Simulating tidal disruption events in nuclear star clusters

@misc{cho2026simulating,
  title = {{Simulating tidal disruption events in nuclear star clusters}},
  author = {Philip Cho and Kai Wu and Francesco Flammini Dotti and Taras Panamarev and Shuo Li and Shiyan Zhong and Klaus Reuter and Rainer Spurzem},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.31083},
  eprint = {2609.31083},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.31083},
}

TY  - UNPB
TI  - Simulating tidal disruption events in nuclear star clusters
AU  - Philip Cho
AU  - Kai Wu
AU  - Francesco Flammini Dotti
AU  - Taras Panamarev
AU  - Shuo Li
AU  - Shiyan Zhong
AU  - Klaus Reuter
AU  - Rainer Spurzem
PY  - 2026
DA  - 2026/09/25
PB  - arXiv
DO  - 10.48550/arxiv.2609.31083
UR  - https://arxiv.org/abs/2609.31083
AB  - Context. Nuclear star clusters (NSCs) and supermassive black holes (SMBHs) often coexist at the centers of galaxies, engaging in complex dynamical interactions that influence SMBH growth. Stars that approach the SMBH too closely are tidally disrupted, and a fraction of their debris is accreted onto the black hole. Such events may contribute to SMBH growth in gas-deficient galaxies. Aims. Our work aims to improve the theoretical framework for understanding the mass accretion of stellar debris following tidal disruption events (TDEs) through numerical simulations. We perform direct N-body simulations of an NSC with a central SMBH embedded in a fully self-consistent dynamical model to test a new TDE accretion prescription in a set of pilot simulations. Methods. The previous TDE prescription used a fixed accretion radius and assumed that the entire stellar mass was accreted after disruption. In the new partial-mass accretion model, the mass added to the SMBH depends on the orbital eccentricity and penetration factor of the disrupted star. Results. We find that most TDEs involving main-sequence stars are marginally eccentric or marginally hyperbolic and contribute approximately half of the stellar mass to SMBH growth, consistent with recent hydrodynamical simulations. In all simulated models, the TDE-driven mass accretion rate exhibits an early peak followed by a rapid decline. Models with higher initial SMBH masses exhibit a faster decline in the accretion rate, consistent with more rapid loss-cone depletion and inefficient replenishment
ER  -