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Profile of strong magnetic field By component in magnetotail current sheets

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Profile of strong magnetic field By component in magnetotail...

中国科学院地质与地球物理研究所2012年度（第12届）学术年会

作者： Z.J.Rong W.X.Wan C.Shen X.Li M.W.Dunlop A.A.Petrukovich L.-N.Hau T.L.Zhang H.Reme A.M.Du E.Lucek Beijing National observatory of Space Environment Institute of Geology and GeophysicsChinese Academy of Sciences State Key Laboratory of Space Weather Center for Space Science and Applied ResearchChinese Academy of Sciences Laboratory for Atmosphere and Space Physics Department of Aerospace and Engineering SciencesUniversity of Colorado at BoulderBoulderColoradoUSA. Rutherford Appleton Laboratory OxfordUK. Space Research Institute MoscowRussia. Institute of Space Science National Central UniversityJhongliTaiwan. Department of Geophysics and Planetary Sciences University of Science and Technology of ChinaHefeiChina Space Research Institute Austrian Academy of SciencesGrazAustria. IRAP University of ToulouseToulouseFrance.CNRSIRAPToulouseFrance. Blackett Laboratory Imperial College LondonLondonUK.

[1]The strong magnetic field B component(in GSM coordinates) has been increasingly noticed to play an important role in the dynamics of tail current sheet (CS).The distribution profile of strong B components in the ta...

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Long-duration exohiss wave outside the plasmasphere: observed by Van Allen Probes

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Long-duration exohiss wave outside the plasmasphere: observe...

2014年中国地球科学联合学术年会——专题29：空间天气与人类活动

作者： Hui Zhu Zhenpeng Su Fuliang Xiao Huinan Zheng Yuming Wang Zhaoguo He Chao Shen Min Zhang Shui Wang C.A.Kletzing W.S.Kurth G.B.Hospodarsky H.E.Spence G.D.Reeves H.O.Funsten J.B.Blake D.N.Baker CAS Key Laboratory of Geospace Environment Department of Geophysics and Planetary Sciences University of Science and Technology of China State Key Laboratory of Space Weather Chinese Academy of Sciences Mengcheng National Geophysical observatory School of Earth and Space Sciences University of Science and Technology of China School of Physics and Electronic Sciences Changsha University of Science and Technology Center for Space Science and Applied Research Chinese Academy of Sciences State Key Laboratory of Space Weather Center for Space Science and Applied ResearchChinese Academy of Sciences Department of Physics and Astronomy University of Iowa Institute for the Study of Earth Oceans and Space University of New Hampshire Space Science and Applications Group Los Alamos National Laboratory ISR Division Los Alamos National Laboratory The Aerospace Corporation Los Angeles California USA Laboratory for Atmospheric and Space Physics University of Colorado Boulder

We report an exohiss event in the low-density trough region observed by Van Allen Probes on 2February *** exohiss waves are discovered in the wide MLT distribution[9.1,13.4]and low magnetic latitude,with narrow-band structure and weak intensity compared with plasmaspheric *** the Continue Waveform Burst Mode data and MAG data on the EMFISIS,we analyze the normal angle,electromagnetic planarity and antiparallel-propagating Poynting flux of exohiss *** results show indicate that exohiss waves are the result of plasmaspheric hiss leakage into the trough

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青藏高原东北缘兰州盆地记录的始新世/渐新世气候转型期

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青藏高原东北缘兰州盆地记录的始新世/渐新世气候转型期

2016中国地球科学联合学术年会

作者：张鹏敖红 Andrew P.Roberts 安芷生吴福莉中国科学院地球环境研究所黄土与第四纪地质国家重点实验室 Lamont-Doherty Earth observatory Columbia University Research School of Earth Sciences The Australian National University 中国科学院青藏高原研究所大陆碰撞与高原隆升重点实验室

