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Geometrical reconstruction of fluorescence events observed by the lHAASO experiment

The Ⅶ International Symposium on the Nutrition of Herbivores(ISNH-7)

作者： x.l.chen J.K.Wang Y.M.Wu J.x.liu~1 College of Animal Sciences Institute of Dairy Science Ministry of Education Key laboratory of Molecular Animal Nutrition Zhejiang University Hangzhou 310029 P.R.China

＜正＞The study was conducted to investigate the effect of ammonium bicarbonate and casein on rumen fermentation and relative populations of fibre-associated cellulolytic microbes in untreated and sodium hydroxide treated rice straw in *** of nitrogen had different effect on rumen fermentation and fibre-associated microbial *** gas production significantly increased with addition of *** of casein significantly improved rumen fermentation and microbial *** had higher efficiency to supply available nitrogen to microbial growth and degradation of straw than ammonium *** is inferred that a supply of protein nitrogen would be needed for maximum degradation of straw.

关键词： ammonium bicarbonate casein rumen fermentation fibre-associated microbes treated rice straw

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Chinese Physics C 2021年第4期45卷 416-425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 Z.Cao Z.Cao J.Chang J.F.Chang x.C.Chang 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.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.DEtorre Piazzoli x.J.Dong J.H.Fan Y.Z.Fan Z.x.Fan J.Fang J.Fang C.F.Feng l.Feng S.H.Feng Y.l.Feng B.Gao C.D.Gao Q.Gao W.Gao M.M.Ge l.S.Geng G.H.Gong Q.B.Gou M.H.Gu 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 x.Hou H.B.Hu S.Hu S.C.Hu x.J.Hu D.H.Huang Q.l.Huang W.H.Huang x.T.Huang Z.C.Huang F.Ji x.l.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.levochkin 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.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.l.liu J.S.liu J.Y.liu M.Y.liu R.Y.liu S.M.liu W.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 W.Mitthumsiri T.Montaruli Y.C.Nan B.Y..Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi D.Ruffolo V.Rulev A.Saiz l.Shao O.Shchegolev x.D.Sheng J.R.Shi H.C.Song Yu.V.Stenkin V.Stepanov 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 W.Wang x.G.Wang x.J.Wang x.Y.Wang Y.D.Wang Y.J.Wang Y.P.Wang Z.Wang Z.Wang Z.H.Wang Z.x.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 G.xiao H.B.xiao G.G.xin Y.l.xin Y.xing D.l.xu R.x.xu l.xue D.H.Yan C.W.Yang F.F.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.D.Zeng T.x.Zeng W.Zeng Z.K.Zeng M.Zha x.x.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang J.l.Zhang J.W.Zhang l.Zhang l.Zhang l.x.Zhang P.F.Zhang P.F.Zhang R.Zhang S.R.Zhang S.S.Zhang x.Zhang x.P.Zhang Y.Zhang Y.Zhang Y.F.Zhang Y.l.Zhang B.Zhao J.Zhao l.Zhao l.Z.Zhao S.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou J.N.Zhou P 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 State Key laboratory of Paricle Detection and Electronics China University of Science and Technology of China HefeiAnhui 230026China Department of Engineering Physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science Center Chinese Academy of SciencesBeijing 100190China School of Physics Peking UniversityBeijing 100871China Center for Astrophysics Guangzhou UniversityGuangzhouGuangdong 510006China School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhaiGuangdong 519000China School of Physical Science and Technology Guangxi UniversityNanningGuangxi 530004China Hebei Normal University ShijiazhuangHebei 050024China School of Physics and Microelectronics Zhengzhou UniversityZhengzhouHenan 450001China School of Astronomy and Space Science Nanjing UniversityNanjingJiangsu 210023China Key laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjingJiangsu 210023China Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdaoShandong 266237China Key laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-Dao lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of Physical Science and Technology Southwest Jiaotong UniversityChengduSichuan 610031China College of Physics Sichuan UniversityChengduSichuan 610065China Key laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasaTibet 850000China School of physics and technology Wuhan UniversityWuhanHubei 430072Ch

