发表机构
Astroparticule et Cosmologie, CNRS; Université Paris Cité; Centre for mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven（法国国家科学研究中心天体粒子与宇宙学研究所; 巴黎西岱大学; 荷语鲁汶大学数学系数学等离子体天体物理中心）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究结合辐射动力学模拟与强子级联预测，区分黑洞冕伽马射线的轻子与强子贡献，发现轻子主导MeV波段，并获COSI可探测性及观测支持。
AI 中文摘要
冰立方（IceCube）探测到邻近西佛（Seyfert）星系发出的太电子伏特（TeV）中微子，若得到证实，则意味着伴随的伽马射线被电磁级联过程大幅再处理至兆电子伏特（MeV）能段，这为多信使中微子发射模型施加了约束。然而，伽马射线也可能由X射线冕中的初级非热电子产生，正如近期磁化湍流的辐射动力学模拟所显示的那样。为区分轻子与强子贡献，我们自洽地将这些模拟结果与强子诱导电磁级联的预测相结合。聚焦于NGC 4151，我们发现当非热电子尾携带电子能量的约5%或以上时，轻子通道主导MeV能段，并在约0.1 GeV以下与强子级联保持相当。轻子贡献可能被即将开展的康普顿光谱仪与成像仪（COSI）任务在软伽马射线波段探测到，而我们预测的强子成分则低于其灵敏度。我们还发现，同一非热电子群体可以同时解释宇宙X射线背景的0.1-1 MeV超出（通常归因于活动星系核）以及天鹅座X-1（Cygnus X-1）硬态下的MeV尾，这为我们的模型提供了观测支持。我们的结果为黑洞冕的多信使信号提供了基于其非热动力学物理的精细视角。
英文摘要
IceCube detections of TeV neutrinos from nearby Seyfert galaxies imply, if confirmed, that the accompanying gamma rays are substantially reprocessed down to the MeV range by electromagnetic cascades, which places multi-messenger constraints on neutrino emission models. However, gamma rays can also be produced by the primary nonthermal electrons of the X-ray corona, as recent radiative kinetic simulations of magnetized turbulence have shown. To disentangle the leptonic and hadronic contributions, we self-consistently combine results from these simulations with predictions for hadronically induced electromagnetic cascades. Focusing on NGC 4151, we find that the leptonic channel dominates the MeV band, and remains comparable to the hadronic cascade up to $\lesssim$0.1 GeV, when the nonthermal electron tail carries $\gtrsim5\%$ of the electron energy. The leptonic contribution may be detectable in soft gamma rays by the upcoming Compton Spectrometer and Imager (COSI) mission, whereas our predicted hadronic component falls below its sensitivity. We also find that the same nonthermal electron population can account for both the $0.1-1$ MeV excess of the cosmic X-ray background, generally attributed to AGNs, and the MeV tail of Cygnus~X-1 in the hard state, lending observational support to our model. Our results offer a refined view of multi-messenger signals from black-hole coronae, grounded in their nonthermal kinetic physics.
Comments10 pages, 4 figures, submitted to ApJL
