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arXiv 2025年

作者： Ma, Lingquan Hua, Jun Schäfer, Andreas Shu, Hai-Tao Su, Yushan Sun, Peng Walter, Lisa Wang, Wei Xiong, Xiaonu Yang, Yi-Bo Zhang, Jian-Hui Zhang, Qi-An Center of Advanced Quantum Studies Department of Physics Beijing Normal University Beijing100875 China School of Science and Engineering The Chinese University of Hong Kong Shenzhen518172 China Guangdong Basic Research Center of Excellence for Structure and Fundamental Interactions of Matter Institute of Quantum Matter South China Normal University Guangzhou510006 China Guangdong-Hong Kong Joint Laboratory of Quantum Matter Guangdong Provincial Key Laboratory of Nuclear Science Southern Nuclear Science Computing Center South China Normal University Guangzhou510006 China Institut für Theoretische Physik Universität Regensburg RegensburgD-93040 Germany Institute of Particle Physics Central China Normal University Wuhan430079 China Department of Physics University of Maryland College ParkMD20742 United States Institute of Modern Physics Chinese Academy of Sciences Gansu Province Lanzhou730000 China Shanghai Key Laboratory for Particle Physics and Cosmology School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Institute of Modern Physics Chinese Academy of Sciences Guangdong Province Huizhou516000 China School of Physics Central South University Changsha418003 China CAS Key Laboratory of Theoretical Physics Institute of Theoretical Physics Chinese Academy of Sciences Beijing100190 China School of Fundamental Physics and Mathematical Sciences Hangzhou Institute for Advanced Study UCAS Hangzhou310024 China International Centre for Theoretical Physics Asia-Pacific Hangzhou Beijing China University of Chinese Academy of Sciences School of Physical Sciences Beijing100049 China School of Physics Beihang University Beijing102206 China

We present the first lattice QCD calculation of the quark transverse spin-momentum correlation, i.e., the naive time-reversal-odd Boer-Mulders function, of the nucleon, using large-momentum effective theory (LaMET). The calculation is carried out on an ensemble with lattice spacing a = 0.098 fm and pion mass 338 MeV, at various proton momenta up to 2.11 GeV. We have implemented perturbative matching up to the next-to-next-to-leading order together with a renormalization-group resummation improvement. The result exhibits a decay behavior with increasing transverse separation b̝. We also compare the results in the nucleon and pion. Copyright © 2025, The Authors. All rights reserved.

关键词： Momentum

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Search for Double Beta Decay of 136Xe to the 0+1 Excited State of 136Ba with PandaX-4T

