射电星系核心磁重联中中微子和伽马射线发射的数值模型

J. C. Rodr'iguez-Ram'irez, E. Pino, R. A. Batista
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引用次数: 2

摘要

非耀变体射电星系发射高能(VHE;>100 GeV)状态为探测黑洞吸积喷射系统中的粒子加速和发射过程提供了一个独特的视角。这些源的错位性质表明存在一种可能是强子起源的发射成分,并且位于核心区。本文认为射电星系BH吸积流中的湍流磁重联是宇宙射线(CR)加速和VHE发射的潜在机制。为了研究这种情况是否能够解释观测到的VHE数据,我们结合了三种数值技术来自洽地模拟吸积流环境和吸积流区域内cr和电磁级联的传播。在这里,我们将我们的方法应用于射电星系半人马座A,发现注入与磁重联功率一致的CRs部分重现了VHE数据,前提是吸积流对射电gev成分没有实质性贡献。相关的中微子发射峰值为$\sim10^{16}$ eV,比冰立方的最小通量低两个数量级。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Numerical models of neutrino and gamma-ray emission from magnetic reconnection in the core of radio-galaxies
Non-blazar radio-galaxies emitting in the very-high-energy (VHE; >100 GeV) regime offer a unique perspective for probing particle acceleration and emission processes in black hole (BH) accretion-jet systems. The misaligned nature of these sources indicates the presence of an emission component that could be of hadronic origin and located in the core region. Here we consider turbulent magnetic reconnection in the BH accretion flow of radio-galaxies as a potential mechanism for cosmic-ray (CR) acceleration and VHE emission. To investigate if this scenario is able to account for the observed VHE data, we combine three numerical techniques to self-consistently model the accretion flow environment and the propagation of CRs plus electromagnetic cascades within the accretion flow zone. Here we apply our approach to the radio-galaxy Centaurus A and find that injection of CRs consistent with magnetic reconnection power partially reproduce the VHE data, provided that the accretion flow makes no substantial contribution to the radio-GeV components. The associated neutrino emission peaks at $\sim10^{16}$ eV and is two orders of magnitude below the minimum IceCube flux.
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