论文标题
部分可观测时空混沌系统的无模型预测
Simulations of AGN Driven Galactic Outflow Morphology and Content
论文作者
论文摘要
储层计算是预测湍流的有力工具，其简单的架构具有处理大型系统的计算效率。然而，其实现通常需要完整的状态向量测量和系统非线性知识。我们使用非线性投影函数将系统测量扩展到高维空间，然后将其输入到储层中以获得预测。我们展示了这种储层计算网络在时空混沌系统上的应用，该系统模拟了湍流的若干特征。我们表明，使用径向基函数作为非线性投影器，即使只有部分观测并且不知道控制方程，也能稳健地捕捉复杂的系统非线性。最后，我们表明，当测量稀疏、不完整且带有噪声，甚至控制方程变得不准确时，我们的网络仍然可以产生相当准确的预测，从而为实际湍流系统的无模型预测铺平了道路。
Using a series of 3D relativistic hydrodynamical simulations of active galactic nuclei (AGN) we investigate how AGN power, a clumpy ISM structure, and AGN jet angle with respect to the galactic disk affect the morphology and content of the resulting galactic outflow. For low power AGN across three orders of magnitude of AGN luminosities ($10^{41}-10^{43}$ erg s$^{-1}$) our simulations did not show significant changes to either the morphology or total mass of the outflow. Changing the angle of the AGN jet with respect to the galaxy did show small changes in the total outflow mass of a factor of 2-3. Jets perpendicular to the galactic disk were created hot single phase outflows, while jets close to parallel with the disk created the outflows were multi-phase with equal parts warm and hot, and significant cold gas. Overall The final morphology of low power AGN outflows depends primarily on how the jet impacts and interacts with large, dense clouds in the clumpy ISM. These clouds can disrupt, deflect, split, or suppress the jet preventing it from leaving the galactic disk as a coherent structure. But for simulations with AGN luminosities $> 10^{44}$ erg s$^{-1}$ the ISM played a minor role in determining the morphology of the outflow with an undisrupted jet leaving the disk. The final morphology of AGN outflows is different for low power AGNs vs. high power AGNs with the final morphology of low power AGN outflows dependent on the ISM structure within the first kpc surrounding the AGN.
