scholarly journals Late-time evolution of a self-interacting scalar field in the spacetime of a dilaton black hole

2001 ◽  
Vol 64 (4) ◽  
Author(s):  
Rafał Moderski ◽  
Marek Rogatko
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Time Evolution ◽  
Late Time ◽  
Dilaton Black Hole

scholarly journals Entanglement of coupled massive scalar field in background of dilaton black hole

2009 ◽  
Vol 677 (3-4) ◽  
pp. 186-189 ◽  
Author(s):  
Jieci Wang ◽  
Qiyuan Pan ◽  
Songbai Chen ◽  
Jiliang Jing
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Massive Scalar ◽  
Massive Scalar Field ◽  
Dilaton Black Hole

scholarly journals Late time evolution of a nonminimally coupled scalar field system

2019 ◽  
Vol 51 (9) ◽  
Author(s):  
M. Shahalam ◽  
R. Myrzakulov ◽  
Maxim Yu. Khlopov
Keyword(s):  
Scalar Field ◽  
Time Evolution ◽  
Late Time ◽  
Field System

scholarly journals LATE-TIME TAIL OF A COUPLED SCALAR FIELD IN THE BACKGROUND OF A BLACK HOLE WITH A GLOBAL MONOPOLE

2008 ◽  
Vol 23 (05) ◽  
pp. 359-369 ◽  
Author(s):  
SONGBAI CHEN ◽  
JILIANG JING
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Scalar Fields ◽  
Massless Scalar ◽  
Late Time ◽  
Massless Scalar Field ◽  
Global Monopole ◽  
Massive Scalar Field ◽  
Gravitational Fields ◽  
Field Decay

Using the technique of spectral decomposition, we investigated the late-time tails of massless and massive coupled scalar fields in the background of a black hole with a global monopole. We found that due to the existence of the coupling between the scalar and gravitational fields, the massless scalar field decay faster at timelike infinity i+, and so does the massive one in the intermediate late time. But the asymptotically late-time tail for the massive scalar field is not affected and its decay rate is still t-5/6.

DECAY OF MASSIVE DIRAC HAIRS ON BRANE-WORLD BLACK HOLES

2008 ◽  
Vol 17 (11) ◽  
pp. 2065-2078
Author(s):  
JILIANG JING ◽  
QIYUAN PAN ◽  
CHIKUN DING
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Decay Rate ◽  
Time Evolution ◽  
Wave Mode ◽  
Brane World ◽  
Late Time ◽  
Schwarzschild Black Hole ◽  
Dirac Fields

The late-time evolution of massive Dirac fields in the backgrounds of brane-world black holes is investigated. We find that the dumping exponent depends on both the multiple number of the wave mode and the mass of the Dirac fields, but almost does not depend on the parameter ϒ of the brane-world black holes. We also find that the decay rate of the asymptotic late-time tail is t-5/6. Our results show that the decay of massive Dirac hairs on brane-world black holes has the same behavior as that of the Schwarzschild black hole.

scholarly journals QUANTUM AMPLITUDES IN BLACK-HOLE EVAPORATION: COMPLEX APPROACH AND SPIN-0 AMPLITUDE

2011 ◽  
Vol 20 (02) ◽  
pp. 133-159
Author(s):  
A. N. St. J. FARLEY ◽  
P. D. D'EATH
Keyword(s):  
Black Hole ◽  
Gravitational Field ◽  
Scalar Field ◽  
Boundary Value Problem ◽  
Boundary Data ◽  
Proper Time ◽  
Boundary Value ◽  
Constrained Systems ◽  
Time Interval ◽  
Late Time

This paper is concerned with the quantum-mechanical decay of a Schwarzschild-like black hole, formed by gravitational collapse, into almost-flat space–time and weak radiation at a very late time. We evaluate quantum amplitudes (not just probabilities) for transitions from initial to final states. This quantum description shows that no information is lost in collapse to a black hole. Boundary data for the gravitational field and (in this paper) a scalar field are posed on an initial space-like hypersurface ΣI and a final surface ΣF. These asymptotically flat three-surfaces are separated by a Lorentzian proper-time interval T (typically very large), as measured at spatial infinity. The boundary-value problem is made well-posed, both classically and quantum-mechanically, by a rotation of T into the lower-half complex plane: T → |T| exp (- iθ), with 0 < θ ≤ π/2. This corresponds to Feynman's +iϵ prescription. We consider the classical boundary-value problem and calculate the second-variation classical Lorentzian action [Formula: see text] as a functional of the boundary data. Following Feynman, the Lorentzian quantum amplitude is recovered in the limit θ → 0+ from the well-defined complex-T amplitude. Dirac's canonical approach to the quantisation of constrained systems shows that, for locally supersymmetric theories of gravity, the amplitude is exactly semi-classical, namely [Formula: see text] for weak perturbations, apart from delta functionals of the supersymmetry constraints. We treat such quantum amplitudes for weak scalar-field configurations on ΣF, taking (for simplicity) the weak final gravitational field to be spherically symmetric. The treatment involves adiabatic solutions to the scalar wave equation. This considerably extends work reported in previous papers, by giving explicit expressions for the real and imaginary parts of such quantum amplitudes.

scholarly journals Probing black hole microstate evolution with networks and random walks

2020 ◽  
Vol 8 (5) ◽  
Author(s):  
Anthony Charles ◽  
Daniel Mayerson
Keyword(s):  
Hilbert Space ◽  
Black Hole ◽  
Time Evolution ◽  
Network Theory ◽  
Quantum Tunneling ◽  
Emergent Property ◽  
Late Time ◽  
Time Behavior ◽  
Relative Importance ◽  
Time Behaviour

We model black hole microstates and quantum tunneling transitions between them with networks and simulate their time evolution using well-established tools in network theory. In particular, we consider two models based on Bena-Warner three-charge multi-centered microstates and one model based on the D1-D5 system; we use network theory methods to determine how many centers (or D1-D5 string strands) we expect to see in a typical late-time state. We find three distinct possible phases in parameter space for the late-time behaviour of these networks, which we call ergodic, trapped, and amplified, depending on the relative importance and connectedness of microstates. We analyze in detail how these different phases of late-time behavior are related to the underlying physics of the black hole microstates. Our results indicate that the expected properties of microstates at late times cannot always be determined simply by entropic arguments; typicality is instead a highly non-trivial, emergent property of the full Hilbert space of microstates.

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