论文标题
关于AGN与GRMHD模拟的比较：I。SGR A*
On the Comparison of AGN with GRMHD Simulations: I. Sgr A*
论文作者
论文摘要
我们提出了使用电子温度或能量密度参数化的射手座A*附近银河中心发射的模型。这些模型包括受到两种元素一般相对论磁流失动力学（GRMHD）模拟的启发的模型，以及跨越粒子和磁能的电均电气的喷射动机处方。从这些模型中，我们计算光谱和图像，并根据其独特的观察特征对它们进行分类。某些模型产生形态和光谱特征，例如图像大小，次数凸起和低频频谱斜率与观测值兼容。具有与观察结果一致的光谱的模型产生最紧凑的图像，具有最突出的不对称光子环。在许多型号中，肢体明亮的流出也可见。在我们考虑的所有模型中，代表当前数据的模型最好的是当磁力大于热压时电子相对热的模型，但否则冷（即忽略有助于发射）。这项工作是一个系列的一部分，该系列还将“观察”模拟方法应用于M87和3C 279中超大型黑洞的近水压区域。
We present models of Galactic Center emission in the vicinity of Sagittarius A* that use parametrizations of the electron temperature or energy density. These models include those inspired by two-temperature general relativistic magnetohydrodynamic (GRMHD) simulations as well as jet-motivated prescriptions generalizing equipartition of particle and magnetic energies. From these models, we calculate spectra and images and classify them according to their distinct observational features. Some models produce morphological and spectral features, e.g., image sizes, the sub-mm bump and low frequency spectral slope compatible with observations. Models with spectra consistent with observations produce the most compact images, with the most prominent, asymmetric photon rings. Limb brightened outflows are also visible in many models. Of all the models we consider, that which represents the current data the best is one in which electrons are relativistically hot when magnetic pressure is larger than the thermal pressure, but cold (i.e., negligibly contributing to the emission) otherwise. This work is part of a series also applying the "observing" simulations methodology to near-horizon regions of supermassive black holes in M87 and 3C 279.
