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Reconstruction of Cherenkov image bymultiple telescopes of LhAASO-WFCTA

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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’region.The 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 goal.multiple telescopes are put together and point to connected directions for a larger FoV.method Telescopes are deployed spatially as close as possible,but due to their own size,the distance between two adjacent telescopes is about 10 m.Therefore,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 telescopes.An event building method for Cherenkov images measured by multiple telescopes of WFCTA is developed.The performance of the shower measurements using the combined images is evaluated by comparing with showers that are fully contained by a virtual telescope in simulation.Results 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

Optimization of performance of the Km2A full array using the Crab Nebula

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Chinese Physics C 2024年第6期48卷 169-178页

作者：曹臻 F.Aharonian 安琪阿西克古白云翔包逸炜 D.Bastieri 毕效军毕玉江蔡金庭曹晴曹文羽曹喆常进常劲帆陈尚明陈恩生陈亮陈林陈龙陈明君陈玛丽陈起辉陈素弘陈天禄陈阳程宁程耀东崔明阳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 董绪强段凯凯樊军辉范一中方军方堃冯存峰封莉冯少辉丰晓婷冯有亮 S.Gabici 高博高川东高林青高启高卫高伟康葛茂茂耿利斯 G.Giacinti 龚光华苟全补顾旻皓郭福来郭晓磊郭义庆郭莹莹韩毅昂何会海贺昊宁何佳银何新波何钰 m.heller 贺远强侯博文侯超侯贤胡红波胡铨胡世聪黄代绘黄天奇黄文俊黄性涛黄晓渊黄勇黄志成季筱璐贾焕玉贾康江琨姜晓巍姜泽军金敏康明铭柯通 D.Kuleshov.K.Kurinov 李兵兵李澄李骢李丹李飞李海波李会财李华阳李军李剑李捷李凯李文龙李文莲李秀荣李昕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金艳刘茂元柳若愚刘四明刘伟刘怡刘以农鲁睿罗晴吕洪魁马伯强马玲玲马欣华毛基荣闵振 W.mitthumsiri 穆慧君南云程 A.Neronov 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 D.Semikoz 邵澄宇邵琅 O.Shchegolev 盛祥东舒富文宋慧超 Yu.V.Stenkin V.Stepanov 苏扬孙秦宁孙晓娜孙志斌谭柏轩唐庆文唐泽波田文武王超王昌贝王广威王洪光王惠惠王建成汪凯王利苹王玲玉王培汉王冉王为王祥高王祥玉王阳王玉东王岩谨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峰徐仁新徐伟立薛良闫大海颜景志颜田杨朝文杨帆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查敏张彬彬张丰张海明张恒英张建立张丽霞张力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毅张勇赵兵赵静赵雷赵立志赵世平郑福周斌周浩周佳能周猛周平周荣周勋秀祝成光祝凤荣朱辉朱科军左雄 LhAASO Collaboration 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 Chengdu 610000China 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 School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Center for Astrophysics Guangzhou UniversityGuangzhou 510006China hebei Normal University Shijiazhuang 050024China Key Laboratory of Dark matter and Space Astronomy&Key Laboratory of Radio Astronomy Purple Mountain ObservatoryChinese Academy of SciencesNanjing 210023China 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 UniversityZhuhai 519000&Guangzhou 510275China School of Physics and Astronomy Yunnan UniversityKunming 650091China Département de Physique Nucléaire et Corpusculaire Facultéde SciencesUniversitéde Genève24 Quai Ernest Ansermet1211 GenevaSwitzerland Institute of Frontier and Interdisciplinary Science Shandong UniversityQingdao 266237China APC Universit'e Paris Cit'eCNRS/IN2P3CEA/IRFUObservat

The full array of the Large high Altitude Air Shower Observatory(LhAASO)has been in operation since July 2021.For its kilometer-square array(Km2A),we optimized the selection criteria for very high and ultrahigh energyγ-rays using data collected from August 2021 to August 2022,resulting in an improvement in significance of the detection in the Crab Nebula of approximately 15%,compared with that of previous cuts.With the implementation of these new selection criteria,the angular resolution was also significantly improved by approximately 10%at tens of TeV.Other aspects of the full Km2A array performance,such as the pointing error,were also calibrated using the Crab Nebula.The resulting energy spectrum of the Crab Nebula in the energy range of 10-1000 TeV are well fitted by a log-parabola model,which is consistent with the previous results from LhAASO and other experiments.

