检索结果-内蒙古大学图书馆

Charge Radii of Neutron-Rich Scandium Isotopes and the Seniority Symmetry in the 0f7/2 Shell

Physical Review Letters 2025年第18期134卷 182501-182501页

作者： S. W. Bai X. F. Yang Á. Koszorús J. C. Berengut J. Billowes M. L. Bissell K. Blaum A. Borschevsky P. Campbell B. Cheal C. S. Devlin K. T. Flanagan R. F. Garcia Ruiz H. Heylen J. D. Holt B. S. Hu A. Kanellakopoulos J. Krämer V. Lagaki B. Maaß S. Malbrunot-Ettenauer T. Miyagi K. König M. Kortelainen W. Nazarewicz R. Neugart G. Neyens W. Nörtershäuser P.-G. Reinhard M. L. Reitsma L. V. Rodríguez F. Sommer Z. Y. Xu School of Physics and State Key Laboratory of Nuclear Physics and Technology Peking University Beijing 100871 China KU Leuven Instituut voor Kern-en Stralingsfysica B-3001 Leuven Belgium School of Physics University of New South Wales Sydney New South Wales 2052 Australia UNSW Nuclear Innovation Centre UNSW Sydney Kensington New South Wales 2052 Australia Department of Physics and Astronomy The University of Manchester Manchester M13 9PL United Kingdom Max-Planck-Institut für Kernphysik D-69117 Heidelberg Germany Faculty of Science and Engineering Van Swinderen Institute for Particle Physics and Gravity University of Groningen 9747 AG Groningen The Netherlands Oliver Lodge Laboratory Oxford Street University of Liverpool Liverpool L69 7ZE United Kingdom Photon Science Institute Alan Turing Building University of Manchester Manchester M13 9PY United Kingdom Massachusetts Institute of Technology Cambridge Massachusetts USA Experimental Physics Department CERN CH-1211 Geneva 23 Switzerland TRIUMF 4004 Wesbrook Mall Vancouver British Columbia V6T 2A3 Canada Department of Physics McGill University 3600 Rue University Montreal Quebec H3A 2T8 Canada National Center for Computational Sciences and Physics Division Oak Ridge National Laboratory Oak Ridge Tennessee 37831 USA Cyclotron Institute and Department of Physics and Astronomy Texas A& M University College Station Texas 77843 USA Institut für Kernphysik Technische Universität Darmstadt D-64289 Darmstadt Germany Center for Computational Sciences University of Tsukuba 1-1-1 Tennodai Tsukuba 305-8577 Japan ExtreMe Matter Institute EMMI GSI Helmholtzzentrum für Schwerionenforschung GmbH 64291 Darmstadt Germany Department of Physics University of Jyväskylä PB 35(YFL) FIN-40351Jyväskylä Finland Facility for Rare Isotope Beams Michigan State University East Lansing Michigan 48824 USA Department of Physics and Astronomy Michigan State University East Lansing Michigan 48824 USA Institut für Kernchemie

Nuclear charge radii of neutron-rich Sc47–49 isotopes were measured using collinear laser spectroscopy at CERN-ISOLDE. The new data reveal that the charge radii of scandium isotopes exhibit a distinct trend between N=20 and N=28, with Sc41 and Sc49 isotopes having similar values, mirroring the closeness of the charge radii of Ca40 and Ca48. Theoretical models that successfully interpret the radii of calcium isotopes could not account for the observed behavior in scandium radii, in particular the reduced odd-even staggering. Remarkably, the inclusion of the new Sc49 radius data has unveiled a similar trend in the charge radii of N=28 isotones and Z=20 isotopes when adding the protons atop the Ca48 core and the neutrons atop the Ca40 core, respectively. We demonstrate that this trend is consistent with the prediction of the seniority model.

