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arXiv 2602.08710astro-ph.HE
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反磁流体动力学中磁片介导的重联是否真的在吸积流中驱动AGN中的耀斑中起重要作用？

Is plasmoid-mediated reconnection really important in accretion flows to drive flares in AGNs?

Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo（圣保罗大学天体物理学、地球物理学和大气科学研究所）；Princeton Gravity Initiative, Princeton University（普林斯顿大学引力倡议计划）；School of Natural Sciences, Institute for Advanced Study（高等研究院自然科学学院）；Center for Gravitation, Cosmology and Astrophysics, Department of Physics, University of Wisconsin–Milwaukee（威斯康星大学密尔沃基分校物理系引力、宇宙学天体物理中心）；Department of Astrophysical Sciences, Peyton Hall, Princeton University（普林斯顿大学天体物理科学系）；Escola de Artes, Ciências e Humanidades, Universidade de São Paulo（圣保罗大学艺术、科学与人文学院）；Department of Astronomy, University of Wisconsin-Madison（威斯康星大学麦迪逊分校天文系）

Giovani H. Vicentin, Elisabete M. de Gouveia Dal Pino, George N. Wong, Lia Medeiros, Grzegorz Kowal, James M. Stone, Alex Lazarian

备注：
8 pages, 3 figures. Proceedings of the High Energy Phenomena in Relativistic Outflows IX (HEPRO-IX)
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AI总结：

研究发现湍流介导的重联比磁片介导的重联快十倍，表明湍流驱动的重联是AGN中快速重联和耀斑的主要机制。

摘要：

基于高分辨率电阻性二维和三维磁流体动力学（MHD）模拟，我们的研究发现，这个问题的答案可能是否定的。相反，湍流介导的重联产生显著更快的重联速率—大约比所谓的通用率（V_rec/V_A ~ 0.01）高一个数量级。我们得出结论，在如吸积流和相对论喷流等系统中，湍流驱动的重联是快速重联和耀斑的主要机制。在这些环境中，湍流由如磁旋转不稳定性（MRI）、帕克-拉格朗日-泰勒不稳定性（PRTI）和电流驱动的膝状不稳定性（CDKI）等不稳定性驱动。最后，我们展示了吸积流的三维广义相对论MHD模拟，证实了湍流介导的重联在AGN系统中的关键作用。这些发现对理解这些极端环境中耀斑、粒子加速和偏振辐射的起源具有重要意义。

英文摘要：

Based on very high-resolution resistive 2D and 3D magnetohydrodynamical (MHD) simulations of current sheets, our findings suggest that the answer to this question is likely no. In contrast, turbulence-mediated reconnection yields significantly faster reconnection rates - about an order of magnitude higher than the so-called universal rate for plasmoid-mediated reconnection in MHD flows ($V_\text{rec}/V_A \sim 0.01$). We conclude that turbulence-driven reconnection is the dominant mechanism responsible for fast reconnection and flares in systems such as accretion flows and relativistic jets in Active Galactic Nuclei (AGNs). In these environments, turbulence is driven by instabilities such as the magneto-rotational instability (MRI), Parker-Rayleigh-Taylor instability (PRTI), and current-driven kink instability (CDKI). Finally, we present 3D General Relativistic MHD simulations of accretion flows that confirm the crucial role of turbulence-mediated reconnection in AGN systems. These findings have important implications for understanding the origin of flares, particle acceleration, and the production of polarized radiation in these extreme environments.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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