Limiting effects in tori clusters

TL;DR

This paper models clusters of misaligned, thick accretion tori orbiting a supermassive black hole, analyzing their stability, collision potential, and oscillatory behaviors to understand their physical constraints and dynamics.

Contribution

It introduces a unified model for tilted torus clusters around black holes, deriving constraints on their existence, stability, and interactions based on geometrical and energetic parameters.

Findings

Constraints on tilted tori existence and properties.

Conditions for torus collision and instability.

Effects of geometrical thickness and oscillations.

Abstract

We consider agglomerates of misaligned tori orbiting a supermassive black hole. The aggregate of tilted tori is modeled as a single orbiting configuration by introducing a leading function governing the distribution of toroids (and maximum pressure points inside the disks) around the black hole attractor. The orbiting clusters are composed by geometrically thick, pressure supported, perfect fluid tori. This analysis places constraints on the existence and properties of tilted tori and more general aggregates of orbiting disks. We study the constraints on the tori collision emergence and the instability of the agglomerates of tori with general relative inclination angles, the possible effects of the tori geometrical thickness and on the oscillatory phenomena. Some notes are discussed on the orbiting ringed structure in dependence of the dimensionless parameter ${\xi}$ representing the (total) BH rotational energy extracted versus the mass of the BH, associating ${\xi}$ to the characteristics of the accretion processes.