检索结果-南通市图书馆

deformation behavior of Mg-Y-Ni alloys containing different volume fraction of LpSO phase during tension and compression through in-situ synchrotron diffraction

引用

Journal of Magnesium and Alloys 2024年第9期12卷 3631-3645页

作者： S.z.wu Y.Q.Chi G.Garces X.h.zhou h.G.Brokmeier X.G.Qiao M.Y.zheng School of Materials Science and Engineering Harbin Institute of TechnologyHarbin 150001China School of Electromechanical Engineering Guangdong University of TechnologyGuangzhou 510006China d.p.rtment of physical Metallurgy CENIM-CSICAvenida Gregorio del Amo 828040 MadridSpain Institute of Materials Science and Engineering Clausthal University of TechnologyAgricolastrasse 6D-38678 Clausthal-ZellerfeldGermany

The deformation behavior of the as-extruded Mg-Y-Ni alloys with different volume fraction of long period stacking ordered(LpSO)phase during tension and compression was investigated by in-situ synchrotron *** micro-yielding,macro-yielding,tension-compression asymmetry and strain hardening behavior of the alloys were explored by combining with deformation *** micro-yielding is dominated by basal slip of dynamic recrystallized(dRXed)grains in tension,while it is dominated by extension twinning of non-dynamic recrystallized(non-dRXed)grains in *** macro-yielding,the non-dRXed grains are still elastic deformed in tension and the basal slip of dRXed grains in compression are ***,the LpSO phase still retains elastic deformation,but can bear more load,so the higher the volume fraction of hard LpSO phase,the higher the tensile/compressive macro-yield strength of the *** from the low volume fraction of the non-dRXed grains and the delay effect of LpSO andγphases on extension twinning,the as-extruded alloys exhibit excellent tension-compression *** the volume fraction of LpSO phase reaches∼50%,tension-compression asymmetry is reversed,which is due to the fact that the LpSO phase is stronger in compression than in *** tensile strain hardening behavior is dominated by dislocation slip,while the dominate mechanism for compressive strain hardening changes from twinning in theα-Mg grains to kinking of the LpSO phase with increasing volume fraction of LpSO *** activation of kinking leads to the constant compressive strain hardening rate of∼2500 Mpa,which is significantly higher than the tensile strain hardening rate.

关键词： Mg-Y-Ni alloys LpSO phase In-situ synchrotron diffraction Micro-yielding Tensile-compression asymmetry Strain hardening

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

Specificity-preserving RGB-d saliency detection

引用

Computational Visual Media 2023年第2期9卷 297-317页

作者： tao zhou deng-ping Fan Geng Chen Yi zhou huazhu Fu School of Computer Science and Engineering Nanjing University of Science and TechnologyNanjing 210094China Key Laboratory of System Control and Information processing Ministry of EducationShanghaiChina Computer Vision Lab ETH Z¨urichZ¨urichSwitzerland School of Computer Science and Engineering Northwestern Polytechnical UniversityXi’anChina School of Computer Science and Engineering Southeast UniversityNanjingChina Inception Institute of Artificial Intelligence Abu DhabiUnited Arab Emirates

Salient object detection(SOd)in RGB and d.p.h images has attracted increasing research *** RGB-d SOd models usually ad.p. fusion strategies to learn a shared representation from RGB and d.p.h modalities,while few methods explicitly consider h.w.to preserve modality-specific *** this study,we propose a novel framework,the specificity-preserving network(SpNet),which improves SOd.p.rformance by exploring both the shared information and modality-specific ***,we use two modality-specific networks and a shared learning network to generate individual and shared saliency prediction *** effectively fuse cross-modal features in the shared learning network,we propose a cross-enhanced integration module(CIM)and.p.opagate the fused feature to the next layer to integrate cross-level ***,to capture rich complementary multi-modal information to boost SOd.p.rformance,we use a multi-modal feature aggregation(MFA)module to integrate the modalityspecific features from each individual decoder into the shared *** using skip connections between encoder and decoder layers,hierarchical features can be fully *** experiments demonstrate that our SpNet outperforms cutting-edge approaches on six popular RGB-d SOd and three camouflaged object detection *** project is publicly available at https://***/taozh2017/SpNet.

