检索结果-内蒙古大学图书馆

Observation of high-energy neutrinos from the Galactic plane

science 2023年第6652期380卷 1338-1343页

作者： Fei Huang Department of Physics Loyola University Chicago Chicago IL 60660 USA. Deutsches Elektronen-Synchrotron D-15738 Zeuthen Germany. Department of Physics and Astronomy University of Canterbury Private Bag 4800 Christchurch New Zealand. Université Libre de Bruxelles Science Faculty CP230 B-1050 Brussels Belgium. Niels Bohr Institute University of Copenhagen DK-2100 Copenhagen Denmark. Oskar Klein Centre and Department of Physics Stockholm University SE-10691 Stockholm Sweden. Department of Physics TU Dortmund University D-44221 Dortmund Germany. Karlsruhe Institute of Technology Institute for Astroparticle Physics D-76021 Karlsruhe Germany. Bartol Research Institute and Department of Physics and Astronomy University of Delaware Newark DE 19716 USA. Department of Physics Marquette University Milwaukee WI 53201 USA. Department of Physics and Astronomy Uppsala University Box 516 S-75120 Uppsala Sweden. Erlangen Centre for Astroparticle Physics Friedrich-Alexander-Universität Erlangen-Nürnberg D-91058 Erlangen Germany. Department of Physics and Laboratory for Particle Physics and Cosmology Harvard University Cambridge MA 02138 USA. Department of Physics and Wisconsin IceCube Particle Astrophysics Center University of Wisconsin–Madison Madison WI 53706 USA. Department of Physics Massachusetts Institute of Technology Cambridge MA 02139 USA. Physics Department South Dakota School of Mines and Technology Rapid City SD 57701 USA. Department of Physics and Astronomy University of California Irvine CA 92697 USA. Department of Physics University of California Berkeley CA 94720 USA. Department of Astronomy Ohio State University Columbus OH 43210 USA. Department of Physics and Center for Cosmology and Astro-Particle Physics Ohio State University Columbus OH 43210 USA. Department of Physics University of Wuppertal D-42119 Wuppertal Germany. Fakultät für Physik & Astronomie Ruhr-Universität Bochum D-44780 Bochum Germany. Physik-department Technische Unive

The origin of high-energy cosmic rays, atomic nuclei that continuously impact Earth's atmosphere, is unknown. Because of deflection by interstellar magnetic fields, cosmic rays produced within the Milky Way arrive at Earth from random directions. However, cosmic rays interact with matter near their sources and during propagation, which produces high-energy neutrinos. We searched for neutrino emission using machine learning techniques applied to 10 years of data from the IceCube Neutrino Observatory. By comparing diffuse emission models to a background-only hypothesis, we identified neutrino emission from the Galactic plane at the 4.5s level of significance. The signal is consistent with diffuse emission of neutrinos from the Milky Way but could also arise from a population of unresolved point sources.

关键词：

来源：评论

学校读者我要写书评

暂无评论

Cogenesis of baryon and dark matter with PBHs and the QCD axion

引用

Physical Review D 2024年第11期110卷 115013-115013页

作者： Debasish Borah Nayan Das Suruj Jyoti Das Rome Samanta Department of Physics Indian Institute of Technology Guwahati Assam 781039 India Particle Theory and Cosmology Group Center for Theoretical Physics of the Universe Institute for Basic Science (IBS) Daejeon 34126 Korea CEICO Institute of Physics of the Czech Academy of Sciences Na Slovance 1999/2 182 21 Prague 8 Czech Republic Scuola Superiore Meridionale Largo San Marcellino 10 I-80138 Napoli Italy Istituto Nazionale di Fisica Nucleare (INFN) sezione di Napoli Via Cinthia 9 I-80126 Napoli Italy

