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

Author

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

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
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., Comment: 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/

Published
2021
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12. Overview to the Hard X-ray Modulation Telescope (Insight-HXMT) Satellite

Author

Zhang, ShuangNan, Li, TiPei, Lu, FangJun, Song, LiMing, Xu, YuPeng, Liu, CongZhan, Chen, Yong, Cao, XueLei, Bu, QingCui, Cai, Ce, Chang, Zhi, Chen, Gang, Chen, Li, Chen, TianXiang, Chen, Wei, Chen, YiBao, Chen, YuPeng, Cui, Wei, Cui, WeiWei, Deng, JingKang, Dong, YongWei, Du, YuanYuan, Fu, MinXue, Gao, GuanHua, Gao, He, Gao, Min, Ge, MingYu, Gu, YuDong, Guan, Ju, Gungor, Can, Guo, ChengCheng, Han, DaWei, Hu, Wei, Huang, Yan, Huang, Yue, Huo, Jia, Jia, ShuMei, Jiang, LuHua, Jiang, WeiChun, Jin, Jing, Jin, YongJie, Kong, Lingda, Li, Bing, Li, ChengKui, Li, Gang, Li, MaoShun, Li, Wei, Li, Xian, Li, XiaoBo, Li, XuFang, Li, YanGuo, Li, ZiJian, Li, ZhengWei, Liang, XiaoHua, Liao, JinYuan, Liu, Baisheng, Liu, GuoQing, Liu, HongWei, Liu, ShaoZhen, Liu, XiaoJing, Liu, Yuan, Liu, YiNong, Lu, Bo, Lu, XueFeng, Luo, Qi, Luo, Tao, Ma, Xiang, Meng, Bin, Nang, Yi, Nie, JianYin, Ou, Ge, Qu, JinLu, Sai, Na, Shang, RenCheng, Shen, GuoHong, Song, XinYing, Sun, Liang, Tan, Ying, Tao, Lian, Tao, WenHui, Tuo, YouLi, Wang, ChunQin, Wang, GuoFeng, Wang, HuanYu, Wang, Juan, Wang, WenShuai, Wang, YuSa, Wen, XiangYang, Wu, BoBing, Wu, Mei, Xiao, GuangCheng, Xiao, Shuo, Xiong, ShaoLin, Xu, He, Yan, LinLi, Yang, JiaWei, Yang, Sheng, Yang, YanJi, Yi, Qibin, Yu, JiaXi, Yuan, Bin, Zhang, AiMei, Zhang, ChunLei, Zhang, ChengMo, Zhang, Fan, Zhang, HongMei, Zhang, Juan, Zhang, Liang, Zhang, Qiang, Zhang, ShenYi, Zhang, Shu, Zhang, Tong, Zhang, Wei, Zhang, WanChang, Zhang, WenZhao, Zhang, Yi, Zhang, Yue, Zhang, YiFei, Zhang, YongJie, Zhang, Zhao, Zhang, Zhi, Zhang, ZiLiang, Zhao, HaiSheng, Zhao, JianLing, Zhao, XiaoFan, Zheng, ShiJie, Zhu, Yue, Zhu, YuXuan, Zhuang, Renlin, and Zou, ChangLin

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

As China's first X-ray astronomical satellite, the Hard X-ray Modulation Telescope (HXMT), which was dubbed as Insight-HXMT after the launch on June 15, 2017, is a wide-band (1-250 keV) slat-collimator-based X-ray astronomy satellite with the capability of all-sky monitoring in 0.2-3 MeV. It was designed to perform pointing, scanning and gamma-ray burst (GRB) observations and, based on the Direct Demodulation Method (DDM), the image of the scanned sky region can be reconstructed. Here we give an overview of the mission and its progresses, including payload, core sciences, ground calibration/facility, ground segment, data archive, software, in-orbit performance, calibration, background model, observations and some preliminary results., Comment: 29 pages, 40 figures, 6 tables, to appear in Sci. China-Phys. Mech. Astron. arXiv admin note: text overlap with arXiv:1910.04434

Published
2019
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13. Insight-HXMT observations of Swift J0243.6+6124 during its 2017-2018 outburst

