The recent 230 GHz observations from the Event Horizon Telescope collaboration can image the innermost structure of the M87 galaxy showing the shadow of the black hole, a photon ring, and a ring-like structure that agrees with thermal synchrotron emission from the accretion disc. However, at lower frequencies, M87 is characterized by a large-scale jet with clear signatures of nonthermal emission. It is necessary to explore the impacts of nonthermal emission on black hole shadow images and extended jets, especially at lower frequencies. In this study, we aim to compare models with different electron heating prescriptions and investigate how these prescriptions and nonthermal electron distributions may affect black hole shadow images and the broadband spectrum energy distribution (SED) function. We performed general relativistic radiative transfer (GRRT) calculations in various two-temperature general relativistic magnetohydrodynamic (GRMHD) models utilizing different black hole spins and different electron heating prescriptions coupled with different electron distribution functions (eDFs). Through a comparison with GRRT images and SEDs, we found that when considering a variable kappa eDF, the parameterized prescription of the R-beta model with Rh = 1 is similar to the model with electron heating in the morphology of images, and the SEDs at a high-frequency. This is consistent with previous studies using the thermal eDF. However, the nuance between them could be differentiated through the diffuse extended structure seen in GRRT images, especially at a lower frequency, and the behavior of SEDs at low frequency. The emission from the nearside jet region is enhanced in the reconnection heating case and it will increase the contribution from the regions with stronger magnetization is included or if the magnetic energy contribution to kappa eDF mainly in the magnetized regions is considered.
The imitation game (r)evolutions: $Q$-star effective shadow from GRMHD analysis
University of Science and Technology of China（中国科学技术大学）；Universidad de Guadalajara（瓜达拉哈拉大学）；Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México（墨西哥国立自治大学核科学研究所）；Universidade de Aveiro（阿威罗大学）；Centre for Research and Development in Mathematics and Applications (CIDMA)（数学与应用研究发展中心 (CIDMA)）；Universidade Federal do Pará（帕拉联邦大学）；Interdisciplinary Center for Theoretical Study, University of Science and Technology of China（中国科学技术大学理论交叉研究中心）；Peng Huanwu Center for Fundamental Theory（彭桓武理论物理中心）
Impacts of radiative cooling on the images of a black hole shadow and extended jets in two-temperature GRMHD simulations
Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交大李政道学院）；School of Physics and Astronomy, Shanghai Jiao Tong University（上海交通大学物理与天文学院）；Key Laboratory for Particle Astrophysics and Cosmology (MOE) and Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai Jiao Tong University（上海交通大学粒子天体物理与宇宙学教育部重点实验室及粒子物理与宇宙学上海市重点实验室）；Institut für Theoretische Physik, Goethe Universität（法兰克福大学理论物理研究所）；Institute of Fundamental Physics and Quantum Technology, School of Physical Science and Technology, Ningbo University（宁波大学物理科学与技术学院基础物理与量子技术研究所）；Institut für Theoretische Physik und Astrophysik, Universität Würzburg（维尔茨堡大学理论与天体物理研究所）
GRMHD accretion beyond the black hole paradigm: Light from within the shadow
Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Instituto de Astrofísica de Andalucía-CSIC（安达卢西亚天体物理研究所-CSIC）；Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo（圣保罗大学天文、地球物理与大气科学研究所）；International Centre for Space and Cosmology, Ahmedabad University（艾哈迈达巴德大学国际空间与宇宙学中心）
Observational appearance of inefficient accretion flows and jets in 3D GRMHD simulations: Application to Sgr~A*
辐射低效吸积流（RIAF）被认为是星系暗核中超大质量黑洞（SMBH）的动力来源。这种黑洞通常伴随着平谱射电核心，表明存在适度相对论性喷流。其中一个最受约束的RIAF与银河系中心的SMBH有关，Sgr A *。由于RIAF中的等离子体只有弱碰撞，这些系统的动力学和辐射特性是非常不确定的。在这里，我们要研究的影响，不同的电子温度的外观吸积流和喷流。使用3-D GRMHD吸积流模拟，我们使用射线追踪方法来预测RIAF的光谱和射电图像，允许不同的电子加热机制在模拟的流入和流出部分。我们发现，电子温度的微小变化可能导致喷流和吸积流的相对优势的显着差异。应用到Sgr A * 表明，该源的无线电频谱和大小可以很好地再现与模型，其中电子更有效地加热的射流。X射线发射对喷流和盘中的电子加热机制敏感，因此X射线观测对吸积流和喷流的电子温度和几何形状有很强的约束。对于Sgr A *，射流模型还预测了显著的频率依赖性核心偏移，一旦精确测量，该偏移可以对模型施加独立的约束。我们的结论是，更复杂的电子分布函数的模型是至关重要的约束GRMHD模拟与实际观测。对于Sgr A *，射电外观很可能是由流出的等离子体主导的。尽管如此，在最高的射频，事件视界的阴影应该仍然可以通过未来的甚长基线干涉测量观测探测到。
Probing anisotropic particle acceleration and limb-brightening in Centaurus A's jet
University of Würzburg（维尔茨堡大学）；Goethe Universität Frankfurt（法兰克福歌德大学）；Shanghai Jiao Tong University（上海交通大学）；Radboud University（拉德堡德大学）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）
Resolving Nearby Supermassive Black Holes with the Black Hole Explorer
Yamaguchi University（山口大学）；Heriot-Watt University（赫瑞-瓦特大学）；Massachusetts Institute of Technology Haystack Observatory（麻省理工学院海斯观测站）；National Astronomical Observatory of Japan（日本国立天文台）；Black Hole Initiative at Harvard University（哈佛大学黑洞倡议项目）
Impact of Equation of State on Black Hole Accretion Flows and Radiative Properties
Tsung-Dao Lee Institute, Shanghai Jiao-Tong University（上海交大李政道研究所）；Institute of Fundamental Physics and Quantum Technology, School of Physical Science and Technology, Ningbo University（宁波大学物理科学与技术学院基础物理与量子技术研究所）；Zhejiang Key Laboratory of Extreme Universe（浙江极端宇宙重点实验室）；School of Physics & Astronomy, Shanghai Jiao-Tong University（上海交通大学物理与天文学院）；Key Laboratory for Particle Physics, Astrophysics and Cosmology, Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai Jiao-Tong University（上海交通大学粒子物理、天体物理与宇宙学重点实验室）；Institut für Theoretische Physik, Goethe Universität（法兰克福歌德大学理论物理研究所）；Mullard Space Science Laboratory, University College London（伦敦大学学院穆拉德空间科学实验室）；Institut für Theoretische Physik und Astrophysik, Universität Würzburg（维尔茨堡大学理论与天体物理研究所）
