General relativistic magnetohydrodynamical simulations of the jet in M 87
General relativistic magnetohydrodynamical simulations of the jet in M 87
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DOI：
10.1051/0004-6361/201526630
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发表时间：
2015-10
影响因子：
6.5
通讯作者：
M. Mościbrodzka;H. Falcke;H. Shiokawa
中科院分区：
文献类型：
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作者：
M. Mościbrodzka;H. Falcke;H. Shiokawa
黑洞、吸积盘和射电喷流之间的联系可以通过将模型拟合到附近低光度星系核的观测结果来最好地约束，特别是研究得很好的源Sgr~A* 和M87。利用吸积超大质量黑洞耦合相对论等离子体喷流来模拟活动星系核的中心引擎，已经取得了相当大的进展。然而，一个单一的模型可以适用于一系列的黑洞质量和吸积率？在这里，我们想将最新的三维数值模型（最初是为银河系中心的Sgr A* 开发的）与M87中更强大、更大质量的黑洞的射电观测进行比较。我们后处理的三维GRMHD模型的喷气生产辐射效率低下的吸积流周围的旋转黑洞使用相对论辐射传输和射线跟踪产生模型的光谱和图像。作为这些模型的一个关键的新成分，我们允许在这些模拟中的质子-电子耦合取决于等离子体的磁性。我们发现M87的射电辐射可以用双温吸积流和热单温喷流的组合来描述。该模型符合M87射电核心的基本观测特征。最佳拟合模型的质量吸积速率为Mdot约9 × 10 ^{-3} MSUN/YR，总喷流功率为P_j \sim 10^{43} erg/s。1.3mm的发射是由靠近事件视界的反喷流产生的。它围绕黑洞阴影的特征性新月形状可以通过未来的毫米波VLBI实验来解决。通过对质量和吸积率的适当标度，成功地从银河系中心超大质量黑洞的模型导出了该模型。这表明该模型也可以适用于更大范围的低光度黑洞。
(abridged) The connection between black hole, accretion disk, and radio jet can be best constrained by fitting models to observations of nearby low luminosity galactic nuclei, in particular the well studied sources Sgr~A* and M87. There has been considerable progress in modeling the central engine of active galactic nuclei by an accreting supermassive black hole coupled to a relativistic plasma jet. However, can a single model be applied to a range of black hole masses and accretion rates? Here we want to compare the latest three-dimensional numerical model, originally developed for Sgr A* in the center of the Milky Way, to radio observations of the much more powerful and more massive black hole in M87. We postprocess three-dimensional GRMHD models of a jet-producing radiatively inefficient accretion flow around a spinning black hole using relativistic radiative transfer and ray-tracing to produce model spectra and images. As a key new ingredient to these models, we allow the proton-electron coupling in these simulations depend on the magnetic properties of the plasma. We find that the radio emission in M87 is well described by a combination of a two-temperature accretion flow and a hot single-temperature jet. The model fits the basic observed characteristics of the M87 radio core. The best fit model has a mass-accretion rate of Mdot approx 9x10^{-3} MSUN/YR and a total jet power of P_j \sim 10^{43} erg/s. Emission at 1.3mm is produced by the counter jet close to the event horizon. Its characteristic crescent shape surrounding the black hole shadow could be resolved by future millimeter-wave VLBI experiments. The model was successfully derived from one for the supermassive black hole in center of the Milky Way by appropriately scaling mass and accretion rate. This suggests the possibility that this model could also apply to a larger range of low-luminosity black holes.