How the super-Eddington regime affects black hole spin evolution in high-redshift galaxies

Abstract

By performing three-dimensional hydrodynamical simulations of a galaxy in an isolated dark matter halo, we follow the evolution of the spin parameter $a$ of a black hole (BH) undergoing super-Eddington phases throughout its growth. This regime, suspected to be accompanied by powerful jet outflows, is expected to decrease the BH spin magnitude. We combine super-Eddington accretion with sub-Eddington phases (quasar and radio modes) and follow the BH spin evolution. Due to the low frequency of super-Eddington episodes, relativistic jets in this regime are not able to decrease the magnitude of the spin effectively, as thin disc accretion in the quasar mode inevitably increases the BH spin. The combination of super- and sub-Eddington accretion does not lead to a simple explicit expression for the spin evolution because of feedback from super-Eddington events. An analytical expression can be used to calculate the evolution for $a\lesssim 0.3$, assuming the super-Eddington feedback is consistently weak. Finally, BHs starting with low spin magnitude are able to grow to the highest mass, and if they initially start misaligned with the galactic disc, they get a small boost of accretion through retrograde accretion.

Updated the paper to the published A&A version

References in corpus (14)

• Stability of Relativistic Jets from Rotating, Accreting Black Holes via Fully Three-Dimensional Magnetohydrodynamic Simulations
• Magnetic acceleration of relativistic AGN jets
• The Relation Between SFR and Stellar Mass for Galaxies at 3.5 $\le z\le$ 6.5 in CANDELS
• The Evolution of Black Hole Mass and Spin in Active Galactic Nuclei
• Super-Critical Growth of Massive Black Holes from Stellar-Mass Seeds
• On the final spin from the coalescence of two black holes
• Slim disks around Kerr black holes revisited
• Black hole evolution: II. Spinning black holes in a supernova-driven turbulent interstellar medium
• Spin-driven jet feedback in idealised simulations of galaxy groups and clusters
• Jet efficiencies and black hole spins in jetted quasars
• On Constraining the Growth History of Massive Black Holes via Their Distribution on the Spin-Mass Plane
• High-redshift SMBHs can grow from stellar-mass seeds via chaotic accretion
• AGN jets do not prevent the suppression of conduction by the heat buoyancy instability in simulated galaxy clusters
• Effects of spin on constraining the seeds and growth of $\gtrsim 10^9{M}_{\odot }$ supermassive black holes in $z>6.5$ Quasars

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• A unified framework for hot accretion flows with finite angular momentum: from Bondi-like to disc-like regimes
• A novel sub-grid model for super-Eddington accretion of spinning black holes in galaxy-scale simulations