Spherical harmonic modes of 5.5 post-Newtonian gravitational wave polarizations and associated factorized resummed waveforms for a particle in circular orbit around a Schwarzschild black hole

2010 ◽  
Vol 82 (4) ◽  
Author(s):  
Ryuichi Fujita ◽  
Bala R. Iyer
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Circular Orbit ◽  
Spherical Harmonic ◽  
Schwarzschild Black Hole

scholarly journals Conservative, gravitational self-force for a particle in circular orbit around a Schwarzschild black hole in a radiation gauge

2011 ◽  
Vol 83 (6) ◽  
Author(s):  
Abhay G. Shah ◽  
Tobias S. Keidl ◽  
John L. Friedman ◽  
Dong-Hoon Kim ◽  
Larry R. Price
Keyword(s):  
Black Hole ◽  
Circular Orbit ◽  
Schwarzschild Black Hole ◽  
Self Force

scholarly journals Geodesic motion near self-gravitating scalar field configurations

2019 ◽  
Vol 27 (3) ◽  
pp. 231-241
Author(s):  
Ivan M. Potashov ◽  
Julia V. Tchemarina ◽  
Alexander N. Tsirulev
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Circular Orbit ◽  
Naked Singularity ◽  
Schwarzschild Black Hole ◽  
Null Geodesics ◽  
Naked Singularities ◽  
Test Particles ◽  
Stable Circular Orbit ◽  
Innermost Stable Circular Orbit

We study the geodesics motion of neutral test particles in the static spherically symmetric spacetimes of black holes and naked singularities supported by a selfgravitating real scalar field. The scalar field is supposed to model dark matter surrounding some strongly gravitating object such as the centre of our Galaxy. The behaviour of timelike and null geodesics very close to the centre of such a configuration crucially depends on the type of spacetime. It turns out that a scalar field black hole, analogously to a Schwarzschild black hole, has the innermost stable circular orbit and the (unstable) photon sphere, but their radii are always less than the corresponding ones for the Schwarzschild black hole of the same mass; moreover, these radii can be arbitrarily small. In contrast, a scalar field naked singularity has neither the innermost stable circular orbit nor the photon sphere. Instead, such a configuration has a spherical shell of test particles surrounding its origin and remaining in quasistatic equilibrium all the time. We also show that the characteristic properties of null geodesics near the centres of a scalar field naked singularity and a scalar field black hole of the same mass are qualitatively different.

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.

scholarly journals Spinning test body orbiting around a Schwarzschild black hole: Circular dynamics and gravitational-wave fluxes

2016 ◽  
Vol 94 (10) ◽  
Author(s):  
Enno Harms ◽  
Georgios Lukes-Gerakopoulos ◽  
Sebastiano Bernuzzi ◽  
Alessandro Nagar
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Test Body ◽  
Schwarzschild Black Hole

STABILITY OF SCHWARZSCHILD BLACK HOLE IN THE MASSIVE BRANS-DICKE THEORY

1986 ◽  
Vol 01 (03) ◽  
pp. 709-729 ◽  
Author(s):  
O.J. KWON ◽  
Y.D. KIM ◽  
Y.S. MYUNG ◽  
B.H. CHO ◽  
Y.J. PARK
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Gravitational Wave ◽  
Scalar Wave ◽  
Schwarzschild Black Hole ◽  
The Real ◽  
Gravitational Perturbations ◽  
Scalar Perturbations

For the nontachyonic mass (c<0, µ2<6), we have found that all nonstatic perturbations (odd-, even-parity and scalar perturbations) allow only the real values of frequency k. This means that the black hole in the massive Brans-Dicke theory is classically stable. However, for the tachyonic mass of scalar field (c>0, µ2>6), we find that the massive Brans-Dicke theory is classically unstable. We also emphasize that the potential forms of odd-parity perturbations is simply given by the pure-gravitational perturbations. For the even-parity case, we obtain the same potential just as Zerilli’s case by combining the even-parity gravitational wave and scalar wave. For static perturbations (k=0) and c>0, only the odd- and even-parity cases with L=0, 1 is allowed to avoid exponentially growing modes.

scholarly journals Chaotic motion around a black hole under minimal length effects

2020 ◽  
Vol 80 (8) ◽  
Author(s):  
Xiaobo Guo ◽  
Kangkai Liang ◽  
Benrong Mu ◽  
Peng Wang ◽  
Mingtao Yang
Keyword(s):  
Black Hole ◽  
Phase Space ◽  
Homoclinic Orbit ◽  
Circular Orbit ◽  
Chaotic Behavior ◽  
Melnikov Method ◽  
Minimal Length ◽  
Geodesic Motion ◽  
Schwarzschild Black Hole ◽  
Length Effects

Abstract We use the Melnikov method to identify chaotic behavior in geodesic motion perturbed by the minimal length effects around a Schwarzschild black hole. Unlike the integrable unperturbed geodesic motion, our results show that the perturbed homoclinic orbit, which is a geodesic joining the unstable circular orbit to itself, becomes chaotic in the sense that Smale horseshoes chaotic structure is present in phase space.

scholarly journals Self-Force on a Scalar Charge in Circular Orbit around a Schwarzschild Black Hole

2001 ◽  
Vol 106 (2) ◽  
pp. 339-362 ◽  
Author(s):  
Hiroyuki Nakano ◽  
Yasushi Mino ◽  
Misao Sasaki
Keyword(s):  
Black Hole ◽  
Circular Orbit ◽  
Schwarzschild Black Hole ◽  
Scalar Charge ◽  
Self Force

scholarly journals Unsettling Physics in the Quantum-Corrected Schwarzschild Black Hole

Symmetry ◽  
2020 ◽  
Vol 12 (8) ◽  
pp. 1264 ◽  
Author(s):  
Valerio Faraoni ◽  
Andrea Giusti
Keyword(s):  
Black Hole ◽  
Energy Density ◽  
Circular Orbit ◽  
Loop Quantum Gravity ◽  
Schwarzschild Black Hole ◽  
Spatial Infinity ◽  
Quantum Energy ◽  
Stable Circular Orbit ◽  
Innermost Stable Circular Orbit ◽  
Quasilocal Mass

We study a quantum-corrected Schwarzschild black hole proposed recently in Loop Quantum Gravity. Prompted by the fact that corrections to the innermost stable circular orbit of Schwarzschild diverge, we investigate time-like and null radial geodesics. Massive particles moving radially outwards are confined, while photons make it to infinity with infinite redshift. This unsettling physics, which deviates radically from both Schwarzschild (near the horizon) and Minkowski (at infinity) is due to repulsion by the negative quantum energy density that makes the quasilocal mass vanish as one approaches spatial infinity.

OPEN STRING IN (3+1)-DIMENSIONAL REISSNER–NORDSTRÖM BLACK HOLE

2010 ◽  
Vol 25 (15) ◽  
pp. 1233-1238 ◽  
Author(s):  
HIROMI SUZUKI
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Equatorial Plane ◽  
Cosmic String ◽  
Circular Orbit ◽  
Open String ◽  
Spherically Symmetric ◽  
Schwarzschild Black Hole ◽  
Charged Black Holes ◽  
Open Strings

Previously we investigated the Nambu–Goto string and the wiggly cosmic string in (3+1)-dimensional Schwarzschild black hole. As an extension the solutions in (3+1)-dimensional spherically symmetric charged black holes are investigated. The solution for the wiggly string exhibits open strings lying along the circular orbit in the equatorial plane outside horizon, while the Nambu–Goto string has only a point-like solution.

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