Details

Autor(en) / Beteiligte

• 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.

Titel

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

Ist Teil von

• The Astrophysical journal, 2022-10, Vol.938 (2), p.108

Ort / Verlag

Philadelphia: The American Astronomical Society

Erscheinungsjahr

2022

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• 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.