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Einstein Probe discovery of EP2.0408a:A peculiar X-ray transient with an intermediate timescale

Science china(Physics,Mechanics & Astronomy) 2024年

作者： Wenda Zhang weimin Yuan Zhixing Ling Yong Chen Nanda Rea Arne Rau Zhiming Cai Huaqing Cheng Francesco Coti Zelati Lixin Dai Jingwei Hu Shumei {2. Chichuan Jin Dongyue Li Paul O’Brien Rongfeng Shen Xinwen Shu Shengli Sun Xiaojin Sun Xiaofeng Wang Lei Yang Bing Zhang Chen Zhang Shuang-Nan Zhang Yonghe Zhang Jie An David Buckley Alexis Coleiro Bertrand Cordier Liming Dou Rob Eyles-Ferris Zhou Fan Hua Feng Shaoyu Fu Johan P. U. Fynbo Lluis Galbany Saurabh W. Jha Shuaiqing {2.ng Albert Kong Erik Kuulkers weihua Lei Wenxiong Li Bifang Liu Mingjun Liu Xing Liu Yuan Liu Zhu Liu Chandreyee Maitra Alessio Marino Itumeleng Monageng Kirpal Nandra Jeremy Sanders Roberto Soria Lian Tao Junfeng Wang Song Wang Tinggui Wang Zhongxiang Wang Qingwen Wu Xuefeng Wu Dong Xu Yanjun Xu Sui{2.n Xue Yongquan Xue Zi{2.n Zhang Zipei Zhu Hu Zou Congying Bao Fansheng Chen Houlei Chen Tianxiang Chen wei Chen Yehai Chen Yifan Chen Chenzhou Cui weiwei Cui Yanfeng Dai Dongwei Fan Ju Guan Dawei Han Dongjie Hou Haibo Hu Maohai Huang {2. Huo Zhenqing {2. Bowen {2.ng Ge Jin Chengkui Li Junfei Li Longhui Li Maoshun Li wei Li Zhengda Li Tianying Lian Congzhan Liu Heyang Liu Huaqiu Liu Fangjun Lu Laidan Luo {2. Ma Xuan Mao Haiwu Pan Xin Pan Liming Song Hui Sun Yunyin Tan Qingjun Tang Yihan Tao Hao Wang Juan Wang Lei Wang Wenxin Wang Yilong Wang Yusa Wang Qinyu Wu Haitao Xu Jingjing Xu Xinpeng Xu Yunfei Xu Zhao Xu Changbin Xue Yulong Xue Ailiang Yan Haonan Yang Xiongtao Yang Yanji Yang Juan Zhang Mo Zhang Wenjie Zhang Zhen Zhang Zhen Zhang Ziliang Zhang Donghua Zhao Haisheng Zhao Xiaofan Zhao Zi{2.n Zhao Hongyan Zhou Yilin Zhou Yuxuan Zhu Zhencai Zhu Institut d’Estudis Espacials de Catalunya (IEEC) Max Planck Institute for Extraterrestrial Physics Innovation academy for Microsatellites chinese academy of sciences Department of Physics University of Hong Kong School of Physics and Astronomy University of Leicester School of Physics and Astronomy Sun Yat-sen University national astronomical {2. Department of Physics Anhui Normal University Shanghai Institute of Technical Physics chinese academy of sciences Physics Department Tsinghua University Nevada Center for Astrophysics University of Nevada Las Vegas Department of Physics and Astronomy University of Nevada Las Vegas chinese academy of sciences South African astronomical observatory Department of Astronomy University of Cape Town Department of Physics University of the Free State Universite' Paris Cite' CNRS Astroparticule et Cosmologie Universite' Paris Cite' CEA Paris-Saclay School of Astronomy and Space sciences IRFU/DAp-AIM Department of Astronomy Guangzhou University Cosmic Dawn Center (DAWN) Niels Bohr Institute University of Copenhagen Department of Physics and Astronomy Rutgers the State University of New Jersey Institute for Cosmic Ray Research University of chinese academy of sciences The University of Tokyo ESA/ESTEC Noordwijk 2.01 AZ The Netherlands Department of Astronomy School of Physics Huazhong University of Science and Technology INAF-Osservatorio Astrofisico di Torino Sydney Institute for Astronomy School of Physics Key Laboratory of Particle Astrophysics The University of Sydney Department of Astronomy Xiamen University Institute for Frontiers in Astronomy and Astrophysics Beijing Normal University Department of Astronomy University of Science and Technology Hefei School of Astronomy and Space sciences University of Science and Technology of china Institute of High Energy Physics Institute of Deep Space sciences Deep Space Exploration Laboratory Department of Astronomy School of Physics and Astronomy Yunnan University Shanghai astronomical observatory chinese academy of Science

