AI 中文总结
本研究在基于MESA恒星摄动理论的潮汐瓦解牛顿模型中加入相对论修正，发现恒星瓦解更早、回落时间更长，黑洞自旋仅在近心点极近时影响回落时间，所得模型计算准确且成本低。
AI 中文摘要
潮汐瓦解事件（TDEs）发生于恒星靠近黑洞的距离过近时，其自引力被外部潮汐场克服。恒星经过时会先发生形变，随后被撕裂，部分物质最终沿束缚轨道回落，在黑洞周围形成吸积盘。最近，基于MESA恒星恒星摄动理论的潮汐瓦解事件牛顿模型被提出，作为计算密集型流体动力学模拟的替代方案。本研究在该模型中加入相对论修正，整合赤道Kerr测地线、相对论性潮汐场及相对论性回落时间。与牛顿情况相比，研究发现恒星在轨道上更早被瓦解，导致其积累物理形变的时间更短；此外，瓦解时与黑洞的距离增大使得回落时间更长。不过，黑洞自旋对回落时间的影响可忽略不计，仅在近心点极近的轨道上例外。研究结果可实现比牛顿模型更准确的回落率计算，同时保持计算成本低廉。该代码可在GitHub上获取。
英文摘要
Tidal disruption events (TDEs) occur when a star passes so close to a black hole that its self-gravity is overcome by the external tidal field. As the star passes, it initially deforms, then is ripped apart, and some of its material eventually falls back on bound orbits, forming an accretion disk around the black hole. A Newtonian model of TDEs, based on stellar perturbation theory of MESA stars, was recently introduced as an alternative to computationally intensive hydrodynamical simulations. In this work, we add relativistic corrections to the model, incorporating equatorial Kerr geodesics, relativistic tidal fields, and relativistic fallback times. Compared to the Newtonian case, we find that stars are disrupted earlier in their orbit, which gives them less time to accumulate physical deformations. Additionally, we find that the increased distance from the black hole at the time of disruption makes the fallback time longer. However, the black hole spin has a negligible impact on fallback time, except for orbits with exceptionally close pericenter. Our results allow for a more accurate calculation of fallback rates than the Newtonian model, while also remaining computationally cheap. The code is available on GitHub.
Comments9 pages, 5 figures
