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4 results on '"Guangcheng Xiao"'

1. A Timing View of the Additional High-energy Spectral Component Discovered in the Black Hole Candidate Swift J1727.8-1613

Author

Zi-Xu Yang, Liang Zhang, Shuang-Nan Zhang, Lian Tao, Shu Zhang, Ruican Ma, Qing-Cui Bu, Yue Huang, He-Xin Liu, Wei Yu, Guangcheng Xiao, Peng-Ju Wang, Hua Feng, Li-Ming Song, Xiang Ma, Mingyu Ge, Qing-Chang Zhao, and Jin-Lu Qu

Subjects
Low-mass x-ray binary stars, Accretion, Astrophysical black holes, Stellar mass black holes, Astrophysics, QB460-466
Abstract

We present an energy-dependent analysis for the type-C quasiperiodic oscillations (QPOs) observed in the black hole X-ray binary Swift J1727.8–1613 using Insight-HXMT observations. We find that the QPO fractional rms at energies above 40 keV is significantly higher than that below 20 keV. This is the first report of a high energy (HE) rms excess in the rms spectrum of a black hole X-ray binary. In the high energy band, an extra hard component is observed in addition to the standard thermal Comptonization component at a similar energy band. The value of the QPO HE rms excess is not only correlated with the disk parameters and the photon index of the standard Comptonization component but also exhibits a moderate positive correlation with the flux of the additional hard spectral component. No features in the QPO phase-lag spectra are seen corresponding to the additional hard component. We propose that the additional hard component in the spectrum may originate from jet emission and the associated QPO HE rms excess can be explained by the precession of the jet base.

Published
2024
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2. Insight-HXMT observations of jet-like corona in a black hole X-ray binary MAXI J1820+070

Author

Bei You, Yuoli Tuo, Chengzhe Li, Wei Wang, Shuang-Nan Zhang, Shu Zhang, Mingyu Ge, Chong Luo, 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, and Yue Zhu

Subjects
Science
Abstract

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.

Published
2021
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4. Multiwavelength observations of Swift J0243.6+6124 from 2017 to 2022

Author

Wei Liu, Jingzhi Yan, Pablo Reig, Xiaofeng Wang, Guangcheng Xiao, Han Lin, Xinhan Zhang, Hanna Sai, Zhihao Chen, Shengyu Yan, and Qingzhong Liu

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

We have obtained optical spectroscopy and photometry data during four years after the event. The long-term photometric light-curve and the equivalent widths of the Halpha and He I 6678 lines were used to monitor the state of the Be star disk. The Halpha line profiles show evidence for V/R variability that was accounted for by fitting the Halpha spectral line profile with two Gaussian functions. We divided our data into three phases according to the intensity of the X-ray, optical, and infrared emission. Phase I covers the rise and decay of the giant X-ray outburst that took place in October to November 2017. We interpret phase II as the dissipation of the Be star equatorial disk and phase III as its recovery. The timescale of a complete formation and dissipation process is about 1250 days. The epoch when the dissipation process stopped and the reformation period began is estimated to be around MJD 58530. We find a delay of about 100 to 200 days between the minimum of the optical or infrared intensity and the strength of the Halpha line after the X-ray outburst, which may indicate that the dissipation of the disk begins from the inner parts. The motion of the density perturbation inside the disk is prograde, with a V/R quasi-period of about four years. The source shows a positive correlation in the (B-V) color index versus V-band magnitude diagram, which implies that the system is seen at a small or moderate inclination angle., 15 pages, 5 figures

Published
2022

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