We report the discovery of a peculiar X-ray transient,EP2.0408a,by Einstein Probe （EP） and follow-up studies made with EP,Swift,NICER,GROND,ATCA and other ground-based multiwavelength *** new transient was first detected with Wide-field X-ray Telescope （WXT） on board EP on April 8th,2.2.,manifested in an intense yet brief X-ray flare lasting for *** flare reached a peak flux of 3.9×10-9erg cm-2.-1in 0.5-4 keV,300 times brighter than the underlying X-ray emission detected throughout the *** and more precise follow-up observations by EP/FXT,Swift and NICER confirmed the finding of this new *** X-ray spectrum is non-thermal in 0.5-10 keV,with a power-law photon index varying *** X-ray light curve shows a plateau lasting for4d,followed by a steep decay till becoming undetectable10 d after the initial *** on its temporal property and constraints from previous EP observations,an unusual timescale in the range of 7-2. d is found for EP2.0408a,which is intermediate between the commonly found fast and long-term *** counterparts have been found in optical and near-infrared,with the earliest observation at 17 h after the initial X-ray detection,suggestive of intrinsically weak emission in these *** demonstrate that the remarkable properties of EP2.0408a are inconsistent with any of the transient types known so far,by comparison with,in particular,jetted tidal disruption events,gamma-ray bursts,X-ray binaries and fast blue optical *** nature of EP2.0408a thus remains an *** suggest that EP2.0408a may represent a new type of transients with intermediate timescales of the order of10 *** detection and follow-ups of more of such objects are essential for revealing their origin.

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Predicting the start and maximum amplitude of solar cycle 2. using similar phases and a cycle grouping

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chinese Journal of Astronomy and Astrophysics 2009年第2期9卷 133-136页

作者： jia-Long Wang wei-Guo Zong Gui-Ming Le Hai-Juan Zhao Yun-Qiu Tang Yang Zhang national astronomical {2. Chinese Academy of Sciences Beijing 100012 China national Center for Space Weather China Meteorological Administration Beijing 100081 China

We find that the solar cycles 9, 11, and 2. are similar to cycle 2. in their respective descending phases. Using this similarity and the observed data of smoothed monthly mean sunspot numbers （SMSNs） available for the descending phase of cycle 2., we make a date calibration for the average time sequence made of the three descending phases of the three cycles, and predict the start of March or April 2.08 for cycle 2.. For the three cycles, we also find a linear correlation of the length of the descending phase of a cycle with the difference between the maximum epoch of this cycle and that of its next cycle. Using this relationship along with the known relationship between the rise-time and the maximum amplitude of a slowly rising solar cycle, we predict the maximum SMSN of cycle 2. of 100.2.7.5 to appear during the period from May to October 2.12.

关键词： Sun cycle- Sun activity

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Binary Star Fractions from the LAMOST DR4

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Research in Astronomy and Astrophysics 2018年第5期18卷 47-58页

作者： Zhi-jia Tian Xiao-wei Liu Hai-Bo Yuan Bing-Qiu Chen Mao-Sheng Xiang Yang Huang Chun Wang Hua-wei Zhang Jin-Cheng Guo Juan-Juan Ren Zhi-Ying Huo Yong Yang Meng Zhang Shao-lan Bi Wu-Ming Yang Kang Liu Xian-Fei Zhang Tan-Da Li Ya-Qian Wu Jing-Hua Zhang Department of Astronomy Peking University Beijing 100871 China Department of Astronomy Beijing Normal University Beijing 100875 China national astronomical {2. Chinese Academy of Sciences Beijing 100101 China Department of Astronomy Yunnan University Kunming 650091 China

Stellar systems composed of single, double, triple or higher-order systems are rightfully regarded as the fundamental building blocks of the Milky Way. Binary stars play an important role in formation and evolution of the Galaxy. Through comparing the radial velocity variations from multiepoch observations, we analyze the binary fraction of dwarf stars observed with LAMOST. Effects of different model assumptions, such as orbital period distributions on the estimate of binary fractions,are investigated. The results based on log-normal distribution of orbital periods reproduce the previous complete analyses better than the power-law distribution. We find that the binary fraction increases with Teff and decreases with [Fe/H]. We first investigate the relation between α-elements and binary fraction in such a large sample as provided by LAMOST. The old stars with high [α/Fe] dominate with a higher binary fraction than young stars with low [α/Fe]. At the same mass, earlier forming stars possess a higher binary fraction than newly forming ones, which may be related with evolution of the Galaxy.