With entropy injection, an early matter-dominated epoch (EMD) impels the axion decay constant fa toward larger values to produce correct axion dark matter (DM) abundance, thereby unfolding the low-mass axion (ma≲10−5 eV) parameter space to be searched for in axion experiments. We implement this proposition in a scenario where fa and the leptogenesis scale in a seesaw mechanism are equivalent. We show that if, instead, the EMD is provided by evaporating ultralight primordial black holes (PBHs), the scenario becomes strikingly testable with gravitational wave (GW) background alongside the axion searches. In particular, while being consistent with correct axion DM abundance, the scale fa≳1012 GeV, corresponding to the unflavored regime of leptogenesis with hierarchical right-handed neutrinos, can be probed with GW and axion experiments, which is otherwise not testable at neutrino or collider experiments. Additionally, axions produced from PBH evaporation can give rise to dark radiation within reach of future cosmic microwave background experiments.

关键词：

来源：评论

学校读者我要写书评

暂无评论

Towards a full wCDM map-based analysis for weak lensing surveys

arXiv

引用

arXiv 2022年

作者： Zürcher, Dominik Fluri, Janis Ajani, Virginia Fischbacher, Silvan Refregier, Alexandre Kacprzak, Tomasz Department of Physics Institute for Particle Physics and Astrophysics ETH Zürich Wolfgang Pauli Strasse 27 Zürich8093 Switzerland Swiss Data Science Center Paul Scherrer Institute PSI Villigen5232 Switzerland

The next generation of weak lensing surveys will measure the matter distribution of the local universe with unprecedented precision, allowing the resolution of non-Gaussian features of the convergence field. This encourages the use of higher-order mass-map statistics for cosmological parameter inference. We extend the forward-modelling based methodology introduced in a previous forecast paper to match these new requirements. We provide multiple forecasts for the wCDM parameter constraints that can be expected from stage 3 and 4 weak lensing surveys. We consider different survey setups, summary statistics and mass map filters including wavelets. We take into account the shear bias, photometric redshift uncertainties, and intrinsic alignment. The impact of baryons is investigated and the necessary scale cuts are applied. We compare the angular power spectrum analysis to peak and minima counts as well as Minkowski functionals of the mass maps. We find a preference for Starlet over Gaussian filters. Our results suggest that using a survey setup with 10 instead of 5 tomographic redshift bins is beneficial. Adding cross-tomographic information improves the constraints on cosmology and especially on galaxy intrinsic alignment for all statistics. In terms of constraining power, we find the angular power spectrum and the peak counts to be equally matched for stage 4 surveys, followed by minima counts and the Minkowski functionals. Combining different summary statistics significantly improves the constraints and compensates the stringent scale cuts. We identify the most ‘cost-effective’ combination to be the angular power spectrum, peak counts and Minkowski functionals following Starlet filtering. © 2022, CC BY.

关键词： Cost effectiveness

来源：评论

学校读者我要写书评

暂无评论

Measurement of differential cross sections of neutron-induced deuteron production reactions on carbon from 25 to 52 MeV