＜正＞始新世/渐新世（E/O）之交（约34 Ma）的全球气候变冷是新生代气候演化过程中最显著的变冷事件之一,它导致了南极大陆冰盖的出现,标志着地球从两极无冰的"温室气候"转变成了有冰的"冰室气候"。这一转变伴随着一系列重大地球环境变... 详细信息

＜正＞始新世/渐新世（E/O）之交（约34 Ma）的全球气候变冷是新生代气候演化过程中最显著的变冷事件之一,它导致了南极大陆冰盖的出现,标志着地球从两极无冰的"温室气候"转变成了有冰的"冰室气候"。这一转变伴随着一系列重大地球环境变化,例如,全球海平面大幅快速下降,全球范围显著降温,大气CO2浓度明显降低,赤道太平洋碳酸盐补偿深度大幅增加,全球生物和植被大量演替等。E/O变

关键词：气候转型期青藏高原兰州盆地始新世渐新世

Accretion in strong field gravity with eXTP

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Science China(Physics,Mechanics & Astronomy) 2019年第2期62卷 45-73页

作者： Alessandra De Rosa Phil Uttley LiJun Gou Yuan Liu Cosimo Bambi Didier Barret Tomaso Belloni Emanuele Berti Stefano Bianchi Ilaria Caiazzo Piergiorgio Casella Marco Feroci Valeria Ferrari Leonardo Gualtieri Jeremy Heyl Adam Ingram Vladimir Karas FangJun Lu Bin Luo Giorgio Matt Sara Motta Joseph Neilsen Paolo Pani Andrea Santangelo XinWen Shu JunFeng Wang Jian-Min Wang YongQuan Xue YuPeng Xu WeiMin Yuan YeFei Yuan Shuang-Nan Zhang Shu Zhang Ivan Agudo Lorenzo Amati Nils Andersson Cristina Baglio Pavel Bakala Altan Baykal Sudip Bhattacharyya Ignazio Bombaci NiccolóBucciantini Fiamma Capitanio Riccardo Ciolfi Wei K.Cui Filippo D'Ammando Thomas Dauser Melania Del Santo Barbara De Marco Tiziana Di Salvo Chris Done Michal Dovciak Andrew C.Fabian Maurizio Falanga Angelo Francesco Gambino Bruce Gendre Victoria Grinberg Alexander Heger Jeroen Homan Rosario Iaria JiaChen Jiang ChiChuan Jin Elmar Koerding Manu Linares Zhu Liu Thomas J.Maccarone Julien Malzac Antonios Manousakis Frédéric Marin Andea Marinucci Missagh Mehdipour Mariano Méndez Simone Migliari Cole Miller Giovanni Miniutti Emanuele Nardini Paul T.O'Brien Julian P.Osborne Pierre Olivier Petrucci Andrea Possenti Alessandro Riggio Jerome Rodriguez Andrea Sanna LiJing Shao Malgosia Sobolewska Eva Sramkova Abigail L.Stevens Holger Stiele Giulia Stratta Zdenek Stuchlik Jiri Svoboda Fabrizio Tamburini Thomas M.Tauris Francesco Tombesi Gabriel Torok Martin Urbanec Frederic Vincent QingWen Wu Feng Yuan Jean J.M.in't Zand Andrzej A.Zdziarski XinLin Zhou INAF-Istituto di Astrofisica e Planetologie Spaziali Via Fosso del Cavaliere Anton Pannekoek Institute for Astronomy University of Amsterdam National Astronomical Observatories Chinese Academy of Science Institute of High Energy Physics Chinese Academy of Science Center for Field Theory and Particle Physics and Department of Physics Fudan University IRAP Universitéde ToulouseCNRSUPSCNES INAF-Osservatorio Astronomico di Brera Department of Physics and Astronomy The University of MississippiUniversity Dipartimento di Matematica e Fisica Universitàdegli studi Roma Tre University of British Columbia INAF-Osservatorio Astronomico di Roma INFN-Roma 2 c/o Dipartimento di Fisica II Universit?di Roma"Tor Vergata" Dipartimento di Fisica Universitàdegli Studi di Roma"La Sapienza"&Sezione INFN Roma1 Department of Physics University of OxfordClarendon Laboratory Astronomical Institute Academy of Sciences School of Astronomy and Space Science Nanjing University MIT Kavli Institute for Astrophysics and Space Research Institut für Astronomie und Astrophysik Eberhard Karls Universität Department of Physics Anhui Normal University Department of Astronomy and Institute of Theoretical Physics and Astrophysics Xiamen University CAS Key Laboratory for Research in Galaxies and Cosmology Department of AstronomyUniversity of Science and Technology of China Instituto de Astrofísica de Andalucia(CSIC) Glorieta de la Astronomía s/n INAF-Istituto di Astrofisica Spaziale e Fisica cosmica di Bologna Mathematical Sciences and STAG Research Centre University of Southampton New York University Abu Dhabi Institute of Physics and Research Centre for Computational Physics and Data Processing Faculty of Philosophy&ScienceSilesian University in OpavaíBezru?ovo nám. Department of Physics Middle East Technical University Department of Astronomy and Astrophysics Tata Institute of Fundamental Research Dipartimento di Fisica Universit?di Pisa&INFN INAF-Osservatorio Astrofisico di Arcetri INAF-Osservatorio Astronomico di Padova INFN-TIFPA Trento Ins