关键词： binaries general- binaries spectroscopic - Galaxy stellar content - stars statistics- surveys

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How can FAST improve study of the pulsar emission mechanism and magnetospheric dynamics?

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Research in Astronomy and Astrophysics 2019年第2期19卷 55-64页

作者： Hong-Guang Wang Guo-Jun Qiao Yuan-Jie Du Ji-Guang Lu Ren-Xin Xu Ke-jia Lee Xiong-wei Liu School of Physics and Electronic Engineering Guangzhou University Department of Astronomy Peking University Qian Xuesen Laboratory of Space Technology China Academy of Space Technology national astronomical {2. Chinese Academy of Sciences School of Physics and Electronic Information China West Normal University

The Five-hundred-meter Aperture Spherical radio Telescope(FAST) has the potential to discover many new pulsars and new phenomena. In this paper we mainly concentrate on how FAST can impact study of the pulsar emission mechanism and magnetospheric dynamics. Several observational programs heading to this direction are reviewed. To make full use of the superior performance of FAST and maximize the scientific outcome, these programs can be arranged in different phases of FAST according to their demands for observational conditions. We suggest that programs can be performed following the test phase, which are observations of multifrequency mean pulse profiles, anomalous X-ray pulsars(AXPs)/soft gamma-ray repeaters(SGRs), mode changing, drifting subpulse and nulling. The long-term monitoring can be carried out for mode changing, AXPs/SGRs and precessional pulsars. Others programs, including polarization observations of radio and γ-ray pulsars, searching for weak pulse components, and multifrequency observations of subpulse drifting, microstructure and giant pulses, can be conducted in all the normal operating phases(the first and second phases). These programs will push forward the frontier in this field in different respects. The search for sub-millisecond pulsars and follow-up observations of their emission properties are very important projects for FAST, but they may be covered by other papers in this mini-volume; therefore,they are not discussed here.

关键词： pulsars:general pulsars: radio emission radiation mechanisms:non-thermal

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Mapping the emission line strengths and kinematics of supernova remnant S147 with extensive LAMOST spectroscopic observations

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Research in Astronomy and Astrophysics 2018年第9期18卷 63-78页

作者： Juan-Juan Ren Xiao-wei Liu Bing-Qiu Chen Mao-Sheng Xiang Hai-Bo Yuan Yang Huang Hua-wei Zhang Chun Wang Zhi-{2. Tian Gao-Chao Liu Hong Wu Department of Astronomy Peking University Key Laboratory of Optical Astronomy National Astronomy Observatories Chinese Academy of Sciences Kavli Institute for Astronomy and Astrophysics Peking University South-Western Institute for Astronomy Research Yunnan University Department of Astronomy Beijing Normal University College of Science China Three Gorges University

We present extensive spectroscopic observations of supernova remnant （SNR） S 147 collected with the Large sky Area Multi-Object fiber Spectroscopic Telescope （LAMOST）. The spectra were care- fully sky-subtracted taking into account the complex filamentary structure of S 147. We have utilized all available LAMOST spectra toward S 147, including sky and stellar spectra. By measuring the prominent optical emission lines including Ha, [NII] ）λ 6584 and [S n] λλ6717, 6731, we present maps of radial velocity and line intensity ratio covering the whole nebula of S 147 with unprecedented detail. The maps spatially correlate well with the complex filamentary structure of S147. For the central 2. of S147, the radial velocity varies from - 100 to 100 krn s^-1 and has peaks between - 0 and 10 km s^-1. The intensity ratios of Hα/[S n）λλ6717,6731, [Sn] λ 6717/λ 6731 and Ha/IN Hα/λ 6584 peak at about 0.77, 1.35 and 1.48, respectively, with a scatter of 0.17, 0.19 and 0.37, respectively. The intensity ratios are consistent with the literature values. However, the range of variations of line intensity ratios estimated here, which are representative of the whole nebula, is larger than previously estimated.

