Timing and Spectral Analysis of the Black Hole X-Ray Binary MAXI J1803-298 with Insight-HXMT Data  

作　　者：Ying-Chen Xu Jin-Lu Qu MMéndez Rui-Can Ma Long Ji Liang Zhang Yue Huang Qing-Cui Bu Li-Ming Song 

机构地区：[1]Key Laboratory of Particle Astrophysics,Institute of High Energy Physics,Chinese Academy of Sciences,Beijing 100049,China [2]University of Chinese Academy of Sciences,Chinese Academy of Sciences,Beijing 100049,China [3]Kapteyn Astronomical Institute,University of Groningen,P.O.BOX 800,9700 AV Groningen,The Netherlands [4]Dongguan Neutron Science Center,Dongguan 523808,China [5]School of Physics and Astronomy,Sun Yat-Sen University,Zhuhai 519082,China [6]Institut für Astronomie und Astrophysik,Kepler Center for Astro and Particle Physics,Eberhard Karls Universität,Sand 1,D-72076 Tübingen,Germany

出　　处：《Research in Astronomy and Astrophysics》2024年第6期209-224,共16页天文和天体物理学研究（英文版）

基　　金：supported by the National Key R&D Program of China(2021YFA0718500);the National Natural Science Foundation of China(NSFC,Grant No.12133007);partially supported by the International Partnership Program of Chinese Academy of Sciences(Grant No.113111KYSB20190020)。

摘　　要：We present a comprehensive analysis of the 2021 outburst of MAXI J1803–298 utilizing observations of the Insight-Hard X-ray Modulation Telescope(Insight-HXMT)spanning from the low hard state to the high soft state.Within the Insight-HXMT data set,compared to the previous work,we identify a more prolonged presence of typeC quasi-periodic oscillations(QPOs)with centroid frequencies ranging from~0.16 to 6.3 Hz,which present correlations with the hardness ratio and the photon index of the Comptonized component.For QPO frequencies less than~2 Hz,the QPO phase lags are hard(photons of 10–19 keV arrive later than those of 1–4 keV),while at higher frequencies,the lags become soft at and above~4 Hz.Furthermore,the spectra in all Insight-HXMT observations consist of a multi-color blackbody component and a Comptonized component,as commonly observed in classical black hole X-ray binaries.We analyze state transitions and the evolution of accretion geometry in this work.The fitted inner disk radius increases abnormally during the low hard state,hypothesized to result from the corona condensing onto the inner disk.Additionally,two significant drops in flux are observed during the soft intermediate state,maybe implying changes in the corona/jet and the disk,respectively.

关 键 词：X-rays:binaries ACCRETION accretion disks stars:black holes 

分 类 号：P145.8[天文地球—天体物理] P172.2[天文地球—天文学]