In this paper we describe the potential of the enhanced X-ray Timing and Polarimetry(eXTP) mission for studies related to accretion flows in the strong field gravity regime around both stellar-mass and supermassive black-holes. eXTP has the unique capability of using advanced "spectral-timing-polarimetry" techniques to analyze the rapid variations with three orthogonal diagnostics of the flow and its geometry, yielding unprecedented insight into the inner accreting regions, the effects of strong field gravity on the material within them and the powerful outflows which are driven by the accretion process.

关键词： X-ray black holes physics accretion

1999年土耳其Izmit M_W7.6地震的持续成核过程

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国际地震动态 2011年第5期32卷 18-26页

作者： Michel Bouchon Hayrullah Karabulut Mustafa Aktar Serdar zalaybey Jean Schmittbuhl Marie-Paule Bouin 左玉玲 Centre National de la Recherche Scientifique and Université Joseph Fourier GrenobleISTerre Kandilli observatory and Earthquake Research Institute Bogazii University TBITAK Marmara Research CenterEarth and Marine Sciences Institute Centre National de la Recherche Scientifique and Université de Strasbourg Ecole et Observatoire des Sciences de la Terre Centre National de la Recherche Scientifique and Institut de Physique du Globe de Paris Observatoire Volcanologique et Sismologique de Guadeloupe 中国地震局地球物理研究所

实验室和理论研究表明,地震之前会出现一个渐进性的滑动不稳定阶段,在此期间,断层缓慢滑动,而后突然加速并最终导致动态破裂。本文中,我们报道了迄今记录最为完整的大地震之一,即1999年土耳其Izmit MW7.6地震之前出现了持续时间很久的... 详细信息

实验室和理论研究表明,地震之前会出现一个渐进性的滑动不稳定阶段,在此期间,断层缓慢滑动,而后突然加速并最终导致动态破裂。本文中,我们报道了迄今记录最为完整的大地震之一,即1999年土耳其Izmit MW7.6地震之前出现了持续时间很久的源自震源的地震信号。这种信号包含一连串的地震破裂,破裂随时间和低频地震噪声的增加而加速。这些观测结果表明,此次地震之前在脆性地壳底部出现了44min的缓慢滑动。滑动最初呈缓慢加速,然后在地震发生前2min内又突然加速。

关键词：大地震土耳其成核过程地震破裂地震信号持续时间地震噪声地震发生

The Giant Radio Array for Neutrino Detection(GRAND):Science and design

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Science China(Physics,Mechanics & Astronomy) 2020年第1期Mechanics & Astronomy) .卷 5-47页