arXiv

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arXiv 2025年

作者： Luo, Lingyin Bo, Zihao Chen, Wei Chen, Xun Chen, Yunhua Cheng, Zhaokan Cui, Xiangyi Fan, Yingjie Fang, Deqing Gao, Zhixing Geng, Lisheng Giboni, Karl Guo, Xunan Guo, Xuyuan Guo, Zichao Han, Chencheng Han, Ke He, Changda He, Jinrong Huang, Di Huang, Houqi Huang, Junting Hou, Ruquan Hou, Yu Ji, Xiangdong Ji, Xiangpan Ju, Yonglin Li, Chenxiang Li, Tao Li, Jiafu Li, Mingchuan Li, Shuaijie Li, Zhiyuan Lin, Qing Liu, Jianglai Lu, Congcong Lu, Xiaoying Luo, Yunyang Ma, Wenbo Ma, Yugang Mao, Yajun Meng, Yue Ning, Xuyang Pang, Binyu Qi, Ningchun Qian, Zhicheng Ren, Xiangxiang Shan, Dong Shang, Xiaofeng Shao, Xiyuan Shen, Guofang Shen, Manbin Sun, Wenliang Tao, Yi Wang, Anqing Wang, Guanbo Wang, Hao Wang, Jiamin Wang, Lei Wang, Meng Wang, Qiuhong Wang, Shaobo Wang, Siguang Wang, Wei Wang, Xiuli Wang, Xu Wang, Zhou Wei, Yuehuan Wu, Weihao Wu, Yuan Xiao, Mengjiao Xiao, Xiang Xiong, Kaizhi Xu, Yifan Yao, Shunyu Yan, Binbin Yan, Xiyu Yang, Yong Ye, Peihua Yu, Chunxu Yuan, Ying Yuan, Zhe Yun, Youhui Zeng, Xinning Zhang, Minzhen Zhang, Peng Zhang, Shibo Zhang, Shu Zhang, Tao Zhang, Wei Zhang, Yang Zhang, Yingxin Zhang, Yuanyuan Zhao, Li Zhou, Jifang Zhou, Jiaxu Zhou, Ning Zhou, Xiaopeng Zhou, Yubo Zhou, Zhizhen New Cornerstone Science Laboratory Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai201210 China State Key Laboratory of Nuclear Physics and Technology School of Physics Peking University Beijing100871 China Shanghai Key Laboratory for Particle Physics and Cosmology Shanghai200240 China Jinping Deep Underground Frontier Science and Dark Matter Key Laboratory of Sichuan Province China Yalong River Hydropower Development Company Ltd. 288 Shuanglin Road Chengdu610051 China Sino-French Institute of Nuclear Engineering and Technology Sun Yat-Sen University Zhuhai519082 China Department of Physics Yantai University Yantai264005 China Institute of Modern Physics Fudan University Shanghai200433 China School of Physics Beihang University Beijing102206 China Peng Huanwu Collaborative Center for Research and Education Beihang University Beijing100191 China International Research Center for Nuclei and Particles in the Cosmos Beijing Key Laboratory of Advanced Nuclear Materials and Physics Beihang University Beijing100191 China Institute of Modern Physics Chinese Academy of Sciences Huizhou516000 China SJTU Paris Elite Institute of Technology Shanghai Jiao Tong University Shanghai200240 China Shanghai Jiao Tong University Sichuan Research Institute Chengdu610213 China School of Mechanical Engineering Shanghai Jiao Tong University Shanghai200240 China Department of Physics University of Maryland College ParkMD20742 United States School of Physics Nankai University Tianjin300071 China School of Physics Sun Yat-Sen University Guangzhou510275 China State Key Laboratory of Particle Detection and Electronics University of Science and Technology of China Hefei230026 China Department of Modern Physics University of Science and Technology of China Hefei230026 China Research Center for Particle Science and Technology Institute of Frontier and Interdisciplinary Science Shandong University Shandong Qingdao266237 China Key Laboratory o

We perform a search of double beta decay of 136Xe to the excited state, 0+1 , of 136Ba (2νββ-0+1 ), using the dual-phase xenon detector of PandaX-4T with the first 94.9-day commissioning data. The multi-site events are reconstructed up to the MeV energy scale, which helps to improve the background model significantly. The background contribution from the stainless steel platform outside PandaX-4T cryostat is evaluated for the first time. No significant evidence for 2νββ-0+1 is observed, resulting in a lower limit on half-life of 7.5×1022 yr at the 90% confidence level. This is the first experimental limit on such a rare decay in a natural xenon-based detector. © 2025, CC BY.

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Impact of the reionization history on constraining primordial gravitational waves in future all-sky cosmic microwave background experiments

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Physical Review D 2025年第8期111卷 083555-083555页

作者： Hanchun Jiang Toshiya Namikawa Department of Physics Graduate School of Science The University of Tokyo Tokyo 113- 0033 Japan Department of Applied Mathematics and Theoretical Physics University of Cambridge Wilberforce Road Cambridge CB3 0WA United Kingdom Center for Data-Driven Discovery Kavli IPMU (WPI) UTIAS The University of Tokyo Kashiwa 277-8583 Japan Kavli Institute for Cosmology Cambridge Madingley Road Cambridge CB3 0HA United Kingdom

We explore the impact of the reionization history on examining the shape of the power spectrum of the primordial gravitational waves (PGWs) with the cosmic microwave background (CMB) polarization. The large-scale CMB generated from the reionization epoch is important in probing the PGWs from all-sky experiments, such as LiteBIRD. The reionization model has been constrained by several astrophysical observations. However, its uncertainty could impact constraining models of the PGWs if we use large-scale CMB polarization. Here, by expanding the analysis of Mortonson and Hu (2007), we estimate how reionization uncertainty impacts constraints on a generic primordial tensor power spectrum. We assume that CMB polarization is measured by a LiteBIRD-like experiment and the tanh model is adopted for a theoretical template when we fit data. We show that constraints are almost unchanged even if the true reionization history is described by an exponential model, where all parameters are within 68% confidence level (CL). We also show an example of the reionization history that the constraints on the PGWs are biased more than 68% CL. Even in that case, using E-mode power spectrum on large scales would exclude such a scenario and make the PGW constraints robust against the reionization uncertainties.