关键词： salient object detection(SOd) RGB-d cross-enhanced integration module(CIM) multi-modal feature aggregation(MFA)

来源：

维普期刊数据库评论

在线全文

维普期刊数据库

学校读者我要写书评

暂无评论

STRUCTURAL dETERMINATION OF TITANIUM-OXIdE NANOpARTICLES BY X-RAY ABSORpTION SpECTROSCOpY

引用

Acta Metallurgica Sinica(English Letters) 2002年第1期15卷 53-57页

作者： z.Y. wu J. zhang K. Ibrahim M.I. Abbas G. Li Y. tao T.d. hu F.Q. Liu h.J. Qian Y.N. Xie Q.h. zhang L. Gao z.z. Chen Beijing Synchrotron Radiation Facility Institute of High Energy PhysicsThe Chinese Academy of SciencesBeijing 100039China Laboratori Nazionali di Frascati Istituto Nazionali di Fisica Nucleare Via Enrico Fermi 40P.O. Box 13I-00044 FrascatiItaly Beijing Synchrotron Radiation Facility Institute of High Energy PhysicsThe Chinese Academy of Sciences Beijing 100039China Shanghai Institute of Ceramics The Chinese Academy of SciencesShanghai200050China

As a potential application of titanium-oxide nanoparticles, it is extremely important to investigate a detailed.p.cture of the surface and interior structural properties of nanocrystalline materials, such as rutile and anatase with diameters 7.0 and 4.5nm, respectively. X-ray absorption spectroscopy has been used to identify the local Ti environment and related electronic structure. we combine the experimental results at the Ti edge in both bulk and nano-crystals to determine the lattice distortion in terms of differently characteristic preedge features and the variation in the multiple-scattering region of X-ray absorption near-edge structure (XANES) spectra. The relationship between the transition peaks and the surface-to volume ratio is also discussed.

关键词： X-ray absorption near edge structure nano particle transition metal oxide

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

RESEARCh ON ChEMICAL COMpOSITION ANd MICROSTRUCTURE OF NEwLY-dEVELOpEd hIGh STRENGTh ANd hIGh ELONGATION STEELS

引用

Acta Metallurgica Sinica(English Letters) 2003年第2期16卷 122-131页

作者： Y.Chen X.Chen A.M.Guo d.X.Luo B.F.Xu z.X.Yuan p.h.Li S.K.pu S.B.zhou TechnicalcenterofwuhanIronandSteelCo. Wuhan430080China wuhanUniversityofScienceandTechnology Wuhan430081China

The different chemical composition of silicon and manganese as well as different retained austenite fraction ranged from 4% to 10% of the high strength and high elongation steels were studied in the paper. The dislocations and carbon concentration in retained austenite were observed by a transmission electron microscope and an electric probe analyzer, respectively. The experimental results sh.w.d that silicon and manganese are two fundamental alloying elements to stabilize austenite effectively but retaining austenite in different mechanisms. Meanwhile, the cooling processing played an important role in controlling the fraction of retained austenite of the hot-rolled high strength and high plasticity steels.

关键词： high strength high plasticity carbon silicon manganese hot- rolling retained austenite Ms point

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

EFFECT OF CARBON CONTENT ON MICROSTRUCTURE ANd.p.OpERTIES OF hIGh STRENGTh ANd hIGh ELONGATION STEELS

引用

Acta Metallurgica Sinica(English Letters) 2003年第1期16卷 65-71页

作者： Y.Chen X.Chen p.h.Li S.K.pu z.X.Yuan B.F.Xu d.X.Lou A.M.Guo S.B.zhou wuhan University of Science and Technology Wuhan 430081 China Technical Center of wuhan Iron and Steel Corp. Wuhan 430080 China Technical Center of wuhan Iron and Steel Corp. Wuhan 430080 China wuhan University of Science and Technology Wuhan 430081 China

The micro structure and mechanical properties of new kind of hot-rolled high strength and high elongation steels with retained austenite were studied by discussing the influence of different carbon content. The research results indicate that carbon content has a significant effect on retaining austenite and consequently resulting in high elongation. Besides, new findings about relationship between carbon content and retained austenite as well as properties were discussed in the paper.

