| Literature DB >> 33589623 |
Bei You1,2, Yuoli Tuo3,4, Chengzhe Li1, Wei Wang5,6, Shuang-Nan Zhang7,8, Shu Zhang3, Mingyu Ge3, Chong Luo1,2, Bifang Liu9,10, Weimin Yuan9,10, Zigao Dai11, Jifeng Liu10,12,13, Erlin Qiao9,10, Chichuan Jin9,10, Zhu Liu9,10, Bozena Czerny14, Qingwen Wu15, Qingcui Bu3,16, Ce Cai3,4, Xuelei Cao3, Zhi Chang3, Gang Chen3, Li Chen17, Tianxiang Chen3, Yibao Chen18, Yong Chen3, Yupeng Chen3, Wei Cui19, Weiwei Cui3, Jingkang Deng18, Yongwei Dong3, Yuanyuan Du3, Minxue Fu18, Guanhua Gao3,4, He Gao3,4, Min Gao3, Yudong Gu3, Ju Guan3, Chengcheng Guo3,4, Dawei Han3, Yue Huang3, Jia Huo3, Shumei Jia3, Luhua Jiang3, Weichun Jiang3, Jing Jin3, Yongjie Jin20, Lingda Kong3,4, Bing Li3, Chengkui Li3, Gang Li3, Maoshun Li3, Tipei Li3,4,19, Wei Li3, Xian Li3, Xiaobo Li3, Xufang Li3, Yanguo Li3, Zhengwei Li3, Xiaohua Liang3, Jinyuan Liao3, Congzhan Liu3, Guoqing Liu18, Hongwei Liu3, Xiaojing Liu3, Yinong Liu20, Bo Lu3, Fangjun Lu3, Xuefeng Lu3, Qi Luo3,4, Tao Luo3, Xiang Ma3, Bin Meng3, Yi Nang3,4, Jianyin Nie3, Ge Ou21, Jinlu Qu3, Na Sai3,4, Rencheng Shang18, Liming Song3,4, Xinying Song3, Liang Sun3, Ying Tan3, Lian Tao3, Chen Wang4,9, Guofeng Wang3, Juan Wang3, Lingjun Wang3, Wenshuai Wang21, Yusa Wang3, Xiangyang Wen3, Baiyang Wu3,4, Bobing Wu3, Mei Wu3, Guangcheng Xiao3,4, Shuo Xiao3,4, Shaolin Xiong3, Yupeng Xu3,4, Jiawei Yang3, Sheng Yang3, Yanji Yang3, Qibin Yi3,22, Qianqing Yin3, Yuan You3,4, Aimei Zhang3, Chengmo Zhang3, Fan Zhang3, Hongmei Zhang22, Juan Zhang3, Tong Zhang3, Wanchang Zhang3, Wei Zhang4, Wenzhao Zhang17, Yi Zhang3, Yifei Zhang3, Yongjie Zhang3, Yue Zhang3,4, Zhao Zhang18, Ziliang Zhang3, Haisheng Zhao3, Xiaofan Zhao3,4, Shijie Zheng3, Dengke Zhou3,4, Jianfeng Zhou20, Yuxuan Zhu3,23, Yue Zhu3.
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.Entities:
Year: 2021 PMID： 33589623 DOI： 10.1038/s41467-021-21169-5
Source DB: PubMed Journal: Nat Commun ISSN： 2041-1723 Impact factor: 14.919