QPOs and Orbital elements of X-ray binary 4U 0115+63 during the 2017 outburst observed by Insight-HXMT
Y. Z. Ding, W. Wang, P. Zhang, Q. C. Bu, C. Cai, X. L. Cao, C. Zhi, L. Chen, T. X. Chen, Y. B. Chen, Y. Chen, Y. P. Chen, W. W. Cui, Y. Y. Du, G. H. Gao, H. Gao… 展开作者
Y. Z. Ding, W. Wang, P. Zhang, Q. C. Bu, C. Cai, X. L. Cao, C. Zhi, L. Chen, T. X. Chen, Y. B. Chen, Y. Chen, Y. P. Chen, W. W. Cui, Y. Y. Du, G. H. Gao, H. Gao, M. Y. Ge, Y. D. Gu, J. Guan, C. C. Guo, D. W. Han, Y. Huang, J. Huo, S. M. Jia, W. C. Jiang, J. Jin, L. D. Kong, B. Li, C. K. Li, G. Li, T. P. Li, W. Li, X. Li, X. B. Li, X. F. Li, Z. W. Li, X. H. Liang, J. Y. Liao, B. S. Liu, C. Z. Liu, H. X. Liu, H. W. Liu, X. J. Liu, F. J. Lu, X. F. Lu, Q. L., L. T., R. C. Ma, X. Ma, B. Meng, Y. Nang, J. Y. Nie, J. L. Qu, X. Q. Ren, N. Sai, L. M. Song, X. Y. Song, L. Sun, Y. Tan, L. Tao, Y. L. Tuo, L. J. Wang, P. J. Wang, W. S. Wang, Y. S. Wang, X. Y. Wen, B. Y. Wu, B. B. Wu, M. Wu, G. C. Xiao, S. Xiao, S. L. Xiong, Y. P. Xu, R. J. Yang, S. Yang, Y. J. Yang, Q. B. Yi, Q. Q. Yin, Y. You, F. Zhang, H. M. Zhang, J. Zhang, P. Zhang, S. Zhang, S. N. Zhang, W. C. Zhang, W. Zhang, Y. F. Zhang, Y. H. Zhang, H. S. Zhao, X. F. Zhao, S. J. Zheng, Y. G. Zheng, D. K. Zhou
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14 pages, 9 figures, and 6 tables. This work has been submitted to MNRAS after the referee's report
In this paper, we presented a detailed timing analysis of a prominent outburst of 4U 0115+63 detected by \textit{Insight}-HXMT in 2017 August. The spin period of the neutron star was determined to be $3.61398\pm 0.00002$ s at MJD 57978. We measured the period variability and extract the orbital elements of the binary system. The angle of periastron evolved with a rate of $0.048\pm0.003$ $yr^{-1}$. The light curves are folded to sketch the pulse profiles in different energy ranges. A multi-peak structure in 1-10 keV is clearly illustrated. We introduced wavelet analysis into our data analysis procedures to study QPO signals and perform a detailed wavelet analysis in many different energy ranges. Through the wavelet spectra, we report the discovery of a QPO at the frequency $\sim 10$ mHz. In addition, the X-ray light curves showed multiple QPOs in the period of $\sim 16-32 $ s and $\sim 67- 200 $ s. We found that the $\sim100$ s QPO was significant in most of the observations and energies. There exist positive relations between X-ray luminosity and their Q-factors and S-factors, while the QPO periods have no correlation with X-ray luminosity. In wavelet phase maps, we found that the pulse phase of $\sim 67- 200 $ s QPO drifting frequently while the $\sim 16-32 $ s QPO scarcely drifting. The dissipation of oscillations from high energy to low energy was also observed. These features of QPOs in 4U 0115+63 provide new challenge to our understanding of their physical origins.
The prolific thermonuclear X-ray bursts from the outburst of the newly discovered millisecond pulsar MAXI~J1816--195 observed by Insight-HXMT and NICER
Timing and spectral studies of the Be/X-ray binary EXO 2030+375 using Insight-HXMT observations
Institut für Astronomie und Astrophysik, Universität Tübingen（蒂宾根大学天文与天体物理研究所）；ISDC Data Center for Astrophysics, Université de Genève（日内瓦大学天体物理学数据中心）；School of Physics and Astronomy, Sun Yat-Sen University（中山大学物理学院）；Institute of Astrophysics, Central China Normal University（华中师范大学天体物理研究所）
Hour time-scale QPOs in the X-ray and radio emission of LS I +61$^{\circ}$303
LS I +61 $^{\circ}$ 303是一颗X射线双星，每27天会有一次射电爆发。先前对该恒星系统的研究揭示了叠加在大型射电爆发上的射电微耀斑。本文介绍了利用Westerbork综合射电望远镜（WSRT）对LS I +61 $^{\circ}$ 303进行的2.2 GHz射电观测。使用各种定时分析方法，我们发现显着的准周期振荡（QPO）的55分钟稳定超过4天的持续时间。我们还使用从朱雀卫星获得的X射线波长的档案数据。我们在这里报告的第一次显着的X射线QPO约2小时，目前超过21小时的时间跨度。我们将我们的结果与之前报道的QPO观测结果进行了比较，得出的结论是QPO似乎与射电爆发有关，而与爆发的幅度无关。最后，在磁重联的背景下讨论了不同的QPO时间尺度。
Revisiting the 2021 Outburst of the BHC MAXI J1803-298 Using NICER, NuSTAR, and Insight-HXMT Data
South-Western Institute for Astronomy Research, Yunnan University（西南天体物理研究所，云南大学）；Indian Center for Space Physics（印度空间物理中心）；Institute of Astronomy, National Tsing Hua University（国立清华大学天文研究所）
LAXPC / AstroSat Study of ~ 1 and ~ 2 mHz Quasi-periodic Oscillations in the Be/X-ray Binary 4U 0115+63 During its 2015 Outburst
Be X射线双星4U 0115+63是由AstroSat上的大面积X射线正比计数器（LAXPC）仪器于2015年10月24日在巨大的II型爆发的高峰期间观测到的。突出的强度振荡在~ 1和~ 2兆赫的频率检测到的爆发。核光谱望远镜阵列（NuSTAR）在同一爆发期间进行的观测也显示出mHz的准周期振荡（QPO）。本文详细介绍了从LAXPC/AstroSat和NuSTAR观测中推导出的振荡及其特征。档案罗西X射线定时探测器（RXTE）/正比计数器阵列（PCA）的数据在2001-11年的分析也表明，在一些爆发和这些QPO的详细信息，这些QPO的存在。可能的模型来解释的起源的兆赫振荡进行检查。类似的QPO，虽然在更高的频率，已报告从其他中子星和黑洞来源，两者可能有一个共同的起源。讨论了解释内吸积盘不稳定性引起剧烈振荡的现有模型。
Return of 4U~1730--22 after 49 years silence: the spectral properties of the 2021/2022 outbursts observed by NICER and Insight-HXMT and the soft-to-hard state transition caused by the propeller effect
The bright black hole X-ray binary 4U 1543-47 during 2021 outburst. A clear state transition from super-Eddington to sub-Eddington accretion revealed by Insight-HXMT
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
