Numerical investigations of the inner regions of black hole accretion discs

黑洞吸积盘内部区域的数值研究

• 批准号: 2738304
• 金额: --
• 依托单位: University of Oxford
• 依托单位国家: 英国
• 项目类别: Studentship
• 财政年份: 2023
• 资助国家: 英国
• 起止时间: 2023 至 无数据
• 项目状态: 未结题
• 来源: https://gtr.ukri.org/projects?ref=studentship-2738304
• 关键词: Numerical; investigations; inner; regions; black

Black hole accretion studies have history spanning some 54 years, going back to Donald Lynden-Bell's seminal paper (1969, Nature, 223, 690) in which he put forth the case that the then deeply mysterious quasars and active galactic nuclei were being powered by large black holes accreting gas from their surroundings in the form of a disc. In the ensuing half century, the field of black hole accretion disc studies has grown enormously on many fronts: observational, phenomenological modelling, numerical simulations and fundamental MHD processes. In particular, a steady-state model of accretion discs developed by Shakura and Sunyaev (1973, AA, 24, 347) has become a bedrock standard for both theory and observations. It combines both dynamical and radiation physics. Because of Shakura-Sunyaev theory applies to "thin discs," in which the vertical scale height is much less than the radial extent of interest, direct numerical study of such (turbulent) discs has been very difficult. In fact, the theory itself has never been verified directly, even though it is widely used. We are now in a position where this has become possible, in no small part because of the availability of state-of-the-art hardware and code development. In this thesis, which is designed to be a detailed study of the accretion flow near the innermost edge of black hole accretion discs, we will set up a suite of test problems to explicitly test Shakura-Sunyaev theory as well to explore more generally how the theory breaks down, as we know it must at some point. The observational setting in which this will be done is the rapidly growing field of tidal disruption events, or TDEs. This is an event that occurs when a star approaches a massive black hole at the centre of its galaxy in such a way that it is tidally torn apart. While some stellar debris invariably escapes, some also remains behind, and in its later evolutionary stages forms a time-dependent accretion disc whose emission is potentially ripe with information about the central black hole. The computational tool that will be used to study this problem is the Athena ++ code, developed by Prof James Stone and his co-workers at the IAS in Princeton. The first part of this thesis will be to use Athena ++ in its full radiative mode to study time dependent disc accretion in a set of controlled problems. The code is remarkable in that it is fully relativistic, MHD, and allows radiation to be included self-consistently not just in a post-processing sense. We benefit greatly from the additional presence of Prof Stone on this project, who has agreed to become involved at a hands-on level, so that technical details of setting up and running the code on the appropriate cluster can be done with maximum efficiency. The impact of this work promises to be enormous, bearing upon both fundamental disc theory and observation, the disc spectrum being an integral part of the calculation itself. The primary application will be to the light curves of TDEs. This includes such problems as the Lightman-Eardley Instability, a coupling between the disc turbulence and the radiative heating whose role in disc evolution is still not fully understood. This study has the numerical resolution and radiation physics capabilities to investigate this problem at a far higher level than previous studies. We shall also investigate the effect of magnetic field geometry, especially its role in setting the overall evolutionary behaviour of the disc, which is important for understanding when an MHD jet emerges from the inner regions and when it does not. A second major part of this thesis will be the investigation of the flow within what is normally considered the inner edge of the disc. Black hole discs extend down toward smaller and smaller radii until at some point, still well outside of the event horizon, the circular orbits become unstable. This transition radius is known as the innermost stable

黑洞吸积研究的历史跨越了54年，可以追溯到唐纳德·林登-贝尔的开创性论文（1969，自然，223，690），他提出了当时非常神秘的类星体和活动星系核是由大型黑洞以圆盘的形式从周围吸积气体提供动力的情况。在随后的半个世纪里，黑洞吸积盘的研究在许多方面都取得了巨大的进展：观测、唯象建模、数值模拟和基本的MHD过程。特别是由Shakura和Sunyaev（1973，AA，24，347）开发的吸积盘的稳态模型已经成为理论和观测的基础标准。它结合了动力学和辐射物理学。由于Shakura-Sunyaev理论适用于“薄圆盘”，其中垂直尺度高度远小于感兴趣的径向范围，因此对这种（湍流）圆盘的直接数值研究非常困难。事实上，该理论本身从未被直接验证过，尽管它被广泛使用。我们现在已经能够做到这一点，这在很大程度上是因为有了最先进的硬件和代码开发。在这篇论文中，这是一个详细的研究黑洞吸积盘的最里面的边缘附近的吸积流，我们将建立一套测试问题，明确测试Shakura-Sunyaev理论以及更一般地探索如何理论崩溃，因为我们知道它必须在某些时候。观测环境中，这将是这样做的是迅速增长的领域的潮汐中断事件，或TDEs。当一颗星星接近其星系中心的一个大质量黑洞时，它会被潮汐撕裂。虽然一些恒星碎片总是逃脱，但也有一些留在后面，并在其后期演化阶段形成一个依赖时间的吸积盘，其发射可能是关于中心黑洞的信息。将用于研究这个问题的计算工具是Athena ++代码，由普林斯顿IAS的James Stone教授和他的同事开发。本论文的第一部分将利用Athena ++的全辐射模式来研究一系列受控问题中的含时盘吸积。该代码是显着的，因为它是完全相对论性的，MHD，并允许辐射包括自洽不只是在后处理的意义。我们从Stone教授在这个项目中的额外参与中受益匪浅，他同意亲自参与，以便在适当的集群上设置和运行代码的技术细节可以以最高的效率完成。这项工作的影响将是巨大的，影响到基本的光盘理论和观测，光盘光谱是计算本身的一个组成部分。主要应用将是TDE的光变曲线。这包括像莱特曼-厄德利不稳定性（Lightman-Eardley Instability）这样的问题，它是圆盘湍流和辐射加热之间的耦合，其在圆盘演化中的作用仍然没有完全理解。这项研究具有数值分辨率和辐射物理能力，可以在比以前的研究更高的水平上研究这个问题。我们还将研究磁场几何形状的影响，特别是它的作用，在设置的整体进化行为的光盘，这是很重要的了解时，磁流体射流出现从内部区域，当它不。本论文的第二个主要部分是研究通常被认为是圆盘内边缘的流动。黑洞圆盘向下延伸，半径越来越小，直到在某个点，仍然在视界之外，圆形轨道变得不稳定。这个过渡半径被称为最内层的稳定半径