State Key Lab Baiyunobo Rare Earth Resource Res & Baotou 014030 Peoples R China Peking Univ Beijing Natl Lab Mol Sci State Key Lab Rare Earth Mat Chem & Applicat PKU HKU Joint Lab Rare Earth Mat & Bioinorgan Chem Beijing 100871 Peoples R China

Demonstrate that the key factor to determine the activity of reconstructed surfaces is the surface chemistry, instead of reconstruction degree using the popular perovskite LaNi1-xFexO3 oxides as model *** content can influence both the surface reconstruction degree, the activation degree, and the activity of reconstructed *** oxygen evolution reaction activity of reconstructed catalysts is primarily governed by the chemistry of the reconstructed surface species. Water splitting hinges crucially on the availability of electrocatalysts for the oxygen evolution reaction. The surface reconstruction has been widely observed in perovskite catalysts, and the reconstruction degree has been often correlated with the activity enhancement. Here, a systematic study on the roles of Fe substitution in activation of perovskite LaNiO3 is reported. The substituting Fe content influences both current change tendency and surface reconstruction degree. LaNi0.9Fe0.1O3 is found exhibiting a volcano-peak intrinsic activity in both pristine and reconstructed among all substituted perovskites in the LaNi1-xFexO3 (x = 0.00, 0.10, 0.25, 0.50, 0.75, 1.00) series. The reconstructed LaNi0.9Fe0.1O3 shows a higher intrinsic activity than most reported NiFe-based catalysts. Besides, density functional theory calculations reveal that Fe substitution can lower the O 2p level, which thus stabilize lattice oxygen in LaNi0.9Fe0.1O3 and ensure its long-term stability. Furthermore, it is vital interesting that activity of the reconstructed catalysts relied more on the surface chemistry rather than the reconstruction degree. The effect of Fe on the degree of surface reconstruction of the perovskite is decoupled from that on its activity enhancement after surface reconstruction. This finding showcases the importance to customize the surface chemistry of reconstructed catalysts for water oxidation.

关键词： Oxygen evolution reaction Perovskite oxides Doping Activation and reconstruction

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Boosting hydrocarbon conversion via Cu-doping induced oxygen vacancies on CeO2 in CO2 electroreduction

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journal of Energy Chemistry 2025年第1期100卷 66-76页

作者： Lei Xue Tong Shi Chenhui Han Heng zhang Fenrong Liu Haorun Li yan Wang Xiaojun Gu Shanghong zeng Inner Mongolia Key Laboratory of Chemistry and Physics of Rare Earth Materials School of Chemistry and Chemical Engineering Inner Mongolia University State Key Laboratory of Coal Conversion Institute of Coal Chemistry Chinese Academy of Sciences Institute of Catalysis Department of Chemistry Zhejiang University National Key Laboratory of Baiyunobo Rare Earth Resource Research and Comprehensive Utilization Baotou Research Institute of Rare Earths

Conversion of CO2back to hydrocarbons is the most direct way of closing the“carbon cycle”,and its significance is further enlarged if this process is driven by renewable energies such as ***,precisely controlling the product selectivity towards hydrocarbons against the competitive hydrogen evolution remains challenging,especially for Cu-based ***,we report a novel defect engineering strategy,by which Cu-doping-induced oxygen vacancies on CeO2nanorods were effectively created,with adjustable vacancy/Cu *** resulting optimum catalyst shows up to 79% catalytic current density to hydrocarbons （excluding CO）,with 49% faradaic efficiency to *** and density functional theory unveil that the ratio between oxygen vacancy and Cu affects significantly the formation of*CHO and activation of H2O,which leads to the following deep hydrogenation to *** findings may spur new insights for designing and developing more controllable chemical process relevant to CO2utilization.

关键词： Oxygen vacancy Hydrocarbon production Reaction mechanism

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Synergistic promotion strategy of “dual-site” and “dual-path” to enhance the C–C coupling between CO2 and HCHO driven by photoelectrocatalysis

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journal of Energy Chemistry 2025年第1期100卷 39-49页

作者： Hongqiang yang jianfeng zheng Guoyu Wang Yifei Gao Yatao yang jia Li Xiaojin Han yan Cui zhanggen Huang National Key Laboratory of High Efficiency and Low Carbon Utilization of Coal Institute of Coal Chemistry Chinese Academy of Science University of Chinese Academy of Science Shenyang University of Chemical Technology

