Aspects of GRMHD in high-energy astrophysics: geometrically thick disks and tori agglomerates around spinning black holes

Pugliese, Daniela; Montani, Giovanni

doi:10.1007/s10714-021-02820-4

Cited by 6 publications

(7 citation statements)

References 145 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…(F β α is the Faraday tensor and is a quantity related to the metric signature 29,30 ). The electric field does not affect the continuity equation or the equation for the entropy.…”

Section: Ideal Grmhd and Grhdmentioning

confidence: 99%

See 1 more Smart Citation

Limiting effects in tori clusters

Pugliese¹,

Stuchlık²

2022

Preprint

Self Cite

View full text Add to dashboard Cite

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 ξ representing the (total) BH rotational energy extracted versus the mass of the BH, associating ξ to the characteristics of the accretion processes.

show abstract

“…(F β α is the Faraday tensor and is a quantity related to the metric signature 29,30 ). The electric field does not affect the continuity equation or the equation for the entropy.…”

Section: Ideal Grmhd and Grhdmentioning

confidence: 99%

“…structure is defined by the boundary conditions determining the tori (edges)-see for more details 9,29,31 .…”

Section: Ideal Grmhd and Grhdmentioning

confidence: 99%

Limiting effects in tori clusters

Pugliese¹,

Stuchlık²

2022

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

“…As a result, substituting relations ( 9) and ( 10) into Faraday's and Gauss' laws (see equations ( 20) and (21b) in section 4.1) does not provide any additional propagation or constraint equations, but instead leads to trivial identities. 9 An alternative way of extracting the wave-like equations ( 22) and ( 23) is by substituting (6) into Maxwell's formulae (see equation (18) in section 4.1) and then projecting the resulting expression along and orthogonal to the u a -field.…”

Section: Wave Equations For the Potentialsmentioning

confidence: 99%

“…This area also appears to be one of the most challenging, since the study of electromagnetism in curved spaces has led to rather unconventional phenomenology in a number of occasions (e.g. see [3][4][5][6][7][8][9] for a representative though incomplete list)…”

Section: Introductionmentioning

confidence: 99%

Electromagnetic potentials in curved spacetimes

Mavrogiannis¹,

Tsagas²

2021

Class. Quantum Grav.

View full text Add to dashboard Cite

Electromagnetic potentials allow for an alternative description of the Maxwell field, the electric and magnetic components of which emerge as gradients of the vector and the scalar potentials. We provide a general relativistic analysis of these potentials, by deriving their wave equations in an arbitrary Riemannian spacetime containing a generalised imperfect fluid. Some of the driving agents in the resulting wave formulae are explicitly due to the curvature of the host spacetime. Focusing on the implications of non-Euclidean geometry, we look into the linear evolution of the vector potential in Friedmann universes with nonzero spatial curvature. Our results reveal a qualitative difference in the evolution of the potential between the closed and the open Friedmann models, solely triggered by the different spatial geometry of these spacetimes. We then consider the interaction between gravitational and electromagnetic radiation and the effects of the former upon the latter. In so doing, we apply the wave formulae of both potentials to a Minkowski background and study the Weyl–Maxwell coupling at the second perturbative level. Our solutions, which apply to low-density interstellar environments away from massive compact stars, allow for the resonant amplification of both the electromagnetic potentials by gravitational-wave distortions.

show abstract

“…An RAD is a fully general relativistic model of orbiting multiple tori, introduced in Pugliese & Montani (2015) and detailed in Pugliese & Stuchlík (2016); Pugliese & Stuchlík (2017); Pugliese & Stuchlík (2018b); Pugliese & Stuchlík (2018c); Pugliese & Stuchlík (2019); Pugliese & Montani (2021). Each torus is part of the coplanar axisymmetrical structured toroidal disk, composed of an aggregate of toroids orbiting in the equatorial plane of a single central BH.…”

Section: Introductionmentioning

confidence: 99%

GRMHD Evolution of Interacting Double Accretion Tori Orbiting a Central Black Hole

Bardiev¹,

Kološ²,

Pugliese³

et al. 2022

ApJ

View full text Add to dashboard Cite

The matter orbiting black holes (BHs) in microquasars or active galactic nuclei forms toroidal accretion disk structures, and multiple torus structures have been recently described as ringed accretion disks (RADs) in a full general relativistic approach. Here we realize full general relativistic magnetohydrodynamic (GRMHD) numerical simulations related to double toroidal structure immersed in the equatorial plane of the gravitomagnetic field of a central Schwarzschild BH in an asymptotically uniform magnetic field. We study the merging dynamics of an initial RAD structure constructed by two corotating or counterrotating tori, where accretion of matter from the outer torus is assumed onto the inner torus, using the 2.5D GRMHD simulation schemes with the HARM numerical code. We study the dynamics of the system assuming various initial conditions, and we have demonstrated that the initial matter density is the relevant factor governing the system evolution.

show abstract

Aspects of GRMHD in high-energy astrophysics: geometrically thick disks and tori agglomerates around spinning black holes

Cited by 6 publications

References 145 publications

Limiting effects in tori clusters

Limiting effects in tori clusters

Electromagnetic potentials in curved spacetimes

GRMHD Evolution of Interacting Double Accretion Tori Orbiting a Central Black Hole

Contact Info

Product

Resources

About