The internal evolution of black holes

1994 ◽  
Vol 72 (11-12) ◽  
pp. 755-759 ◽  
Author(s):  
Alfio Bonanno ◽  
Serge Droz ◽  
Werner Israel ◽  
Sharon Morsink
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Initial Data ◽  
Progress Report ◽  
Inner Horizon ◽  
Evolutionary Problem ◽  
Open Questions ◽  
Physical Laws ◽  
Internal Evolution

Determining the inner structure of a black hole is really an evolutionary problem, with precisely known initial data. The evolution can in principle be followed to within Planck distances of the singularity at the inner horizon, using only well-established physical laws. This article is a progress report and a review of open questions.

scholarly journals Approaching the Black Hole by Numerical Simulations

Universe ◽  
2019 ◽  
Vol 5 (5) ◽  
pp. 99 ◽  
Author(s):  
Christian Fendt
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Direct Evidence ◽  
Dynamical Evolution ◽  
Numerical Code ◽  
Physical Processes ◽  
Hydrodynamic Simulations ◽  
Environmental Material ◽  
Physical Laws ◽  
Radiative Interaction

Black holes represent extreme conditions of physical laws. Predicted about a century ago, they are now accepted as astrophysical reality by most of the scientific community. Only recently has more direct evidence of their existence been found—the detection of gravitational waves from black hole mergers and of the shadow of a supermassive black hole in the center of a galaxy. Astrophysical black holes are typically embedded in an active environment which is affected by the strong gravity. When the environmental material emits radiation, this radiation may carry imprints of the black hole that is hosting the radiation source. In order to understand the physical processes that take place in the close neighborhood of astrophysical black holes, numerical methods and simulations play an essential role. This is simply because the dynamical evolution and the radiative interaction are far too complex in order to allow for an analytic solution of the physical equations. A huge progress has been made over the last decade(s) in the numerical code development, as well as in the computer power that is needed to run these codes. This review tries to summarize the basic questions and methods that are involved in the undertaking of investigating the astrophysics of black holes by numerical means. It is intended for a non-expert audience interested in an overview over this broad field. The review comes along without equations and thus without a detailed expert discussion of the underlying physical processes or numerical specifics. Instead, it intends to illustrate the richness of the field and to motivate further reading. The review puts some emphasis on magneto-hydrodynamic simulations but also touches radiation transfer and merger simulations, in particular pointing out differences in these approaches.

scholarly journals THERMODYNAMICS IN BLACK-HOLE/CFT CORRESPONDENCE

2013 ◽  
Vol 22 (12) ◽  
pp. 1342012 ◽  
Author(s):  
BIN CHEN ◽  
JIA-JU ZHANG
Keyword(s):  
Field Theory ◽  
Black Holes ◽  
Black Hole ◽  
Two Dimensional ◽  
Charged Black Holes ◽  
Conformal Field ◽  
Inner Horizon ◽  
Holographic Description ◽  
Area Law ◽  
Lower Dimensional

The area law of Bekenstein–Hawking entropy of the black hole suggests that the black hole should have a lower-dimensional holographic description. It has been found recently that a large class of rotating and charged black holes could be holographically described a two-dimensional (2D) conformal field theory (CFT). We show that the universal information of the dual CFT, including the central charges and the temperatures, is fully encoded in the thermodynamics laws of both outer and inner horizons. These laws, characterizing how the black hole responds under the perturbation, allows us to read different dual pictures with respect to different kinds of perturbations. The remarkable effectiveness of this thermodynamics method suggest that the inner horizon could play a key role in the study of holographic description of the black hole.

scholarly journals Black hole initial data by numerical integration of the parabolic–hyperbolic form of the constraints

2021 ◽  
Author(s):  
Anna Nakonieczna ◽  
Łukasz Nakonieczny ◽  
István Rácz
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Initial Data ◽  
Fourth Order ◽  
Main Part ◽  
Strong Field ◽  
Method Of Lines ◽  
Time Integration ◽  
The Method Of Lines ◽  
Hyperbolic Form

