scholarly journals Kerr black hole in canonically deformed space-time

2014 ◽  
Vol 8 ◽  
pp. 1113-1123
Author(s):  
Marcin Daszkiewicz ◽  
Cezary J. Walczyk
Keyword(s):  
Black Hole ◽  
Kerr Black Hole ◽  
Space Time

The gravitational perturbations of the Kerr black hole IV. The completion of the solutiont

1980 ◽  
Vol 372 (1751) ◽  
pp. 475-484 ◽  
Keyword(s):  
Black Hole ◽  
Kerr Black Hole ◽  
Space Time ◽  
Gravitational Perturbations ◽  
Kerr Space ◽  
The One

This paper eliminates the last remaining lacuna in the information that was needed to make the solution for the perturbations in the metric coefficients of the Kerr space-time fully explicit. The requisite information is obtained from a pair of equations which is complementary to the one considered in paper III; and the solution of the Newman-Penrose equations governing the perturbations is, thus, completed.

scholarly journals A pseudo-Newtonian description of any stationary space-time

2016 ◽  
Vol 12 (S324) ◽  
pp. 45-46
Author(s):  
Vojtěch Witzany ◽  
Claus Lämmerzahl
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Strong Field ◽  
Kerr Black Hole ◽  
Space Time ◽  
Schwarzschild Black Hole ◽  
Test Particles ◽  
Kerr Field ◽  
Alternative Gravity Theories ◽  
Static Space

AbstractSince the first investigations into accretion onto black holes, astrophysicists have proposed effective Newtonian-like potentials to mimic the strong-field behavior of matter near a Schwarzschild or Kerr black hole. On the other hand, the fields of neutron stars or black holes in many of the alternative gravity theories differ from the idealized Schwarzschild or Kerr field which would require a number of new potentials. To resolve this, we give a Newtonian-like Hamiltonian which almost perfectly mimics the behavior of test particles in any given stationary space-time. The properties of the Hamiltonian are excellent in static space-times such as the Schwarzschild black hole, but become worse for space-times with gravito-magnetic or dragging effects such as near the Kerr black hole.

scholarly journals Test particle motion in the space-time of a Kerr black hole pierced by a cosmic string

2010 ◽  
Vol 82 (4) ◽  
Author(s):  
Eva Hackmann ◽  
Betti Hartmann ◽  
Claus Lämmerzahl ◽  
Parinya Sirimachan
Keyword(s):  
Black Hole ◽  
Test Particle ◽  
Cosmic String ◽  
Particle Motion ◽  
Kerr Black Hole ◽  
Space Time

NONEQUILIBRIUM THERMODYNAMIC FLUCTUATIONS OF (2+1)-DIMENSIONAL BLACK HOLES

1995 ◽  
Vol 10 (18) ◽  
pp. 1269-1276 ◽  
Author(s):  
WANG BIN ◽  
ZHU JIONG-MING
Keyword(s):  
Phase Transition ◽  
Black Hole ◽  
Dimensional Space ◽  
Nonequilibrium Thermodynamic ◽  
Kerr Black Hole ◽  
Space Time ◽  
Schwarzschild Black Hole ◽  
Second Moments ◽  
Dimensional Space Time ◽  
Second Order Phase Transition

Applying the Landau-Lifshitz theory for thermodynamic fluctuations and the structure of (2 +1)-dimensional space-time, we calculate and estimate the second moments of some relevant quantities for (2+1)-dimensional Schwarzschild black hole, Kerr black hole and Reissner-Nordstrom black hole. The nonequilibrium second-order phase transition for extremal (2+1)-dimensional space-time is discussed.

scholarly journals Spinning test body orbiting around a Kerr black hole: Eccentric equatorial orbits and their asymptotic gravitational-wave fluxes

2021 ◽  
Vol 103 (10) ◽  
Author(s):  
Viktor Skoupý ◽  
Georgios Lukes-Gerakopoulos
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Kerr Black Hole ◽  
Test Body

scholarly journals Spherical orbits around a Kerr black hole

2021 ◽  
Vol 53 (1) ◽  
Author(s):  
Edward Teo
Keyword(s):  
Black Hole ◽  
Kerr Black Hole

scholarly journals Choked accretion onto a Kerr black hole

2021 ◽  
Vol 103 (2) ◽  
Author(s):  
Alejandro Aguayo-Ortiz ◽  
Olivier Sarbach ◽  
Emilio Tejeda
Keyword(s):  
Black Hole ◽  
Kerr Black Hole

scholarly journals Influence of the geometric configuration of accretion flow on the black hole spin dependence of relativistic acoustic geometry

2018 ◽  
Vol 27 (03) ◽  
pp. 1850023 ◽  
Author(s):  
Pratik Tarafdar ◽  
Tapas K. Das
Keyword(s):  
Black Hole ◽  
Kerr Black Hole ◽  
Geometric Configuration ◽  
Surface Gravity ◽  
Linear Perturbation ◽  
Flow Profile ◽  
White Hole ◽  
Accretion Flow ◽  
Black Hole Spin ◽  
General Relativistic

Linear perturbation of general relativistic accretion of low angular momentum hydrodynamic fluid onto a Kerr black hole leads to the formation of curved acoustic geometry embedded within the background flow. Characteristic features of such sonic geometry depend on the black hole spin. Such dependence can be probed by studying the correlation of the acoustic surface gravity [Formula: see text] with the Kerr parameter [Formula: see text]. The [Formula: see text]–[Formula: see text] relationship further gets influenced by the geometric configuration of the accretion flow structure. In this work, such influence has been studied for multitransonic shocked accretion where linear perturbation of general relativistic flow profile leads to the formation of two analogue black hole-type horizons formed at the sonic points and one analogue white hole-type horizon which is formed at the shock location producing divergent acoustic surface gravity. Dependence of the [Formula: see text]–[Formula: see text] relationship on the geometric configuration has also been studied for monotransonic accretion, over the entire span of the Kerr parameter including retrograde flow. For accreting astrophysical black holes, the present work thus investigates how the salient features of the embedded relativistic sonic geometry may be determined not only by the background spacetime, but also by the flow configuration of the embedding matter.

RELATIVISTIC TWISTED ACCRETION DISC AROUND A KERR BLACK HOLE

2015 ◽  
Author(s):  
VIACHESLAV V. ZHURAVLEV ◽  
PAVEL B. IVANOV
Keyword(s):  
Black Hole ◽  
Kerr Black Hole ◽  
Accretion Disc

Renormalised electromagnetic energy density on the horizon of a Kerr black hole

1988 ◽  
Vol 5 (11) ◽  
pp. L187-L189 ◽  
Author(s):  
B Jensen ◽  
J McLaughlin ◽  
A Ottewill
Keyword(s):  
Black Hole ◽  
Energy Density ◽  
Kerr Black Hole ◽  
Electromagnetic Energy
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