Paper

{
  "raw_xml": "<entry>\n    <id>http://arxiv.org/abs/2602.23724v1</id>\n    <title>X-ray Quasi-Periodic Oscillations in Active Galactic Nuclei and Their Implications for the Changing Look Phenomenon</title>\n    <updated>2026-02-27T06:46:29Z</updated>\n    <link href='https://arxiv.org/abs/2602.23724v1' rel='alternate' type='text/html'/>\n    <link href='https://arxiv.org/pdf/2602.23724v1' rel='related' title='pdf' type='application/pdf'/>\n    <summary>X-ray timing of active galactic nuclei (AGN) provides a unique probe of gas accretion onto supermassive black holes (SMBHs). Quasi-periodic oscillations (QPOs), which trace gas dynamics in the strongly curved spacetime around SMBHs, are rare in AGN. These signals often are analogs of high-frequency QPOs occasionally seen in some black-hole X-ray binaries, and their scarcity in AGN can partly be attributed to the low frequencies expected for typical SMBH masses. Intriguingly, robust X-ray QPO detections in SMBH systems have so far been reported only in narrow-line Seyfert 1 galaxies (NLS1s) and tidal disruption events (TDEs). Here we report the discovery of a QPO candidate during the 2018 outburst of the changing-look AGN (CL-AGN) NGC 1566. Numerical simulations indicate that the disk epicyclic oscillations responsible for high-frequency QPOs are damped by magnetohydrodynamic turbulence unless the accretion flow is misaligned and/or eccentric. In TDEs, the stellar debris stream is naturally misaligned with the SMBH spin, while NLS1s may host misaligned disks due to their youth. Motivated by the QPO candidate in NGC 1566, we propose that CL-AGN accretion is also misaligned -- potentially fueled by captured, free-falling broad-line region clouds. This model naturally explains why CL-AGN transition timescales are much shorter than the standard disk viscous timescale. This picture can be tested by searching for QPOs or quasi-periodic eruptions in other CL-AGN.</summary>\n    <category scheme='http://arxiv.org/schemas/atom' term='astro-ph.HE'/>\n    <published>2026-02-27T06:46:29Z</published>\n    <arxiv:comment>10 pages, 3 figures, 1 table, accepted to A&amp;A</arxiv:comment>\n    <arxiv:primary_category term='astro-ph.HE'/>\n    <author>\n      <name>Mouyuan Sun</name>\n      <arxiv:affiliation>XMU</arxiv:affiliation>\n    </author>\n    <author>\n      <name>Shuying Zhou</name>\n      <arxiv:affiliation>XMU</arxiv:affiliation>\n    </author>\n    <author>\n      <name>Jihong Liu</name>\n      <arxiv:affiliation>XMU</arxiv:affiliation>\n    </author>\n    <author>\n      <name>Ning Jiang</name>\n      <arxiv:affiliation>USTC</arxiv:affiliation>\n    </author>\n    <author>\n      <name>Zhen-Yi Cai</name>\n      <arxiv:affiliation>USTC</arxiv:affiliation>\n    </author>\n    <author>\n      <name>Hai-Cheng Feng</name>\n      <arxiv:affiliation>YNO</arxiv:affiliation>\n    </author>\n    <author>\n      <name>Hengxiao Guo</name>\n      <arxiv:affiliation>SHAO</arxiv:affiliation>\n    </author>\n    <author>\n      <name>Zhi-Xiang Zhang</name>\n      <arxiv:affiliation>QZNU</arxiv:affiliation>\n    </author>\n    <author>\n      <name>Qinbo Han</name>\n      <arxiv:affiliation>XMU</arxiv:affiliation>\n    </author>\n    <author>\n      <name>Juan Li</name>\n      <arxiv:affiliation>XMU</arxiv:affiliation>\n    </author>\n    <author>\n      <name>Linyue Jiang</name>\n      <arxiv:affiliation>XMU</arxiv:affiliation>\n    </author>\n    <author>\n      <name>Yu-Jing Xu</name>\n      <arxiv:affiliation>XMU</arxiv:affiliation>\n    </author>\n    <author>\n      <name>Junfeng Wang</name>\n      <arxiv:affiliation>XMU</arxiv:affiliation>\n    </author>\n    <author>\n      <name>Jun-Xian Wang</name>\n      <arxiv:affiliation>USTC</arxiv:affiliation>\n    </author>\n    <author>\n      <name>Yongquan Xue</name>\n      <arxiv:affiliation>USTC</arxiv:affiliation>\n    </author>\n  </entry>"
}