Insight-HXMT observations of jet-like corona in a black hole X-ray binary MAXI J1820+070

被引：50

作者：

You, Bei ^{[1
,2
]}

Tuo, Yuoli ^{[3
,4
]}

Li, Chengzhe ^{[1
]}

Wang, Wei ^{[1
,2
]}

Zhang, Shuang-Nan ^{[3
,4
]}

Zhang, Shu ^{[3
]}

Ge, Mingyu ^{[3
]}

Luo, Chong ^{[1
,2
]}

Liu, Bifang ^{[5
,6
]}

Yuan, Weimin ^{[5
,6
]}

Dai, Zigao ^{[7
]}

Liu, Jifeng ^{[6
,8
,9
]}

Qiao, Erlin ^{[5
,6
]}

Jin, Chichuan ^{[5
,6
]}

Liu, Zhu ^{[5
,6
]}

Czerny, Bozena ^{[10
]}

Wu, Qingwen ^{[11
]}

Bu, Qingcui ^{[3
,12
]}

Cai, Ce ^{[3
,4
]}

Cao, Xuelei ^{[3
]}

Chang, Zhi ^{[3
]}

Chen, Gang ^{[3
]}

Chen, Li ^{[13
]}

Chen, Tianxiang ^{[3
]}

Chen, Yibao ^{[14
]}

Chen, Yong ^{[3
]}

Chen, Yupeng ^{[3
]}

Cui, Wei ^{[15
]}

Cui, Weiwei ^{[3
]}

Deng, Jingkang ^{[14
]}

Dong, Yongwei ^{[3
]}

Du, Yuanyuan ^{[3
]}

Fu, Minxue ^{[14
]}

Gao, Guanhua ^{[3
,4
]}

Gao, He ^{[3
,4
]}

Gao, Min ^{[3
]}

Gu, Yudong ^{[3
]}

Guan, Ju ^{[3
]}

Guo, Chengcheng ^{[3
,4
]}

Han, Dawei ^{[3
]}

Huang, Yue ^{[3
]}

Huo, Jia ^{[3
]}

Jia, Shumei ^{[3
]}

Jiang, Luhua ^{[3
]}

Jiang, Weichun ^{[3
]}

Jin, Jing ^{[3
]}

Jin, Yongjie ^{[16
]}

Kong, Lingda ^{[3
,4
]}

Li, Bing ^{[3
]}

Li, Chengkui ^{[3
]}

机构：

[1] Wuhan Univ, Sch Phys & Technol, Wuhan, Peoples R China

[2] Wuhan Univ, Astron Ctr, Wuhan, Peoples R China

[3] Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing, Peoples R China

[4] Univ Chinese Acad Sci, Chinese Acad Sci, Beijing, Peoples R China

[5] Chinese Acad Sci, Key Lab Space Astron & Technol, Beijing, Peoples R China

[6] Univ Chinese Acad Sci, Sch Astron & Space Sci, Beijing, Peoples R China

[7] Nanjing Univ, Sch Astron & Space Sci, Nanjing, Peoples R China

[8] Chinese Acad Sci, Natl Astron Observ, Key Lab Opt Astron, Beijing 100101, Peoples R China

[9] Wuhan Univ, WHU NAOC Joint Ctr Astron, Wuhan, Peoples R China

[10] Polish Acad Sci, Ctr Theoret Phys, Warsaw, Poland

[11] Huazhong Univ Sci & Technol, Sch Phys, Wuhan, Peoples R China

[12] Tuebingen Univ, Tubingen, Germany

[13] Beijing Normal Univ, Dept Astron, Beijing, Peoples R China

[14] Tsinghua Univ, Dept Phys, Beijing, Peoples R China

[15] Tsinghua Univ, Dept Astron, Beijing, Peoples R China

[16] Tsinghua Univ, Dept Engn Phys, Beijing, Peoples R China

[17] Chinese Acad Sci, Inst High Energy Phys, Comp Div, Beijing, Peoples R China

[18] Xiangtan Univ, Sch Phys & Optoelect, Xiangtan, Hunan, Peoples R China

[19] Jilin Univ, Coll Phys, Changchun, Peoples R China

来源：

NATURE COMMUNICATIONS | 2021年 / 12卷 / 01期

关键词：

ACCRETION FLOWS; REFLECTION; SPECTRUM; DISC; NUSTAR; STATE;

D O I：

10.1038/s41467-021-21169-5

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

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. Evolution of accretion disk and corona during outbursts in black hole binary systems is still unclear. Here, the authors show spectral analysis of MAXI J1820+070 and propose a scenario of a dynamical corona to explain the evolution of the reflection fraction observed by Insight-HXMT.

引用

页数：11

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