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Liu, H. X.; Huang, Y.; Bu, Q. C.; Yu, W.; Yang, Z. X.; Zhang, L.; Kong, L. D.; Xiao, G. C.; Qu, J. L.; Zhang, S. N.; Zhang, S.; Song, L. M.; Jia, S. M.; Ma, X.; Tao, L.; Ge, M. Y.; Liu, Q. Z.; Yan, J. Z.; Ma, R. C.; Ren, X. Q.; Zhou, D. K.; Li, T. M.; Wu, B. Y.; Xu, Y. C.; Du, Y. F.; Fu, Y. C.; Xiao, Y. X.; Ding, G. Q.; Yu, X. X.
Astrophysical journal/The Astrophysical journal, 10/2022, Letnik: 938, Številka: 2Journal Article
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 ∼9.2 Hz (C) 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.
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JCR | SNIP | JCR | SNIP | JCR | SNIP | JCR | SNIP |
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in: SICRIS
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