A Grid of Relativistic, Non‐LTE Accretion Disk Models for Spectral Fitting of Black Hole Binaries

2006 ◽  
Vol 164 (2) ◽  
pp. 530-535 ◽  
Author(s):  
Shane W. Davis ◽  
Ivan Hubeny
Keyword(s):  
Black Hole ◽  
Accretion Disk ◽  
Black Hole Binaries ◽  
Spectral Fitting

scholarly journals Warm and thick corona for a magnetically supported disk in galactic black hole binaries

2020 ◽  
Vol 633 ◽  
pp. A35 ◽  
Author(s):  
D. Gronkiewicz ◽  
A. Różańska
Keyword(s):  
Magnetic Field ◽  
Black Hole ◽  
Accretion Disk ◽  
Thermal Instability ◽  
Stellar Mass ◽  
Rotational Instability ◽  
X Ray ◽  
Black Hole Binaries ◽  
Radiative Processes ◽  
Gas Heating

Context. We self-consistently model a magnetically supported accretion disk around a stellar-mass black hole with a warm optically thick corona based on first principles. We consider the gas heating by magneto-rotational instability dynamo. Aims. Our goal is to show that the proper calculation of the gas heating by magnetic dynamo can build up the warm optically thick corona above the accretion disk around a black hole of stellar mass. Methods. Using the vertical model of the disk supported and heated by the magnetic field together with radiative transfer in hydrostatic and radiative equilibrium, we developed a relaxation numerical scheme that allowed us to compute the transition form the disk to corona in a self-consistent way. Results. We demonstrate here that the warm (up to 5 keV) optically thick (up to 10 τes) Compton-cooled corona can form as a result of magnetic heating. A warm corona like this is stronger in the case of the higher accretion rate and the greater magnetic field strength. The radial extent of the warm corona is limited by local thermal instability, which purely depends on radiative processes. The obtained coronal parameters are in agreement with those constrained from X-ray observations. Conclusions. A warm magnetically supported corona tends to appear in the inner disk regions. It may be responsible for soft X-ray excess seen in accreting sources. For lower accretion rates and weaker magnetic field parameters, thermal instability prevents a warm corona, giving rise to eventual clumpiness or ionized outflow.

scholarly journals SUPERMASSIVE BLACK HOLE BINARIES AT HIGH ENERGIES

2014 ◽  
Vol 28 ◽  
pp. 1460183
Author(s):  
GUSTAVO E. ROMERO ◽  
DANIELA PÉREZ ◽  
GABRIELA S. VILA
Keyword(s):  
Black Hole ◽  
Accretion Disk ◽  
Spectral Energy Distribution ◽  
Radiative Properties ◽  
Spectral Energy ◽  
Electromagnetic Spectrum ◽  
Relativistic Electrons ◽  
Black Hole Binaries ◽  
Supermassive Black Hole ◽  
Tidal Torques

An accretion disk around a supermassive black hole may be strongly perturbed by the presence of a secondary black hole. Recent simulations have shown that, under certain conditions, the tidal torques exerted by the secondary black hole may open an annular gap in the disk. In this regime, matter "overflows" across the secondary's orbit to accrete onto the primary and may feed a pair of relativistic jets. In this work we study the radiative properties of a binary system of supermassive black holes, assuming that a relativistic jet is launched from the primary and the migration of the secondary across the disk proceeds in the "overflowing" regime. The modified radiative spectrum of the disk is calculated accounting for strong gravitational effects in the innermost region. The jet emits non-thermal radiation all along the electromagnetic spectrum by interaction of locally accelerated electrons with the jet's magnetic field and internal and external radiation. In particular, we investigate whether the interaction of the relativistic electrons with the photons emitted by the accretion disk induces any signature in the spectral energy distribution of the jet that may reveal the presence of the secondary black hole.

