Self-similar evolution of self-gravitating viscous accretion discs

Illenseer, Tobias F.; Duschl, W. J.

doi:10.1093/mnras/stv587

Cited by 8 publications

(6 citation statements)

References 53 publications

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“…A power law with negative exponent is necessary for the surface density, because otherwise a local minimum of the gravitational potential, generated by the self-gravitation, would lead to nonphysical solutions. Illenseer & Duschl (2015) describe in detail which power laws are sensible choices for accretion disks. Our choice for the power law and the initial density generate densities at radius R κ , which are comparable to those in .…”

Section: Initial and Boundary Conditionsmentioning

confidence: 99%

“…Given that the region outside the accretion disk is very gas poor, no effective coupling with the disk can be established. Angular momentum cannot be transported from the accretion disk to outside regions (see Illenseer & Duschl 2015). Without angular momentum transport, there can be no accretion.…”

Section: Cold Accretionmentioning

confidence: 99%

“…This applies also to vertically isothermal self-gravitating accretion disks (Illenseer & Duschl 2015). Using a scale height H (r) we can calculate the vertical structure and the Green's function: we can rewrite the integral Eq.…”

Section: Self-gravity Solver In Polar Coordinatesmentioning

confidence: 99%

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Multi-scale simulations of black hole accretion in barred galaxies

Jung

Illenseer

Duschl

2018

A&A

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Due to the non-axisymmetric potential of the central bar, barred spiral galaxies form, in addition to their characteristic arms and bar, a variety of structures within the thin gas disk, like nuclear rings, inner spirals and dust-lanes. In this first of two papers, we present a method to accurately simulate the gas flow within the galactic plane in the 2D finite volume software package FOSITE, which solves the transport equations for mass, momentum and energy, and apply it to this class of objects. To this extent, we introduced a new transport scheme for angular momentum and a very efficient pseudo-spectral Poisson solver. Moreover, we provide a simple and generally applicable method of how to take care of gravity in the energy equation.

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Section: Initial and Boundary Conditionsmentioning

confidence: 99%

Section: Cold Accretionmentioning

confidence: 99%

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Multi-scale simulations of black hole accretion in barred galaxies

Jung

Illenseer

Duschl

2018

A&A

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“…Recent advances in theoretical astrophysics have mostly been led by the rapid progress in supercomputing, of the computers themselves and the numerical techniques. In particular, hydrodynamical simulations coupled with gravity have proved to be a powerful tool to reveal the dynamics of many astrophysical and cosmological phenomena such as supernovae, star formation, relativistic jets, accretion discs, formation of large scale structure etc [1][2][3][4][5][6][7][8]. Most simulations deal with simplified models, assuming some symmetry and solving equations with reduced dimensions.…”

Section: Introductionmentioning

confidence: 99%

Hyperbolic self-gravity solver for large scale hydrodynamical simulations

et al. 2016

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A new computationally efficient method has been introduced to treat self-gravity in Eulerian hydrodynamical simulations. It is applied simply by modifying the Poisson equation into an inhomogeneous wave equation. This roughly corresponds to the weak field limit of the Einstein equations in general relativity, and as long as the gravitation propagation speed is taken to be larger than the hydrodynamical characteristic speed, the results agree with solutions for the Poisson equation. The solutions almost perfectly agree if the domain is taken large enough, or appropriate boundary conditions are given. Our new method cannot only significantly reduce the computational time compared with existent methods, but is also fully compatible with massive parallel computation, nested grids, and adaptive mesh refinement techniques, all of which can accelerate the progress in computational astrophysics and cosmology.

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“…Furthermore, Shlosman et al (1990) found that the α ansatz is not efficient enough to fuel the observed rapid mass growth of AGN (Fan et al 2003). Thus, Illenseer & Duschl (2015;hereafter ID15) neglected the α ansatz and used -among others -the more general and physically faithful β description (Duschl et al 2000) when they developed their dynamical model for self-gravitating accretion disks.…”

Section: Introductionmentioning

confidence: 99%

Accretion disk dynamics

Kubsch

Illenseer

Duschl

2016

A&A

Self Cite

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Aims. We investigate the suitability of α-viscosity in self-similar models for self-gravitating disks with a focus on active galactic nuclei (AGN) disks. Methods. We use a self-similar approach to simplify the partial differential equations arising from the evolution equation, which are then solved using numerical standard procedures. Results. We find a self-similar solution for the dynamical evolution of self-gravitating α-disks and derive the significant quantities. In the Keplerian part of the disk our model is consistent with standard stationary α-disk theory, and self-consistent throughout the self-gravitating regime. Positive accretion rates throughout the disk demand a high degree of self-gravitation. Combined with the temporal decline of the accretion rate and its low amount, the model prohibits the growth of large central masses.Conclusions. α-viscosity cannot account for the evolution of the whole mass spectrum of super-massive black holes (SMBH) in AGN. However, considering the involved scales it seems suitable for modelling protoplanetary disks.

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Self-similar evolution of self-gravitating viscous accretion discs

Cited by 8 publications

References 53 publications

Multi-scale simulations of black hole accretion in barred galaxies

Multi-scale simulations of black hole accretion in barred galaxies

Hyperbolic self-gravity solver for large scale hydrodynamical simulations

Accretion disk dynamics

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