Report
Transitions and Origin of the Type-B Quasi-Periodic Oscillation in the Black Hole X-ray Binary MAXI~ J1348--630
| العنوان: | Transitions and Origin of the Type-B Quasi-Periodic Oscillation in the Black Hole X-ray Binary MAXI~ J1348--630 |
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| المؤلفون: | 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. |
| سنة النشر: | 2022 |
| المجموعة: | Astrophysics |
| مصطلحات موضوعية: | Astrophysics - High Energy Astrophysical Phenomena |
| الوصف: | 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 on the timing and spectral properties of the transitions of type-B QPOs in MAXI~J1348--630, observed by \emph{Insight}-HXMT. The fractional rms variability--energy relationship and energy spectra reveal that type-B QPOs probably originate from jet precession. Compared to weak power-law dominated power spectrum, when type-B QPO is present, the corresponding energy spectrum shows an increase in Comptonization component and the need for {\tt\string xillverCp} component, and a slight increase of height of the corona when using {\tt\string relxilllp} model. Therefore, we suggest that a coupled inner disk-jet region is responsible for the observed type-B QPOs transitions. The time scale for the appearance/disappearance of type-B QPOs is either long or short (seconds), which may indicate an instability of disk-jet structure. For these phenomena, we give the hypothesis that the Bardeen-Petterson effect causes disk-jet structure to align with BH spin axis, or that the disappearance of small-scale jets bound by the magnetic flux tubes lead to the disappearance of type-B QPOs. We observed three events regarding the B/C transitions, one of which occurred in a short time from $\sim 9.2$ Hz (C) to $\sim 4.8$ 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 disk changes insignificantly. We suggest that type-C QPOs probably originate from relatively stronger jets or corona. Comment: 26 pages, 9 figures |
| نوع الوثيقة: | Working Paper |
| DOI: | 10.3847/1538-4357/ac88c6 |
| URL الوصول: | http://arxiv.org/abs/2208.07066 |
| رقم الانضمام: | edsarx.2208.07066 |
| قاعدة البيانات: | arXiv |
| DOI: | 10.3847/1538-4357/ac88c6 |
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