关键词：

来源：评论

学校读者我要写书评

暂无评论

The physical properties of γ-ray quiet flat-spectrum radio quasars: Why are they undetected by Fermi-LAT?

arXiv

引用

arXiv 2021年

作者： Deng, Xue-Jiao Xue, Rui Wang, Ze-Rui Xi, Shao-Qiang Xiao, Hu-Bing Du, Lei-Ming Xie, Zhao-Hua Department of Physics Yunnan Normal University Kunming650500 China Department of Physics Zhejiang Normal University Jinhua321004 China School of Astronomy and Space Science Nanjing University Nanjing0110093 China Key laboratory of Modern Astronomy and Astrophysics Nanjing University Ministry of Education Nanjing210023 China Key Laboratory of Particle Astrophysics Experimental Physics Division & Computing Center Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China Key Lab for Astrophysics Shanghai Normal University Shanghai200234 China

During a decade of the Fermi-Large Area Telescope (LAT) operation, thousands of blazars have been detected in the γ-ray band. However, there are still numbers of blazars that have not been detected in the γ-ray band. In this work, we focus on investigating why some flat-spectrum radio quasars (FSRQs) are undetected by Fermi-LAT. By cross-matching the Candidate Gamma-ray Blazars Survey catalog with the Fourth Catalog of Active Galactic Nuclei Detected by the Fermi-LAT, we select 11 γ-ray undetected (γ-ray quiet) FSRQs as our sample whose quasi-simultaneous multi-wavelength data are collected. In the framework of the conventional one-zone leptonic model, we investigate their underlying physical properties and study the possibility that they are undetected with γ-ray by modeling their quasi-simultaneous spectral energy distributions. In contrast to a smaller bulk Lorentz factor suggested by previous works, our results suggest that the dissipation region located relatively far away from the central super-massive black hole is more likely to be the cause of some γ-ray quiet FSRQs being undetected by Fermi-LAT. © 2021, CC BY.

关键词： Physical properties

来源：评论

学校读者我要写书评

暂无评论

Periodic Gamma-ray Modulation of the blazar PG 1553+113 Confirmed by Fermi-LAT and Multi-wavelength Observations

arXiv

引用

arXiv 2025年

作者： Abdollahi, S. Baldini, L. Barbiellini, G. Bellazzini, R. Berenji, B. Bissaldi, E. Blandford, R.D. Bonino, R. Bruel, P. Buson, S. Cameron, R.A. Caraveo, P.A. Casaburo, F. Cavazzuti, E. Cheung, C.C. Chiaro, G. Ciprini, S. Cozzolongo, G. Orestano, P. Cristarella Cutini, S. D’Ammando, F. Di Lalla, N. Dirirsa, F. Di Venere, L. Domínguez, A. Fegan, S.J. Ferrara, E.C. Fiori, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Garrappa, S. Gasparrini, D. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Green, D. Grenier, I.A. Guiriec, S. Hays, E. Horan, D. Kuss, M. Larsson, S. Laurenti, M. Li, J. Liodakis, I. Longo, F. Loparco, F. Lott, B. Lovellette, M.N. Lubrano, P. Maldera, S. Malyshev, D. Manfreda, A. Marcotulli, L. Martí-Devesa, G. Mazziotta, M.N. Mereu, I. Michelson, P.F. Mitthumsiri, W. Mizuno, T. Monzani, M.E. Morselli, A. Moskalenko, I.V. Negro, M. Omodei, N. Orienti, M. Orlando, E. Ormes, J.F. Paneque, D. Perri, M. Persic, M. Pesce-Rollins, M. Porter, T.A. Principe, G. Rainò, S. Rando, R. Rani, B. Razzano, M. Reimer, A. Reimer, O. Parkinson, P.M. Saz Scotton, L. Serini, D. Sesana, A. Sgrò, C. Siskind, E.J. Spandre, G. Spinelli, P. Suson, D.J. Tajima, H. Takahashi, M.N. Tak, D. Thayer, J.B. Thompson, D.J. Torres, D.F. Valverde, J. Verrecchia, F. Zaharijas, G. IRAP Université de Toulouse CNRS UPS CNES ToulouseF-31028 France Università di Pisa Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Istituto Nazionale di Fisica Nucleare Sezione di Trieste TriesteI-34127 Italy Dipartimento di Fisica Università di Trieste TriesteI-34127 Italy Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy California State University Los Angeles Department of Physics and Astronomy Los AngelesCA90032 United States Dipartimento di Fisica "M. Merlin" dell’Università e del Politecnico di Bari via Amendola 173 BariI-70126 Italy Istituto Nazionale di Fisica Nucleare Sezione di Bari BariI-70126 Italy W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics SLAC National Accelerator Laboratory Stanford University StanfordCA94305 United States Istituto Nazionale di Fisica Nucleare Sezione di Torino TorinoI-10125 Italy Dipartimento di Fisica Università degli Studi di Torino TorinoI-10125 Italy Laboratoire Leprince-Ringuet CNRS IN2P3 École polytechnique Institut Polytechnique de Paris Palaiseau91120 France Institut für Theoretische Physik and Astrophysik Universität Würzburg WürzburgD-97074 Germany INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Milano via E. Bassini 15 MilanoI-20133 Italy Istituto Nazionale di Fisica Nucleare Sezione di Roma "Tor Vergata" RomaI-00133 Italy Space Science Data Center - Agenzia Spaziale Italiana Via del Politecnico snc RomaI-00133 Italy Italian Space Agency Via del Politecnico snc Roma00133 Italy Space Science Division Naval Research Laboratory WashingtonDC20375-5352 United States Friedrich-Alexander Universität Erlangen-Nürnberg Erlangen Centre for Astroparticle Physics Erwin-Rommel-Str. 1 Erlangen91058 Germany Friedrich-Alexander-Universität Erlangen-Nürnberg Schlossplatz 4 Erlangen91054 Germany Dipartimento di Fisica Università degli Studi di Perugia Perugia