The parabolic–hyperbolic form of the constraints is integrated numerically. The applied numerical stencil is fourth-order accurate (in the spatial directions) while “time”-integration is made by using the method of lines with a fourth-order order accurate Runge–Kutta scheme. The proper implementation of the applied numerical method is verified by convergence tests and monitoring the relative and absolute errors is determined by comparing numerically and analytically known solutions of the constraints involving boosted and spinning vacuum single black hole configurations. The main part of our investigations is, however, centered on the construction of initial data for distorted black holes which, in certain cases, have non-negligible gravitational wave content. Remarkably, the applied new method is unprecedented in that it allows to construct initial data for highly boosted and spinning black holes, essentially for the full physical allowed ranges of these parameters. In addition, the use of the evolutionary form of the constraints is free from applying any sort of boundary conditions in the strong field regime.

scholarly journals The Cosmic History of Black Hole Growth from Deep Multiwavelength Surveys

2012 ◽  
Vol 2012 ◽  
pp. 1-21 ◽  
Author(s):  
Ezequiel Treister ◽  
C. Megan Urry
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Optical Emission ◽  
Supermassive Black Holes ◽  
X Ray ◽  
Open Questions ◽  
Black Hole Growth ◽  
History Of ◽  
Hole Growth ◽  
Cosmic History

Significant progress has been made in the last few years on understanding how supermassive black holes form and grow. In this paper, we begin by reviewing the spectral signatures of active galactic nuclei (AGN) ranging from radio to hard X-ray wavelengths. We then describe the most commonly used methods to find these sources, including optical/UV, radio, infrared, and X-ray emission, and optical emission lines. We then describe the main observational properties of the obscured and unobscured AGN population. Finally, we summarize the cosmic history of black hole accretion, that is, when in the history of the universe supermassive black holes were getting most of their mass. We finish with a summary of open questions and a description of planned and future observatories that are going to help answer them.

scholarly journals Can We Prescribe the Physical Parameters of Multiple Black Holes?

Mathematics ◽  
2021 ◽  
Vol 9 (24) ◽  
pp. 3170
Author(s):  
István Rácz
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Initial Data ◽  
Physical Parameters ◽  
Binary Black Hole ◽  
Hyperbolic Form

The parabolic-hyperbolic form of the constraints and superposed Kerr-Schild black holes have already been used to provide a radically new initialization of binary black hole configurations. The method generalizes straightforwardly to multiple black hole systems. This paper is to verify that each of the global Arnowitt-Deser-Misner quantities of the constructed multiple black hole initial data can always be prescribed, as desired, in advance of solving the constraints. These global charges are shown to be uniquely determined by the physical parameters of the involved individual Kerr-Schild black holes.

scholarly journals NONSINGULAR BLACK HOLES FROM GRAVITY–MATTER-BRANE LAGRANGIANS

2010 ◽  
Vol 25 (08) ◽  
pp. 1571-1596 ◽  
Author(s):  
EDUARDO GUENDELMAN ◽  
ALEXANDER KAGANOVICH ◽  
EMIL NISSIMOV ◽  
SVETLANA PACHEVA
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Cosmological Constant ◽  
Radial Coordinate ◽  
De Sitter ◽  
Wormhole Solution ◽  
Interior Region ◽  
Exterior Region ◽  
Inner Horizon ◽  
Self Consistent

We consider self-consistent coupling of bulk Einstein–Maxwell–Kalb–Ramond system to codimension-one charged lightlikep-brane with dynamical (variable) tension (LL-brane). The latter is described by a manifestly reparametrization-invariant worldvolume action significantly different from the ordinary Nambu–Goto one. We show that the LL-brane is the appropriate gravitational and charge source in the Einstein–Maxwell–Kalb–Ramond equations of motion needed to generate a self-consistent solution describing nonsingular black hole. The latter consists of de Sitter interior region and exterior Reissner–Nordström region glued together along their common horizon (it is the inner horizon from the Reissner–Nordström side). The matching horizon is automatically occupied by the LL-brane as a result of its worldvolume Lagrangian dynamics, which dynamically generates the cosmological constant in the interior region and uniquely determines the mass and charge parameters of the exterior region. Using similar techniques we construct a self-consistent wormhole solution of Einstein–Maxwell system coupled to electrically neutral LL-brane, which describes two identical copies of a nonsingular black hole region being the exterior Reissner–Nordström region above the inner horizon, glued together along their common horizon (the inner Reissner–Nordström one) occupied by the LL-brane. The corresponding mass and charge parameters of the two black hole "universes" are explicitly determined by the dynamical LL-brane tension. This also provides an explicit example of Misner–Wheeler "charge without charge" phenomenon. Finally, this wormhole solution connecting two nonsingular black holes can be transformed into a special case of Kantowski–Sachs bouncing cosmology solution if instead of Reissner–Nordström we glue together two copies of the exterior Reissner–Nordström–de Sitter region with big enough bare cosmological constant, such that the radial coordinate becomes a timelike variable everywhere in the two "universes," except at the matching hypersurface occupied by the LL-brane.

