期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 508, 期 2, 页码 1973-1985出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stab2713
关键词
black hole physics; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: kinematics and dynamics
资金
- NSF CAREER grant [1455342]
- NASA [80NSSC18K0562, 17-ATP17-0067, HST-AR-15800.001-A]
- NSF [AST-2009687, AST-1715216, AST-1652522, 1911233, 20009234]
- Flatiron Institute - Simons Foundation
- Cottrell Scholar Award from the Research Corporation for Science Advancement
- Scialog Award from the Research Corporation for Science Advancement
- NASA HEC [SMD-16-7592]
Supermassive black holes in the early universe may not efficiently sink in high-z galaxies, but solutions such as increasing the number of seeds or embedding seed BHs in dense structures can be considered.
Possible formation scenarios of supermassive black holes (BHs) in the early universe include rapid growth from less massive seed BHs via super-Eddington accretion or runaway mergers, yet both of these scenarios would require seed Blis to efficiently sink to and be trapped in the Galactic Centre via dynamical friction. This may not be true for their complicated dynamics in clumpy high-z galaxies. In this work, we study this 'sinking problem' with state-of-the-art high-resolution cosmological simulations, combined with both direct N-body integration of seed BH trajectories and post-processing of randomly generated test particles with a newly developed dynamical friction estimator. We find that seed BHs less massive than 10(8) M-circle dot (i.e. all but the already-supermassive seeds) cannot efficiently sink in typical high-z galaxies. We also discuss two possible solutions: dramatically increasing the number of seeds such that one seed can end up trapped in the Galactic Centre by chance, or seed BHs being embedded in dense structures (e.g. star clusters) with effective masses above the mass threshold. We discuss the limitations of both solutions.
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