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

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.

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

scholarly journals OBLIQUE MAGNETIC FIELDS AND THE ROLE OF FRAME DRAGGING NEAR ROTATING BLACK HOLE

2014 ◽  
Vol 54 (6) ◽  
pp. 398-413 ◽  
Author(s):  
Vladimír Karas ◽  
Ondřej Kopáček ◽  
Devaky Kunneriath
Keyword(s):  
Magnetic Field ◽  
Black Hole ◽  
Large Scale ◽  
Frame Dragging ◽  
Rotating Black Hole ◽  
Large Scale Magnetic Field ◽  
Set Up ◽  
Magnetic Null ◽  
Future Work

<p>Magnetic null points can <span style="font-size: 10px;">develop near the ergosphere boundary of a rotating black hole by the combined effects of strong gravitational field and the frame-dragging mechanism. The induced electric component does not vanish in the magnetic null and an efficient process of particle acceleration can occur in its immediate vicinity. Furthermore, the effect of imposed (weak) magnetic field can trigger an onset of chaos in the motion of electrically charged particles. The model set-up appears to be relevant for low-accretion-rate nuclei of some galaxies which exhibit episodic accretion events (such as the Milky Way's supermassive black hole) embedded in a large-scale magnetic field of external origin with respect to the central black hole. In this contribution we summarise recent results and we give an outlook for future work with the focus on the role of gravito-magnetic effects caused by rotation of the black hole.</span></p>

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 Spectral evolution of the galactic microquasars XTE J1550-564 and GRO J1655-40 during outbursts

2010 ◽  
Vol 6 (S275) ◽  
pp. 321-322
Author(s):  
Alexander A. Lutovinov ◽  
Sergei S. Tsygankov ◽  
Vadim A. Arefiev ◽  
Mikhail G. Revnivtsev
Keyword(s):  
Black Hole ◽  
Accretion Disk ◽  
Line Emission ◽  
Plasma Zone ◽  
Spectral Evolution ◽  
Spectral Parameters ◽  
Hot Plasma ◽  
Upper Limits ◽  
Using Data ◽  
Broadband Spectroscopy

AbstractWe present results of a broadband spectroscopy of the galactic microquasars and black hole candidates XTE J1550-564 and GRO J1655-40, performed with the INTEGRAL and RXTE observatories during strong outbursts in 2003 and 2005, respectively. The spectral parameters evolution was traced during brightening and fading phases of each outburst to search a possible hysteresis and transitions from state to state. We estimated a size and optical depth of different regions around XTE J1550-564, like a hot plasma zone and optically thick accretion disk. Upper limits to the annihilation 511 keV line emission were obtained for both sources using data of the SPI spectrometer onboard the INTEGRAL observatory.

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