A 2.1 year periodic oscillation of the γ-ray flux from the blazar PG 1553+113 has previously been tentatively identified in ∼ 7 years of data from the Fermi Large Area Telescope. After 15 years of Fermi sky-survey observations, doubling the total time range, we report > 7-cycle γ-ray modulation with an estimated significance of 4 σ against stochastic red noise. Independent determinations of oscillation period and phase in the earlier and the new data are in close agreement (chance probability © 2025, CC BY-NC-SA.

关键词： Giant stars

来源：评论

学校读者我要写书评

暂无评论

由超拍电子伏特加速器产生的超高能伽马射线气泡

引用

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

来源：评论

学校读者我要写书评

暂无评论

Search for neutrino signals correlated with LHAASO diffuse Galactic emission

arXiv

引用

arXiv 2024年

作者： Li, Wenlian Huang, Tian-Qi Xu, Donglian He, Huihai Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai201210 China Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai200240 China Key Laboratory of Particle Astrophysics and Experimental Physics Division and Computing Center Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China TIANFU Cosmic Ray Research Center Sichuan Chengdu China School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China University of Chinese Academy of Sciences Beijing100049 China

The diffuse Galactic γ-ray emission originates from the interactions between cosmic rays and the interstellar medium or radiation fields within our Galaxy, where the production of neutrinos is also anticipated. Recently, the Large High Altitude Air Shower Observatory (LHAASO) reported measurements of diffuse γ-rays from the Galactic plane with energies ranging from sub-TeV to 1 PeV. Using publicly available 7 years of IceCube track data with the full detector, we conduct a template search using the γ-ray flux map observed by LHAASO-KM2A as the neutrino emission template and perform a scan search of the Galactic plane. In the template search, a mild excess of neutrinos is observed in the Galactic plane with a pretrial (posttrial) significance of 1.9σ (1.1σ). The measured muon neutrino intensity at 25 TeV is 4.73+2.53−251 × 10−14 TeV−1 cm−2 s−1 sr−1, consistent with the expected neutrino flux assuming that all the diffuse Galactic γ-rays originate from hadronic interactions. In the Galactic plane scan search, the most significant location is found at l = 63.57◦ and b = 0.93◦ with a pretrial (posttrial) significance of 4.6σ (1.8σ). © 2024, CC BY.