关键词： γ-ray Crab Nebula significance

microstructure evolution and shape memory behaviors of Ni_(47)Ti_(44)Nb_(9)alloy subjected to multistep thermomechanical loading with different prestrain levels

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Journal of materials Science & Technology 2024年第4期171卷 80-93页

作者： Y.h.Zhang h.Li Z.W.Yang X.Liu Q.F.gu State Key Laboratory of Solidification Processing School of Materials Science and EngineeringNorthwestern Polytechnical UniversityXi’an 710072China Shaanxi Key Laboratory of high-Performance Precision Forming Technology and Equipment Northwestern Polytechnical UniversityXi’an 710072China

Ni_(47)Ti_(44)Nb_(9)shape memory alloy(SmA)is a promising material in the aerospace field due to its wide transformation hysteresis.The application of shape memory effect depends on multistep thermomechan-ical loading,viz.,low-temperature deformation and subsequent heating to recovery.Low-temperature deformation prestrain plays a pivotal role in shape memory properties tailoring of SmA components.however,microstructure evolution and deformation mechanisms of Ni_(47)Ti_(44)Nb_(9)SmA subjected to vari-ous prestrain levels are still unclear.To this end,microstructure evolution and shape memory behaviors of Ni_(47)Ti_(44)Nb_(9)alloy subjected to multistep thermomechanical loading with prestrain levels of 8%-16%at-28℃(m_(s)+30℃)were investigated.The results demonstrate that the stress-strain curve of the specimen exhibits four distinct stages at a maximal prestrain of 16%.Whereas stageⅡand stageⅢend at prestrains of∼8%and∼12%,respectively.In stageⅡ,the stress-induced martensitic transformation is accompanied by the dislocation slip of the NiTi matrix andβ-Nb inclusions.In stageⅢ,in addition to the higher density of dislocations and further growth of stress-induced martensite variants(SImVs),(001)compound twins are introduced as a result of the(001)deformation twinning in stress-induced martensite.more{20-1}martensite twins are gradually introduced in stageⅣ.Correspondingly,after subsequent unloading and heating,a higher density of{114}austenite twins form in the specimen with a larger prestrain of 16%.With increasing prestrain from 8%to 16%,the recoverable strainε_(re)^(T)upon heating increases first and then decreases.Theε_(re)^(T)obtains a maximum of 7.03%at 10%prestrain and de-creases to 6.17%at 16%prestrain.The increase ofε_(re)^(T)can be attributed to the formation of new SImVs,the further growth of existing SImVs,and the recoverable(001)compound twins.While the decrease ofε_(re)^(T)is mainly associated with the irrecoverable strain by{20−1}martensite twins.The effect ofβ-Nb inclusions on the evolution of SImVs i

关键词： Ni_(47)Ti_(44)Nb_(9)shape memory alloy Wide transformation hysteresis Thermomechanical loading microstructure evolution Shape memory behaviors Stress-induced martensitic transformation Deformation twinning

Free vibration and buckling analysis of polymeric composite beams reinforced by functionally graded bamboo fbers

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Applied mathematics and mechanics(English Edition) 2024年第3期45卷 543-562页

作者： h.m.FEIZABAD m.h.YAS Department of mechanical Engineering Razi UniversityKermanshah ***Iran

Natural fibers have been extensively researched as reinforcement materials in polymers on account of their environmental and economic advantages in comparison with synthetic fibers in the recent years.Bamboo fibers are renowned for their good mechanical properties,abundance,and short cycle growth.As beams are one of the fundamental structural components and are susceptible to mechanical loads in engineering applications,this paper performs a study on the free vibration and buckling responses of bamboo fiber reinforced composite(BFRC)beams on the elastic foundation.Three different functionally graded(FG)layouts and a uniform one are the considered distributions for unidirectional long bamboo fibers across the thickness.The elastic properties of the composite are determined with the law of mixture.Employing hamilton’s principle,the governing equations of motion are obtained.The generalized differential quadrature method(GDQm)is then applied to the equations to obtain the results.The achieved outcomes exhibit that the natural frequency and buckling load values vary as the fiber volume fractions and distributions,elastic foundation stiffness values,and boundary conditions(BCs)and slenderness ratio of the beam change.Furthermore,a comparative study is conducted between the derived analysis outcomes for BFRC and homogenous polymer beams to examine the effectiveness of bamboo fibers as reinforcement materials,demonstrating the significant enhancements in both vibration and buckling responses,with the exception of natural frequencies for cantilever beams on the Pasternak foundation with the FG-◇fiber distribution.Eventually,the obtained analysis results of BFRC beams are also compared with those for carbon nanotube reinforced composite(CNTRC)beams found in the literature,indicating that the buckling loads and natural frequencies of BFRC beams are lower than those of CNTRC beams.

