{
  "id": "2208.07066",
  "version": "v1",
  "published": "2022-08-15T08:28:31.000Z",
  "updated": "2022-08-15T08:28:31.000Z",
  "title": "Transitions and Origin of the Type-B Quasi-Periodic Oscillation in the Black Hole X-ray Binary MAXI~ J1348--630",
  "authors": [
    "H. X. Liu",
    "Y. Huang",
    "Q. C. Bu",
    "W. Yu",
    "Z. X. Yang",
    "L. Zhang",
    "L. D. Kong",
    "G. C. Xiao",
    "J. L. Qu",
    "S. N. Zhang",
    "S. Zhang",
    "L. M. Song",
    "S. M. Jia",
    "X. Ma",
    "L. Tao",
    "M. Y. Ge",
    "Q. Z. Liu",
    "J. Z. Yan",
    "R. C. Ma",
    "X. Q. Ren",
    "D. K. Zhou",
    "T. M. Li",
    "B. Y. Wu",
    "Y. C. Xu",
    "Y. F. Du",
    "Y. C. Fu",
    "Y. X. Xiao",
    "G. Q. Ding",
    "X. X. Yu"
  ],
  "comment": "26 pages, 9 figures",
  "categories": [
    "astro-ph.HE"
  ],
  "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 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.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2022-08-15T08:28:31.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "black hole x-ray binary",
      "type-b quasi-periodic oscillation",
      "type-b qpo",
      "transitions",
      "power-law dominated power spectrum"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 26,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}