关键词： Gamma rays

来源：评论

学校读者我要写书评

暂无评论

Optimization of performance of the KM2A full array using the Crab Nebula

引用

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 *** 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 *** the implementation of these new selection criteria,the angular resolution was also significantly improved by approximately 10%at tens of *** aspects of the full KM2A array performance,such as the pointing error,were also calibrated using the Crab *** 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

来源：评论

学校读者我要写书评

暂无评论

Event generator for jet tomography in electron-ion collisions

引用

Physical Review D 2024年第3期110卷 034001-034001页

作者： Weiyao Ke Yuan-Yuan Zhang Hongxi Xing Xin-Nian Wang Institute of Particle Physics and Key Laboratory of Quark and Lepton Physics (MOE) Theoretical Division Nuclear Science Division MS 70R0309 Physics Department School of Science and Engineering Hefei 230026 China Guangdong Provincial Key Laboratory of Nuclear Science Institute of Quantum Matter Guangdong-Hong Kong Joint Laboratory of Quantum Matter Southern Nuclear Science Computing Center

We develop the first event generator, the electron-heavy-ion-jet-interaction-generator (eHIJING), for the jet tomography study of electron-ion collisions. In this generator, energetic jet partons produced from the initial hard scattering undergo multiple collisions with the nuclear target. The collision rate is proportional to the transverse-momentum-dependent (TMD) gluon density in the nucleus, which is given by a simple model inspired by the physics of gluon saturation. Medium-modified QCD splitting functions within the higher-twist (HT) and generalized higher-twist (GHT) frameworks are utilized to simulate parton showering in the nuclear medium that takes into account the non-Abelian Landau-Pomeranchuck-Midgal interference effect. Employing eHIJING, we revisit hadron production in semi-inclusive deep inelastic scattering (SIDIS) as measured by EMC, HERMES, and recent CLAS experiments. eHIJING with both GT and GHT frameworks gives reasonably good descriptions of these experimental data. Predictions for experiments at the future electron-ion colliders are also provided. It is demonstrated that future measurements of the transverse momentum broadening of single hadron spectra can be used to map out the two-dimensional kinematic (Q2, xB) dependence of the jet transport coefficient q^ in cold nuclear matter.

关键词： Electron-ion collisions Fragmentation into hadrons QCD in nuclear reactions

来源：评论

学校读者我要写书评

暂无评论

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

引用

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

来源：评论

学校读者我要写书评

暂无评论

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

引用

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

来源：评论

学校读者我要写书评

暂无评论

Global constraint on the jet transport coefficient from single-hadron, dihadron, and γ-hadron spectra in high-energy heavy-ion collisions

引用

Physical Review C 2024年第6期109卷 064917-064917页

作者： Man Xie Weiyao Ke Hanzhong Zhang Xin-Nian Wang Key Laboratory of Quark and Lepton Physics (MOE) & Institute of Particle Physics Central China Normal University Wuhan 430079 China Key Laboratory of Atomic and Subatomic Structure and Quantum Control (MOE) Guangdong Basic Research Center of Excellence for Structure and Fundamental Interactions of Matter Institute of Quantum Matter Guangdong-Hong Kong Joint Laboratory of Quantum Matter Guangdong Provincial Key Laboratory of Nuclear Science Southern Nuclear Science Computing Center Department of Physics Nuclear Science Division MS 70R0319 Theoretical Division

Modifications of large transverse momentum single-hadron, dihadron, and γ-hadron spectra in relativistic heavy-ion collisions are direct consequences of parton-medium interactions in the quark-gluon plasma (QGP). The interaction strength and underlying dynamics can be quantified by the jet transport coefficient q̂. We carry out the first global constraint on q̂ using a next-to-leading order pQCD parton model with higher-twist parton energy loss and combining world experimental data on single-hadron, dihadron, and γ-hadron suppression at both RHIC and LHC energies with a wide range of centralities. The global Bayesian analysis using the information field (IF) priors provides the most stringent constraint on q̂(T). We demonstrate in particular the progressive constraining power of the IF Bayesian analysis on the strong temperature dependence of q̂ using data from different centralities and colliding energies. We also discuss the advantage of using both inclusive and correlation observables with different geometric biases. As a verification, the obtained q̂(T) is shown to describe data on single-hadron anisotropy at high transverse momentum well. Predictions for future jet quenching measurements in oxygen-oxygen collisions are also provided.

关键词： Hard scattering Jet quenching Jets & heavy flavor physics Quark-gluon plasma Relativistic heavy-ion collisions Bayesian methods Information theory

来源：评论

学校读者我要写书评

暂无评论

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

请选择保存的检索档案：

请选择收藏分类：

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

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

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：