引用

Chinese physics C 2021年第6期45卷 109-120页

作者： Zengqi Cui Haoyu Jiang Kang Sun Guohui Zhang Ruirui Fan Wei Jiang Huaiyong Bai Yiwei Hu Jie Liu Han Yi Changjun Ning Zhijia Sun Jingyu Tang Qi An Jie Bao Yu Bao Ping Cao Haolei Chen Qiping Chen Yonghao Chen Yukai Chen Zhen Chen Changqing Feng Keqing Gao Minhao Gu Changcai Han Zijie Han Guozhu He Yongcheng He Yang Hong Hanxiong Huang Weiling Huang Xiru Huang Xiaolu Ji Xuyang Ji Zhijie Jiang Hantao Jing Ling Kang Mingtao Kang Bo Li Chao Li Jiawen Li Lun Li Qiang Li Xiao Li Yang Li Rong Liu Shubin Liu Xingyan Liu Guangyuan Luan Qili Mu Binbin Qi Jie Ren Zhizhou Ren Xichao Ruan Zhaohui Song Yingpeng Song Hong Sun Xiaoyang Sun Zhixin Tan Hongqing Tang Xinyi Tang Binbin Tian Lijiao Wang Pengcheng Wang Qi Wang Taofeng Wang Zhaohui Wang Jie Wen Zhongwei Wen Qingbiao Wu Xiaoguang Wu Xuan Wu Likun Xie Yiwei Yang Li Yu Tao Yu Yongji Yu Linhao Zhang Qiwei Zhang Xianpeng Zhang Yuliang Zhang Zhiyong Zhang Yubin Zhao Luping Zhou Zuying Zhou Danyang Zhu Kejun Zhu Peng Zhu State Key Laboratory of Nuclear Physics and Technology School of PhysicsPeking UniversityBeijing 100871China Institute of High Energy Physics Chinese Academy of Sciences(CAS)Beijing 100049China Spallation Neutron Source Science Center Dongguan 523803China University of Chinese Academy of Sciences Beijing 100049China State Key Laboratory of Particle Detection and Electronics Department of Modern Physics University of Science and Technology of ChinaHefei 230026China Key Laboratory of Nuclear Data China Institute of Atomic EnergyBeijing 102413China Institute of Nuclear Physics and Chemistry China Academy of Engineering PhysicsMianyang 621900China Northwest Institute of Nuclear Technology Xi'an 710024China Department of Engineering and Applied Physics University of Science and Technology of ChinaHefei 230026China School of Physics Beihang UniversityBeijing 100083China

The angle-differential cross sections of neutron-induced deuteron production from carbon were measured at six neutron energies from 25 to 52 MeV relative to those of n-p elastic scattering at the China Spallation Neutron Source(CSNS)Back-n white neutron *** employing theΔE-E telescopes of the Light-charged particle Detector Array(LPDA)system at 15.1°to 55.0°in the laboratory system,ratios of the angle-differential cross sections of the ^(12)C(n,xd)reactions to those of the n-p scattering were measured,and then,the angle-differential cross sections of the ^(12)C(n,xd)reactions were obtained using the angle-differential cross sections of the n-p elastic scattering from the JENDL-4.0/HE-2015 library as the *** obtained results are compared with data from previous measurements,all of which are based on mono-energic neutrons,the evaluated data from the JENDL-4.0/HE-2015 library and the ENDF-B/VIII.0 library,and those from theoretical calculations based on INCA code and Talys-1.9 *** the first white-neutron-source-based systematic measurement of the angle-differential cross sections of neutron-induced deuteron production reactions on carbon in several tens of MeV,the present work can provide a reference to the data library considering the lack of experimental data.

关键词： ^(12)C(n,xd)reactions relative angle-differential cross sections CSNS Back-n white neutron source LPDA

来源：评论

学校读者我要写书评

暂无评论

Progress towards an array-wide diffuse UHE neutrino search with the Askaryan Radio Array 10

Progress towards an array-wide diffuse UHE neutrino search w...

引用

10th International Workshop on Acoustic and Radio EeV Neutrino Detection Activities, ARENA 2024

