On the Eddington limit in accretion discs

@article{Heinzeller2007OnTE,
  title={On the Eddington limit in accretion discs},
  author={Dominikus Heinzeller and W. J. Duschl Institut fuer Theoretische Astrophysik and Universitaet Heidelberg and Germany now at Institut fuer Theoretische Physik und Astrophysik and Universitaet Kiel and Germany Steward Observatory and The University of Arizona and Usa},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2007},
  volume={374},
  pages={1146-1154}
}
Although the Eddington limit has originally been derived for stars, recently its relevance for the evolution of accretion discs has been realized. We discuss the question whether the classical Eddington limit – which has been applied globally for almost all calculations on accretion discs – is a good approximation if applied locally in the disc. For this purpose, a critical accretion rate corresponding to this type of modified classical Eddington limit is calculated from thin α-disc models and… 

The cosmogony of supermassive black holes

We report calculations of the evolution, under Reynolds viscosity, of the massive gaseous accretion discs thought to form in the centres of galaxies as a result of major galactic mergers at early

The growth of supermassive black holes fed by accretion disks

Context. Supermassive black holes are probably present in the centre of the majority of the galaxies. There is consensus that these exotic objects are formed by the growth of seeds either by mass

TIDAL DISRUPTION FLARES: THE ACCRETION DISK PHASE

The evolution of an accretion disk, formed as a consequence of the disruption of a star by a black hole, is followed by solving numerically hydrodynamic equations. The present investigation aims to

Why Is Supercritical Disk Accretion Feasible?

Although the occurrence of steady supercritical disk accretion onto a black hole has been speculated about since the 1970s, it has not been accurately verified so far. For the first time, we

Modelling the spectral energy distribution of super-Eddington quasars

We develop a broad-band spectral model, agnslim, to describe super-Eddington black hole accretion disc spectra. This is based on the slim disc emissivity, where radial advection keeps the surface

The role of viscosity in AGN outflows in relation to jet periodicities

Aims. Adopting the Smoothed Particle Hydrodynamics (SPH) numerical method, we performed a grid of evolving models of a 3D axially-symmetric, viscous accretion disc around a supermassive black hole

General relativistic radiative transfer in black hole systems

Accretion onto compact objects plays a central role in high-energy astrophysics. The presence of a compact object considerably alters the structure and dynamics of the accreting plasma, as well as

A group of outbursts with exponential decays in the Rapid Burster

Aims. We present an analysis focused on a specific group of six intense outbursts (abbreviated as group A) that displays strong persistent emission in the unique low-mass X-ray binary Rapid Burster

THE PHYSICS OF THE “HEARTBEAT” STATE OF GRS 1915+105

We present the first detailed phase-resolved spectral analysis of a joint Chandra High-Energy Transmission Grating Spectrometer and Rossi X-ray Timing Explorer observation of the ρ variability class

References

SHOWING 1-10 OF 20 REFERENCES

Super-Eddington accretion rates in Narrow Line Seyfert 1 galaxies

We use the BH masses deduced from the empirical relation of Kaspi et al. (2000) between the size of the Broad Line Region (BLR) of Active Galactic Nuclei (AGN) and the optical luminosity, to compute

Basic Properties of Supercritical Accretion Disks

At the turn of the millennium, supercritical accretion disks (superdisks), where the mass-accretion rate highly exceeds the Eddington's one, are being resurrected under recent observational and

Super-Eddington Fluxes from Thin Accretion Disks?

Radiation pressure-dominated accretion disks are predicted to exhibit strong density inhomogeneities on scales much smaller than the disk scale height as a result of the nonlinear development of

Thick accretion disks with super-Eddington luminosities

We describe a Newtonian version of the theory of thick accretion disks orbiting black holes. In view of the present inadequate knowledge of microscopic viscosity process, this theory adopts a

Photon bubbles in accretion discs

We show that radiation-dominated accretion discs are likely to suffer from a ‘photon bubble’ instability similar to that described by Arons in the context of accretion on to neutron star polar caps.

Supercritical Accretion Flows around Black Holes: Two-dimensional, Radiation Pressure-dominated Disks with Photon Trapping

The quasi-steady structure of supercritical accretion flows around a black hole is studied based on two-dimensional radiation-hydrodynamic (2D-RHD) simulations. The supercritical flow is composed of

Eddington Limit and Radiative Transfer in Highly Inhomogeneous Atmospheres

Radiation-dominated accretion disks are likely to be subject to the "photon bubble" instability, which may lead to strong density inhomogeneities on scales much shorter than the disk scale height.

Does the Slim-Disk Model Correctly Consider Photon-trapping Effects?

We investigate the photon-trapping effects in the supercritical black hole accretion flows by solving radiation transfer as well as the energy equations of radiation and gas. It is found that the

Radiative Disk Winds from a Self-Similar Slim Disk

We investigated the radiation fields of a self-similar slim disk and the behavior of wind particles, which are driven by the radiation pressure of a self-similar slim disk. When the accretion rate is

USING FU ORIONIS OUTBURSTS TO CONSTRAIN SELF-REGULATED PROTOSTELLAR DISK MODELS

One-dimensional, convective, vertical structure models and one dimensional time-dependent, radial diffusion models are combined to create a self-consistent picture in which FU Orionis outbursts occur