关键词： bamboo fiber free vibration buckling analysis functionally graded(FG)beam elastic foundation generalized differential quadrature method(GDQm)

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 TeV.Even though the detector construction is still underway,half of the Km2A array has been operating stably since the end of 2019.In 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 astronomy.We 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 2020.With the observations,we test the detector performance,including angular resolution,pointing accuracy and cosmic-ray background rejection power.The 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 experiments.This 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

Geometrical reconstruction of fluorescence events observed by the LhAASO experiment

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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 telescopes.To 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 fundamental.This 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)detectors.Two approaches,which take full advantage ofthe WFCTA detectors.are investigated.One 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 SiPms.The 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

Study of BESIII trigger efficiencies with the 2018 J/ψ data

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Chinese Physics C 2021年第2期45卷 48-55页

作者： m.Ablikim m.N.Achasov P.Adlarson S.Ahmed m.Albrecht R.Aliberti A.Amoroso m.R.An Q.An X.h.Bai Y.Bai O.Bakina R.Baldini Ferroli I.Balossino Y.Ban K.Begzsuren N.Berger m.Bertani D.Bettoni F.Bianchi J.Bloms A.Bortone I.Boyko R.A.Briere h.Cai X.Cai A.Calcaterra G.F.Cao N.Cao S.A.Cetin J.F.Chang W.L.Chang G.Chelkov D.Y.Chen G.Chen h.S.Chen m.L.Chen S.J.Chen X.R.Chen Y.B.Chen Z.J Chen W.S.Cheng G.Cibinetto F.Cossio X.F.Cui h.L.Dai X.C.Dai A.Dbeyssi R.E.de Boer D.Dedovich Z.Y.Deng A.Denig I.Denysenko m.Destefanis F.De mori Y.Ding C.Dong J.Dong L.Y.Dong m.Y.Dong X.Dong S.X.Du Y.L.Fan J.Fang S.S.Fang Y.Fang R.Farinelli L.Fava F.Feldbauer G.Felici C.Q.Feng J.h.Feng m.Fritsch C.D.Fu Y.Gao Y.Gao Y.Gao Y.G.Gao I.Garzia P.T.Ge C.Geng E.m.Gersabeck A Gilman K.Goetzen L.Gong W.X.Gong W.Gradl m.Greco L.m.gu m.h.gu S.gu Y.T.gu C.Y guan A.Q.guo L.B.guo R.P.guo Y.P.guo A.guskov T.T.han W.Y.han X.Q.hao F.A.harris h hüsken K.L.he F.h.heinsius C.h.heinz T.held Y.K.heng C.herold m.himmelreich T.holtmann Y.R.hou Z.L.hou h.m.hu J.F.hu T.hu Y.hu G.S.huang L.Q.huang X.T.huang Y.P.huang Z.huang T.hussain W.Ikegami Andersson W.Imoehl m.Irshad S.Jaeger S.Janchiv Q.Ji Q.P.Ji X.B.Ji X.L.Ji h.B.Jiang X.S.Jiang J.B.Jiao Z.Jiao S.Jin Y.Jin T.Johansson N.Kalantar-Nayestanaki X.S.Kang R.Kappert m.Kavatsyuk B.C.Ke I.K.Keshk A.Khoukaz P.Kiese R.Kiuchi R.Kliemt L.Koch O.B.Kolcu B.Kopf m.Kuemmel m.Kuessner A.Kupsc m.G.Kurth W.Kühn J.J.Lane J.S.Lange P.Larin A.Lavania L.Lavezzi Z.h.Lei h.Leithoff m.Lellmann T.Lenz C.Li C.h.Li Cheng Li D.m.Li F.Li G.Li h.Li h.Li h.B.Li h.J.Li J.L.Li J.Q.Li J.S.Li Ke Li L.K.Li Lei Li P.R.Li S.Y.Li W.D.Li W.G.Li X.h.Li X.L.Li Z.Y.Li h.Liang h.Liang h.Liang Y.F.Liang Y.T.Liang L.Z.Liao J.Libby C.X.Lin B.J.Liu C.X.Liu D.Liu F.h.Liu Fang Liu Feng Liu h.B.Liu h.m.Liu huanhuan Liu huihui Liu J.B.Liu J.L.Liu J.Y.Liu K.Liu K.Y.Liu Ke Liu L.Liu m.h.Liu P.L.Liu Q.Liu Q.Liu S.B.Liu Shuai Liu T.Liu W.m.Liu X.Liu Y.Liu Y.B.Liu Z.A.Liu Z.Q.Liu X.C.Lou F.X.Lu h.J.Lu J.D.Lu J.G.Lu X.L.Lu Y.Lu Y.P.Lu C.L.Luo m.X.Luo b P.W.Luo T.Luo X.L.Luo S Institute of high Energy Physics Beijing 100049China Beihang University Beijing 100191China Beijing Institute of Petrochemical Technology Beijing 102617China Bochum Ruhr-University D-44780 BochumGermany Carnegie mellon University PittsburghPennsylvania 15213USA Central China Normal University Wuhan 430079China China Center of Advanced Science and Technology Beijing 100190China COmSATS University Islamabad Lahore CampusDefence RoadOff Raiwind Road54000 LahorePakistan Fudan University Shanghai 200443China GIBudker Institute of Nuclear Physics SB RAS(BINP) Novosibirsk 630090Russia GSI helmholtzcentre for heavy Ion Research Gmbh D-64291 DarmstadtGermany guangxi Normal University Guilin 541004China guangxi University Nanning 530004China hangzhou Normal University Hangzhou 310036China helmholtz Institute mainz Johann-Joachim-Becher-Weg 45D-55099 MainzGermany henan Normal University Xinxiang 453007China henan University of Science and Technology Luoyang 471003China huangshan College Huangshan 245000China hunan Normal University Changsha 410081China hunan University Changsha 410082China Indian Institute of Technology madras Chennai 600036India Indiana University BloomingtonIndiana 47405USA (A)INFN Laboratori Nazionali di Frascati I-00044FrascatiItaly(B)INFN Sezione di PerugiaI-06100PerugiaItaly(C)University of PerugiaI-06100PerugiaItaly (A)INFN Sezione di Ferrara I-44122FerraraItaly(B)University of FerraraI-44122FerraraItaly Institute of modern Physics Lanzhou 730000China Institute of Physics and Technology Peace Ave54BUlaanbaatar 13330Mongolia Jilin University Changchun 130012China Johannes gutenberg University of mainz Johann-Joachim-Becher-Weg 45D-55099 MainzGermany Joint Institute for Nuclear Research 141980 DubnaMoscow regionRussia Justus-Liebig-Universitaet Giessen IIPhysikalisches InstitutHeinrich-Buff-Ring 16D-35392GiessenGermany KVI-CART University of GroningenNL-9747 AA GroningenThe Netherlands Lanzhou University Lanzhou 730000China Liaoning Normal Unive