scholarly journals RELATING QUANTUM INFORMATION TO CHARGED BLACK HOLES

2005 ◽  
Vol 14 (08) ◽  
pp. 1321-1331 ◽  
Author(s):  
XIAN-HUI GE ◽  
YOU-GEN SHEN
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Thought Experiment ◽  
Two Dimensional ◽  
Cauchy Horizon ◽  
Charged Black Holes ◽  
Inner Horizon ◽  
Local Measurements ◽  
Non Local ◽  
Dilaton Black Holes

Quantum non-cloning theorem and a thought experiment are discussed for charged black holes whose global structure exhibits an event and a Cauchy horizon. We take Reissner–Norström black holes and two-dimensional dilaton black holes as concrete examples. The results show that the quantum non-cloning theorem and the black hole complementarity are far from consistent inside the inner horizon. The relevance of this work to non-local measurements is briefly discussed.

scholarly journals Fractionated branes and black hole interiors

2015 ◽  
Vol 24 (12) ◽  
pp. 1543004 ◽  
Author(s):  
Emil J. Martinec
Keyword(s):  
Black Holes ◽  
General Relativity ◽  
Black Hole ◽  
String Theory ◽  
Inner Horizon ◽  
Black Hole Interior ◽  
Tension State ◽  
Low Tension

Combining a variety of results in string theory and general relativity, a picture of the black hole interior is developed wherein spacetime caps off at an inner horizon and the inter-horizon region is occupied by a Hagedorn gas of a very low tension state of fractionated branes. This picture leads to natural resolutions of a variety of puzzles concerning quantum black holes.

Instability of black hole inner horizons

1978 ◽  
Vol 358 (1695) ◽  
pp. 499-517 ◽  
Keyword(s):  
Black Hole ◽  
Initial Data ◽  
Causal Structure ◽  
Rest Mass ◽  
Scalar Perturbation ◽  
Data Sets ◽  
Propagation Equation ◽  
Inner Horizon ◽  
Symmetry Properties ◽  
Spin Fields

Linear perturbations of black hole models by a variety of fields are considered. Perturbing fields include the zero rest mass scalar field in the case of Reissner-Nordstrom, and gravitational, electromagnetic and zero rest mass scalar perturbation in the case of the Kerr model. The analysis deals with the Ψ 0 components (in the Newman-Penrose (1962) formalism) of non-zero spin fields. The symmetry properties of the models are used to derive the crucial condition th at the field be singular on the inner horizon. This condition is independent of the field propagation equation. Initial data are then given in terms of incoming radiation from f - is shown that there exist wellbehaved initial data sets for which the resultant fields are singular on the inner horizon. It is emphasized that this instability result is dependent only on the global symmetries and causal structure of the models considered, and is independent of the precise nature of the perturbing field.

scholarly journals Inner horizon instability and the unstable cores of regular black holes

2021 ◽  
Vol 2021 (5) ◽  
Author(s):  
Raúl Carballo-Rubio ◽  
Francesco Di Filippo ◽  
Stefano Liberati ◽  
Costantino Pacilio ◽  
Matt Visser
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Quantum Gravity ◽  
Inner Core ◽  
Singularity Problem ◽  
Regular Black Holes ◽  
Black Hole Spacetimes ◽  
Stellar Collapse ◽  
Inner Horizon ◽  
Linear Perturbations

Abstract Regular black holes with nonsingular cores have been considered in several approaches to quantum gravity, and as agnostic frameworks to address the singularity problem and Hawking’s information paradox. While in a recent work we argued that the inner core is destabilized by linear perturbations, opposite claims were raised that regular black holes have in fact stable cores. To reconcile these arguments, we discuss a generalization of the geometrical framework, originally applied to Reissner-Nordtsröm black holes by Ori, and show that regular black holes have an exponentially growing Misner-Sharp mass at the inner horizon. This result can be taken as an indication that stable nonsingular black hole spacetimes are not the definitive endpoint of a quantum gravity regularization mechanism, and that nonperturbative backreation effects must be taken into account in order to provide a consistent description of the quantum-gravitational endpoint of gravitational stellar collapse.

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