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Gravitational Wave Decoupling in Retrograde Circumbinary Disks

arXiv

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arXiv 2025年

作者： O’Neill, David Tiede, Christopher D’Orazio, Daniel J. Haiman, Zoltán MacFadyen, Andrew Niels Bohr International Academy Niels Bohr Institute Blegdamsvej 17 Copenhagen ØDK-2100 Denmark Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21 United States Department of Astronomy Columbia University 550 West 120th Street New YorkNY10027 United States Department of Physics Columbia University 550 West 120th Street New YorkNY10027 United States Am Campus 1 Klosterneuburg3400 Austria Center for Cosmology and Particle Physics Physics Department New York University New YorkNY10003 United States

We present a study of the late-time interaction between supermassive black hole binaries and retrograde circumbinary disks during the period of gravitational wave-driven inspiral. While mergers in prograde disks have received extensive study, retrograde disks offer distinct dynamics that could promote mergers and produce unique observational signatures. Through numerical simulations, we explore the process of binary-disk decoupling, where the binary’s orbital decay rate is faster than the disk’s viscous response rate. We find the point of decoupling to be comparable in prograde and retrograde disks, suggesting that any associated electromagnetic (EM) signatures will be produced at comparable times preceding merger. However, we find smaller central cavities for retrograde disks, likely leading to higher-frequency EM emissions and shorter post-merger rebrightening timescales compared to their prograde counterparts. Additionally, we identify quasi-periodic flaring due to instabilities unique to low-viscosity retrograde disks, which may produce distinctive EM signatures. © 2025, CC BY.

关键词： Gravitational effects

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Spectro-polarimetry of GRB 180427A: evidence for distinct emission sites with varying polarisation

arXiv

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arXiv 2025年

作者： Sonawane, Rushikesh Iyyani, Shabnam Gupta, Soumya Chattopadhyay, Tanmoy Bhattacharya, Dipankar Bhalerao, Varun B. Vadawale, Santosh V. Dewangan, G.C. Centre for High Performance Computing Indian Institute of Science Education and Research Thiruvananthapuram Thiruvananthapuram695551 India School of Physics Indian Institute of Science Education and Research Thiruvananthapuram Thiruvananthapuram695551 India Homi Bhabha National Institute Anushakti Nagar Maharashtra Mumbai400094 India Kavli Institute of Particle Astrophysics and Cosmology Stanford University 452 Lomita Mall StanfordCA94305 United States Department of Physics Ashoka University Haryana Sonepat131029 India Indian Institute of Technology Bombay Mumbai India Physical Research Laboratory Gujarat Ahmedabad380009 India Inter-University Center for Astronomy and Astrophysics Maharashtra Pune411007 India

The dynamics of the origin of gamma-ray emissions in gamma-ray bursts (GRBs) remains an enigma. Through a joint analysis of GRB 180427A, observed by the Fermi Gamma-ray Space Telescope and AstroSat’s Cadmium Zinc Telluride Imager, we identify emissions from two distinct regions with varying polarisation properties. Time-resolved polarisation analysis reveals a synchronous evolution of the polarisation angle (PA) and fraction (PF) with two emission pulses, peaking with a delay of 4.82 ± 0.12 s. Spectral analysis indicates that the first pulse is dominated by blackbody radiation, while the second pulse exhibits a non-thermal spectrum (power law with an exponential cutoff). Using a bottom-to-top approach through simulations, we decouple the polarisation properties of the individual spectral components, revealing polarisation fractions of 25% - 40% for the blackbody spectrum and 30% - 60% for the non-thermal spectrum. At a redshift of z ∼ 0.05, the blackbody emission originates from the jet photosphere at 1011 cm, whereas the non-thermal emission arises from an optically thin region at 1015 cm. The changing dominance of these emissions explains the observed PA shift of 60◦ ±22.3◦. The spectral cutoff at 1 MeV suggests pair opacity due to the jet’s low bulk Lorentz factor (Γ ∼ tens). The high polarisation and hard spectral slopes (α > −0.5) imply a top-hat jet structure observed off-axis, near the jet’s edge. This off-axis viewing introduces anisotropy in the radiation within the viewing cone (1/Γ), accounting for the observed polarisation. © 2025, CC BY.

