发表机构
College of Charleston; University of Southampton; University of California at Santa Barbara（查尔斯顿学院; 南安普顿大学; 加州大学圣塔芭芭拉分校）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究建立了一个辐射压主导的翘曲吸积盘的半解析模型，自洽连接盘翘曲、质量流入、风与能量输运，并确定了盘变为对流的半径，重现了数值模拟结果。
AI 中文摘要
高红移处发现数十亿太阳质量黑洞对任何标准爱丁顿极限增长模型提出了挑战。先前的研究表明，对流吸积盘可以通过间歇性吸积来解释这些早期黑洞的形成。研究还表明，如果黑洞的吸积盘与黑洞自旋轴错位，吸积盘在特定半径内可能变为对流的。虽然翘曲和错位的吸积盘已在数值模拟中探索，但目前尚无完全或半解析框架能自洽地连接超爱丁顿状态下的盘翘曲、质量流入、风以及能量输运。在本工作中，我们从质量、能量和角动量的耦合守恒方程出发，建立了辐射压主导的翘曲吸积盘的第一性原理半解析模型。我们得到了径向速度和面密度的分布，这些分布明确考虑了盘翘曲和质量损失，并确定了盘变为对流时的半径。我们探讨了黑洞自旋、错位角和粘度的变化，重现了数值研究的相关结果。
英文摘要
The discovery of billion solar mass black holes at high redshift challenges any standard Eddington-limited growth model. Previous work has shown that an advective accretion disk can account for these early black holes with episodic accretion. It has also been shown that if the accretion disk of a black hole is misaligned from the spin axis of the black hole, the disk can become advective within a certain radius. While warped and misaligned accretion disks have been explored in numerical simulations, there is no fully or semi-analytic framework that self-consistently connects disk warp, mass inflow, winds, and energy transport in the super-Eddington regime. In this work, we develop a first-principles semi-analytic model of a radiation-pressure-dominated, warped accretion disk, starting from the coupled conservation equations for mass, energy, and angular momentum. We find profiles for the radial velocity and surface density that explicitly account for disk warping and mass loss and determine the radius at which the disk becomes advective. We explore changes with black hole spin, misalignment angle and viscosity, reproducing relevant results from numerical studies.