作者： Muzio, Marco Stein Ali, S. Allison, P. Archambault, S. Beatty, J.J. Besson, D.Z. Bishop, A. Chen, P. Chen, Y.C. Chen, Y.-C. Clark, B.A. Connolly, A. Couberly, K. Cremonesi, L. Cummings, A. Dasgupta, P. Debolt, R. de Kockere, S. de Vries, K.D. Deaconu, C. DuVernois, M.A. Flaherty, J. Friedman, E. Gaior, R. Giri, P. Hanson, J. Harty, N. Hoffman, K.D. Huang, M.H. Hughes, K. Ishihara, A. Karle, A. Kelley, J.L. Kim, K.-C. Kim, M.-C. Kravchenko, I. Krebs, R. Kuo, C.Y. Kurusu, K. Latif, U.A. Liu, C.H. Liu, T.C. Luszczak, W. Mase, K. Muzio, M.S. Nam, J. Nichol, R.J. Novikov, A. Nozdrina, A. Oberla, E. Pan, Y. Pfendner, C. Punsuebsay, N. Roth, J. Salcedo-Gomez, A. Seckel, D. Seikh, M.F.H. Shiao, Y.-S. Su, S.C. Toscano, S. Torres, J. Touart, J. van Eijndhoven, N. Varner, G.S. Vieregg, A. Wang, M.-Z. Wang, S.-H. Wissel, S.A. Xie, C. Yoshida, S. Young, R. Center for Multi-Messenger Astrophysics Institute for Gravitation and the Cosmos Pennsylvania State University University ParkPA16802 United States Department of Physics Pennsylvania State University University ParkPA16802 United States Department of Astronomy and Astrophysics Pennsylvania State University University ParkPA16802 United States Dept. of Physics and Astronomy University of Kansas LawrenceKS66045 United States Dept. of Physics Center for Cosmology and AstroParticle Physics The Ohio State University ColumbusOH43210 United States Dept. of Physics Chiba University Chiba Japan Dept. of Physics University of Wisconsin-Madison MadisonWI53706 United States Dept. of Physics Grad. Inst. of Astrophys. Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei Taiwan Dept. of Physics University of Maryland College ParkMD20742 United States Dept. of Physics and Astronomy University College London London United Kingdom Center for Multi-Messenger Astrophysics Institute for Gravitation and the Cosmos Pennsylvania State University University ParkPA16802 United States Dept. of Physics Pennsylvania State University University ParkPA16802 United States Dept. of Astronomy and Astrophysics Pennsylvania State University University ParkPA16802 United States Vrije Universiteit Brussel Brussels Belgium Dept. of Physics Enrico Fermi Institue Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Dept. of Physics and Astronomy University of Nebraska LincolnNE68588 United States Dept. Physics and Astronomy Whittier College WhittierCA90602 United States Dept. of Physics University of Delaware NewarkDE19716 United States Dept. of Energy Engineering National United University Miaoli Taiwan Dept. of Applied Physics National Pingtung University Pingtung County Pingtung City900393 Taiwan Dept. of Physics and Astronomy Denison University GranvilleOH43023 United States Nat

The Askaryan Radio Array (ARA) is an in-ice ultrahigh energy (UHE) neutrino experiment at the South Pole. ARA aims to detect the radio emissions from neutrino-induced particle showers using in-ice clusters of antennas buried ∼200 m deep on a roughly cubical lattice with side length of ∼10 m. ARA has five such independent stations which have collectively accumulated ∼30 station-years of livetime through 2023. The fifth station of ARA has an additional sub-detector, known as the phased array, which pioneered an interferometric trigger constructed by beamforming the signals of 7 tightly packed, vertically-polarized antennas. This scheme has been demonstrated to significantly improve the trigger efficiency for low SNR signals. In this talk, we will present the current state of the first array-wide diffuse neutrino search using 24 station-years of data (through 2021). We anticipate that this analysis will result in the first UHE neutrino observation or world-leading limits from a radio neutrino detector below 100 EeV. Additionally, this analysis will demonstrate the feasibility for multi-station in-ice radio arrays to successfully conduct an array-wide neutrino search — paving the way for future, large detector arrays such as RNO-G and IceCube-Gen2 Radio. © Copyright owned by the author(s).

关键词： Neutrons

来源：评论

学校读者我要写书评

暂无评论

Search for Solar B8 Neutrinos in the PandaX-4T Experiment Using Neutrino-Nucleus Coherent Scattering

