Insight-HXMT observations of 4U~1636-536: Corona cooling revealed with single short type-I X-ray burst
Y. P. Chen, S. Zhang, S. N. Zhang, L. Ji, L. D. Kong, X. L. Cao, Z. Chang, G. Chen, L. Chen, T. X. Chen, Y. Chen, Y. B. Chen, W. Cui, W. W. Cui, J. K. Deng, Y. … 展开作者
Y. P. Chen, S. Zhang, S. N. Zhang, L. Ji, L. D. Kong, X. L. Cao, Z. Chang, G. Chen, L. Chen, T. X. Chen, Y. Chen, Y. B. Chen, W. Cui, W. W. Cui, J. K. Deng, Y. W. Dong, Y. Y. Du, M. X. Fu, G. H. Gao, H. Gao, M. Gao, M. Y. Ge, Y. D. Gu, J. Guan, C. C. Guo, D. W. Han, W. Hu, Y. Huang, J. Huo, S. M. Jia, L. H. Jiang, W. C. Jiang, J. Jin, Y. J. Jin, B. Li, C. K. Li, G. Li, M. S. Li, T. P. Li, W. Li, X. Li, X. B. Li, X. F. Li, Y. G. Li, Z. J. Li, Z. W. Li, X. H. Liang, J. Y. Liao, C. Z. Liu, G. Q. Liu, H. W. Liu, S. Z. Liu, X. J. Liu, Y. Liu, Y. N. Liu, B. Lu, F. J. Lu, X. F. Lu, T. Luo, X. Ma, B. Meng, Y. Nang, J. Y. Nie, G. Ou, J. L. Qu, N. Sai, L. M. Song, L. Sun, Y. Tan, L. Tao, W. H. Tao, Y. L. Tuo, G. F. Wang, H. Y. Wang, J. Wang, W. S. Wang, Y. S. Wang, X. Y. Wen, B. B. Wu, M. Wu, G. C. Xiao, S. L. Xiong, H. Xu, Y. P. Xu, L. L. Yan, J. W. Yang, S. Yang, Y. J. Yang, A. M. Zhang, C. L. Zhang, C. M. Zhang, F. Zhang, H. M. hang, J. Zhang, Q. Zhang, T. Zhang, W. Zhang, W. C. Zhang, W. Z. Zhang, Y. Zhang, Y. Zhang, Y. F. Zhang, Y. J. Zhang, Z. Zhang, Z. L. Zhang, H. S. Zhao, J. L. Zhao, X. F. Zhao, S. J. Zheng, Y. Zhu, Y. X. Zhu, C. L. Zou
Corona cooling was detected previously from stacking a series of short type-I bursts occurred during the low/had state of atoll outburst. Type-I bursts are hence regarded as sharp probe to our better understanding on the basic property of the corona. The launch of the first Chinese X-ray satellite Insight-HXMT has large detection area at hard X-rays which provide almost unique chance to move further in this research field. We report the first detection of the corona cooling by Insight-HXMT from single short type-I burst showing up during {\bf flare} of 4U 1636-536. This type-I X-ray burst has a duration of $\sim$13 seconds and hard X-ray shortage is detected with significance 6.2~$σ$ in 40-70 keV. A cross-correlation analysis between the lightcurves of soft and hard X-ray band, shows that the corona shortage lag the burst emission by 1.6 $\pm$1.2~s. These results are consistent with those derived previously from stacking a large amount of bursts detected by RXTE/PCA within a series of {\bf flares} of 4U 1636-536. Moreover, the broad bandwidth of Insight-HXMT allows as well for the first time to infer the burst influence upon the continuum spectrum via performing the spectral fitting of the burst, which ends up with the finding that hard X-ray shortage appears at around 40 keV in the continuum spectrum. These results suggest that the evolution of the corona along with the outburst{\bf /flare} of NS XRB may be traced via looking into a series of embedded type-I bursts by using Insight-HXMT.