Photoelectrocatalytic coupling CO2and volatile organic compounds （VOCs） is a promising green strategy for the synergistic conversion of the two carbon-containing resources to *** catalytic efficiency is always at the mercy of chemical inertness of CO2and the competitive hydrogen evolution of ***,a modified g-C3N4/znAl-LDH z-scheme heterojunction catalyst with dual reaction site was rationally designed and precisely *** Faraday efficiency of ethanol reached 68.67%with a corresponding formation rate of 227.3μmol *** revealed by in-situ characterizations and density functional theory calculations,CO2and HCHO were absorbed at zn site and N site,***,*CO generated from CO2and HCHO was converted to*CH3O and*CHO on the dual-active-site *** detailed reaction mechanism experiments indicated that C–C coupling only occurred between*CO and*CH3O in electrocatalysis *** from the“*CO+*CH3O”path,another“*CO+*CHO”coupling path was also detected in photoelectrocatalytic *** selectivity of ethanol was significantly enhanced due to the synthesis of dual-site catalyst and the dual-path coupling path between CO2and HCHO simultaneously driven by light and electricity.

关键词： Photoelectrocatalysis z-scheme C–C coupling Ethanol

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Flux variations of cosmic ray air showers detected by LHAASO-KM2A during a thunderstorm on june 10,2021

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Chinese Physics C 2023年第1期47卷 193-203页

作者： F.Aharonian 安琪阿西克古白立新白云翔包逸炜 D.Bastieri 毕效军毕玉江蔡金庭曹喆曹臻常进常劲帆陈恩生陈良陈亮陈龙陈明君陈玛丽陈素弘陈松战陈天禄陈学健陈阳程皓麟程宁程耀东崔树旺崔晓红崔昱东戴本忠代洪亮戴子高单增罗布 D.della Volpe 段凯凯樊军辉范一中范志香方军方堃冯存峰封莉冯少辉丰晓婷冯有亮高博高川东高林青高启高卫高伟康葛茂茂耿利斯龚光华苟全补顾旻皓郭福来郭俊广郭晓磊郭义庆郭莹莹韩毅昂何会海贺昊宁何思乐何新波何钰 M.Heller 贺远强侯超侯贤胡红波胡铨胡森胡世聪呼晓军黄代绘黄文昊黄性涛黄晓渊黄勇黄志成季筱璐贾焕玉贾康江琨姜泽军金敏康明铭柯通 D.Kuleshov 李兵兵李澄李骢李飞李海波李会财李华阳李军李剑李捷李凯李文龙李秀荣李昕李新李一卓李哲黎卓梁恩维梁云峰林苏杰刘冰刘成刘栋刘虎刘海东刘佳刘江来刘佳松刘金艳刘茂元柳若愚刘四明刘伟刘怡刘以农龙文杰鲁睿罗晴吕洪魁马伯强马玲玲马欣华毛基荣 A.Masood 闵振 W.Mitthumsiri 南云程区子维庞彬宇 P.Pattarakijwanich 裴致远齐孟尧祁业情乔冰强秦家军 D.Ruffolo A.Sáiz 邵澄宇邵琅 O.Shchegolev 盛祥东石京燕宋慧超 Yu.V.Stenkin V.Stepanov 苏扬孙秦宁孙晓娜孙志斌谭柏轩唐泽波田文武王博东王超王辉王洪光王建成王界双王利苹王玲玉王冉王润娜王为王祥高王祥玉王阳王玉东王岩谨王亚平王忠海王仲翔王振王铮韦大明魏俊杰魏永健文韬吴超勇吴含荣武莎吴雪峰吴雨生席邵强夏捷夏君集项光漫肖迪泫肖刚辛广广辛玉良邢祎熊峥徐东莲徐仁新薛良闫大海颜景志杨朝文杨冯帆杨何文杨佳盈杨莉莉杨明洁杨睿智杨深邦姚玉华姚志国叶一锰尹丽巧尹娜游晓浩游智勇于艳红袁强岳华曾厚敦曾婷轩曾玮曾宗康查敏翟徐徐张彬彬张丰张海明张恒英张建立张丽霞张力张路张鹏飞张佩佩张瑞张少博张少如张寿山张潇张笑鹏张云峰张月雷张毅张勇赵兵赵静赵雷赵立志赵世平郑福郑应周斌周浩周佳能周平周荣周勋秀祝成光祝凤荣朱辉朱科军左雄 Key Laboratory of Particle Astrophyics&Experimental Physics Division&Computing Center of Sciences Beijing 100049China University of Chinese Academy of Sciences Beijing 100049China TIANFU Cosmic Ray Research Center ChengduSichuanChina Dublin Institute for Advanced Studies 31 Fitzwilliam Place2 DublinIreland Max-Planck-Institut for Nuclear Physics P.O.Box 10398069029 HeidelbergGermany State Key Laboratory of Particle Detection and Electronics China University of Science and Technology of China Hefei 230026China School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031China College of Physics Sichuan UniversityChengdu 610065China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Center for Astrophysics Guangzhou UniversityGuangzhou 510006China Key Laboratory of Dark Matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Key Laboratory of Cosmic Rays(Tibet University) Ministry of Education850000 LhasaTibetChina National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China Hebei Normal University Shijiazhuang 050024China School of Physics and Astronomy(zhuhai)&School of Physics(Guangzhou)&Sino-French Institute of Nuclear Engineering and Technology(zhuhai) Sun Yat-sen University519000 Zhuhai&510275 GuangzhouGuangdongChina Dipartimento di Fisica dell’Universitàdi Napoli"Federico II" Complesso Universitario di Monte Sant’Angelovia Cinthia80126 NapoliItaly School of Physics and Astronomy Yunnan UniversityKunming 650091China D´epartement de Physique Nucléaire et Corpusculaire Facultéde SciencesUniversitéde Genève24 Quai Ernest Ansermet1211 GenevaSwitzerland Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China Depar