引用

Physical Review Letters 2023年第2期130卷 021802-021802页

作者： Wenbo Ma Abdusalam Abdukerim Chen Cheng Zihao Bo Wei Chen Xun Chen Yunhua Chen Zhaokan Cheng Xiangyi Cui Yingjie Fan Deqing Fang Changbo Fu Mengting Fu Lisheng Geng Karl Giboni Linhui Gu Xuyuan Guo Chencheng Han Ke Han Changda He Jinrong He Di Huang Yanlin Huang Zhou Huang Ruquan Hou Xiangdong Ji Yonglin Ju Chenxiang Li Jiafu Li Mingchuan Li Shu Li Shuaijie Li Qing Lin Jianglai Liu Xiaoying Lu Lingyin Luo Yunyang Luo Yugang Ma Yajun Mao Nasir Shaheed Yue Meng Xuyang Ning Ningchun Qi Zhicheng Qian Xiangxiang Ren Changsong Shang Xiaofeng Shang Guofang Shen Lin Si Wenliang Sun Andi Tan Yi Tao Anqing Wang Meng Wang Qiuhong Wang Shaobo Wang Siguang Wang Wei Wang Xiuli Wang Zhou Wang Yuehuan Wei Mengmeng Wu Weihao Wu Jingkai Xia Mengjiao Xiao Xiang Xiao Pengwei Xie Binbin Yan Xiyu Yan Jijun Yang Yong Yang Chunxu Yu Jumin Yuan Ying Yuan Zhe Yuan Xinning Zeng Dan Zhang Minzhen Zhang Peng Zhang Shibo Zhang Shu Zhang Tao Zhang Yingxin Zhang Yuanyuan Zhang Li Zhao Qibin Zheng Jifang Zhou Ning Zhou Xiaopeng Zhou Yong Zhou Yubo Zhou School of Physics and Astronomy Shanghai Jiao Tong University Key Laboratory for Particle Astrophysics and Cosmology (MoE) Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai 200240 China School of Physics Sun Yat-Sen University Guangzhou 510275 China Shanghai Jiao Tong University Sichuan Research Institute Chengdu 610213 China Yalong River Hydropower Development Company Ltd. 288 Shuanglin Road Chengdu 610051 China Sino-French Institute of Nuclear Engineering and Technology Sun Yat-Sen University Zhuhai 519082 China Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai 200240 China School of Physics Nankai University Tianjin 300071 China Key Laboratory of Nuclear Physics and Ion-beam Application (MOE) Institute of Modern Physics Fudan University Shanghai 200433 China School of Physics Peking University Beijing 100871 China School of Physics Beihang University Beijing 102206 China International Research Center for Nuclei and Particles in the Cosmos and Beijing Key Laboratory of Advanced Nuclear Materials and Physics Beihang University Beijing 100191 China School of Physics and Microelectronics Zhengzhou University Zhengzhou Henan 450001 China School of Medical Instrument and Food Engineering University of Shanghai for Science and Technology Shanghai 200093 China Department of Physics University of Maryland College Park Maryland 20742 USA School of Mechanical Engineering Shanghai Jiao Tong University Shanghai 200240 China State Key Laboratory of Particle Detection and Electronics University of Science and Technology of China Hefei 230026 China Department of Modern Physics University of Science and Technology of China Hefei 230026 China Research Center for Particle Science and Technology Institute of Frontier and Interdisciplinary Science Shandong University Qingdao 266237 Shandong China Key Laboratory of Particle Physics and Particle Irradiation of Ministry of Education Shandong University Qingdao 266237 Shandong China SJTU Pa

A search for interactions from solar B8 neutrinos elastically scattering off xenon nuclei using PandaX-4T commissioning data is reported. The energy threshold of this search is further lowered compared with the previous search for dark matter, with various techniques utilized to suppress the background that emerges from data with the lowered threshold. A blind analysis is performed on the data with an effective exposure of 0.48 tonne year, and no significant excess of events is observed. Among the results obtained using the neutrino-nucleus coherent scattering, our results give the best constraint on the solar B8 neutrino flux. We further provide a more stringent limit on the cross section between dark matter and nucleon in the mass range from 3 to 9 GeV/c2.