The lHAASO-WFCTA experiment,which aims to observe cosmic rays in the sub-EeV range using the fluorescence technique,uses a new generation of high-performance *** ensure that the experiment has ex-cellent detection capability associated with the measurement of the energy spectrum,the primary composition of cosmic rays,and so on,an accurate geometrical reconstruction of air-shower events is *** paper de-scribes the development and testing of geometrical reconstruction for stereo viewed events using the WFCTA(Wide Field of view Cherenkov/Fluorescence Telescope Array)*** approaches,which take full advantage ofthe WFCTA *** *** is the stereo-angular method,which uses the pointing of triggered SiPMs in the shower trajectory,and the other is the stereo-timing method,which uses the triggering time of the fired *** results show that both methods have good geometrical resolution:the resolution of the stereo-timing method is slightly better than the stereo-angular method because the resolution of the latter is slightly limited by the shower track length.

关键词： cosmic ray fluorescence telescope stereo observation geometrical reconstruction

Observation of the Crab Nebula with lHAASO-KM2A−a performance study

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Chinese Physics C 2021年第2期45卷 518-530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 Z.Cao J.Chang J.F.Chang x.C.Chang B.M.chen J.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.chen N.cheng Y.D.cheng S.W.Cui x.H.Cui Y.D.Cui B.Z.Dai H.l.Dai Z.G.Dai D.della Volpe B.D'Ettorre Piazzoli x.J.Dong 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 Q.Gao W.Gao M.M.Ge l.S.Geng G.H.Gong Q.B.Gou M.H.Gu 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 x.Hou H.B.Hu S.Hu S.C.Hu x.J.Hu D.H.Huang Q.l.Huang W.H.Huang x.T.Huang Z.C.Huang F.Ji x.l.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.levochkin B.B.li C.li F.li H.B.li H.C.li H.Y.li J.li K.li W.l.li x.li x.R.li Y.li Y.Z.li Z.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.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 W.Mitthumsiri T.Montaruli Y.C.Nan B.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi D.Ruffolo V.Rulev A.Sáiz l.Shao O.Shchegolev x.D.Sheng J.R.Shi H.C.Song Yu.V.Stenkin V.Stepanov 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.D.Wang Y.J.Wang Y.P.Wang Z.Wang Z.H.Wang Z.x.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 G.xiao H.B.xiao G.G.xin Y.l.xin Y.xing D.l.xu R.x.xu l.xue D.H.Yan C.W.Yang F.F.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.D.Zeng T.x.Zeng W.Zeng Z.K.Zeng M.Zha x.x.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang J.l.Zhang J.W.Zhang l.Zhang l.x.Zhang P.F.Zhang P.P.Zhang R.Zhang S.R.Zhang S.S.Zhang x.Zhang x.P.Zhang Y.Zhang Y.F.Zhang Y.l.Zhang B.Zhao J.Zhao l.Zhao l.Z.Zhao S.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou J.N.Zhou P.Zhou R.Zhou x.x.Zhou C.G.Zhu F.R.Zhu H.Zhu K.J.Zhu x.Zuo Key laboratory of Particle Astrophyics&Experimental Physics Division&Computing Center Institute of High Energy PhysicsChinese Academy of Sciences100049 BeijingChina University of Chinese Academy of Sciences 100049 BeijingChina TIANFU Cosmic Ray Research Center ChengduSichuanChina State Key laboratory of Particle Detection and Electronics China University of Science and Technology of China 230026 HefeiAnhuiChina Department of Engineering Physics Tsinghua University100084 BeijingChina National Astronomical Observatories Chinese Academy of Sciences100101 BeijingChina National Space Science Center Chinese Academy of Sciences100190 BeijingChina School of Physics Peking University100871 BeijingChina Center for Astrophysics Guangzhou University510006 GuangzhouGuangdongChina School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen University519000 ZhuhaiGuangdongChina School of Physical Science and Technology Guangxi University530004 NanningGuangxiChina Hebei Normal University 050024 ShijiazhuangHebeiChina School of Physics and Microelectronics Zhengzhou University450001 ZhengzhouHenanChina School of Astronomy and Space Science Nanjing University210023 NanjingJiangsuChina Key laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of Sciences210023 NanjingJiangsuChina Institute of Frontier and Interdisciplinary Science Shandong University266237 QingdaoShandongChina Key laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of Sciences200030 ShanghaiChina Tsung-Dao lee Institute&School of Physics and Astronomy Shanghai Jiao Tong University200240 ShanghaiChina School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong University610031 ChengduSichuanChina College of Physics Sichuan University610065 ChengduSichuanChina Key laboratory of Cosmic Rays(Tibet University) Ministry of Education850000 LhasaTibetChina School of Physics and Tec

