我们认为，活动星系核1 ES 1927+654中的外观变化事件以及随后X射线亮度下降3个数量级，是由吸积率的变化和磁滞盘（MAD）中的磁通量反转控制的。在改变外观事件之前，黑洞上的强磁通量通过Blandford-Znajek过程为X射线发射提供动力，而紫外线发射是由辐射效率低下的磁化圆盘产生的。平流事件，带来相反极性的通量，向内传播导致，首先，在紫外线/光学光度上升，然后，在X射线光度下降时，它到达黑洞。我们估计的时间尺度为磁通量平流，并发现观察到的时间尺度之间的变化看事件的开始和最小的X射线光度，$\approx200$天，是在协议所需的时间，以取消磁通量在MAD延伸到$\approx180\:r_g$。虽然通量反转事件可能是罕见的，由于大的流量比，质量是必要的，我们认为，活动星系核显示出异常高的X射线紫外线光度比是这样的事件的主要候选人。我们还认为，类似的事件可能会导致射流中断无线电响亮的对象。
英文摘要：
We argue that the changing-look event in the active galactic nucleus 1ES 1927+654, followed by a dip of 3 orders of magnitude in the X-ray luminosity, is controlled by a change in the accretion rate and an inversion of magnetic flux in a magnetically arrested disk (MAD). Before the changing-look event, strong magnetic flux on the black hole powers X-ray emission via the Blandford-Znajek process while the UV emission is produced by a radiatively inefficient magnetized disk. An advection event, bringing flux of the opposite polarity, propagates inward leading, first, to a rise in the UV/optical luminosity and, then, to a dip in the X-ray luminosity when it reaches the black hole. We estimate the timescale for magnetic flux advection and find that the observed timescale between the beginning of the changing-look event and the minimum in the X-ray luminosity, $\approx200$ days, is in agreement with the time needed to cancel the magnetic flux in a MAD extending to $\approx180\:r_g$. Although flux inversion events might be rare due to the large ratio of flux-to-mass that is needed, we argue that AGN showing an unusually high ratio of X-ray to UV luminosity are prime candidates for such events. We also suggest that similar events may lead to jet interruptions in radio-loud objects.
AT 2022csn: A Photometrically Peculiar Optical/UV Tidal Disruption Event in a Type II AGN
Tel Aviv University（特拉维夫大学）；University of Texas at Austin（德克萨斯大学奥斯汀分校）；University of Florida（佛罗里达大学）；Stanford University（斯坦福大学）；Kavli Institute for Particle Astrophysics & Cosmology, Stanford University（斯坦福大学卡弗里粒子天体物理与宇宙学研究所）；Center for Decoding the Universe, Stanford University（斯坦福大学解码宇宙中心）；NASA Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）
本研究报道了II型AGN中一颗测光特殊的光学/紫外TDE AT 2022csn，其为遥远且明亮的TDE，或属于低温高半径TDE新子群，提出TDE与AGN吸积盘相互作用等场景解释其特性。
Peculiar black hole accretion rates in AGN with highest star formation rates in the universe
Pouliasis et al（2022 b）研究了恒星形成率、黑洞吸积率和红移大于3.5的活动星系的恒星质量，发现恒星形成率在高恒星质量时趋于平稳，他们认为这是活动星系核反馈的证据。他们的数据显示，当活动星系核接近恒星形成率-恒星质量平面曲线的平坦化时，吸积率开始下降。我们描述的活动星系核反馈的性质负责这方面的强大FRII喷气机提高恒星形成率，但最终也引发了吸积从近爱丁顿率平流为主的转变。这些系统正处于一个戏剧性的转变的风口浪尖上，活动星系从强烈的增强到对恒星形成的巨大抑制，在这种方式下，与高红移的射电活动星系核和无喷流的活动星系核相比，低红移的射电活动星系核的斜率更陡。因此，我们认为，Pouliasis等人的数据构成了Singh等人（2021）预测的高红移天体，这些天体与Comerford等人（2020）所示的射电活动星系核的低红移行为有关。
Host galaxy morphologies of X-ray selected AGN: assessing the significance of different black hole fueling mechanisms to the accretion density of the Universe at z~1
Challenging the AGN scenario for JWST/NIRSpec LRD and non-LRD broad H$α$ emitters in light of non-detection of NIRCam photometric variability and X-ray
National Astronomical Observatory of Japan, National Institutes of Natural Sciences（日本国立天文台，国立自然科学研究院）；Institute for Cosmic Ray Research, The University of Tokyo（东京大学宇宙射线研究所）
NTT, Spitzer and Chandra spectroscopy of SDSSJ095209.56+214313.3: the most luminous coronal-line supernova ever observed, or a stellar tidal disruption event ?