关键词： Dark matter particle dark matter Solar neutrinos

来源：评论

学校读者我要写书评

暂无评论

Layout optimization and Performance of Large Array of imaging atmospheric Cherenkov Telescope (LACT)

arXiv

引用

arXiv 2024年

作者： Zhang, Zhipeng Yang, Ruizhi Zhang, Shoushan Xie, Zhen Liu, Jiali Yin, Liqiao Wang, Yudong Ma, Lingling Cao, Zhen School of Astronomy and Space Science University of Science and Technology of China Anhui Hefei230026 China CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Anhui Hefei230026 China Deep Space Exploration Laboratory School of Physical Sciences University of Science and Technology of China Hefei230026 China Key Laboratory of Particle Astrophysics Institute of High Energy Physics Beijing China Department of Physics University of Chinese Academy of Sciences Beijing China Tianfu Cosmic Ray Research Center Chengdu China

Large Array of imaging atmospheric Cherenkov Telescope (LACT) is an array of 32 Cherenkov telescopes with 6-meter diameter mirrors to be constructed at the LHAASO site. In this work, we present a study on the layout optimization and performance analysis of LACT. We investigate two observation modes: large zenith angle observations for ultra-high energy events and small zenith angle observations for lower energy thresholds. For large zenith angles (60°), simulations show that an 8-telescope subarray can achieve an effective area of 3 km2 and excellent angular resolution. For small zenith angles, we optimize the layout of 4-telescope cells and the full 32-telescope array. The threshold of the full array is about 200 GeV, which is particularly crucial for studying transient phenomena, including gamma-ray bursts (GRBs) and active galactic nuclei (AGNs). This study provides important guidance for the final LACT layout design and performance estimates under different observational conditions, demonstrating LACT's potential for deep observations of ultra-high energy γ-ray sources and morphological studies of PeVatrons, as well as time-domain γ-ray astronomy. Copyright © 2024, The Authors. All rights reserved.

关键词： cosmology

来源：评论

学校读者我要写书评

暂无评论

Forecast constraints on the baryonic feedback effect from the future kinetic Sunyaev-Zel'dovich effect detection

arXiv

引用

arXiv 2024年

作者： Zheng, Yi Zhang, Pengjie School of Physics and Astronomy Sun Yat-sen University 2 Daxue Road Tangjia Zhuhai519082 China CSST Science Center for the Guangdong-Hong kong-Macau Greater Bay Area SYSU Zhuha 519082 China Department of Astronomy School of Physics and Astronomy Shanghai JiaoTong University Shanghai200240 China Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai200240 China Shanghai Key Laboratory for Particle Physics and Cosmology China

The baryonic feedback effect is an important systematic error in the weak lensing (WL) analysis. It contributes partly to the S8 tension in the literature. With the next generations of large scale structure (LSS) and CMB experiments, the high signal-to-noise kinetic Sunyaev-Zel'dovich (kSZ) effect detection can tightly constrain the baryon distribution in and around dark matter halos, and quantify the baryonic effect in the weak lensing statistics. In this work, we apply the Fisher matrix technique to predict the future kSZ constraints on 3 kSZ-sensitive Baryon Correction Model (BCM) parameters. Our calculations show that, in combination with next generation LSS surveys, the 3rd generation CMB experiments such as AdvACT and Simon Observatory can constrain the matter power spectrum damping S(k) to the precision of σS(k) 3h−3/V at k 10h/Mpc, where V is the overlapped survey volume between the future LSS and CMB surveys. For the 4th generation CMB surveys such as CMB-S4 and CMB-HD, the constraint will be enhanced to σS(k) 3h−3/V. If extra-observations, e.g. X-ray detection and thermal SZ observation, can effectively fix the gas density profile slope parameter δ, the constraint on S(k) will be further boosted to σS(k) 3h−3/V and σS(k) 3h−3/V for the 3rd and 4th generation CMB surveys. © 2024, CC BY-NC-ND.

关键词： Density of gases

来源：评论

学校读者我要写书评

暂无评论

Variations of secondary particle arrival time detected by LHAASO-KM2A during thunderstorms 38

Variations of secondary particle arrival time detected by LH...