作者： Jaime álvarez-Mu?iz Rafael Alves Batista Aswathi Balagopal V. Julien Bolmont Mauricio Bustamante Washington Carvalho Jr. Didier Charrier Isma?l Cognard Valentin Decoene Peter B.Denton Sijbrand De Jong Krijn D.De Vries Ralph Engel Ke Fang Chad Finley Stefano Gabici Quan Bu Gou Jun Hua Gu Claire Guépin Hong Bo Hu Yan Huang Kumiko Kotera Sandra Le Coz Jean-Philippe Lenain Guo Liang Léü Olivier Martineau-Huynh Miguel Mostafá Fabrice Mottez Kohta Murase Valentin Niess Foteini Oikonomou Tanguy Pierog Xiang Li Qian Bo Qin Duan Ran Nicolas Renault-Tinacci Markus Roth Frank G.Schr ?der Fabian Schüssler Cyril Tasse Charles Timmerman Matías Tueros Xiang Ping Wu Philippe Zarka Andreas Zech B.Theodore Zhang Jian Li Zhang Yi Zhang Qian Zheng Anne Zilles Departamento de Física de Partículas & Instituto Galego de Física de Altas Enerxías Universidad de Santiago de Compostela Instituto de Astronomia Geofísica e Ciências Atmosféricas Universidade de S?o Paulo Department of Physics—Astrophysics University of Oxford DWB Institute of Experimental Particle Physics (ETP) Karlsruhe Institute of Technology (KIT) Laboratoire de Physique Nucléeaire et de Hautes Energies (LPNHE) Sorbonne Université Université Paris Diderot Sorbonne Paris Cité Niels Bohr International Academy and DARK Niels Bohr Institute Discovery Center Niels Bohr Institute Center for Cosmology and Astro Particle Physics (CCAPP) & Department of Physics Ohio State University Universidade de Santiago de Compostela SUBATECH Institut Mines-Telecom Atlantique – CNRS/IN2P3 – Université de Nantes Laboratoire de Physique et Chimie de l’Environnement et de l’Espace LPC2E CNRS-Université d’Orléans Station de Radioastronomie de Nan?cay Observatoire de Paris Sorbonne Université UMR 7095 Institut d’Astrophysique de Paris Institute for Mathematics Astrophysics and Particle Physics (IMAPP) Radboud Universiteit Nationaal Instituut voor Kernfysica en Hoge Energie Fysica (NIKHEF) IIHE/ELEM Vrije Universiteit Brussel Institute for Nuclear Physics (IKP) Karlsruhe Institute of Technology (KIT) Einstein Fellow Stanford University Department of Astronomy University of Maryland Joint Space-Science Institute Oskar Klein Centre Stockholm University Department of Physics Stockholm University Astro Particule et Cosmologie (APC) Université Paris Diderot CNRS/IN2P3 CEA/Irfu Observatoire de Paris Institute of High Energy Physics Chinese Academy of Sciences National Astronomical Observatories Chinese Academy of Sciences School of Physical Science and Technology Xinjiang University Center for Particle and Gravitational Astrophysics Pennsylvania State University Department of Physics Pennsylvania State University Department of Astronomy & Astrophysics Pennsylvania State University LUTH Observatoire de Paris

The Giant Radio Array for Neutrino Detection（GRAND） is a planned large-scale observatory of ultra-high-energy（UHE） cosmic particles, with energies exceeding 10～8 Ge V. Its goal is to solve the long-standing mystery of the origin of UHE cosmic rays. To do this, GRAND will detect an unprecedented number of UHE cosmic rays and search for the undiscovered UHE neutrinos and gamma rays associated to them with unmatched sensitivity. GRAND will use large arrays of antennas to detect the radio emission coming from extensive air showers initiated by UHE particles in the atmosphere. Its design is modular: 20 separate, independent sub-arrays, each of 10000 radio antennas deployed over 10000 km2. A staged construction plan will validate key detection techniques while achieving important science goals early. Here we present the science goals, detection strategy, preliminary design, performance goals, and construction plans for GRAND.

