发表机构
Huazhong University of Science and Technology; Universität Heidelberg（华中科技大学; 海德堡大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过N体模拟结合解析公式，发现吸积盘诱导的恒星潮汐瓦解（dTDEs）可为中等质量黑洞（IMBHs）提供超爱丁顿极限的高效恒星吸积，或助力小质量IMBHs成长为大质量黑洞种子。
AI 中文摘要
致密核星团为研究恒星与大质量黑洞之间的动力学相互作用提供了独特环境。当存在吸积盘时，耗散性的恒星-吸积盘相互作用可捕获周围恒星，驱动其向内迁移，最终引发吸积盘诱导的潮汐瓦解事件（dTDEs）。然而，仅通过单轨道迁移估算无法推断该过程的长期吸积率，因为它取决于恒星吸积盘捕获、碰撞弛豫、恒星耗尽与补充以及星团内物理并合的耦合演化。本研究中，我们采用高性能直接N体模拟结合恒星-吸积盘相互作用的解析公式，追踪嵌入致密星团且带有吸积盘的中等质量黑洞（IMBHs）的耦合演化。模拟追踪恒星尖峰的形成、恒星因多次穿越吸积盘被捕获、后续轨道阻尼与迁移，以及最终被中心IMBH吞噬的过程。我们发现，dTDEs可维持约10⁻³M☉/年的恒星质量供给率，这超过了M•<10⁵M☉的IMBH的爱丁顿极限气体吸积率。这些结果表明，在富气致密恒星系统中，dTDEs是IMBH的高效恒星吸积通道。作为一种可能的应用，若致密恒星团与吸积盘持续存在超过30百万年，该机制或可将约10³M☉的IMBHs转化为更大质量的黑洞种子。
英文摘要
Dense nuclear star clusters provide unique environments for studying the dynamical interactions between stars and massive black holes. When an accretion disk is present, dissipative star--disk interactions can capture surrounding stars, drive their inward migration, and ultimately lead to disk-induced tidal disruption events\,(dTDEs). The long-term feeding rate from this process, however, cannot be inferred from single-orbit migration estimates alone, as it depends on the coupled evolution of disk capture, collisional relaxation, stellar depletion and replenishment, and physical mergers within the star cluster. In this work, we use high-performance direct $N$-body simulations combined with analytic prescriptions for star--disk interactions to follow this coupled evolution for intermediate-mass black holes\,(IMBHs) with accretion disks embedded in dense stellar clusters. The simulations track the formation of the stellar cusp, the capture of stars by repeated disk crossings, their subsequent orbital damping and migration, and their eventual consumption by the central IMBH. We find that dTDEs can sustain stellar mass supply rates of $\sim10^{-3}\,M_\odot \,\mathrm{yr}^{-1}$, which exceeds the Eddington-limited gas accretion rate for IMBHs with $M_\bullet<10^5\,M_\odot$. These results identify dTDEs as an efficient stellar feeding channel for IMBHs in gas-rich dense stellar systems. As one possible application, this mechanism may help transform $\sim10^3\,M_\odot$ IMBHs into more massive black-hole seeds, provided that compact stellar clusters and accretion disks persist for $>30$ Myr.
Comments14 pages, 8 figures. Submitted to ApJ