关键词： Gamma rays

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data quality control system and long-term performance monitor of LHAASO-KM2A

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Astroparticle physics 2025年 164卷

作者： Cao, Zhen Aharonian, F. Axikegu Bai, Y.X. Bao, Y.W. Bastieri, D. Bi, X.J. Bi, Y.J. Bian, W. Bukevich, A.V. Cao, Q. Cao, W.Y. Cao, Zhe Chang, J. Chang, J.F. Chen, A.M. Chen, E.S. Chen, H.X. Chen, Liang Chen, Lin Chen, Long Chen, M.J. Chen, M.L. Chen, Q.H. Chen, S. 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 Dong, X.Q. Duan, K.K. Fan, J.H. Fan, Y.Z. Fang, J. Fang, J.H. Fang, K. Feng, C.F. Feng, H. Feng, L. Feng, S.H. Feng, X.T. Feng, Y. Feng, Y.L. Gabici, S. Gao, B. Gao, C.D. 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. Hasan, M. He, H.H. He, H.N. He, J.Y. He, Y. 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. Ji, X.L. Jia, H.Y. Jia, K. Jiang, K. Jiang, X.W. Jiang, Z.J. Jin, M. Kang, M.M. Karpikov, I. Kuleshov, D. Kurinov, K. Li, B.B. Li, C.M. Li, Cheng Li, Cong Li, D. Li, F. Li, H.B. Li, H.C. Li, Jian Li, Jie Li, K. Li, S.D. 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, D.B. Liu, H. Liu, H.D. Liu, J. Liu, J.L. Liu, M.Y. Liu, R.Y. Liu, S.M. Liu, W. Liu, Y. Liu, Y.N. Luo, Q. Luo, Y. 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, L.J. Pattarakijwanich, P. Pei, Z.Y. Qi, J.C. Qi, M.Y. Qiao, B.Q. Qin, J.J. Raza, A. Ruffolo, D. Sáiz, A. Saeed, M. Semikoz, D. Shao, L. Shchegolev, O. Sheng, X.D. Shu, F.W. Song, H.C. Stenkin, Yu.V. Stepanov, V. Su, Y. Sun, D.X. Sun, Q.N. Sun, X.N. Sun, Z.B. Key Laboratory of Particle Astrophysics & 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 2 Dublin Ireland Max–Planck-Institut for Nuclear Physics P.O. Box 103980 Heidelberg69029 Germany 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 Tsung-Dao Lee Institute & School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Institute for Nuclear Research of Russian Academy of Sciences Moscow117312 Russia Hebei Normal University Hebei Shijiazhuang050024 China University of Science and Technology of China Anhui Hefei230026 China State Key Laboratory of Particle Detection and Electronics China Key Laboratory of Dark Matter and Space Astronomy & Key Laboratory of Radio Astronomy Purple Mountain Observatory Chinese Academy of Sciences Jiangsu Nanjing210023 China Research Center for Astronomical Computing Zhejiang Laboratory Zhejiang Hangzhou311121 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China School of Physics and Astronomy Yunnan University Yunnan Kunming650091 China Ministry of Education Tibet Lhasa850000 China Key Laboratory of Radio Astronomy and Technology National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Sun Yat-sen University Guangdong Zhuhai519000 China Sun Yat-sen University Guangdong Guangzhou510275 China Sun Yat-sen University Guangdong Zhuhai519000 Chi

The KM2A is the largest sub-array of the Large High Altitude Air Shower Observatory (LHAASO). It consists of 5216 electromagnetic particle detectors (EDs) and 1188 muon detectors (MDs). The data recorded by the EDs and MDs are used to reconstruct primary information of cosmic-ray and gamma-ray showers. To ensure the reliability of the LHAASO-KM2A data, a three-level quality control system has been established. It is used to monitor the status of detector units, stability of reconstructed parameters and the performance of the array based on observations of the Crab Nebula and Moon shadow. This paper will introduce the control system and its application on the LHAASO-KM2A data collected from August 2021 to July 2023. During this period, the pointing and angular resolution of the array were stable. From the observations of the Moon shadow and Crab Nebula, the results achieved using the two methods are consistent with each other. For example, according to the observation of the Crab Nebula with KM2A at energies from 25 TeV to 100 TeV, the time averaged pointing errors are estimated to be −0.003°±0.005° and 0.001°±0.006° in the R.A. and Dec directions, respectively. © 2024 Elsevier B.V.

