Multi-accretion events from corotating and counterrotating SMBHs tori

TL;DR

This paper investigates the dynamics and formation of ringed accretion disks around Kerr SMBHs, emphasizing the roles of fluid rotation, magnetic fields, and black hole spin in their stability and evolution.

Contribution

It extends the RAD model to include magnetized tori and analyzes how magnetic fields and fluid rotation influence their formation and stability.

Findings

Magnetic fields and fluid rotation significantly constrain RAD formation.

The model identifies specific SMBH spins associated with observable RADs.

Constraints on tori stability and collision emergence are established.

Abstract

Ringed accretion disks (RADs) are aggregates of corotating and counterrotating toroidal accretion disks orbiting a central Kerr super-massive Black Hole (SMBH) in AGNs. The dimensionless spin of the central BH and the fluids relative rotation are proved to strongly affect the RAD dynamics. There is evidence of a strict correlation between SMBH spin, fluid rotation and magnetic fields in RADs formation and evolution. Recently, the model was extended to consider RADs constituted by several magnetized accretion tori and the effects of a toroidal magnetic field in RAD dynamics have been investigated. The analysis poses constraints on tori formation and emergence of RADs instabilities in the phases of accretion onto the central attractor and tori collision emergence. Magnetic fields and fluids rotation are proved to be strongly constrained and influence tori formation and evolution in RADs, in dependence on the toroidal magnetic fields parameters. Eventually, the RAD frame investigation constraints specific classes of tori that could be observed around some specific SMBHs identified by their dimensionless spin