| Autor: |
Xiaobo Li, Zhu Liu, Y. L. Tuo, J. W. Yang, Shuang-Nan Zhang, Aimei Zhang, Yong Chen, Wei Wang, Li Chen, Mao-Shun Li, Hai-Sheng Zhao, C. K. Li, Cheng-Kui Li, Weimin Yuan, Yanji Yang, Juan Wang, Yu-Xuan Zhu, Ju Guan, Xiao-Fan Zhao, Bozena Czerny, Ling-Jun Wang, Qingwen Wu, Xufang Li, Gang Li, R. C. Shang, B. B. Wu, Shaolin Xiong, Yifei Zhang, Tong Zhang, X. Y. Song, Yongjie Zhang, N. Sai, Erlin Qiao, Yi Zhang, Ti-Pei Li, Lian Tao, Wei-Wei Cui, Wan-Chang Zhang, Bin Meng, Yue Zhu, Y. Nang, Liang Sun, Yu-Peng Chen, Ming-Yu Ge, Xiao-Jing Liu, Wei Cui, Zi-Gao Dai, Bobing Wu, Shu Zhang, Gang Chen, Bing Li, Yuan-Yuan Du, Zhi Chang, G. F. Wang, Xiang Ma, Ying Tan, L. D. Kong, T. Luo, Fangjun Lu, Guan-Hua Gao, Shuo Xiao, Juan Zhang, D. K. Zhou, Shu-Mei Jia, Y. P. Chen, Chichuan Jin, Bifang Liu, Wei Li, Jian-Feng Zhou, Ge Ou, Yupeng Xu, Bo Lu, Bei You, He Gao, Chen Wang, Fan Zhang, Yanguo Li, Chong Luo, Qi Luo, Jing Jin, Jing-Kang Deng, Li-Ming Song, Cheng-Cheng Guo, XiangYang Wen, Xiaohua Liang, C. X. Liu, C. Cai, Yue Huang, Yuan You, Jia Huo, Zi-Liang Zhang, J. C. Liu, Zhao Zhang, Yongwei Dong, Qi-Bin Yi, Mei Wu, W. C. Jiang, Jin-Yuan Liao, X. L. Cao, Xue-Feng Lu, Guang-Cheng Xiao, Wei Zhang, Chengmo Zhang, Yu-Dong Gu, Hong-Mei Zhang, Tian-Xiang Chen, GuoQing Liu, Y. N. Liu, Qian-Qing Yin, Zheng-Wei Li, Xian Li, Hongwei Liu, Sheng Yang, Wenshuai Wang, Luhua Jiang, Jin-Lu Qu, Jianyin Nie, Min-Xue Fu, Yu-Sa Wang, YongJie Jin, Yue Zhang, Qingcui Bu, Wen-Zhao Zhang, Da-Wei Han, M. Gao, Shi-Jie Zheng |
| Jazyk: |
angličtina |
| Rok vydání: |
2021 |
| Předmět: |
|
| Zdroj: |
Nature Communications, Vol 12, Iss 1, Pp 1-11 (2021)
Nature Communications |
| ISSN: |
2041-1723 |
| Popis: |
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.
11 pages, 5 figures; published in Nature Communications; An artist's impression of Figure 5 is updated here, and the animation is available at http://youbei.work/research/ |
| Databáze: |
OpenAIRE |
| Externí odkaz: |
|