关键词： radio telescopes neutrinos in astronomical observations cosmic rays in astronomical observations radiowave radiation: sources galactic and extragalactic cosmic rays

GRB 220408B:A Three-episode Burst from a Precessing Jet

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Research in Astronomy and Astrophysics 2023年第11期23卷 214-224页

作者： Zijian Zhang Yi-Han Iris Yin Chenyu Wang Xiangyu Ivy Wang Jun Yang Yan-Zhi Meng Zi-Ke Liu Guo-Yin Chen Xiaoping Fu Huaizhong Gao Sihao Li Yihui Liu Xiangyun Long Yong-Chang Ma Xiaofan Pan Yuanze Sun Wei Wu Zirui Yang Zhizhen Ye Xiaoyu Yu Shuheng Zhao Xutao Zheng Tao Zhou Qing-Wen Tang Qiurong Yan Rong Zhou Zhonghai Wang Hua Feng Ming Zeng Bin-Bin Zhang School of Astronomy and Space Science Nanjing UniversityNanjing 210093China School of Physics Nanjing UniversityNanjing 210093China Department of Astronomy Tsinghua UniversityBeijing 100084China Key Laboratory of Modern Astronomy and Astrophysics Nanjing UniversityMinistry of EducationNanjing 210093China School of Information Engineering Nanchang UniversityNanchang 330031China Department of Engineering Physics Tsinghua UniversityBeijing 100084China Department of Health Physics China Institute for Radiation ProtectionTaiyuan 300000China Key Laboratory of Radiation Physics and Technology of Ministry of Education College of Physics of Sichuan UniversityChengdu 610065China School of Artificial Intelligence Nanjing UniversityNanjing 210093China Key Laboratory of Particle and Radiation Imaging Tsinghua UniversityMinistry of EducationBeijing 100084China Department of Computer Science and Technology Nanjing UniversityNanjing 210093China School of Chemistry and Chemical Engineering Nanjing UniversityNanjing 210093China College of Engineering and Applied Sciences Nanjing UniversityNanjing 210093China Department of Physics School of Physics and Materials ScienceNanchang UniversityNanchang 330031China Purple Mountain observatory Chinese Academy of SciencesNanjing 210023China

Jet precession has previously been proposed to explain the apparently repeating features in the light curves of a few gamma-ray bursts(GRBs).In this paper,we further apply the precession model to a bright GRB 220408B by examining both its temporal and spectral consistency with the predictions of the *** one of the recently confirmed GRBs observed by our GRID CubeSat mission,GRB 220408B is noteworthy as it exhibits three apparently similar emission ***,the similarities are reinforced by their strong temporal correlations and similar features in terms of spectral evolution and spectral *** analysis demonstrates that these features can be well explained by the modulated emission of a Fast-Rise-Exponential-Decay(FRED)shape light curve intrinsically produced by a precessing jet with a precession period of 18.4_(-0.2)~(+0.2)s,a nutation period of11.1_(-0.2)~(+0.2)s and viewed *** study provides a straightforward explanation for the complex yet similar multiepisode GRB light curves.

关键词： gamma-rays:general (stars:)gamma-ray burst:individual(GRB 220408B) stars:jets

Effect of Matching Algorithm and Profile Shape on Pulsar Pulse Time of Arrival Uncertainties

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Research in Astronomy and Astrophysics 2023年第12期23卷 230-241页

作者： J.Wang J.P.W.Verbiest G.M.Shaifullah J.P.Yuan Ruhr-Universität Bochum Fakultät für Physik und AstronomieAstronomisches Institut(AIRUB)D-44801 BochumGermany Advanced Institute of Natural Sciences Beijing Normal UniversityZhuhai 519087China Fakulatät für Physik Universität BielefeldPostfach 100131D-33501 BielefeldGermany Max-Planck-Institut für Radioastronomie Auf dem Hügel 69D-53121 BonnGermany Florida Space Institute University of Central Florida12354 Research ParkwayOrlandoFL 32826USA Dipartimento di Fisica"G.Occhialini "Universitádegli Studi di Milano-BicoccaPiazza della Scienza 3I-20126 MilanoItaly INFN Sezione di Milano-BicoccaPiazza della Scienza 3I-20126 MilanoItaly Xinjiang Astronomical observatory Chinese Academy of SciencesUrumqi 830011China Key Laboratory of Radio Astronomy Chinese Academy of SciencesNanjing 210008China INAF-Osservatorio Astronomico di Cagliari via della Scienza 509047 Selargius(CA)Italy