引用

38th International Cosmic Ray Conference, ICRC 2023

作者： Chen, Xuejian Zhou, Xunxiu Yang, Ci Huang, Daihui Cao, Zhen Aharonian, F. An, Q. Axikegu Bai, Y.X. Bao, Y.W. Bastieri, D. Bi, X.J. Bi, Y.J. Cai, J.T. Cao, Q. Cao, W.Y. Cao, Zhe Chang, J. Chang, J.F. Chen, A.M. Chen, E.S. Chen, Liang Chen, Lin Chen, Long Chen, M.J. Chen, M.L. Chen, Q.H. Chen, S.H. Chen, S.Z. Chen, T.L. Chen, Y. Cheng, N. Cheng, Y.D. Cui, M.Y. Cui, S.W. Cui, X.H. Cui, Y.D. Dai, B.Z. Dai, H.L. Dai, Z.G. Danzengluobu della Volpe, D. Dong, X.Q. Duan, K.K. Fan, J.H. Fan, Y.Z. Fang, J. Fang, K. Feng, C.F. Feng, L. Feng, S.H. Feng, X.T. Feng, Y.L. Gabici, S. Gao, B. Gao, C.D. Gao, L.Q. Gao, Q. Gao, W. Gao, W.K. Ge, M.M. Geng, L.S. Giacinti, G. Gong, G.H. Gou, Q.B. Gu, M.H. Guo, F.L. Guo, X.L. Guo, Y.Q. Guo, Y.Y. Han, Y.A. He, H.H. He, H.N. He, J.Y. He, X.B. He, Y. Heller, M. Hor, Y.K. Hou, B.W. Hou, C. Hou, X. Hu, H.B. Hu, Q. Hu, S.C. Huang, D.H. Huang, T.Q. Huang, W.J. Huang, X.T. Huang, X.Y. Huang, Y. Huang, Z.C. Ji, X.L. Jia, H.Y. Jia, K. Jiang, K. Jiang, X.W. Jiang, Z.J. Jin, M. Kang, M.M. Ke, T. Kuleshov, D. Kurinov, K. Li, B.B. Li, Cheng Li, Cong Li, D. Li, F. Li, H.B. Li, H.C. Li, H.Y. Li, J. Li, Jian Li, Jie Li, K. Li, W.L. Li, W.L. Li, X.R. Li, Xin Li, Y.Z. Li, Zhe Li, Zhuo Liang, E.W. Liang, Y.F. Lin, S.J. Liu, B. Liu, C. Liu, D. Liu, H. Liu, H.D. Liu, J. Liu, J.L. Liu, J.Y. Liu, M.Y. Liu, R.Y. Liu, S.M. Liu, W. Liu, Y. Liu, Y.N. Lu, R. Luo, Q. Lv, H.K. Ma, B.Q. Ma, L.L. Ma, X.H. Mao, J.R. Min, Z. Mitthumsiri, W. Mu, H.J. Nan, Y.C. Neronov, A. Ou, Z.W. Pang, B.Y. Pattarakijwanich, P. Pei, Z.Y. Qi, M.Y. Qi, Y.Q. Qiao, B.Q. Qin, J.J. Ruffolo, D. Sáiz, A. Semikoz, D. Shao, C.Y. Shao, L. Shchegolev, O. Sheng, X.D. Shu, F.W. Song, H.C. Stenkin, Yu.V. Stepanov, V. Su, Y. Sun, Q.N. Sun, X.N. School of Physical Science and Technology Southwest Jiaotong University Chengdu610031 China Key Laboratory of Particle Astrophyics Experimental Physics Division Computing Center Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China University of Chinese Academy of Sciences Beijing100049 China TIANFU Cosmic Ray Research Center Sichuan Chengdu China Dublin Institute for Advanced Studies 31 Fitzwilliam Place Dublin 2 Ireland Max-Planck-Institut for Nuclear Physics P.O. Box 103980 Heidelberg69029 Germany State Key Laboratory of Particle Detection and Electronics China University of Science and Technology of China Anhui Hefei230026 China School of Physical Science and Technology School of Information Science and Technology Southwest Jiaotong University Sichuan Chengdu610031 China School of Astronomy and Space Science Nanjing University Jiangsu Nanjing210023 China Center for Astrophysics Guangzhou University Guangdong Guangzhou510006 China Hebei Normal University Hebei Shijiazhuang050024 China Key Laboratory of Dark Matter and Space Astronomy Key Laboratory of Radio Astronomy Purple Mountain Observatory Chinese Academy of Sciences Jiangsu Nanjing210023 China Tsung-Dao Lee Institute School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Key Laboratory of Cosmic Rays Tibet University Ministry of Education Tibet Lhasa850000 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China School of Physics and Astronomy Sun Yat-sen University Zhuhai519000 China School of Physics Sun Yat-sen University Guangdong Guangzhou510275 China Sino-French Institute of Nuclear Engineering and Technology Sun Yat-sen University Zhuhai519000 China School of Physics and Astronomy Yunnan University Yunnan Kunming650091 China Départeme