A sub-array of the large High Altitude Air Shower Observatory(lHAASO),KM2A is mainly designed to observe a large fraction of the northern sky to hunt for γ-ray sources at energies above 10 *** though the detector construction is still underway,half of the KM2A array has been operating stably since the end of *** this paper,we present the KM2A data analysis pipeline and the first observation of the Crab Nebula,a standard candle in very high energy γ-ray *** detect γ-ray signals from the Crab Nebula in both energy ranges of 10-100 TeV and>100 TeV with high significance,by analyzing the KM2A data of 136 live days between December 2019 and May *** the observations,we test the detector performance,including angular resolution,pointing accuracy and cosmic-ray background rejection *** energy spectrum of the Crab Nebula in the energy range 10-250 TeV fits well with a single power-law function dN/dE=(1.13±0.05stat±0.08sys)×10^(-14).(E/20 TeV)-309±0.06stat±0.02syscm^(-2) s^(-1) TeV^(-1).It is consistent with previous measurements by other *** opens a new window of γ-ray astronomy above 0.1 PeV through which new ultrahigh-energy γ-ray phenomena,such as cosmic PeVatrons,might be discovered.

关键词： γ-ray Crab Nebula extensive air showers cosmic rays

Spalling characteristics of high-temperature treated granitic rock at different strain rates

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Journal of Rock Mechanics and Geotechnical Engineering 2024年第4期16卷 1280-1288页

作者： l.F.Fan Q.H.Yang x.l.Du The Key laboratory of Urban Security and Disaster Engineering of Ministry of Education Beijing University of TechnologyBeijing100124China

The dynamic spalling characteristics of rock are important for stability analysis in rock *** paper presented an experimental investigation on the dynamic spalling characteristics of granite with different temperatures and strain rates.A series of dynamic spalling tests with different impact velocities were conducted on thermally treated granite at different *** dynamic spalling strengths of granite with different temperatures and strain rates were determined.A model was proposed to correlate the dynamic spalling strength of granite,high temperature and strain *** results show that the spalling strength of granite decreases with increasing ***,the spalling strength of granite with a higher strain rate is larger than that with a lower strain *** proposed model can describe the relationship among dynamic spalling strength of granite,high temperature and strain rate.

关键词： Dynamic spalling characteristics High temperature Strain rate Dynamic loading Granite

Rogue wave solutions and rogue-breather solutions to the focusing nonlinear Schr?dinger equation

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Communications in Theoretical Physics 2024年第3期76卷 33-41页

作者： Si-Jia chen xing lü College of Science Tianjin University of TechnologyTianjin 300384People's Republic of China Department of Mathematics Beijing Jiaotong UniversityBeijing 100044People's Republic of China Beijing laboratory of National Economic Security Early-warning Engineering Beijing Jiaotong UniversityBeijing 100044People's Republic of China

Based on the long wave limit method,the general form of the second-order and third-order rogue wave solutions to the focusing nonlinear Schr?dinger equation are given by introducing some arbitrary *** interaction solutions between the first-order rogue wave and one-breather wave are constructed by taking a long wave limit on the two-breather *** applying the same method to the three-breather solutions,two types of interaction solutions are obtained,namely the first-order rogue wave and two breather waves,the second-order rogue wave and one-breather wave,*** influence of the parameters related to the phase on the interaction phenomena is graphically *** occur among the rogue waves and breather *** the collisions,the shape of them remains *** abundant interaction phenomena in this paper will contribute to a better understanding of the propagation and control of nonlinear waves.

