scholarly journals Gravitational radiation from a particle in circular orbit around a black hole. III. Stability of circular orbits under radiation reaction

1993 ◽  
Vol 47 (12) ◽  
pp. 5376-5388 ◽  
Author(s):  
Theocharis Apostolatos ◽  
Daniel Kennefick ◽  
Amos Ori ◽  
Eric Poisson
Keyword(s):  
Black Hole ◽  
Gravitational Radiation ◽  
Circular Orbit ◽  
Radiation Reaction ◽  
Circular Orbits

scholarly journals Gravitational radiation reaction for bound motion around a Schwarzschild black hole

1994 ◽  
Vol 50 (6) ◽  
pp. 3816-3835 ◽  
Author(s):  
Curt Cutler ◽  
Daniel Kennefick ◽  
Eric Poisson
Keyword(s):  
Black Hole ◽  
Gravitational Radiation ◽  
Radiation Reaction ◽  
Schwarzschild Black Hole

scholarly journals Photon Spheres, ISCOs, and OSCOs: Astrophysical Observables for Regular Black Holes with Asymptotically Minkowski Cores

Universe ◽  
2020 ◽  
Vol 7 (1) ◽  
pp. 2
Author(s):  
Thomas Berry ◽  
Alex Simpson ◽  
Matt Visser
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Circular Orbit ◽  
Schwarzschild Black Hole ◽  
Circular Orbits ◽  
Regular Black Hole ◽  
Astrophysical Interest ◽  
Regular Black Holes ◽  
Recent Advances ◽  
Classical Black Holes

Classical black holes contain a singularity at their core. This has prompted various researchers to propose a multitude of modified spacetimes that mimic the physically observable characteristics of classical black holes as best as possible, but that crucially do not contain singularities at their cores. Due to recent advances in near-horizon astronomy, the ability to observationally distinguish between a classical black hole and a potential black hole mimicker is becoming increasingly feasible. Herein, we calculate some physically observable quantities for a recently proposed regular black hole with an asymptotically Minkowski core—the radius of the photon sphere and the extremal stable timelike circular orbit (ESCO). The manner in which the photon sphere and ESCO relate to the presence (or absence) of horizons is much more complex than for the Schwarzschild black hole. We find situations in which photon spheres can approach arbitrarily close to (near extremal) horizons, situations in which some photon spheres become stable, and situations in which the locations of both photon spheres and ESCOs become multi-valued, with both ISCOs (innermost stable circular orbits) and OSCOs (outermost stable circular orbits). This provides an extremely rich phenomenology of potential astrophysical interest.

MULTI-BLACK HOLES SOLUTION WITH COSMIC STRINGS

2004 ◽  
Vol 19 (10) ◽  
pp. 1549-1557 ◽  
Author(s):  
F. ÖZDEMIR ◽  
N. ÖZDEMIR ◽  
B. T. KAYNAK
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Angular Momentum ◽  
Cosmic String ◽  
Circular Orbit ◽  
Cosmic Strings ◽  
De Sitter ◽  
Circular Orbits ◽  
Small Oscillations ◽  
String Models

Some black hole-cosmic string models such as Reissner–Nordström, RN–de Sitter, Kerr–Newman and multi-black holes with cosmic string are given. Energy and angular momentum of a timelike particle in circular orbits in multi-black hole space–time are calculated. The geodesic equations for the timelike particles for the far region of the multi-black hole sources are calculated and small oscillations around the circular orbit obtained. It is seen that the particle's orbit precesses like the Lens–Thirring effect.

THE INFLUENCE OF THE INERTIAL DRAGGING EFFECT ON GRAVITATIONAL RADIATION EMITTED FROM A PARTICLE MOVING IN EQUATORIAL GEODESIC CIRCULAR ORBIT ABOUT A KERR’S BLACK HOLE

1993 ◽  
Vol 02 (02) ◽  
pp. 149-161
Author(s):  
BIPING GONG
Keyword(s):  
Black Hole ◽  
Continuous Function ◽  
Gravitational Radiation ◽  
Circular Orbit ◽  
Turning Point ◽  
Radiation Energy ◽  
Angular Frequency ◽  
Related Function ◽  
Classical Turning Point ◽  
Main Factors

Using Chranowski and Misner’s equations,1 gravitational radiation emitted from a particle moving in an equatorial geodesic circular orbit about a Kerr’s black hole is calculated. Outside the classical turning point, the radiation energy can be represented as a continuous function of orbital radius of the particle, and thus a corresponding curve is obtained. Using Wilkins’ approach,2 two inertial dragging related functions are obtained by restricting the orbit of the particle to the equatorial plane of a Kerr’s black hole. By comparing the curve of the gravitational radiation and the curves of the simulating functions (consisting of the angular frequency and the drag related function), we come to the conclusion that inertial dragging effect on a particle is one of the main factors that influences the gravitational radiation.

Gravitational radiation from a particle in circular orbit around a black hole. II. Numerical results for the nonrotating case

1993 ◽  
Vol 47 (4) ◽  
pp. 1511-1518 ◽  
Author(s):  
Curt Cutler ◽  
Lee Samuel Finn ◽  
Eric Poisson ◽  
Gerald Jay Sussman
Keyword(s):  
Black Hole ◽  
Gravitational Radiation ◽  
Circular Orbit ◽  
Numerical Results

Trajectories of photons in modified Hayward black hole spacetime

2019 ◽  
Vol 34 (23) ◽  
pp. 1950182 ◽  
Author(s):  
Jian-Ping Hu ◽  
Yu Zhang ◽  
Li-Li Shi ◽  
Guang-Hai Guo ◽  
Peng-Fei Duan
Keyword(s):  
Black Hole ◽  
Time Delay ◽  
Effective Potential ◽  
Circular Orbit ◽  
Null Geodesic ◽  
Quantum Corrections ◽  
Circular Orbits ◽  
Black Hole Spacetime ◽  
Bound Orbits ◽  
Lapse Function

We study the trajectories of photons in modified Hayward black hole spacetime. Three kinds of horizons are distinguished by analyzing the lapse function of modified Hayward black hole spacetime. Through plotting the effective potential with different values of parameters, it is found that the parameter [Formula: see text] has more conspicuous effects than parameters [Formula: see text] ([Formula: see text] is associated with the time-delay) and [Formula: see text] ([Formula: see text] is related to the 1-loop quantum corrections) for the effective potential. The change of the parameters ([Formula: see text], [Formula: see text] and [Formula: see text]) has an obvious influence on unstable circular orbits. The structure of null geodesic is simpler than that of time-like geodesic. The stable circular orbits and the bound orbits are not included for the photon trajectories. By analyzing the corresponding effective potential, all possible orbits of null geodesic are found. The radius of unstable circular orbit equals 2.8790 for fixed [Formula: see text], [Formula: see text], [Formula: see text], [Formula: see text] and [Formula: see text].

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