On high-energy particles in accretion disk coronae of supermassive black holes: implications for MeV gamma rays and high-energy neutrinos from AGN cores
Yoshiyuki Inoue, Dmitry Khangulyan, Susumu Inoue, Akihiro Doi
备注：
24 pages, 10 figures, accepted for publication in ApJ
Recent observations with ALMA have revealed evidence for non-thermal synchrotron emission from the core regions of two nearby Seyfert galaxies. This suggests that the coronae of accretion disks in active galactic nuclei (AGNs) can be conducive to the acceleration of non-thermal electrons, in addition to the hot, thermal electrons responsible for their X-ray emission through thermal Comptonization. Here we investigate the mechanism of such particle acceleration, based on observationally inferred parameters for AGN disk coronae. One possibility to account for the observed non-thermal electrons is diffusive shock acceleration, as long as the gyrofactor $η_g$ does not exceed $\sim10^6$. These non-thermal electrons can generate gamma rays via inverse Compton scattering of disk photons, which can appear in the MeV band, while those with energies above $\sim100$ MeV would be attenuated via internal $γγ$ pair production. The integrated emission from all AGNs with thermal and non-thermal Comptonization can reproduce the observed cosmic background radiation in X-rays as well as gamma-rays up to $\sim 10$ MeV. Furthermore, if protons are accelerated in the same conditions as electrons and $η_g\sim30$, our observationally motivated model is also able to account for the diffuse neutrino flux at energies below 100-300 TeV. The next generation of MeV gamma-ray and neutrino facilities can test these expectations by searching for signals from bright, nearby Seyfert galaxies such as NGC 4151 and IC 4329A.
Gamma-ray and Neutrino Signals from Accretion Disk Coronae of Active Galactic Nuclei
为了解释活动星系核（AGN）的X射线谱，过去文献中广泛讨论了活动星系核日冕中的非热活动，如对级联模型。虽然1990年代的X射线和伽马射线观测不支持这种对级联模型，但最近对西弗特附近的毫米波观测证实了微弱的非热日冕活动的存在。此外，IceCube合作报告称，附近的Seyfert NGC 1068是他们10年调查中最热门的地点。这些证据足以再次深入研究活动星系核日冕的非热效应。本文总结了我们目前对活动星系核日冕的观测认识，并描述了活动星系核日冕如何产生高能粒子。我们还提供了无线电，X射线，兆电子伏的伽马射线和高能中微子观测来测试活动星系核日冕模型的方法。
Coupled Time-Dependent Proton Acceleration and Leptonic-Hadronic Radiation in Turbulent Supermassive Black Hole Coronae
Deutsches Elektronen-Synchrotron DESY（德国电子同步加速器）；National and Kapodistrian University of Athens（雅典国立卡波迪斯特里安大学）；Queen’s University（女王大学）；Arthur B. McDonald Canadian Astroparticle Physics Research Institute（阿瑟·B·麦克唐纳加拿大高能天体粒子物理研究所）；Perimeter Institute for Theoretical Physics（理论物理前沿研究所）
Turbulent AGN coronae as the origin of diffuse neutrinos up to PeV energies
School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）；Key laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education（现代天文学和天体物理学教育部重点实验室（南京大学））；Tianfu Cosmic Ray Research Center（天府宇宙线研究中心）
Fast X-ray Variability from the Coronae of Supermassive Black Holes
California Institute of Technology（加州理工学院）；University of Illinois at Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；Columbia University（哥伦比亚大学）；Clemson University（克莱姆森大学）
Diffuse neutrino flux from relativistic reconnection in AGN coronae
National and Kapodistrian University of Athens（雅典国立卡波帝斯特里安大学）；Institute of Accelerating Systems & Applications（加速系统与应用研究所）；Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Napoli（意大利国家核物理研究所（INFN）那不勒斯分部）；National Observatory of Athens（雅典国家天文台）；Columbia University（哥伦比亚大学）；Center for Computational Astrophysics, Flatiron Institute（计算天体物理学中心，平顿研究所）
Supermassive Black Hole Winds in X-rays: SUBWAYS V. Properties of hot coronae in quasars at intermediate redshift
INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna (OAS)（意大利国家天体物理研究所博洛尼亚天文物理与空间科学观测站）；Dipartimento di Fisica e Astronomia (DIFA), Università di Bologna（博洛尼亚大学物理与天文学系）；European Southern Observatory (ESO)（欧洲南方天文台）；Centro de Astrobiología (CAB), CSIC-INTA（西班牙国家科学技术研究委员会-国家航空航天技术研究所天体生物学中心）；Dipartimento di Matematica e Fisica, Università degli Studi Roma Tre（罗马第三大学数学与物理系）；Dep. of Physics and Astronomy, Clemson University（克莱姆森大学物理与天文学系）
Proton Acceleration by Collisionless Shocks in Supermassive Black Hole Coronae: Implications for High-Energy Neutrinos
The University of Osaka（大阪大学）；Institute of Laser Engineering, The University of Osaka（大阪大学激光工程研究所）；Shibaura Institute of Technology（芝浦工业大学）；RIKEN（理化学研究所）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), UTIAS, The University of Tokyo（东京大学宇宙线起源研究教育中心（WPI））
Can magnetic reconnection power neutrino emission from AGN coronae?