A sub-array of the Large High Altitude Air Shower Observatory (LHAASO), KM2A contains 5216 electromagnetic particle detectors (EDs) and 1188 muon detectors (MDs). For each shower event that meets the trigger conditions (at least 20 fired EDs within a time window of 400 ns) in KM2A array, there are many signals from ED and MD detectors. The information on the arrival time and location of each signal are recorded, and the ED hits are used for shower reconstruction. Due to the acceleration and deflection by the atmospheric electric field (AEF) during a thunderstorm, the arrival time and position of the ground-level particles are modified, resulting in the changes in the inferred shower detection. To understand the shower event variation during thunderstorms, the particle arrival time is studied by analyzing the KM2A data. We can measure the distribution of changes of arrival time in the thunderstorm electric field. The variation amplitude is not only dependent on the AEF, but also highly correlated with the direction of the shower event. With the increase of the AEF strength and the zenith angle, the variation in amplitude of the arrival time becomes larger. Our results are useful in understanding the variation of shower rate detected by LHAASO-KM2A, and will also provide important information for shower reconstruction during thunderstorms. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Thunderstorms

来源：评论

学校读者我要写书评

暂无评论

Primordial black hole formation from massless scalar isocurvature

引用

Physical Review D 2022年第10期105卷 103538-103538页

作者： Chul-Moon Yoo Tomohiro Harada Shin’ichi Hirano Hirotada Okawa Misao Sasaki Division of Particle and Astrophysical Science Graduate School of Science Nagoya University Nagoya 464-8602 Japan Department of Physics Rikkyo University Toshima Tokyo 171-8501 Japan Waseda Institute for Advanced Study (WIAS) Waseda University Shinjuku Tokyo 169-0051 Japan Kavli Institute for the Physics and Mathematics of the Universe (WPI) University of Tokyo Kashiwa 277-8583 Japan Center for Gravitational Physics Yukawa Institute for Theoretical Physics Kyoto University Kyoto 606-8502 Japan Leung Center for Cosmology and Particle Astrophysics National Taiwan University Taipei 10617 Taiwan

We numerically study the primordial black hole (PBH) formation by an isocurvature perturbation of a massless scalar field on super Hubble scales in the radiation-dominated Universe. As a first step we perform simulations of spherically symmetric configurations. For the initial condition, we employ the spatial gradient expansion and provide the general form of the growing mode solutions valid up through the second order in this expansion. The initial scalar field profile is assumed to be Gaussian with a characteristic comoving wave number k; ∼exp(−k2R2), where R is the radial coordinate. We find that a PBH is formed for a sufficiently large amplitude of the scalar field profile. Nevertheless, we find that the late time behavior of the gravitational collapse is dominated by the dynamics of the fluid but not by the scalar field, which is analogous to the PBH formation from an adiabatic perturbation in the radiation-dominated Universe.

关键词： Classical black holes Inflation Massive compact halo objects

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：