Using a dedicated data sample taken in 2018 on the J/ψpeak,we perform a detailed study of the trigger efficiencies of the BESIII detector.The efficiencies are determined from three representative physics processes,namely Bhabha scattering,dimuon production and generic hadronic events with charged particles.The combined efficiency of all active triggers approaches 100%in most cases,with uncertainties small enough not to affect most physics analyses.

关键词： BESIII trigger efficiency Bhabha dimuon hadronic events

Volume of fluid simulation of single argon bubble dynamics in liquid steel under Rh vacuum conditions

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Journal of Iron and Steel Research(International) 2024年第4期31卷 828-837页

作者： gu-jun Chen Sheng-ping he College of materials Science and Engineering Yangtze Normal UniversityChongqing 400044China College of materials Science and Engineering Chongqing UniversityChongqing 400044China

Single argon bubble dynamics in liquid steel under Ruhrstahl-heraeus(Rh)vacuum conditions were simulated using the volume of fluid method,and the ideal gas law was used to consider bubble growth due to heat transfer and pressure drop.Additional simulation with a constant bubble density was also performed to validate the numerical method,and the predicted terminal bubble shape and velocity were found to agree with those presented in the Grace diagram and calculated by drag correlation,respectively.The simulation results under Rh conditions indicate that the terminal bubble shape and velocity cannot be reached.The primary bubble growth occurs within a rising distance of 0.3 m owing to heating by the high-temperature liquid steel;subsequently,the bubble continues to grow under equilibrium with the hydrostatic pressure.When the initial diameter is 8-32 mm,the bubble diameter and rising velocity near the liquid surface are 80-200 mm and 0.5-0.8 m/s,respectively.The bubble rises rectilinearly with an axisymmetric shape,and the shape evolution history includes an initial sphere,(dimpled)ellipsoid,and spherical cap with satellite bubbles.

关键词： Bubble dynamics Liquid steel Volume of fluid Bubble growth Bubble shape Rising velocity

Q-homotopy analysis method for time-fractional Newell–Whitehead equation and time-fractional generalized hirota–Satsuma coupled KdV system

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Communications in Theoretical Physics 2024年第3期76卷 70-83页

作者： Di Liu Qiongya gu Lizhen Wang Center for Nonlinear Studies School of MathematicsNorthwest UniversityXi'an710127China

In this paper,two types of fractional nonlinear equations in Caputo sense,time-fractional Newell–Whitehead equation(FNWE)and time-fractional generalized hirota–Satsuma coupled KdV system(hS-cKdVS),are investigated by means of the q-homotopy analysis method(q-hAm).The approximate solutions of the proposed equations are constructed in the form of a convergent series and are compared with the corresponding exact solutions.Due to the presence of the auxiliary parameter h in this method,just a few terms of the series solution are required in order to obtain better approximation.For the sake of visualization,the numerical results obtained in this paper are graphically displayed with the help of maple.

关键词： fractional Newell-Whitehead equation fractional generalized hirota-Satsuma coupled KdV system approximate solution q-homotopy analysis method