Model radiation spectrum for an accretion disk near a rotating black hole

2002 ◽  
Vol 46 (5) ◽  
pp. 360-365 ◽  
Author(s):  
A. F. Zakharov ◽  
S. V. Repin
Keyword(s):  
Black Hole ◽  
Accretion Disk ◽  
Radiation Spectrum ◽  
Rotating Black Hole

Radiation spectrum of a high-dimensional rotating black hole

2010 ◽  
Vol 53 (3) ◽  
pp. 504-507 ◽  
Author(s):  
Ren Zhao ◽  
HuaiFan Li ◽  
LiChun Zhang ◽  
YueQin Wu
Keyword(s):  
Black Hole ◽  
Radiation Spectrum ◽  
High Dimensional ◽  
Rotating Black Hole

scholarly journals Compton Reflection in the Vicinity of a Rotating Black Hole

1998 ◽  
Vol 188 ◽  
pp. 409-410
Author(s):  
A. Maciołek-Niedźwiecki ◽  
P. Magdziarz
Keyword(s):  
Black Hole ◽  
Accretion Disk ◽  
Rotating Black Hole ◽  
Line Shapes

We study the spectra arising from Compton reflection in the innermost parts of the accretion disk. We emphasize that the so far neglected relativistic distortion of the Compton reflection continuum may strongly affect the derived Fe Kα line shapes.

scholarly journals Line Emission from an Accretion Disk around a Rotating Black Hole: Toward a Measurement of Frame Dragging

1997 ◽  
Vol 475 (1) ◽  
pp. 57-64 ◽  
Author(s):  
Benjamin C. Bromley ◽  
Kaiyou Chen ◽  
Warner A. Miller
Keyword(s):  
Black Hole ◽  
Accretion Disk ◽  
Line Emission ◽  
Frame Dragging ◽  
Rotating Black Hole

Magnetic Coupling of a Rotating Black Hole with Its Surrounding Accretion Disk

2003 ◽  
Vol 595 (1) ◽  
pp. 109-119 ◽  
Author(s):  
Ding‐Xiong Wang ◽  
Ren‐Yi Ma ◽  
Wei‐Hua Lei ◽  
Guo‐Zheng Yao
Keyword(s):  
Black Hole ◽  
Accretion Disk ◽  
Magnetic Coupling ◽  
Rotating Black Hole

NUMERICAL TREATMENT OF THIN ACCRETION DISK DYNAMICS AROUND ROTATING BLACK HOLES

2010 ◽  
Vol 19 (13) ◽  
pp. 2111-2133 ◽  
Author(s):  
DENIZ YILDIRAN ◽  
ORHAN DONMEZ
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Steady State ◽  
Accretion Disk ◽  
Outer Boundary ◽  
Adiabatic Index ◽  
Opening Angle ◽  
Computational Domain ◽  
Rotating Black Hole ◽  
Rotating Black Holes

In the present study, we perform the numerical simulation of a relativistic thin accretion disk around the nonrotating and rapidly rotating black holes using the general relativistic hydrodynamic code with Kerr in Kerr–Schild coordinate that describes the central rotating black hole. Since the high energy X-rays are produced close to the event horizon resulting the black hole–disk interaction, this interaction should be modeled in the relativistic region. We have set up two different initial conditions depending on the values of thermodynamical variables around the black hole. In the first setup, the computational domain is filled with constant parameters without injecting gas from the outer boundary. In the second, the computational domain is filled with the matter which is then injected from the outer boundary. The matter is assumed to be at rest far from the black hole. Both cases are modeled over a wide range of initial parameters such as the black hole angular momentum, adiabatic index, Mach number and asymptotic velocity of the fluid. It has been found that initial values and setups play an important role in determining the types of the shock cone and in designating the events on the accretion disk. The continuing injection from the outer boundary presents a tail shock to the steady state accretion disk. The opening angle of shock cone grows as long as the rotation parameter becomes larger. A more compressible fluid (bigger adiabatic index) also presents a bigger opening angle, a spherical shock around the rotating black hole, and less accumulated gas in the computational domain. While results from [J. A. Font, J. M. A. Ibanez and P. Papadopoulos, Mon. Not. R. Astron. Soc.305 (1999) 920] indicate that the tail shock is warped around for the rotating hole, our study shows that it is the case not only for the warped tail shock but also for the spherical and elliptical shocks around the rotating black hole. The warping around the rotating black hole in our case is much smaller than the one by [J. A. Font, J. M. A. Ibanez and P. Papadopoulos, Mon. Not. R. Astron. Soc.305 (1999) 920], due to the representation of results at the different coordinates. Contrary to the nonrotating black hole, the tail shock is slightly warped around the rotating black hole. The filled computational domain without any injection leads to an unstable accretion disk. However much of it reaches a steady state for a short period of time and presents quasi-periodic oscillation (QPO). Furthermore, the disk tends to loose mass during the whole dynamical evolution. The time-variability of these types of accretion flowing close to the black hole may clarify the light curves in Sgr A*.

scholarly journals QUASI-PERIODIC OSCILLATIONS AND FREQUENCIES IN AN ACCRETION DISK AND COMPARISON WITH THE NUMERICAL RESULTS FROM NON-ROTATING BLACK HOLE COMPUTED BY THE GRH CODE

2007 ◽  
Vol 22 (02) ◽  
pp. 141-157 ◽  
Author(s):  
ORHAN DONMEZ
Keyword(s):  
Black Hole ◽  
Accretion Disk ◽  
Numerical Results ◽  
Pressure Gradients ◽  
Periodic Oscillations ◽  
Rotating Black Hole ◽  
Accretion Flows ◽  
Numerical Result ◽  
General Relativistic ◽  
Physical Phenomena

The shocked wave created on the accretion disk after different physical phenomena (accretion flows with pressure gradients, star-disk interaction etc.) may be responsible observed Quasi Periodic Oscillations (QPOs) in X-ray binaries. We present the set of characteristics frequencies associated with accretion disk around the rotating and non-rotating black holes for one particle case. These persistent frequencies are results of the rotating pattern in an accretion disk. We compare the frequency's from two different numerical results for fluid flow around the non-rotating black hole with one particle case. The numerical results are taken from Refs. 1 and 2 using fully general relativistic hydrodynamical code with non-selfgravitating disk. While the first numerical result has a relativistic tori around the black hole, the second one includes one-armed spiral shock wave produced from star-disk interaction. Some physical modes presented in the QPOs can be excited in numerical simulation of relativistic tori and spiral waves on the accretion disk. The results of these different dynamical structures on the accretion disk responsible for QPOs are discussed in detail.

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