关键词： ISM supernova remnants - ISM kinematics and dynamics - ISM general

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A small electron beam ion trap/source facility for electron/neutral-ion collisional spectroscopy in astrophysical plasmas

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Research in Astronomy and Astrophysics 2018年第1期18卷 1-10页

作者： Gui-Yun Liang Hui-Gang wei Da-wei Yuan Fei-Lu Wang Ji-Min Peng {2.-Yong Zhong Xiao-Long Zhu Mike Schmidt Günter Zschornack Xin-Wen Ma Gang Zhao Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing 100012 China Department of Astronomy Beijing Normal University Beijing 100875 China Institute of Modern Physics Chinese Academy of Sciences Lanzhou 730000 China DREEBIT GmbH 01109 Dresden Germany

Spectra are fundamental observation data used for astronomical research,but understanding them strongly depends on theoretical models with many fundamental parameters from theoretical *** models give different insights for understanding a specific ***,laboratory benchmarks for these theoretical models become *** electron beam ion trap is an ideal facility for spectroscopic benchmarks due to its similar conditions of electron density and temperature compared to astrophysical plasmas in stellar coronae,supernova remnants and so *** this paper,we will describe the performance of a small electron beam ion trap/source facility installed at national astronomical observatories,chinese academy of *** present some preliminary experimental results on X-ray emission,ion production,the ionization process of trapped ions as well as the effects of charge exchange on the ionization.

关键词： X-ray:general atomic processes line:formation method:laboratory:atomic

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Detecting and Monitoring Tidal Dissipation of Hot Jupiters in the Era of SiTian

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Research in Astronomy and Astrophysics 2022年第5期22卷 36-46页

作者： Fan Yang wei Wang Xing wei Hui Zhang Ji-Lin Zhou Su-Su Shan Jie Zheng wei-Kai Zong Ming Yang Yu Bai Song Wang jia-Chen Zheng Yu-Ru Xu Yu-Feng Li You-Jun Lu Ji-Feng Liu Department of Astronomy Beijing Normal UniversityBeijing 100875China Key Laboratory of Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China

Transit Timing Variation(TTV)of hot Jupiters provides direct observational evidence of planet tidal *** tidal dissipation through TTV needs high precision transit timings and long timing *** this work,we predict and discuss the potential scientific contribution of the SiTian Survey in detecting and analyzing exoplanet *** develop a tidal dissipation detection pipeline for the SiTian Survey that aims at time-domain astronomy with 72. m optical *** pipeline includes the modules of light curve deblending,transit timing acquisition and TTV *** is capable of detecting more than 2.,000 exoplanets among which we expect~50 sources to show evidence of tidal *** present detection and analysis of tidal dissipating targets,based on simulated SiTian light curves of XO-3b and WASP-161 *** transit light curve modeling gives consistent results within 1σto input values of simulated light ***,the parameter uncertainties predicted by Markov Chain Monte Carlo are consistent with the distribution obtained from simulating and modeling the light curve 1000 *** timing precision of SiTian observations is~0.5 minutes with one transit *** show that differences between TTV origins,e.g.,tidal dissipation,apsidal precession and multiple planets,would be significant,considering the timing precision and *** detection rate of tidal dissipating hot Jupiters would answer a crucial question of whether the planet migrates at an early formation stage or random stages due to perturbations,e.g.,planet scattering or secular *** identified targets would be constructive given that the sample would extend tenfold.

关键词： planets and satellites gaseous planets-planets and satellites physical evolution-planets and satellites dynamical evolutionand stability-planetsandsatellites detection

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FRB 171019:an event of binary neutron star merger?

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Research in Astronomy and Astrophysics 2020年第4期20卷 107-114页

作者： Jin-Chen jiang wei-Yang Wang Rui Luo Shuang Du Xuelei Chen Ke-jia Lee Ren-Xin Xu State Key Laboratory of Nuclear Physics and Technology School of PhysicsPeking UniversityBeijing 100871China national astronomical {2. Chinese Academy of SciencesBeijing 100101China Key Laboratory of Computational Astrophysics National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China School of Astronomy and Space sciences University of Chinese Academy of SciencesBeijing 100049China CSIRO Astronomy and Space Science ATNFBox 76 EppingNSW 1710Australia Kavli Institute for Astronomy and Astrophysics Peking UniversityBeijing 100871China

The fast radio burst,FRB 171019,was relatively bright when discovered first by ASKAP but was identified as a repeater with three faint bursts detected later by GBT and *** observations lead to the discussion of whether the first bright burst shares the same mechanism with the following repeating bursts.A model of binary neutron star merger is proposed for FRB 171019,in which the first bright burst occurred during the merger event,while the subsequent repeating bursts are starquake-induced,and generally fainter,as the energy release rate for the starquakes can hardly exceed that of the catastrophic merger *** scenario is consistent with the observation that no later burst detected is as bright as the first one.