For high-precision pulsar timing analysis and low-frequency gravitational wave detection,it is essential to accurately determine pulsar pulse times of arrival(ToAs)and associated *** measure the ToAs and their uncertainties,various cross-correlation-based techniques can be *** develop methodologies to investigate the impact of the template-matching method,profile shape,signal-to-noise ratio of both template and observation on ToA *** methodologies are then applied to data from the International Pulsar Timing *** demonstrate that the Fourier domain Markov chain Monte Carlo method is generally superior to other methods,while the Gaussian interpolation shift method outperforms other methods in certain cases,such as profiles with large duty cycles or smooth profiles without sharp ***,it is important to note that our study focuses solely on ToA uncertainty,and the optimal method for determining both ToA and ToA uncertainty may differ.

关键词： methods data analysis-(stars:)pulsars general-methods statistical

基于非相干散射雷达和GPS观测研究Millstone Hill地区等离子体层电子含量

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基于非相干散射雷达和GPS观测研究Millstone Hill地区等离子体层...

中国科学院地质与地球物理研究所2013年度（第13届）学术年会

作者：种小燕张满莲张顺荣温晋刘立波宁百齐万卫星中国科学院地质与地球物理研究所电离层空间环境重点实验室中国科学院地质与地球物理研究所北京空间环境国家野外科学观测研究站中国科学院大学 IIaystack observatory Massachusetts Institute of TechnologyWestfordMassachusettsUSA

本文尝试结合非相干散射雷达和GPS TEC观测数据提取等离子体层总电子含量(PTEC).我们首先描述所用的技术方法,然后具体利用了Millstone Hill台站的观测数据研究该地区上空等离子体层总电子含量(PTEC)的变化情况.我们采用变化标高的Chap... 详细信息

本文尝试结合非相干散射雷达和GPS TEC观测数据提取等离子体层总电子含量(PTEC).我们首先描述所用的技术方法,然后具体利用了Millstone Hill台站的观测数据研究该地区上空等离子体层总电子含量(PTEC)的变化情况.我们采用变化标高的Chapman函数对非相干散射雷达测得的电子浓度剖面数据进行拟合,然后通过对剖面积分得到100 km到1000 km高度范围的电离层总电子含量.GPS提供的TEC数据为高度达20200 km的总电子含量,两者之差可近似看成等离子体层的电子含量.本文分别选取太阳活动高年(2000,2002年)和太阳活动低年(2005,2008年)Millstone Hill台站的静日数据进行研究.结果表明,等离子体层电子含量及其所占GPSTEC的比例具有明显的周日变化.PTEC含量在白天高于夜间,而所占GPS TEC的百分比,夜间明显高于白天.太阳活动高年所选月份等离子体层电子含量在4～14 TECU(1TECU=10el/m)范围内变化,夜间所占比例可达60%左右.太阳活动低年所选月份等离子体层电子含量在3～7 TECU范围内变化,所占比例夜间最高可达80%左右.我们所得到的结果与前人基于其它观测手段所得结果在变化趋势上一致,在量级上也大致相当.因此,这从一个侧面证明了我们所用方法的可靠性.非相干散射雷达能够探测包括F2层峰值以下及以上高度的电子浓度,利用这一设备所观测得到的资料来推算电离层电子含量将比前人基于电离层垂测仪观测资料进行的推算更具真实性,由此得到的等离子体层电子含量也将更为接近真实情况.

关键词： TEC 等离子体层非相干散射雷达 GPS TEC 电离层