Author

Zhang, Yue, Ge, Mingyu, Song, Liming, Zhang, Shuangnan, Qu, Jinlu, Zhang, Shu, Doroshenko, Victor, Tao, Lian, Ji, Long, Güngör, Can, Santangelo, Andrea, Shi, Changsheng, Chang, Zhi, Chen, Gang, Chen, Li, Chen, Tianxiang, Chen, Yong, Chen, Yibao, Cui, Wei, Cui, Weiwei, Deng, Jingkang, Dong, Yongwei, Du, Yuanyuan, Fu, Minxue, Gao, Guanhua, Gao, He, Gao, Min, Gu, Yudong, Guan, Ju, Guo, Chengcheng, Han, Dawei, Hu, Wei, Huang, Yue, Huo, Jia, Jia, Shumei, Jiang, Luhua, Jiang, Weichun, Jin, Jing, Jin, Yongjie, Li, Bing, Li, Chengkui, Li, Gang, Li, Maoshun, Li, Wei, Li, Xian, Li, Xiaobo, Li, Xufang, Li, Yanguo, Li, Zijian, Li, Zhengwei, Liang, Xiaohua, Liao, Jinyuan, Liu, Congzhan, Liu, Guoqing, Liu, Hongwei, Liu, Shaozhen, Liu, Xiaojing, Liu, Yuan, Liu, Yinong, Lu, Bo, Lu, Xuefeng, Luo, Tao, Ma, Xiang, Meng, Bin, Nang, Yi, Nie, Jianyin, Ou, Ge, Sai, Na, Sun, Liang, Tan, Ying, Tao, Wenhui, Tuo, Youli, Wang, Guofeng, Wang, Huanyu, Wang, Juan, Wang, Wenshuai, Wang, Yusa, Wen, Xiangyang, Wu, Bobing, Wu, Mei, Xiao, Guangcheng, Xiong, Shaolin, Xu, He, Xu, Yupeng, Yan, Linli, Yang, Jiawei, Yang, Sheng, Yang, Yanji, Zhang, Aimei, Zhang, Chunlei, Zhang, Chengmo, Zhang, Fan, Zhang, Hongmei, Zhang, Juan, Zhang, Tong, Zhang, Wei, Zhang, Wanchang, Zhang, Wenzhao, Zhang, Yi, Zhang, Yifei, Zhang, Yongjie, Zhang, Zhao, Zhang, Ziliang, Zhao, Haisheng, Zhao, Jianling, Zhao, Xiaofan, Zheng, Shijie, Zhu, Yue, Zhu, Yuxuan, and Zou, Changlin

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

The recently discovered neutron star transient Swift J0243.6+6124 has been monitored by {\it the Hard X-ray Modulation Telescope} ({\it Insight-\rm HXMT). Based on the obtained data, we investigate the broadband spectrum of the source throughout the outburst. We estimate the broadband flux of the source and search for possible cyclotron line in the broadband spectrum. No evidence of line-like features is, however, found up to $\rm 150~keV$. In the absence of any cyclotron line in its energy spectrum, we estimate the magnetic field of the source based on the observed spin evolution of the neutron star by applying two accretion torque models. In both cases, we get consistent results with $B\rm \sim 10^{13}~G$, $D\rm \sim 6~kpc$ and peak luminosity of $\rm >10^{39}~erg~s^{-1}$ which makes the source the first Galactic ultraluminous X-ray source hosting a neutron star., Comment: published

Published
2019
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24. Insight-HXMT observations of the first binary neutron star merger GW170817

Author

Li, TiPei, Xiong, ShaoLin, Zhang, ShuangNan, Lu, FangJun, Song, LiMing, Cao, XueLei, Chang, Zhi, Chen, Gang, Chen, Li, Chen, TianXiang, Chen, Yong, Chen, YiBao, Chen, YuPeng, Cui, Wei, Cui, WeiWei, Deng, JingKang, Dong, YongWei, Du, YuanYuan, Fu, MinXue, Gao, GuanHua, Gao, He, Gao, Min, Ge, MingYu, Gu, YuDong, Guan, Ju, Guo, ChengCheng, Han, DaWei, Hu, Wei, Huang, Yue, Huo, Jia, Jia, ShuMei, Jiang, LuHua, Jiang, WeiChun, Jin, Jing, Jin, YongJie, Li, Bing, Li, ChengKui, Li, Gang, Li, MaoShun, Li, Wei, Li, Xian, Li, XiaoBo, Li, XuFang, Li, YanGuo, Li, ZiJian, Li, ZhengWei, Liang, XiaoHua, Liao, JinYuan, Liu, CongZhan, Liu, GuoQing, Liu, HongWei, Liu, ShaoZhen, Liu, XiaoJing, Liu, Yuan, Liu, YiNong, Lu, Bo, Lu, XueFeng, Luo, Tao, Ma, Xiang, Meng, Bin, Nang, Yi, Nie, JianYin, Ou, Ge, Qu, JinLu, Sai, Na, Sun, Liang, Tan, Yin, Tao, Lian, Tao, WenHui, Tuo, YouLi, Wang, GuoFeng, Wang, HuanYu, Wang, Juan, Wang, WenShuai, Wang, YuSa, Wen, XiangYang, Wu, BoBing, Wu, Mei, Xiao, GuangCheng, Xu, He, Xu, YuPeng, Yan, LinLi, Yang, JiaWei, Yang, Sheng, Yang, YanJi, Zhang, AiMei, Zhang, ChunLei, Zhang, ChengMo, Zhang, Fan, Zhang, HongMei, Zhang, Juan, Zhang, Qiang, Zhang, Shu, Zhang, Tong, Zhang, Wei, Zhang, WanChang, Zhang, WenZhao, Zhang, Yi, Zhang, Yue, Zhang, YiFei, Zhang, YongJie, Zhang, Zhao, Zhang, ZiLiang, Zhao, HaiSheng, Zhao, JianLing, Zhao, XiaoFan, Zheng, ShiJie, Zhu, Yue, Zhu, YuXuan, and Zou, ChangLin

