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

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arxiv 2102.07602 v2 pith:SW7IW3XA submitted 2021-02-15 astro-ph.HE astro-ph.GA

Bei You , Yuoli Tuo , Chengzhe Li , Wei Wang , Shuang-Nan Zhang , Shu Zhang , Mingyu Ge , Chong Luo
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Bifang Liu Weimin Yuan Zigao Dai Jifeng Liu Erlin Qiao Chichuan Jin Zhu Liu Bozena Czerny Qingwen Wu Qingcui Bu Ce Cai Xuelei Cao Zhi Chang Gang Chen Li Chen Tianxiang Chen Yibao Chen Yong Chen Yupeng Chen Wei Cui Weiwei Cui Jingkang Deng Yongwei Dong Yuanyuan Du Minxue Fu Guanhua Gao He Gao Min Gao Yudong Gu Ju Guan Chengcheng Guo Dawei Han Yue Huang Jia Huo Shumei Jia Luhua Jiang Weichun Jiang Jing Jin Yongjie Jin Lingda Kong Bing Li Chengkui Li Gang Li Maoshun Li Tipei Li Wei Li Xian Li Xiaobo Li Xufang Li Yanguo Li Zhengwei Li Xiaohua Liang Jinyuan Liao Congzhan Liu Guoqing Liu Hongwei Liu Xiaojing Liu Yinong Liu Bo Lu Fangjun Lu Xuefeng Lu Qi Luo Tao Luo Xiang Ma Bin Meng Yi Nang Jianyin Nie Ge Ou Jinlu Qu Na Sai Rencheng Shang Liming Song Xinying Song Liang Sun Ying Tan Lian Tao Chen Wang Guofeng Wang Juan Wang Lingjun Wang Wenshuai Wang Yusa Wang Xiangyang Wen Baiyang Wu Bobing Wu Mei Wu Guangcheng Xiao Shuo Xiao Shaolin Xiong Yupeng Xu Jiawei Yang Sheng Yang Yanji Yang Qibin Yi Qianqing Yin Yuan You Aimei Zhang Chengmo Zhang Fan Zhang Hongmei Zhang Juan Zhang Tong Zhang Wanchang Zhang Wei Zhang Wenzhao Zhang Yi Zhang Yifei Zhang Yongjie Zhang Yue Zhang Zhao Zhang Ziliang Zhang Haisheng Zhao Xiaofan Zhao Shijie Zheng Dengke Zhou Jianfeng Zhou Yuxuan Zhu Yue Zhu
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classification astro-ph.HEastro-ph.GA
keywords coronablackcoronaldiskholex-raybinarydecrease
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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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Cited by 2 Pith papers

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    astro-ph.HE 2026-07 conditional novelty 6.0 of 10

    For Swift J1727.8–1613, the optical–X-ray correlation flips sign with X-ray energy, and the QPO lag is flat (~60–80 ms) from 2 to 150 keV.

  2. Revisiting the infrared/X-ray correlation of GX 339-4 based on a jet model

    astro-ph.HE 2025-05 conditional novelty 6.0 of 10

    The observed IR/X-ray correlation of GX 339-4, including its break, can be reproduced by varying only the accretion rate in a jet model if the X-rays come from synchrotron self-Compton scattering in the jet.

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