关键词： pulsars:general stars:neutron dense matter gravitational waves

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FAST Observations of an Extremely Active Episode of FRB 2.2.112.A.Ⅱ.Energy Distribution

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Research in Astronomy and Astrophysics 2022年第12期22卷 70-80页

作者： Yong-Kun Zhang Pei Wang Yi Feng Bing Zhang Di Li Chao-wei Tsai Chen-Hui Niu Rui Luo Ju-Mei Yao wei-wei Zhu Jin-Lin Han Ke-jia Lee De-jiang Zhou jia-Rui Niu Jin-Chen jiang wei-Yang Wang Chun-Feng Zhang Heng Xu Bo-Jun Wang jiang-wei Xu national astronomical {2. Chinese Academy of SciencesBeijing 100101China University of chinese academy of sciences Beijing 100049China Research Center for Intelligent Computing Platforms Zhejiang LaboratoryHangzhou 311100China Department of Physics and Astronomy University of NevadaLas VegasNV 89154USA Nevada Center for Astrophysics University of NevadaLas VegasNV 89154USA NAOC-UKZN Computational Astrophysics Centre University of KwaZulu-NatalDurban 4000South Africa CSIRO Space and Astronomy PO Box 76EppingNSW 1710Australia Xinjiang astronomical {2. Chinese Academy of SciencesUrumqi 830011China Kavli Institute for Astronomy and Astrophysics Peking UniversityBeijing 100871China Department of Astronomy Peking UniversityBeijing 100871China

We report the properties of more than 800 bursts detected from the repeating fast radio burst(FRB)source FRB2.2.112.A with the Five-hundred-meter Aperture Spherical radio Telescope(FAST)during an extremely active episode on UTC 2.2. September 2.–2. in a series of four *** this second paper of the series,we study the energy distribution of 881 bursts(defined as significant signals separated by dips down to the noise level)detected in the first four days of our 19 hr observational campaign spanning 17 *** event rate initially increased exponentially but the source activity stopped within 2. hr after the 4th *** detection of 542.bursts in one hour during the fourth day marked the highest event rate detected from one single FRB source so *** bursts have complex structures in the time-frequency *** find a double-peak distribution of the waiting time,which can be modeled with two log-normal functions peaking at 51.2. ms and 10.05 s,*** with the emission from a previous active episode of the source detected with FAST,the second distribution peak time is smaller,suggesting that this peak is defined by the activity level of the *** calculate the isotropic energy of the bursts using both a partial bandwidth and a full bandwidth and find that the energy distribution is not significantly *** find that an exponentially connected broken-power law function can fit the cumulative burst energy distribution well,with the lower and higher-energy indices being-1.2.±0.01 and-4.2.±0.2.,*** a radio radiative efficiency ofη_(r)=10^(-4),the total isotropic energy of the bursts released during the four days when the source was active is already 3.9×10^(46)erg,exceeding~2.%of the available magnetar dipolar magnetic *** challenges the magnetar models which invoke an inefficient radio emission(e.g.,synchrotron maser models).

关键词： (stars:)pulsars:general stars:individual(FRB 2.2.112.A) methods:data analysis

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Laboratory astrophysics with laser-driven strong magnetic fields in china

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High Power Laser Science and Engineering 2016年第3期4卷 67-70页

作者： Fei-Lu Wang Xiao-Xing Pei Bo Han Hui-Gang wei Da-wei Yuan Gui-Yun Liang Gang Zhao {2.-Yong Zhong Zhe Zhang Bao-Jun Zhu Yan-Fei Li Fang Li Yu-Tong Li Si-Liang Zeng Shi-Yang Zou Jie Zhang Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences University of chinese academy of sciences Department of Astronomy Beijing Normal University Beijing national Laboratory of Condensed Matter Physics Institute of Physics Chinese Academy of Sciences Institute of Applied Physics and Computational Mathematics Shanghai jiao Tong University

In this paper, the recent studies of laboratory astrophysics with strong magnetic fields in china have been *** the Shenguang-II laser facility of the national Laboratory on High-Power Lasers and Physics, a laser-driven strong magnetic field up to 2.0 T has been achieved. The experiment was performed to model the interaction of solar wind with dayside magnetosphere. Also the low beta plasma magnetic reconnection(MR) has been studied. Theoretically, the model has been developed to deal with the atomic structures and processes in strong magnetic field. Also the study of shock wave generation in the magnetized counter-streaming plasmas is introduced.

关键词： Laboratory astrophysics laser strong magnetic fields

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