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Finding the electromagnetic (EM) counterpart of binary compact star merger, especially the binary neutron star (BNS) merger, is critically important for gravitational wave (GW) astronomy, cosmology and fundamental physics. On Aug. 17, 2017, Advanced LIGO and \textit{Fermi}/GBM independently triggered the first BNS merger, GW170817, and its high energy EM counterpart, GRB 170817A, respectively, resulting in a global observation campaign covering gamma-ray, X-ray, UV, optical, IR, radio as well as neutrinos. The High Energy X-ray telescope (HE) onboard \textit{Insight}-HXMT (Hard X-ray Modulation Telescope) is the unique high-energy gamma-ray telescope that monitored the entire GW localization area and especially the optical counterpart (SSS17a/AT2017gfo) with very large collection area ($\sim$1000 cm$^2$) and microsecond time resolution in 0.2-5 MeV. In addition, \textit{Insight}-HXMT quickly implemented a Target of Opportunity (ToO) observation to scan the GW localization area for potential X-ray emission from the GW source. Although it did not detect any significant high energy (0.2-5 MeV) radiation from GW170817, its observation helped to confirm the unexpected weak and soft nature of GRB 170817A. Meanwhile, \textit{Insight}-HXMT/HE provides one of the most stringent constraints (~10$^{-7}$ to 10$^{-6}$ erg/cm$^2$/s) for both GRB170817A and any other possible precursor or extended emissions in 0.2-5 MeV, which help us to better understand the properties of EM radiation from this BNS merger. Therefore the observation of \textit{Insight}-HXMT constitutes an important chapter in the full context of multi-wavelength and multi-messenger observation of this historical GW event., Comment: accepted by Science China - Physics, Mechanics & Astronomy. Planned to publish on Oct 17, but postponed due to a problem on pdf file

Published
2017
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30. BN Promoted Heterojunction Ni─Fe─P/BN Electrocatalyst with Excellent Performance of Oxygen Evolution Reaction.

Author

Han, Guoqiang, Wang, Chunyang, Zhao, Shen, Bian, Haowei, Xie, Guangwen, Liu, Xin, Jiang, Luhua, and Roy, Soumyendu

Abstract

In this research, we have successfully synthesized a Ni─Fe─P/h‐BN catalyst through a simple one‐step electrodeposition method for efficient water splitting in a KOH electrolytic cell. Our prepared Ni─Fe─P/h‐BN catalyst showcased exceptional electrocatalytic activity for the oxygen evolution reaction (OER), with an overpotential of only 210 mV at a current density of 10 mA cm⁻2. Notably, this value is significantly lower compared to 248 mV observed for Ni─Fe─P/Fe without h‐BN and also superior to the results reported for other catalysts. Furthermore, through the ball milling, we further enhanced the OER performance of the catalyst, achieving an impressive overpotential of 200 mV at the same density of 10 mA cm−2. The exceptional OER performance displayed by the Ni─Fe─P/h‐BN composite is attributable to the synergistic effects of Ni─Fe─P and h‐BN. Furthermore, the introduction of a heterojunction between h‐BN and Ni─Fe─P serves to further enhance the OER capability of the catalyst. This investigation introduces a straightforward and effective approach for fabricating cost‐effective and high‐performance electrocatalysts intended for water electrolysis. [ABSTRACT FROM AUTHOR]

Published
2024
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43. A review on the bioleaching of toxic metal(loid)s from contaminated soil: Insight into the mechanism of action and the role of influencing factors

Author

Sarkodie, Emmanuel Konadu, primary, Jiang, Luhua, additional, Li, Kewei, additional, Yang, Jiejie, additional, Guo, Ziwen, additional, Shi, Jiaxin, additional, Deng, Yan, additional, Liu, Hongwei, additional, Jiang, Huidan, additional, Liang, Yili, additional, Yin, Huaqun, additional, and Liu, Xueduan, additional

Published
2022
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