The role of magnetospheric current sheets in pair enrichment and ultra-high energy proton acceleration in M87*

IF 5.3 2区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS
S.I. Stathopoulos, M. Petropoulou, L. Sironi and D. Giannios
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Abstract

Recent advances in numerical simulations of magnetically arrested accretion onto supermassive black holes have shed light on the formation and dynamics of magnetospheric current sheets near the black hole horizon. By considering the pair magnetization σe in the upstream region and the mass accretion rate ṁ (in units of the Eddington mass accretion rate) as free parameters we estimate the strength of the magnetic field and develop analytical models, motivated by recent three-dimensional particle-in-cell simulations, to describe the populations of relativistic electrons and positrons (pairs) in the reconnection region. Applying our model to M87*, we numerically compute the non-thermal photon spectra for various values of σe. We show that pairs that are accelerated up to the synchrotron radiation-limited energy while meandering across both sides of the current sheet, can produce MeV flares with luminosity of ∼ 1041 erg s-1 — independent of σe — for a black hole accreting at ṁ=10-5. Pairs that are trapped in the transient current sheet can produce X-ray counterparts to the MeV flares, lasting about a day for current sheets with length of a few gravitational radii. We also show that the upstream plasma can be enriched due to photon-photon pair creation, and derive a new equilibrium magnetization of σe ∼ 103-104 for ṁ = 10-6 - 10-5. Additionally, we explore the potential of magnetospheric current sheets to accelerate protons to ultra-high energies, finding that while acceleration to such energies is limited by various loss mechanisms, such as synchrotron and photopion losses from the non-thermal emission from pairs, maximal proton energies in the range of a few EeV are attainable in magnetospheric sheets forming around supermassive sub-Eddington accreting black holes.
磁层电流片在M87*中对富集和超高能量质子加速中的作用
超大质量黑洞的磁阻吸积数值模拟的最新进展揭示了黑洞视界附近磁层流片的形成和动力学。通过考虑上游区域的对磁化σe和质量吸积率(以Eddington质量吸积率为单位)作为自由参数,我们估计了磁场的强度,并在最近的三维细胞内粒子模拟的激励下建立了解析模型,以描述重连接区域中相对论性电子和正电子(对)的居群。将该模型应用于M87*,对不同σe值下的非热光子光谱进行了数值计算。我们发现,当在电流片的两侧蜿蜒时,被加速到同步辐射限制能量的粒子对可以产生MeV耀斑,其亮度为~ 1041 erg s-1,与σe无关。被困在瞬态电流片中的对可以产生与MeV耀斑相对应的x射线,对于长度为几个引力半径的电流片来说,持续时间约为一天。我们还证明了上游等离子体可以由于光子-光子对的产生而富集,并推导出了一个新的平衡磁化σe ~ 103-104。此外,我们探索了磁层电流片将质子加速到超高能量的潜力,发现虽然加速到超高能量受到各种损失机制的限制,如同步加速器和光子对的非热辐射损失,但在超大质量亚爱丁顿吸积黑洞周围形成的磁层电流片可以达到几个EeV范围内的最大质子能量。
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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来源期刊
Journal of Cosmology and Astroparticle Physics
Journal of Cosmology and Astroparticle Physics 地学天文-天文与天体物理
CiteScore
10.20
自引率
23.40%
发文量
632
审稿时长
1 months
期刊介绍: Journal of Cosmology and Astroparticle Physics (JCAP) encompasses theoretical, observational and experimental areas as well as computation and simulation. The journal covers the latest developments in the theory of all fundamental interactions and their cosmological implications (e.g. M-theory and cosmology, brane cosmology). JCAP''s coverage also includes topics such as formation, dynamics and clustering of galaxies, pre-galactic star formation, x-ray astronomy, radio astronomy, gravitational lensing, active galactic nuclei, intergalactic and interstellar matter.
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