Two-body relaxation in the EMRI-TDE disk model for Quasi Periodic Eruptions
Università degli Studi di Milano-Bicocca（米兰比可卡大学）；INFN, Sezione di Milano-Bicocca（意大利国家核物理研究所米兰比可卡分部）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）
Chiara Maria Allievi, Luca Broggi, Alberto Sesana, Matteo Bonetti
Quasi Periodic Eruptions (QPEs) are luminous bursts of soft X-rays recently discovered in galactic nuclei. They repeat on timescales of hours to weeks, superimposed to an otherwise stable quiescent X-ray level, consistent with emission from a radiatively efficient accretion flow around relatively low-mass MBHs. Although their physical origin is still debated, their quasi-periodicity naturally arises within the 'impact model', in which the X-ray bursts are generated by the interaction between an sBH or a star in a close orbit around the central MBH and the accretion disk formed by a tidal disruption event (TDE). While this model is consistent with the phenomenology of QPEs, it remains unclear whether such specific physical configurations are sufficiently commonto explain the observed QPE number density. We present the first end-to-end quantitative calculation of the expected QPE rate and abundance within the framework of the impact model. To this purpose, we combine the rates of TDEs and extreme mass-ratio inspirals (EMRIs) around MBHs spanning a range of masses masses. We employ the public code \textsc{PhaseFlow} to simulate seven systems with MBH masses between $10^5 M_\odot$ and $10^8 M_\odot$, each sourronded by a three-component population: one composed of $1M_\odot$ stars, and two consisting of sBHs with masses of $10M_\odot$ and $40 M_\odot$. Based on the emission constraints available in the literature, we restrict to sBH EMRIs on prograde orbit with eccentricity $e<0.5$ and inclination $ι<20^{\circ}$ with respect to the accretion disk. For stellar EMRIs the constraints instead arise from the requirement that the star avoid tidal disruption. We find that the predicted QPE number density spans the range $10^{-12} \rm Mpc^{-3}$ to $10^{-6} \rm Mpc^{-3}$, depending on the assumed orbital period interval and on the adopted eccentricity and inclination thresholds.
Massachusetts Institute of Technology（麻省理工学院）；Institute for Advanced Study（高等研究院）；Princeton University（普林斯顿大学）；Harvard University（哈佛大学）；New York University（纽约大学）
Discovery of Quasi-periodic Eruptions in the Tidal Disruption Event and Extreme Coronal Line Emitter AT2022upj: implications for the QPE/TDE fraction and a connection to ECLEs
Evolution of Quasi-Periodic Eruptions in the post-TDE Accretion Disk Perturbed by an Orbiting Star
Masaryk University（马萨里克大学）；Institute of Physics of the Czech Academy of Sciences（捷克科学院物理研究所）；Astronomical Institute of the Czech Academy of Sciences（捷克科学院天文研究所）
Ultraviolet Spectral Evidence for Ansky as a Slowly Evolving Featureless Tidal Disruption Event with Quasiperiodic Eruptions
University of Science and Technology of China（中国科学技术大学）；Guizhou University（贵州大学）；Anhui Normal University（安徽师范大学）；Yunnan University（云南大学）；University of California, Berkeley（加州大学伯克利分校）；University of Hong Kong（香港大学）；University of Arizona（亚利桑那大学）；California Institute of Technology（加州理工学院）；Wuhan University（武汉大学）
Multimessenger prospects of quasi-periodic eruptions
Institute of Theoretical Physics, Faculty of Mathematics and Physics（数学物理学院理论物理研究所）；Dipartimento di Fisica “A. Pontremoli”, Università degli Studi di Milano（米兰大学A. Pontremoli物理系）；Dipartimento di Fisica “G. Occhialini”, Università degli Studi di Milano-Bicocca（米兰比可卡大学G. Occhialini物理系）
Extreme Mass Ratio Inspirals in Light of Quasi-periodic Eruptions: Milli-Hertz Gravitational Wave Background
Tsung-Dao Lee Institute, Shanghai Jiao-Tong University（上海交大李政道研究所）；School of Physics & Astronomy, Shanghai Jiao-Tong University（上海交通大学物理与天文学院）；Department of Astronomy, School of Physics, Peking University（北京大学物理学院天文学系）；Kavli Institute for Astronomy and Astrophysics at Peking University（北京大学科维理天文与天体物理研究所）
Co-evolution of Nuclear Star Clusters and Massive Black Holes: Extreme Mass-Ratio Inspirals
Guangzhou University（广州大学）；Key Laboratory for Astronomical Observation and Technology of Guangzhou（广州市天文观测与技术重点实验室）；Astronomy Science and Technology Research Laboratory of Department of Education of Guangdong Province（广东省教育厅天文科学与技术研究实验室）；Universitat Politècnica de València（瓦伦西亚理工大学）；Max-Planck-Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）
