A statistical study of fast magnetic reconnection in turbulent accretion disks and jets

L. Kadowaki, E. Pino, Tania E. Medina-Torrej'on
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引用次数: 3

Abstract

Fast magnetic reconnection events can play an important role in accretion disk systems. A potential model to explain the non-thermal very-high-energy (VHE) emission (from GeV to TeV) observed in black-hole binaries (BHBs) and Active Galatic Nuclei (AGNs) can be attributed to fast magnetic reconnection induced in the turbulent corona of accretion disks and/or jets. In this work, we will discuss the results of global general relativistic MHD (GRMHD) simulations of accretion disks around black holes, whose turbulence is naturally driven by MHD instabilities, such as the magnetorotational instability (MRI). We will also present studies of magnetic reconnection driven by kink instabilities inside jets employing special relativistic MHD (SRMHD) simulations. As we expect, our simulations reveal the development of a nearly steady-state turbulence driven by these instabilities. We have performed a detailed statistical analysis to identify the presence of current sheets in the turbulent regions of both the accretion flow and jet. We then determined the magnetic reconnection rates in these locations obtaining average reconnection velocities in Alfven speed units of the order of $0.01-0.7$, which are consistent with the predictions of the theory of turbulence-induced fast reconnection.
紊流吸积盘和喷流中快速磁重联的统计研究
快速磁重联事件在吸积盘系统中起着重要的作用。在黑洞双星(BHBs)和活动星系核(agn)中观测到的非热高能(VHE)发射(从GeV到TeV)的一个潜在模型可以归因于吸积盘和/或喷流的湍流日冕中诱导的快速磁重联。在这项工作中,我们将讨论全球广义相对论MHD (GRMHD)模拟黑洞周围吸积盘的结果,黑洞的湍流自然是由MHD不稳定性驱动的,例如磁旋不稳定性(MRI)。我们还将采用狭义相对论MHD (SRMHD)模拟,研究由射流内部扭结不稳定性驱动的磁重联。正如我们所期望的那样,我们的模拟揭示了由这些不稳定性驱动的近乎稳态湍流的发展。我们进行了详细的统计分析,以确定在吸积流和射流的湍流区域中存在电流片。然后,我们确定了这些位置的磁重联率,得到了以Alfven速度单位为0.01-0.7美元的平均重联速度,这与湍流诱导快速重联理论的预测一致。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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