探索M 87中的辐射微观物理I. 总强度和宽带光谱
Probing radiation micro-physics in M 87 I. Total intensity and broad-band spectra
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中文总结 AI 辅助
研究利用下一代VLBI、ngEHT和ngVLA探索M 87辐射微观物理，通过广义相对论磁流体动力学模拟，计算不同电子加热和分布函数下的多频辐射特征，有望区分相关物理过程，为未来观测提供理论预期。
中文摘要 AI 辅助
下一代甚长基线干涉仪（VLBI）将在傅里叶空间提供密集采样并具有高信噪比，能可靠观测和成像M 87毫米波波段的微弱喷流结构。下一代事件视界望远镜（ngEHT）和下一代甚大阵列（ngVLA）能同时分辨和成像M 87超大质量黑洞周围的吸积流以及喷流发射和加速区。为探索这些能力并提供理论预期，进行了黑洞吸积和喷流发射的广义相对论磁流体动力学模拟。M 87是全电磁波段的观测目标，VLBI观测能分辨喷流结构。本文提供了可区分不同电子加热模型和粒子分布的可观测特征。利用广义相对论磁流体动力学对磁化等离子体向克尔黑洞的三维吸积进行模拟，计算不同电子加热和分布函数下的多频辐射特征。模拟结果表明，未来VLBI阵列在1×10⁴的动态范围和86 GHz至345 GHz频率范围内观测，有潜力区分湍流和磁重联电子加热以及电子分布函数。
英文摘要
Next generation Very Long Baseline Interferometers (VLBI) will provide dense sampling of the Fourier space together with high signal to noise ratios allowing to reliably observe and image faint jet structure in M 87 at mm-wavelength. The proposed next generation Event Horizon Telescope (ngEHT) and next generation Very Large Array (ngVLA) offers the unique capability to simultaneously resolve and image the accretion flow around the supermassive black hole in M 87 together with the jet launching and acceleration zone. In order to explore these capabilities and to provide theoretical expectations we perform general relativistic magnetohydrodynamic simulations of accretion on to black holes and jet launching. M 87 has been the target for multiple observations across the entire electromagnetic spectrum. Among these VLBI observations provide unique capability to resolve the jet structure down to several gravitational radii. In this work we provide possible observable signatures which will allow us to distinguish between different electron heating models and particle distributions. We use general relativistic magnetohydrodynamics and simulate the accretion of the magnetised plasma onto Kerr-black holes in 3D. The multi-frequency radiative signatures of these simulations are computed taking different electron heating and distribution functions into account. The results of our simulations show that with a dynamical range of $1\times 10^4$ and a frequency range from 86 GHz to 345 GHz observations with future VLBI arrays have the potential to tell turbulent and magnetic reconnection electron heating and the electron distribution function apart.
