发表机构
Huazhong University of Science and Technology; Universität Heidelberg; Tsinghua University（华中科技大学; 海德堡大学; 清华大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过半解析模型，发现金属增丰晕中盘诱导的星族I/II潮汐瓦解事件可主导重种子黑洞早期增长，使质量在0.1 Gyr内从约1e4太阳质量增至约1e5太阳质量，缓解高红移黑洞候选体的质量张力。
AI 中文摘要
最近的模拟表明，重种子黑洞可能在弱金属增丰的原子冷却晕中形成，在这些晕中，超大质量恒星前身和小尺度恒星碎片几乎同时出现。在这种图景下，新生的重种子自然嵌入在金属增丰的星族I/II核星团中，而非孤立于原始环境中。我们研究了来自这些星族I/II恒星的盘诱导潮汐瓦解事件（TDEs）能否为重种子黑洞提供高效且持续的增长通道。我们构建了一个半解析模型，用于描述重种子黑洞周围的恒星轨道阻尼、盘捕获、迁移和潮汐瓦解，并将由此产生的盘诱导TDE贡献纳入包含重子与金属丰度演化的宇宙学合并树中。重种子宿主晕选自满足快速气体流入判据或强莱曼-沃纳辐射判据的原子冷却晕，其金属丰度$Z\lesssim10^{-3}Z_\odot$。我们发现，盘诱导的星族I/II TDEs可以主导重种子的早期增长：在种子形成后的最初约0.1 Gyr内，黑洞质量中位数从约$10^4\\,M_\odot$增长到约$10^5\\,M_\odot$，并在约0.2 Gyr时达到数个$10^5\\,M_\odot$。TDEs提供的累积质量最初超过气体吸积，并在最初约200 Myr内保持相当。包含盘诱导TDEs使黑洞群体向更高质量偏移，增加了$z\sim9$--10处大质量黑洞的丰度，并产生更大的黑洞与恒星质量比。这一通道有助于缓解但并未完全消除重种子模型与最极端高红移黑洞候选体之间的张力，表明可能仍需要额外的增长机制。
英文摘要
Recent simulations suggest that heavy seed black holes may form in weakly metal-enriched atomic cooling halos, where the supermassive-star progenitor and small-scale stellar fragments emerge nearly coevally. In this picture, the newly born heavy seed is naturally embedded in a metal-enriched Pop~I/II nuclear star cluster rather than in an isolated pristine environment. We investigate whether disk-induced tidal disruption events (TDEs) from these Pop~I/II stars can provide an efficient and sustained growth channel for heavy seed black holes. We construct a semi-analytical model for stellar orbital damping, disk capture, migration, and tidal disruption around a heavy seed black hole, and incorporate the resulting disk-induced TDE contribution into cosmological merger trees with baryonic and metallicity evolution. Heavy seed host halos are selected from atomic cooling halos with $Z\lesssim10^{-3}Z_\odot$ that satisfy either a rapid gas-inflow criterion or a strong Lyman--Werner radiation criterion. We find that disk-induced Pop~I/II TDEs can dominate the early growth of heavy seeds: the median black hole mass grows from $\sim10^4\,M_\odot$ to $\sim10^5\,M_\odot$ within the first $\sim0.1$ Gyr after seed formation, and reaches several $10^5\,M_\odot$ by $\sim0.2$ Gyr. The cumulative mass supplied by TDEs initially exceeds that from gas accretion and remains comparable over the first $\sim200$ Myr. Including disk-induced TDEs shifts the black hole population toward higher masses, increases the abundance of massive black holes at $z\sim9$--10, and produces larger black hole-to-stellar mass ratios. This channel helps alleviate, but does not fully remove, the tension between heavy-seed models and the most extreme high-redshift black hole candidates, suggesting that additional growth mechanisms may still be required.
Comments20 pages, 12 figures
