Journal article
Tidal disruption events in the first billion years of a galaxy
H Pfister, J Lixin Dai, M Volonteri, K Auchettl, M Trebitsch, E Ramirez-Ruiz
Monthly Notices of the Royal Astronomical Society | OXFORD UNIV PRESS | Published : 2021
Abstract
Accretion of stars on massive black holes (MBHs) can feed MBHs and generate tidal disruption events (TDEs). We introduce a new physically motivated model to self-consistently treat TDEs in cosmological simulations, and apply it to the assembly of a galaxy with final mass 3 × 1010M⊙ at z = 6. This galaxy exhibits a TDE rate of ∼ 10-5 yr-1, consistent with local observations but already in place when the Universe was one billion year old. A fraction of the disrupted stars participate in the growth of MBHs, dominating it until the MBH reaches mass ∼ 5 × 105M⊙, but their contribution then becomes negligible compared to gas. TDEs could be a viable mechanism to grow light MBH seeds, but fewer TDEs..
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Grants
Awarded by Deutsche Forschungsgemeinschaft
Funding Acknowledgements
The authors thank the anonymous referee for his/her comments. HP is indebted to the Danish National Research Foundation (DNRF132) and the Hong Kong government (GRF grant HKU27305119) for support. JLD is supported by the Hong Kong government (GRF grant HKU27305119) and the seed funding from the University of Hong Kong (201909185012). KAA and ERR are supported by the Danish National Research Foundation (DNRF132). Parts of this research were supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. MT is supported by Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany's Excellence Strategy EXC-2181/1 390900948 (the Heidelberg STRUCTURES Cluster of Excellence). The authors thank the Yukawa Institute for Theoretical Physics, Kyoto University. Discussions during the YITP workshop YITPT-19-07 on InternationalMolecule-typeWorkshop `Tidal Disruption Events: General Relativistic Transients' were useful to complete this work. This work was made possible with the access to the HPC resources of CINES under allocations DARK no. A0060406955 made by GENCI. This work has made use of the Horizon Cluster hosted by Institut d'Astrophysique de Paris; the authors thank St ' ephane Rouberol for running smoothly this cluster.