University of Colorado, Boulder（科罗拉多大学博尔德分校）；Center for Integrated Plasma Studies（综合等离子体研究中心）；JILA（JILA研究所）；National Institute of Standards and Technology（美国国家标准与技术研究院）；Department of Astrophysical and Planetary Sciences（天体物理与行星科学系）
Relations between phenomenological and physical parameters in the hot coronae of AGNs computed with the MoCA code
活动星系核中的初级X射线辐射被广泛认为是由于来自热电子日冕中吸积盘的热辐射的康普顿化。由此产生的光谱可以，在第一近似，与截止功率定律，光子指数和高能量翻转编码信息的X射线发射区域的物理性质建模。自从10 keV以上的X射线卫星发射以来，人们对活动星系核（$Γ$，E $_c$）的光子指数和高能曲率进行了大量的研究。然而，由于NuSTAR前所未有的高达79 keV的灵敏度，这两个可观测量的高精度测量仅在近年来才获得。我们的目的是推导之间的关系的唯象参数（$Γ$和E $_c$）和X射线发射区域（热日冕）的固有属性，即光学深度和温度。我们使用MoCA（Monte Carlo code for Comptonisation in Astrophysics）产生的合成光谱的情况下，活动星系核的M $_{BH}$ =1.5 $\times$ 10 $^8$ M $_{sun}$和吸积率为10%，然后比较它们与广泛使用的幂律模型与指数高能截止。我们提供了有关$Γ$和E $_c$与冠状电子的不透明度和温度的球形和板状冠的情况下的唯象关系。这些关系给出了一个定义良好的参数空间，其中完全包含观测值的起源。利用文献中引用的越来越多的高能量截止值，我们报告使用MoCA获得的物理量与使用通常采用的光谱康普顿化模型估计的物理量的比较。最后，我们讨论了不同的黑洞质量和吸积率对推导关系的影响。
AGN X-ray coronae at high luminosity: A broadband study of RBS 229 and PG 1407+265
Università degli Studi Roma Tre（罗马三大学）；ASI – Agenzia Spaziale Italiana（意大利航天局）；INAF – Osservatorio Astronomico di Roma（罗马天文台）；INAF – Osservatorio Astrofisico di Arcetri（阿切尔菲天文台）；INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（博洛尼亚天体物理与空间科学天文台）；Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Alma Mater Studiorum, Università degli Studi di Bologna（博洛尼亚大学）
California Institute of Technology（加州理工学院）；Clemson University（克莱姆森大学）；Flatiron Institute（平顿研究所）；INAF, Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天文与空间科学观测站）；Montana State University（蒙大拿州立大学）；Università di Bologna（博洛尼亚大学）；INAF–OAA, Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所-阿切特里天文台）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Columbia University（哥伦比亚大学）
Electron-positron cascade in magnetospheres of supermassive Kerr black holes and the origin of relativistic AGN jets
University of Kansas（堪萨斯大学）；Massachusetts Institute of Technology（麻省理工学院）；Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文中心）
High-Energy Neutrinos from Magnetized Coronae of Active Galactic Nuclei and Prospects for Identification of Seyfert Galaxies and Quasars in Neutrino Telescopes