The Large High Altitude Air Shower Observatory(LHAASO)has three sub-arrays,KM2A,WCDA,and *** flux variations of cosmic ray air showers were studied by analyzing the KM2A data during a thunderstorm on june 10,*** number of shower events that meet the trigger conditions increases significantly in atmospheric electric fields,with a maximum fractional increase of 20%.The variations in trigger rates(increases or decreases)were found to be strongly dependent on the primary zenith *** flux of secondary particles increased significantly,following a trend similar to that of shower *** better understand the observed behavior,Monte Carlo simulations were performed with CORSIKA and G4KM2A(a code based on GEANT4).We found that the experimental data(in saturated negative fields)were in good agreement with the simulations,assuming the presence of a uniform electric field of-700 V/cm with a thickness of 1500 m in the atmosphere above the observation *** to the acceleration/deceleration by the atmospheric electric field,the number of secondary particles with energy above the detector threshold was modified,resulting in the changes in shower detection rate.

关键词： thunderstorm cosmic rays extensive air showers LHAASO-KM2A

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Metal nanoparticles decorated CoFe-(oxy)hydroxysulfides nanosheets fabricated by a general strategy for electrocatalytic water splitting

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journal of Energy Chemistry 2025年第1期100卷 26-38页

作者： Xiaodong yang Haochen Shen Xiaoming Xiao zhichao Li Qi zhou Wei yang Bin jiang Yongli Sun Luhong zhang zhenhua yan School of Chemical Engineering and Technology Tianjin University Key Laboratory of Advanced Energy Materials Chemistry (Ministry of Education) Nankai University

This study presents a novel method to fabricate metal-decorated,sulfur-doped layered double hydroxides （M/SLDH） through spontaneous redox and sulfurization *** developed Ag/SLDH and Pt/SLDH catalysts with abundant heterogeneous interfaces and hierarchical nanostructures demonstrated outstanding oxygen evolution reaction （OER） and hydrogen evolution reaction （HER） performance,achieving low overpotentials of 212 and 35 mV at 10 mA cm-2in 1 M KOH,*** both anode and cathode in water splitting,they required only 1.47 V to reach 10 mA cm-2and exhibited high structural robustness,maintaining stability at 1000 mA cm-2for 300 ***-situ Raman analysis revealed that the synergistic effects of metal nanoparticles and S doping significantly promote the transformation into the S-Co1-xFexOOH layer,which serves as the active phase for water ***,ultraviolet photoelectron spectroscopy （UPS） and density functional theory （DFT） analyses indicated that incorporating metal nanoparticles and S doping increase electron density near the Fermi level and reduce reaction energy barriers,thus enhancing intrinsic OER and HER *** study provides a scalable strategy for synthesizing high-performance electrocatalysts for water splitting,with promising potential for broader applications.

关键词： LDH Spontaneous reaction Metal nanoparticles Water splitting

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