Transitions and Origin of the Type-B Quasi-periodic Oscillations in the Black Hole X-Ray Binary MAXI J1348-630

doi:10.3847/1538-4357/ac88c6

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	Transitions and Origin of the Type-B Quasi-periodic Oscillations in the Black Hole X-Ray Binary MAXI J1348-630
	Liu, H. X.1,2; Huang, Y.1,2; Bu, Q. C.3; Yu, W.1,2; Yang, Z. X.1,2; Zhang, L.1; Kong, L. D.1,2; Xiao, G. C.4; Qu, J. L.1,2; Zhang, S. N.1,2; Zhang, S.1,2; Song, L. M.1,2; Jia, S. M.1,2; Ma, X.1,2; Tao, L.1,2; Ge, M. Y.1,2; Liu, Q. Z.4; Yan, J. Z.4; Ma, R. C.1,2; Ren, X. Q.1,2; Zhou, D. K.1,2; Li, T. M.1,2; Wu, B. Y.1,2; Xu, Y. C.1,2; Du, Y. F.1,2; Fu, Y. C.1,2; Xiao, Y. X.1,2; Ding, G. Q.5 ; Yu, X. X.1,2
	2022-10-01
Source Publication	ASTROPHYSICAL JOURNAL
ISSN	0004-637X
Volume	938 Issue:2 Pages:108
Contribution Rank	5
Abstract	The fast transitions between different types of quasi-periodic oscillations (QPOs) are generally observed in black hole transient sources (BHTs). We present a detailed study of the timing and spectral properties of the transitions of type-B QPOs in MAXI J1348-630, observed by Insight-HXMT. The fractional rms variability-energy relationship and energy spectra reveal that type-B QPOs probably originate from jet precession. Compared to a weak power-law dominated power spectrum, when type-B QPOs are present, the corresponding energy spectrum shows an increase in the Comptonization component and the need for the xillverCp component, and a slight increase in the height of the corona when using the relxilllp model. Therefore, we suggest that a coupled inner disk-jet region is responsible for the observed type-B QPO transitions. The timescale for the appearance/disappearance of type-B QPOs is either long or short (seconds), which may indicate instability of the disk-jet structure. For these phenomena, we hypothesize that the Bardeen-Petterson effect causes the disk-jet structure to align with the BH spin axis or that the disappearance of small-scale jets bound by the magnetic flux tubes leads to the disappearance of type-B QPOs. We observed three events regarding the B/C transitions, one of which occurred over a short time period from similar to 9.2 Hz (C) to similar to 4.8 Hz (B). The energy spectral analysis for the other two transitions shows that when type-C QPO is present, the Comptonization flux is higher, the spectrum is harder, and the inner radius of the disk changes insignificantly. We suggest that type-C QPOs probably originate from relatively stronger jets or the corona.
DOI	10.3847/1538-4357/ac88c6
Indexed By	SCI
Language	英语
WOS Keyword	ACCRETION-EJECTION PARADIGM ; INSIGHT-HXMT ; ENERGY-DEPENDENCE ; BACKGROUND MODEL ; LIGHT CURVES ; PHASE LAGS ; GX 339-4 ; FREQUENCY ; VARIABILITY ; MODULATION
Funding Project	National Key R&D Program of China[2021YFA0718500] ; National Natural Science Foundation of China[11733009] ; National Natural Science Foundation of China[11673023] ; National Natural Science Foundation of China[U1838202] ; National Natural Science Foundation of China[U1838201] ; National Natural Science Foundation of China[U1938102] ; National Natural Science Foundation of China[U1938107] ; National Natural Science Foundation of China[U2038104] ; National Natural Science Foundation of China[U2031205] ; CAS Pioneer Hundred Talent Program ; Scientific and Technological Innovation Project of IHEP[Y7515570U1]
WOS Research Area	Astronomy & Astrophysics
WOS Subject	Astronomy & Astrophysics
WOS ID	WOS:000869457800001
Publisher	IOP Publishing Ltd
Funding Organization	National Key R&D Program of China ; National Natural Science Foundation of China ; CAS Pioneer Hundred Talent Program ; Scientific and Technological Innovation Project of IHEP
Citation statistics	Cited Times:16[WOS] [WOS Record] [Related Records in WOS]
Document Type	期刊论文
Identifier	http://ir.xao.ac.cn/handle/45760611-7/4928
Collection	射电天文研究室_脉冲星研究团组
Corresponding Author	Liu, H. X.
Affiliation	1.Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, 19B Yuquan Rd, Beijing 100049, Peoples R China 2.Chinese Acad Sci, Univ Chinese Acad Sci, Beijing 100049, Peoples R China 3.Eberhard Karls Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany 4.Chinese Acad Sci, Purple Mt Observ, Nanjing 210034, Peoples R China 5.Chinese Acad Sci, Xinjiang Astron Observ, 150,Sci 1 St, Urumqi 830011, Xinjiang, Peoples R China
Recommended Citation GB/T 7714	Liu, H. X.,Huang, Y.,Bu, Q. C.,et al. Transitions and Origin of the Type-B Quasi-periodic Oscillations in the Black Hole X-Ray Binary MAXI J1348-630[J]. ASTROPHYSICAL JOURNAL,2022,938(2):108.
APA	Liu, H. X..,Huang, Y..,Bu, Q. C..,Yu, W..,Yang, Z. X..,...&Yu, X. X..(2022).Transitions and Origin of the Type-B Quasi-periodic Oscillations in the Black Hole X-Ray Binary MAXI J1348-630.ASTROPHYSICAL JOURNAL,938(2),108.
MLA	Liu, H. X.,et al."Transitions and Origin of the Type-B Quasi-periodic Oscillations in the Black Hole X-Ray Binary MAXI J1348-630".ASTROPHYSICAL JOURNAL 938.2(2022):108.

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