关键词： carbon content high strength high elongation steel retained austenite

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

Super Cyclically Edge-connected Vertex-transitive Graphs of Girth at Least 5

引用

Acta Mathematica Sinica,English Series 2013年第8期29卷 1569-1580页

作者： Jin Xin zhou Yan tao LI d.p.rtment of Mathematics Beijing Jiaotong University d.p.rtment of Basic Teaching Beijing Union University

A cyclic edge-cut of a graph G is an edge set, the removal of which separates two cycles. If G has a cyclic edge-cut, then it is called cyclically separable. we call a cyclically separable graph super cyclically edge-connected, in short, super-λc, if the removal of any minimum cyclic edge-cut results in a component which is a shortest cycle. In [zhang, z., wang, B.： Super cyclically edge-connected transitive graphs. J. Combin. Optim., 22, 549–562 （2011）], it is proved that a connected vertex-transitive graph is super-λc if G has minimum degree at least 4 and girth at least 6, and the authors also presented a class of nonsuper-λc graphs which have degree 4 and girth 5. In this paper, a characterization of k （k≥4）-regular vertex-transitive nonsuper-λc graphs of girth 5 is given. Using this, we classify all k （k≥4）-regular nonsuper-λc Cayley graphs of girth 5, and construct the first infinite family of nonsuper-λc vertex-transitive non-Cayley graphs.

关键词： Cyclic edge-cut cyclic edge-connectivity super cyclically edge-connected vertex-transit-ive graphs

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

Geometrical reconstruction of fluorescence events observed by the LhAASO experiment

引用

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.w.ng 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.w.ng 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 d.p.rtment 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-sh.w.r 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 sh.w.r trajectory,and the other is the stereo-timing method,which uses the triggering time of the fired *** results sh.w.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 sh.w.r track length.

关键词： cosmic ray fluorescence telescope stereo observation geometrical reconstruction

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

Formation　and　Confirmation　of　the　“pure”　Laser　Induced.p.pulation　Grating　in　dye　Solution

引用

Chinese Journal of Lasers 1996年第6期B5卷 535-540页

作者： zhou d. J. LI R. h. zhENG Y. z.(Institute of Laser and Spectroscopy, zhongshan University, Guangzhou 510275, China) zhongshan Univ Guangzhou China

ＦｏｒｍａｔｉｏｎａｎｄＣｏｎｆｉｒｍａｔｉｏｎｏｆｔｈｅ“Ｐｕｒｅ”ＬａｓｅｒＩｎｄｕｃｅｄＰｏｐｕｌａｔｉｏｎＧｒａｔｉｎｇｉｎＤｙｅＳｏｌｕｔｉｏｎ￥ＺＨＯＵＤ．Ｊ．；ＬＩＲ．Ｈ．；ＺＨＥＮＧＹ．Ｚ．（Ｉｎｓｔ... 详细信息

ＦｏｒｍａｔｉｏｎａｎｄＣｏｎｆｉｒｍａｔｉｏｎｏｆｔｈｅ“Ｐｕｒｅ”ＬａｓｅｒＩｎｄｕｃｅｄＰｏｐｕｌａｔｉｏｎＧｒａｔｉｎｇｉｎＤｙｅＳｏｌｕｔｉｏｎ￥ＺＨＯＵＤ．Ｊ．；ＬＩＲ．Ｈ．；ＺＨＥＮＧＹ．Ｚ．（ＩｎｓｔｉｔｕｔｅｏｆＬａｓｅｒａｎｄＳｐ...

关键词： laser induced grating refraction index grating dye solution population grating