A Torus Remnant Revealed by the Infrared Echo of Tidal Disruption Event AT 2019qiz: Implications for the Missing Energy and Quasiperiodic Eruption Formation
A positive period derivative in the quasi-periodic eruptions of ZTF19acnskyy
Massachusetts Institute of Technology（麻省理工学院）；Black Hole Initiative at Harvard University（哈佛大学黑洞倡议）；Columbia University（哥伦比亚大学）；New York University（纽约大学）；Centro de Astrobiología (CAB), CSIC-INTA（西班牙国家航空航天技术研究所与西班牙国家科学研究委员会天体生物学中心）；Universidad Adolfo Ibáñez（阿道夫·伊巴涅斯大学）；Millennium Nucleus on Transversal Research and Technology to Explore Supermassive Black Holes (TITANS)（探索超大质量黑洞跨学科研究与技术千年核）；Instituto de Estudios Astrofísicos（天体物理研究所）
Gravitational Wave Signatures of Quasi-Periodic Eruptions: LISA Detection Prospects for RX J1301.9+2747
The University of Hong Kong（香港大学）；Beijing Institute of Mathematical Sciences and Applications（北京数学科学研究所）；Tata Institute of Fundamental Research（塔塔基础研究所）
Even a precessing clock is right twice per orbit -- The super-periods of eRO-QPE2 and challenges for quasi-periodic eruption orbital models
Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理与空间研究所）；Black Hole Initiative at Harvard University（哈佛大学黑洞倡议）；Centro de Astrobiología (CAB), CSIC-INTA（西班牙国家航空航天技术研究所/西班牙高等科学研究理事会天体生物学中心）；Dipartimento di Fisica, Università degli Studi di Milano（米兰大学物理系）；Department of Physics and Columbia Astrophysics Laboratory, Columbia University（哥伦比亚大学物理系及哥伦比亚天体物理学实验室）；Center for Cosmology and Particle Physics, Physics Department, New York University（纽约大学物理系宇宙学与粒子物理中心）；School of Natural Sciences, Institute for Advanced Study（高等研究院自然科学学院）；Università degli Studi di Milano-Bicocca（米兰比可卡大学）；INFN, Sezione di Milano-Bicocca（意大利国家核物理研究所米兰比可卡分部）
QPEs from Warped Disk Collisions with EMRIs: Brightness-Recurrence Diagram and Gravitational-Wave Follow-up
Wuhan University（武汉大学）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），西班牙国家航空航天技术研究委员会-国家航空技术研究所）；University of Science and Technology of China（中国科学技术大学）；Tsung-Dao Lee Institute, Shanghai Jiao-Tong University（上海交大李政道研究所）；Shanghai Jiao-Tong University（上海交通大学）
Extreme mass ratio inspirals from the Hills mechanism, The eccentricity distribution of Hills EMRIs in LISA
Leiden University（莱顿大学）；Università degli Studi di Trento（特伦托大学）；Università degli Studi di Milano-Bicocca（米兰比可卡大学）；INFN - Sezione di Milano-Bicocca（意大利国家核物理研究所米兰比可卡分部）；Institute of Science and Technology Austria (ISTA)（奥地利科学技术研究院）
No evidence for a supermassive black hole binary in GSN 069
Tsung-Dao Lee Institute, Shanghai Jiao-Tong University（上海交大李政道研究所）；School of Physics & Astronomy, Shanghai Jiao-Tong University（上海交通大学物理与天文学院）；Institute for Astronomy, School of Physics, Zhejiang University（浙江大学物理学院天体物理研究所）；Center for Cosmology and Computational Astrophysics, Institute for Advanced Study in Physics, Zhejiang University（浙江大学物理学高等研究院宇宙学与计算天体物理中心）；Department of Astronomy, University of Science and Technology of China（中国科学技术大学天文系）
NICER observations reveal doubled timescales in Ansky's quasi-periodic eruptions (QPEs)
Millennium Nucleus on Transversal Research and Technology to Explore Supermassive Black Holes (TITANS)（探索超大质量黑洞横向研究与技术千年核心）；Millennium Institute of Astrophysics (MAS)（天体物理千年研究所）；Universidad Diego Portales（迭戈·波特莱斯大学）；European Southern Observatory（欧洲南方天文台）；Massachusetts Institute of Technology（麻省理工学院）；Universidad Adolfo Ibáñez（阿道夫·伊巴涅斯大学）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CSIC-INTA））；University of Geneva（日内瓦大学）；Peking University（北京大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Universidad de Chile（智利大学）
Science Opportunities of Wet Extreme Mass-Ratio Inspirals
Leicester International Institute, Dalian University of Technology（大连理工大学莱斯特国际学院）；Tsung-Dao Lee Institute, Shanghai Jiao-Tong University（上海交通大学李政道研究所）；School of Physics & Astronomy, Shanghai Jiao-Tong University（上海交通大学物理与天文学院）；Department of Astronomy, Tsinghua University（清华大学天文系）；CAS Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China（中国科学院星系与宇宙学重点实验室，中国科学技术大学天文系）；School of Astronomy and Space Sciences, University of Science and Technology of China（中国科学技术大学天文与空间科学学院）
