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Insight-HXMT observations of jet-like corona in a black hole X-ray binary MAXI J1820+070.
You, Bei; Tuo, Yuoli; Li, Chengzhe; Wang, Wei; Zhang, Shuang-Nan; Zhang, Shu; Ge, Mingyu; Luo, Chong; Liu, Bifang; Yuan, Weimin; Dai, Zigao; Liu, Jifeng; Qiao, Erlin; Jin, Chichuan; Liu, Zhu; Czerny, Bozena; Wu, Qingwen; Bu, Qingcui; Cai, Ce; Cao, Xuelei; Chang, Zhi; Chen, Gang; Chen, Li; Chen, Tianxiang; Chen, Yibao; Chen, Yong; Chen, Yupeng; Cui, Wei; Cui, Weiwei; Deng, Jingkang; Dong, Yongwei; Du, Yuanyuan; Fu, Minxue; Gao, Guanhua; Gao, He; Gao, Min; Gu, Yudong; Guan, Ju; Guo, Chengcheng; Han, Dawei; Huang, Yue; Huo, Jia; Jia, Shumei; Jiang, Luhua; Jiang, Weichun; Jin, Jing; Jin, Yongjie; Kong, Lingda; Li, Bing; Li, Chengkui.
Afiliação
  • You B; School of Physics and Technology, Wuhan University, Wuhan, PR China.
  • Tuo Y; Astronomical Center, Wuhan University, Wuhan, PR China.
  • Li C; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
  • Wang W; University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing, PR China.
  • Zhang SN; School of Physics and Technology, Wuhan University, Wuhan, PR China.
  • Zhang S; School of Physics and Technology, Wuhan University, Wuhan, PR China. wangwei2017@whu.edu.cn.
  • Ge M; Astronomical Center, Wuhan University, Wuhan, PR China. wangwei2017@whu.edu.cn.
  • Luo C; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China. zhangsn@ihep.ac.cn.
  • Liu B; University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing, PR China. zhangsn@ihep.ac.cn.
  • Yuan W; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
  • Dai Z; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
  • Liu J; School of Physics and Technology, Wuhan University, Wuhan, PR China.
  • Qiao E; Astronomical Center, Wuhan University, Wuhan, PR China.
  • Jin C; Key Laboratory of Space Astronomy and Technology, Chinese Academy of Sciences, Beijing, China.
  • Liu Z; School of Astronomy and Space Sciences, University of Chinese Academy of Sciences, Beijing, PR China.
  • Czerny B; Key Laboratory of Space Astronomy and Technology, Chinese Academy of Sciences, Beijing, China.
  • Wu Q; School of Astronomy and Space Sciences, University of Chinese Academy of Sciences, Beijing, PR China.
  • Bu Q; School of Astronomy and Space Science, Nanjing University, Nanjing, PR China.
  • Cai C; School of Astronomy and Space Sciences, University of Chinese Academy of Sciences, Beijing, PR China.
  • Cao X; Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China.
  • Chang Z; WHU-NAOC Joint Center for Astronomy, Wuhan University, Wuhan, Hubei, China.
  • Chen G; Key Laboratory of Space Astronomy and Technology, Chinese Academy of Sciences, Beijing, China.
  • Chen L; School of Astronomy and Space Sciences, University of Chinese Academy of Sciences, Beijing, PR China.
  • Chen T; Key Laboratory of Space Astronomy and Technology, Chinese Academy of Sciences, Beijing, China.
  • Chen Y; School of Astronomy and Space Sciences, University of Chinese Academy of Sciences, Beijing, PR China.
  • Chen Y; Key Laboratory of Space Astronomy and Technology, Chinese Academy of Sciences, Beijing, China.
  • Chen Y; School of Astronomy and Space Sciences, University of Chinese Academy of Sciences, Beijing, PR China.
  • Cui W; Center for Theoretical Physics, Polish Academy of Sciences, Warsaw, Poland.
  • Cui W; School of Physics, Huazhong University of Science and Technology, Wuhan, China.
  • Deng J; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
  • Dong Y; Tuebingen University, Tübingen, Germany.
  • Du Y; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
  • Fu M; University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing, PR China.
  • Gao G; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
  • Gao H; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
  • Gao M; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
  • Gu Y; Department of Astronomy, Beijing Normal University, Beijing, PR China.
  • Guan J; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
  • Guo C; Department of Physics, Tsinghua University, Beijing, PR China.
  • Han D; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
  • Huang Y; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
  • Huo J; Department of Astronomy, Tsinghua University, Beijing, PR China.
  • Jia S; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
  • Jiang L; Department of Physics, Tsinghua University, Beijing, PR China.
  • Jiang W; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
  • Jin J; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
  • Jin Y; Department of Physics, Tsinghua University, Beijing, PR China.
  • Kong L; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
  • Li B; University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing, PR China.
  • Li C; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, PR China.
Nat Commun ; 12(1): 1025, 2021 Feb 15.
Article em En | MEDLINE | ID: mdl-33589623
ABSTRACT
A black hole X-ray binary produces hard X-ray radiation from its corona and disk when the accreting matter heats up. During an outburst, the disk and corona co-evolves with each other. However, such an evolution is still unclear in both its geometry and dynamics. Here we report the unusual decrease of the reflection fraction in MAXI J1820+070, which is the ratio of the coronal intensity illuminating the disk to the coronal intensity reaching the observer, as the corona is observed to contrast during the decay phase. We postulate a jet-like corona model, in which the corona can be understood as a standing shock where the material flowing through. In this dynamical scenario, the decrease of the reflection fraction is a signature of the corona's bulk velocity. Our findings suggest that as the corona is observed to get closer to the black hole, the coronal material might be outflowing faster.
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Texto completo: 1 Bases de dados: MEDLINE Tipo de estudo: Prognostic_studies Idioma: En Revista: Nat Commun Assunto da revista: BIOLOGIA / CIENCIA Ano de publicação: 2021 Tipo de documento: Article
Texto completo
Adicionar na Minha BVS
Imprimir
XML
PubMed Links
Buscar no Google

Texto completo: 1 Bases de dados: MEDLINE Tipo de estudo: Prognostic_studies Idioma: En Revista: Nat Commun Assunto da revista: BIOLOGIA / CIENCIA Ano de publicação: 2021 Tipo de documento: Article