关键词： nonlinear Schrodinger equation rogue wave solutions interaction solutions

line-of-shower trigger method to lower energy threshold for GRB detection using lHAASO-WCDA

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Radiation Detection Technology and Methods 2021年第4期5卷 531-541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 Z.Cao Z.Cao J.Chang J.F.Chang x.C.Chan 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.chen N.chen Y.D.chen 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.Don J.H.Fan Y.Z.Fan Z.x.Fan J.Fang K.Fan C.F.Feng l.Feng S.H.Fen Y.l.Feng B.Gao C.D.Gao Q.Gao W.Gao M.M.Ge l.S.Gen G.H.Gong Q.B.Gou M.H.Gu 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 x.Hou H.B.Hu S.Hu S.C.Hu x.J.Hu D.H.Huang Q.l.Huan W.H.Huang x.T.Huang Z.C.Huang F.Ji x.l.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.levochkin 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.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.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 W.Mitthumsiri T.Montaruli Y.C.Nan B.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi D.Ruffolo V.Rulev A.Sáiz l.Shao O.Shchegolev x.D.Shen J.R.Shi H.C.Song Yu.V.Stenkin V.Stepanov Q.N.Sun x.N.Sun Z.B.Sun P.H.T.Tam Z.B.Tang W.W.Tian B.D.Wan C.Wang H.Wang H.G.Wang J.C.Wang J.S.Wang l.P.Wang l.Y.Wan R.N.Wang W.Wang W.Wang x.G.Wang x.J.Wan x.Y.Wang Y.D.Wan Y.J.Wan Y.P.Wang Z.Wang Z.Wang Z.H.Wang Z.x.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 G.xiao H.B.xiao G.G.xin Y.l.xin Y.xing D.l.xu R.x.xu l.xue D.H.Yan C.W.Yang F.F.Yang J.Y.Yang l.l.Yang M.J.Yan 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.D.Zeng T.x.Zeng W.Zeng Z.K.Zeng M.Zha x.x.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang J.l.Zhang J.W.Zhang l.Zhang l.Zhang l.x.Zhang P.F.Zhang P.P.Zhang R.Zhang S.R.Zhang S.S.Zhan x.Zhang x.P.Zhan Y.Zhan Y.Zhang Y.F.Zhang Y.l.Zhan B.Zhao J.Zhao l.Zhao l.Z.Zhao S.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou J.N.Zhou P.Zhou R.Zhou x.x.Zhou C.G. 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 ChengduSichuanChina State Key laboratory of Particle Detection and Electronics BeijingChina University of Science and Technology of China Hefei 230026AnhuiChina Department of Engineering Physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science Center Chinese Academy of SciencesBeijing 100190China School of Physics Peking UniversityBeijing 100871China Center for Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519000GuangdongChina School of Physical Science and Technology Guangxi UniversityNanning 530004GuangxiChina Hebei Normal University Shijiazhuang 050024HebeiChina School of Physics and Microelectronics Zhengzhou UniversityZhengzhou 450001HenanChina School of Astronomy and Space Science Nanjing UniversityNanjing 210023JiangsuChina Key laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237ShandongChina Key laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-Dao lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina College of Physics Sichuan UniversityChengdu 610065SichuanChina Key laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina School of Physic

Purpose Observation of high energy and very high emission from Gamma Ray Bursts(GRBs)is crucial to study the gigantic explosion and the underline *** a large field-of-view and almost full duty cycle,the Water Cherenkov Detector Array(WCDA),a sub-array of the large High Altitude Air Shower Observatory(lHAASO),is appropriate to monitor the very high energy emission from unpredictable transients such as *** Nevertheless,the main issue for an extensive air shower array is the high energy threshold which limits the horizon of the *** address this issue a new trigger method is developed in this article to lower the energy threshold of WCDA for GRB *** The proposed method significantly improves the detection efficiency of WCDA for gamma-rays around the GRB direction at 10-300 *** sensitivity of the WCDA for GRB detection with the new trigger method is *** achieved sensitivity of the quarter WCDA array above 10 GeV is comparable with that of *** data analysis process and corresponding fluence upper limit for GRB 190719C is presented as an example.