scholarly journals Disk Instabilities in the Black Hole Binaries

1996 ◽  
Vol 158 ◽  
pp. 135-138 ◽  
Author(s):  
J. K. Cannizzo
Keyword(s):  
Black Hole ◽  
Accretion Disk ◽  
Time Constant ◽  
Accretion Disks ◽  
Binary Systems ◽  
Recent Progress ◽  
Light Curves ◽  
X Ray ◽  
Black Hole Binaries ◽  
Exponential Character

I will briefly review recent progress in our understanding of the global propagation of accretion disk instabilities operating in interacting binary systems in which the accreting star is a ~ 10 M⊙ black hole. A detailed discussion of this work can be found in Cannizzo, Chen & Livio (1995).The X-ray light curves of the brightest and best studied X-ray novae – systems such as A0620–00, GS2000+25, GS1124–68, and GRO J0422+32 – are notable in two respects: the rise times are fast (a few days) and the decays have an exponential character, where the e–folding time constant is about 30 to 40 d (Mineshige, Yamasaki, & Ishizaka 1993, hereafter MYI). It is noteworthy that outbursts in dwarf novae also decay exponentially, with the time constant being about a factor of 10 shorter. In this contribution I will discuss the constraints on the physics of accretion disks which the (observed) exponential decay enables us to make.

scholarly journals On the dynamics of the torus around the kicked black hole

2021 ◽  
Author(s):  
O. Donmez ◽  
Anwar Al-Kandari ◽  
Ahlam Abu Seedou
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Accretion Disk ◽  
Spiral Wave ◽  
Wave Structure ◽  
Global Mode ◽  
Black Hole Binaries ◽  
Spiral Density Waves ◽  
Angular Momentum Loss ◽  
General Relativistic

There is a special interest to understand the dynamical properties of the accretion disk created around the newly formed black hole due to the supermassive black hole binaries which merge inside the gaseous disk. The newly formed black hole would have a kick velocity up to thousands of km/s that drives a perturbation on a newly accreted torus around the black hole. Some of the observed supermassive black holes at the center of the Active Galactic Nucleus (AGN) move with a certain velocity relative to its broader accretion disk. In this paper, the effects of the kicked black holes onto the infinitesimally thin accreted torus are studied by using the general relativistic hydrodynamical code, focusing on changing the dynamics of the accretion disk during the accretion disk–black hole interaction. We have found that the non-axisymmetric global mode [Formula: see text] inhomogeneity, which causes a spiral-wave-structure, is excited on the torus due to kicked black hole. The higher the perturbation velocity produced by the kicked black hole, the longer the time the torus takes to reach the saturation point. The created spiral density waves which rapidly evolve into the spiral shocks are also observed from the numerical simulations. The spiral shock is responsible for accreting matter toward the black hole. First, the spiral-wave-structure is developed and the accretion through the spiral arms is stopped around the black hole. At the later time of simulation, the formed spiral shocks partly cause the angular momentum loss across the torus.

Hydrodynamics of Black Hole–Accretion Disk Collision

1998 ◽  
Vol 507 (1) ◽  
pp. 131-144 ◽  
Author(s):  
Pavel B. Ivanov ◽  
Igor V. Igumenshchev ◽  
Igor D. Novikov
Keyword(s):  
Black Hole ◽  
Accretion Disk ◽  
Black Hole Accretion ◽  
Black Hole Accretion Disk ◽  
Hole Accretion

scholarly journals Effective-one-body waveforms from dynamical captures in black hole binaries

2021 ◽  
Vol 103 (6) ◽  
Author(s):  
Alessandro Nagar ◽  
Piero Rettegno ◽  
Rossella Gamba ◽  
Sebastiano Bernuzzi
Keyword(s):  
Black Hole ◽  
Black Hole Binaries

scholarly journals Peculiar acceleration of stellar-origin black hole binaries: Measurement and biases with LISA

2020 ◽  
Vol 101 (6) ◽  
Author(s):  
Nicola Tamanini ◽  
Antoine Klein ◽  
Camille Bonvin ◽  
Enrico Barausse ◽  
Chiara Caprini
Keyword(s):  
Black Hole ◽  
Black Hole Binaries
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