来源：

同方期刊数据库评论

在线全文

同方期刊数据库

学校读者我要写书评

暂无评论

The Lobster Eye Imager for Astronomy Onboard the SATech-01 Satellite

引用

Research in Astronomy and Astrophysics 2023年第9期23卷 66-78页

作者： z.X.Ling X.J.Sun C.zhang S.L.Sun G.Jin S.N.zhang X.F.zhang J.B.Chang F.S.Chen Y.F.Chen z.w.Cheng w.Fu Y.X.han h.Li J.F.Li Y.Li z.d.Li p.R.Liu Y.h.Lv X.h.Ma Y.J.Tang C.B.wang R.J.Xie Y.L.Xue A.L.Yan Q.zhang C.Y.Bao h.B.Cai h.Q.Cheng C.z.Cui Y.F.dai d.w.Fan h.B.hu J.w.hu M.h.huang z.Q.Jia C.C.Jin d.Y.Li J.Q.Li h.Y.Liu M.J.Liu Y.Liu h.w.pan Y.L.Qiu M.Sugizaki h.Sun w.X.wang Y.L.wang Q.Y.wu X.p.Xu Y.F.Xu h.N.yang X.yang B.zhang M.zhang w.d.zhang z.zhang d.h.zhao X.Q.Cong B.w.Jiang L.h.Li X.B.Qiu J.N.Sun d.T.Su J.wang C.wu z.Xu X.M.yang S.K.zhang z.zhang N.zhang Y.F.zhu h.Y.Ban X.z.Bi z.M.Cai w.Chen X.Chen Y.h.Chen Y.Cui X.L.duan z.G Feng Y.Gao J.w.he T.he J.J.huang F.Li J.S.Li T.J.Li T.T.Li h.Q.Liu L.Liu R.Liu S.Liu N.Meng Q.Shi A.T.Sun Y.M.wang Y.B.wang h.C.wu d.X Xu Y.Q yang Y.yang X.S.Yu K.X.zhang Y.L.zhang Y.h.zhang Y.T.zhang h.zhou X.C.zhu J.S.Cheng L.Qin L.wang Q.L.wang M.Bai R.L.Gao z.Ji Y.R.Liu F.L.Ma Y.J.Shi J.Su Y.Y.Tan J.z.Tong h.T.Xu C.B.Xue G.F.Xue w.Yuan National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China Shanghai Institute of Technical physics Chinese Academy of SciencesShanghai 200083China North Night Vision Technology Co. LTDNanjing 211106China Institute of high Energy physics Chinese Academy of SciencesBeijing 100049China Science and Technology on Low-Light-Level Night Vision Laboratory Xi'an 710065China Innovation Academy for Microsatellites Chinese Academy of SciencesShanghai 201204China Institute of Electrical Engineering Chinese Academy of ScienceBeijing 100190China National Space Science Center Chinese Academy of ScienceBeijing 100190China

The Lobster Eye Imager for Astronomy(LEIA),a pathfinder of the wide-field X-ray Telescope of the Einstein probe mission,was successfully launched onboard the SATech-01 satellite of the Chinese Academy of Sciences on2022 July *** this paper,we introduce the design and on-ground test results of the LEIA *** stateof-the-art Micro-pore Optics(MpO),a wide field of view of 346 square degrees(18.6°×18.6°)of the X-ray imager is *** optical assembly composed of 36 MpO chips is used to focus incident X-ray photons,and four large-format complementary metal-oxide semiconductor(CMOS)sensors,each of size 6 cm×6 cm,are used as the focal plane *** instrument has an angular resolution of 4’-8’(in terms of FwhM)for the central focal spot of the point-spread function,and an effective area of 2-3 cm^(2) at 1 keV in essentially all the directions within the field of *** detection passband is 0.5-4 keV in soft X-rays and the sensitivity is2-3×10^(-11) erg s^(-1) cm^(-2)(about 1 milliCrab)with a 1000 s *** total weight of LEIA is 56 kg and the power is 85 *** satellite,with a design lifetime of 2 yr,operates in a Sun-synchronous orbit of 500 km with an orbital period of 95 *** is paving the way for future missions by verifying in flight the technologies of both novel focusing imaging optics and CMOS sensors for X-ray observation,and by optimizing the working setups of the instrumental *** addition,LEIA is able to carry out scientific observations to find new transients and to monitor known sources in the soft X-ray band,albeit with limited useful observing time available.

关键词： instrumentation detectors-space vehicles instruments-telescopes-X-rays genera

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

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

引用

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.w.ng 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.w.ng 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 d.p.rtment 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 Sh.w.r 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.w.ich new ultrahigh-energy γ-ray phenomena,such as cosmic peVatrons,might be discovered.

关键词： γ-ray Crab Nebula extensive air sh.w.rs cosmic rays

来源：

维普期刊数据库

同方期刊数据库评论

在线全文

学校读者我要写书评

暂无评论

欢迎您,

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

请选择保存的检索档案：

请选择收藏分类：

通借通还

欢迎您,

建议与咨询 留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

在线全文

请选择保存的检索档案： 新增检索档案 确定 取消

请选择收藏分类： 新增自定义分类 确定 取消

通借通还

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

请选择保存的检索档案：

请选择收藏分类：