关键词： lHAASO WCDA GRB

In situ TEM investigation of electron irradiation and aging-induced high-density nanoprecipitates in an Mg-10Gd-3Y-1Zn-0.5Zr alloy

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Journal of Magnesium and Alloys 2024年第5期12卷 1841-1853页

作者： M.lv H.l.Ge Q.Q.Jin x.H.Shao Y.T.Zhou B.Zhang x.l.Ma Shenyang National laboratory for Materials Science Institute of Metal ResearchChinese Academy of Sciences72 Wenhua RoadShenyang 110016China School of Materials Science and Engineering University of Science and Technology of ChinaShenyang 110016China Materials Science and Engineering Research Center Guangxi University of Science and TechnologyLiuzhou 545006China

In-situ electron irradiation and aging are applied to introduce high-density precipitates in an Mg-10Gd-3Y-1Zn-0.5Zr(GWZ1031K,wt.%)alloy to improve the *** results show that the hardness of the Mg alloy after irradiation for 10 h and aging for 9 h at 250℃ is 1.64 GPa,which is approximately 64% higher than that of the samples before being *** is mainly attributed to γ'precipitates on the basal plane after irradiation and the high-density nanoscale β'precipitates on the prismatic plane after aging,which should be closely related to the irradiation-induced homogenous *** latter plays a key role in precipitation *** result paves a way to improve the mechanical properties of metallic materials by tailoring the precipitation through irradiation and aging.

关键词： Mg alloy Electron beam irradiation Hardening Precipitates In-situ TEM

A dynamic range extension system for lHAASOWCDA-1

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Radiation Detection Technology and Methods 2021年第4期5卷 520-530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 Z.Cao Z.Cao J.Chang J.F.Chang x.C.Chang 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.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 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 Q.Gao W.Gao M.M.Ge l.S.Geng G.H.Gong Q.B.Gou M.H.Gu 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 x.Hou H.B.Hu S.Hu S.C.Hu x.J.Hu D.H.Huang Q.l.Huang W.H.Huang x.T.Huang Y.Huang Z.C.Huang F.Ji x.l.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.levochkin 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.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.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 W.Mitthumsiri T.Montaruli Y.C.Nan B.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi D.Ruffolo V.Rulev A.Sáiz l.Shao O.Shchegolev x.D.Sheng J.R.Shi H.C.Song Yu.V.Stenkin V.Stepanov 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 W.Wang x.G.Wang x.J.Wang x.Y.Wang Y.D.Wang Y.J.Wang Y.P.Wang Z.Wang Z.Wang Z.H.Wang Z.x.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 G.xiao H.B.xiao G.G.xin Y.l.xin Y.xing D.l.xu R.x.xu l.xue D.H.Yan C.W.Yang F.F.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.D.Zeng T.x.Zeng W.Zeng Z.K.Zeng M.Zha x.x.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang J.l.Zhang J.W.Zhang l.Zhang l.Zhang l.x.Zhang P.F.Zhang P.P.Zhang R.Zhang S.R.Zhang S.S.Zhang x.Zhang x.P.Zhang Y.Zhang Y.Zhang Y.F.Zhang Y.l.Zhang B.Zhao J.Zhao l.Zhao l.Z.Zhao S.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou J.N.Zhou 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 State Key laboratory of Particle Detection and Electronics BeijingChina University of Science and Technology of China Hefei 230026AnhuiChina Department of Engineering Physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science Center Chinese Academy of SciencesBeijing 100190China School of Physics Peking UniversityBeijing 100871China Center for Astrophysics Guangzhou UniversityGuangzhou 510006GuangdongChina School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519000GuangdongChina School of Physical Science and Technology Guangxi UniversityNanning 530004GuangxiChina Hebei Normal University Shijiazhuang 050024HebeiChina School of Physics and Microelectronics Zhengzhou UniversityZhengzhou 450001HenanChina School of Astronomy and Space Science Nanjing UniversityNanjing 210023JiangsuChina Key laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023JiangsuChina Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237ShandongChina Key laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-Dao lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031SichuanChina College of Physics Sichuan UniversityChengdu 610065SichuanChina Key laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000TibetChina School of Physics

Purpose The main scientific goal of lHAASO-WCDA is to survey gamma-ray sources with energy from 100 GeV to 30 *** observe high-energy shower events,especially to measure the energy spectrum of cosmic rays from 100 TeV to 10 PeV,a dynamic range extension system(WCDA++)is designed to use a 1.5-inch PMT with a dynamic range of four orders of magnitude for each cell in *** The dynamic range is extended by using these PMTs to measure the effective charge density in the core region of air shower events,which is an important parameter for identifying the composition of primary *** and Conclusion The system has been running for more than one *** this paper,the details of the design and performance of WCDA++are presented.