Insight-HXMT observations on thermonuclear X-ray bursts from 4U~1608--52 in the low/hard state: the energy-dependant hard X-ray deficit and cooling saturation of the corona
Mapping the Contracting Corona in GS 1354-64 with Insight-HXMT and XRISM: Evolving X-ray Lags and Quenched Reflection across a Complete State Transition
South-Western Institue For Astronomy Research, Yunnan University（云南大学西南天文研究所）；Key Laboratory of Survey Science of Yunnan Province, Yunnan University（云南大学云南省测绘科学重点实验室）；Department of Astronomy, School of Physics and Astronomy, Yunnan University（云南大学物理与天文学院天文学系）；School of Physics and Astronomy, Sun Yat-Sen University（中山大学物理与天文学院）；Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文中心）；Department of Physics and Electronics, Christ University（克里斯特大学物理与电子系）；Institut für Astronomie und Astrophysik, Eberhard-Karls Universität Tübingen（蒂宾根大学天文与天体物理研究所）；New York University Abu Dhabi（纽约大学阿布扎比分校）；Center for Astrophysics and Space Science (CASS), New York University Abu Dhabi（纽约大学阿布扎比分校天体物理学与空间科学中心）；Xinjiang Astronomical Observatory, Chinese Academy of Sc（中国科学院新疆天文台）
Broad-band spectral-timing: simultaneous NICER and HXMT observations reveal an anticorrelation between the softest and hardest X-ray fluxes in MAXI J1820+070
Anton Pannekoek Institute for Astronomy（安东·潘内科克天文学研究所）；Dr. Karl Remeis-Observatory and Erlangen Centre for Astroparticle Physics（卡尔·雷米斯天文台与埃尔朗根高能粒子物理中心）；School of Physics and Technology, Wuhan University（武汉大学物理科学与技术学院）
New insight into the hard X-ray emission influenced by the type-\uppercase\expandafter{\romannumeral1} bursts observed by Insight-HXMT during outburst of 4U 1636--536
Dynamic disk-corona coupling during the state transition of Swift J1727.8-1613
Wuhan University（武汉大学）；Nanjing University（南京大学）；Shanghai Astronomical Observatory, Chinese Academy of Sciences (CAS)（中国科学院上海天文台）；Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文学中心）
Evolution of the Inner Accretion Flow in Swift J1727.8$-$1613 across Intermediate States: Insights from Broadband Spectral and Timing Analysis
Inter-University Centre for Astronomy and Astrophysics（天文与天体物理大学间中心）；Institute of Astronomy, National Tsing Hua University（国立清华大学天文研究所）；Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文学中心）；Department of Pure and Applied Physics, Guru Ghasidas Vishwavidyalaya (A Central University)（古鲁·加西达斯维什瓦维迪亚亚拉（一所中央大学）纯与应用物理系）
Investigating the Disk-Corona Relation in a Blue AGN Sample
我们从SDSS中编译了蓝色活动星系核样本，并研究了硬X射线与热光度之比与埃丁顿比和黑洞质量的关系。我们的样本包括240个射电宁静的塞弗特1星系和类星体。我们发现硬X射线亮度的分数（log $(L_{\rm 2-10 kev}/L_{\rm bol})$）随着爱丁顿比的增加而减小。我们还发现，硬X射线光度的分数是独立的黑洞质量的射电宁静活动星系核。log $(L_{\rm 2-10 kev}/L_{\rm bol})$随爱丁顿比的增加而减小的关系表明，X射线辐射热校正不是常数，从更大的样本支持Vasudevan和Fabian（2007）的结果。我们通过圆盘电晕蒸发/冷凝模型解释了我们的结果（Meyer et al. \cite{me200} ; Liu et al. 2002 a; Liu et al. 2007）。在这个模型的框架中，康普顿冷却在高吸积速率（以爱丁顿速率为单位）下对日冕的冷却变得有效，导致日冕气体冷凝到圆盘上。因此，当爱丁顿比增大时，日冕与盘的相对强度变弱。因此，硬X射线发射到盘发射的分数，因此到辐射热发射的分数在更高的爱丁顿比下更小。硬X射线光度与黑洞质量的独立性也可以用盘状日冕模型来解释，因为日冕结构和光度（以爱丁顿光度为单位）与黑洞的质量无关。