关键词： cosmology

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Constraints on ultracompact minihalos using neutrino signals from gravitino dark matter decay

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Research in Astronomy and Astrophysics 2014年第10期14卷 1215-1220页

作者： Yun-Long Zheng Yu-Peng Yang Ming-Zhe Li Hong-Shi Zong Department of Physics Nanjing University Department of Astronomy Nanjing University College of Physics and Electrical Engineering Anyang Normal University Joint Center for Particle Nuclear Physics and CosmologyNanjing University-Purple Mountain Observatory Interdisciplinary Center for Theoretical Study University of Science and Technology of China

Ultracompact dark matter minihalos （UCMHs） would be formed during the early universe if there were large density perturbations. If dark matter can decay into particles described by the standard model, such as neutrinos, these objects would become potential astrophysical sources of emission which could be detected by in- struments such as IceCube. In this paper, we investigate neutrino signals from nearby UCMHs due to gravitino dark matter decay and compare these signals with the back- ground neutrino flux which is mainly from the atmosphere to obtain constraints on the abundance of UCMHs.

关键词： dark matter -- early universe -- dark matter halos

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Ultrasonic positioning system for the calibration of central detector

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Nuclear science and Techniques 2019年第1期30卷 27-33页

作者： Guo-Lei Zhu Jiang-Lai Liu Qi Wang Meng-Jiao Xiao Tao Zhang School of Marine Science and Technology Northwestern Polytechnical University Shanghai Laboratory for Particle Physics and Cosmology INPAC and School of Physics and Astronomy Shanghai Jiao Tong University Department of Physics University of Maryland Center of High Energy Physics Peking University

A thorough detector response calibration using radioactive sources is necessary for the Jiangmen Underground Neutrino Observatory. Herein, we discuss the design of a source positioning system based on ultrasonic technology, aiming for a 3-cm precision over the entire35-m diameter detector sphere. A prototype system is constructed and demonstrated for the experiment.

关键词： JUNO Calibration Ultrasonic positioning

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Chiral phase diagram of strongly interacting matter at finite volume

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science China(physics,Mechanics & Astronomy) 2018年第8期61卷 93-96页

作者： Chao Shi YongHui Xia WenBao Jia HongShi Zong Department of Physics Nanjing University College of Materials Science and Engineering Nanjing University of Aeronautics and Astronautics Key Laboratory of Theoretical Physics Institute of Theoretical Physics Chinese Academy Sciences Joint Center for Particle Nuclear Physics and Cosmology

At extremely high temperature T～200 Me V and low chemical potentialμ,the quarks and gluons get released from the nucleon and form the quark-gluon plasma(QGP)state,which is accessible in the heavy ion collisions(HIC)globally[1,2].Theoretically,ab initio lattice QCD simulation found the transition from hadrons to QGP at lowμis continuous crossover instead of phase *** this connection,RHIC is running the beam energy scan program to look into the territory with higherμ[3].One important goal is to determine if there is the first order phase transition as expected by many model studies and locate the critical end point(CEP)if it exists.

关键词：有限体积物质交往 initio 阶段转变重离子碰撞 RHIC 扫描程序

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Theoretical Study on N=126 Shell Evolution

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Communications in Theoretical physics 2009年第8期52卷 323-328页

作者： SHENG Zong-Qiang REN Zhong-Zhou Department of Physics Nanjing University Nanjing 210093 China Center of Theoretical Nuclear Physics National Laboratory of Heavy-Ion Accelerator at Lanzhou Lanzhou 730000 China Joint Center for Particle Nuclear Physics and Cosmology Nanjing 210093 China School of Science Anhui University of Science and Technology Huainan 232001 China

The nuclei around magic number N=126 are investigated in the deformed relativistic mean field (RMF)model with effective interactions *** focus investigations on the N=126 isotonic *** N=126 shellevolution is studied by analyzing the variations of two-neutron (proton) separation energies,quadruple deformations,single particle levels *** good agreement of two-neutron separation energies between experimental data and calculatedvalues is *** RMF theory predicts that the sizes of N=126 shell become smaller and smaller withthe increasing of proton number ***,the N=126 shell exists in our calculated region all *** tothe calculated two-proton separation energies,the RMF theory suggests ^(220)Pu is a two-proton drip-line nucleus in theN=126 isotonic chain.

关键词： shell evolution magic number N = 126 relativistic mean field theory

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