关键词： lHAASO-WCDA WCDA++ Water Cherenkov detector Performance

Performance of lHAASO-WCDA and observation of the Crab Nebula as a standard candle

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Chinese Physics C 2021年第8期45卷 166-181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 Z.Cao Z.Cao J.Chang J.F.Chang x.C.Chang 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.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 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 Q.Gao W.Gao M.M.Ge l.S.Geng G.H.Gong Q.B.Gou M.H.Gu 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 x.Hou H.B.Hu S.Hu S.C.Hu x.J.Hu D.H.Huang Q.l.Huang W.H.Huang x.T.Huang Z.C.Huang F.Ji x.l.Ji H.Y.Jia K.Jiang Z.J.Jiang C.Jin D.Kuleshov K.levochkin 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.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.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 W.Mitthumsiri T.Montaruli Y.C.Nan B.Y.Pang P.Pattarakijwanich Z.Y.Pei M.Y.Qi B.Q.Qiao D.Ruffolo V.Rulev A.Saiz l.Shao O.Shchegolev x.D.Sheng J.R.Shi H.C.Song Yu.V.Stenkin V.Stepanov 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 W.Wang x.G.Wang x.J.Wang x.Y.Wang Y.D.Wang Y.J.Wang Y.P.Wang Z.Wang Z.Wang Z.H.Wang Z.x.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 G.xiao H.B.xiao G.G.xin Y.l.xin Y.xing D.l.xu R.x.xu l.xue D.H.Yan C.W.Yang F.F.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.D.Zeng T.x.Zeng W.Zeng Z.K.Zeng M.Zha x.x.Zhai B.B.Zhang H.M.Zhang H.Y.Zhang J.l.Zhang J.W.Zhang l.Zhang l.Zhang l.x.Zhang P.F.Zhang P.P.Zhang R.Zhang S.R.Zhang S.S.Zhang x.Zhang x.P.Zhang Y.Zhang Y.Zhang Y.F.Zhang Y.l.Zhang B.Zhao J.Zhao l.Zhao l.Z.Zhao S.P.Zhao F.Zheng Y.Zheng B.Zhou H.Zhou J.N.Zhou 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 State Key laboratory of Particle Detection and Electronics China University of Science and Technology of China Hefei 230026China Department of Engineering Physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science Center Chinese Academy of SciencesBeijing 100190China School of Physics Peking UniversityBeijing 100871China Center for Astrophysics Guangzhou UniversityGuangzhou 510006China School of Physics and Astronomy&School of Physics(Guangzhou) Sun Yat-sen UniversityZhuhai 519082China School of Physical Science and Technology Guangxi UniversityNanning 530004China Hebei Normal University Shijiazhuang 050024China School of Physics and Microelectronics Zhengzhou UniversityZhengzhou 450001China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Key laboratory of Dark Matter and Space Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China Key laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of SciencesShanghai 200030China Tsung-Dao lee Institute&School of Physics and Astronomy Shanghai Jiao Tong UniversityShanghai 200240China School of Physical Science and Technology&School of Information Science and Technology Southwest Jiaotong UniversityChengdu 610031China College of Physics Sichuan UniversityChengdu 610065China Key laboratory of Cosmic Rays(Tibet University) Ministry of EducationLhasa 850000China School of Physics and Technology Wuhan UniversityWuhan 430072China School of Physics and Astronomy Yunnan University

The first Water Cherenkov detector of the lHAASO experiment(WCDA-1)has been operating since April *** data for the first year have been analyzed to test its performance by observing the Crab Nebula as a standard *** WCDA-1 achieves a sensitivity of 65 mCU per year,with a statistical threshold of 5 *** accomplish this,a 97.7%cosmic-ray background rejection rate around 1 TeV and 99.8%around 6 TeV with an ap proximate photon acceptance of 50%is achieved after applying an algorithm to separate gamma-induced *** angular resolution is measured using the Crab Nebula as a point source to be approximately 0.45°at 1 TeV and better than 0.2°above 6 TeV,with a pointing accuracy better than 0.05°.These values all match the design *** energy resolution is found to be 33%for gamma rays around 6 *** spectral energy distribution of the Crab Nebula in the range from 500 GeV to 15.8 TeV is measured and found to be in agreement with the results from other TeV gamma ray observatories.

关键词： lHAASO-WCDA Crab Nebula angular resolution spectral energy distribution