Collisions with black holes and deconfined plasmas

Amsel, Aaron J.; Marolf, Donald; Virmani, Amitabh

doi:10.1088/1126-6708/2008/04/025

Cited by 23 publications

(26 citation statements)

References 61 publications

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“…3 It may be more appropriate to refer to the intersection as a focus rather than a caustic, but the latter terminology is rather common. 4 This and subsequent numerical solutions of transcendental equations are obtained using Mathematica's FindRoot, which gives better precision than we are showing. Caustic generators.…”

Section: Structure Of the Event Horizon And Parameters Of The Mergermentioning

confidence: 94%

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Exact event horizon of a black hole merger

Montero

2016

Class. Quantum Grav.

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We argue that the event horizon of a binary black hole merger, in the extreme-mass-ratio limit where one of the black holes is much smaller than the other, can be described in an exact analytic way. This is done by tracing in the Schwarzschild geometry a congruence of null geodesics that approaches a null plane at infinity. Its form can be given explicitly in terms of elliptic functions, and we use it to analyze and illustrate the time-evolution of the horizon along the merger. We identify features such as the line of caustics at which light rays enter the horizon, and the critical point at which the horizons touch. We also compute several quantities that characterize these aspects of the merger.

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Section: Structure Of the Event Horizon And Parameters Of The Mergermentioning

confidence: 94%

“…Refs. [4,5,6,7] apply the idea that the event horizon for the fall of any gravitating object into an acceleration horizon is obtained by appropriate light-ray-tracing in the spacetime of that object. Ref.…”

Section: Introductionmentioning

confidence: 99%

Exact event horizon of a black hole merger

Montero

2016

Class. Quantum Grav.

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“…One tool that is available to calculate realtime dynamics in quantum field theories in the limit of large number of colors and strong coupling is the conjectured duality between gauge theories and gravity [3]. Within gauge/gravity duality, the collision of two heavyions may be recast as the problem of black hole collisions in classical gravity in five-dimensional asymptotic antide-Sitter (AdS) space-time [4][5][6][7][8], for which numerical solutions exist [9] (see also [10][11][12][13][14][15][16][17]). The gravitational dual description is not an exact map of the real-world collision problem, given that the gravitational dual to QCD is not known, and no proof for gauge/gravity duality itself exists to date.…”

Section: Introductionmentioning

confidence: 99%

“…ω 1 =0 5,. ω 2 =0.05 Left: Average vorticity and polarization vector for ω2 = 0.05 as a function of angular frequency ω1 for isochronous decoupling at τ f = 10L (results are essentially insensitive to the choice of τ f ).…”

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confidence: 99%

Holographic heavy-ion collisions: Analytic solutions with longitudinal flow, elliptic flow and vorticity

2018

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We consider phenomenological consequences arising from simple analytic solutions for holographic heavy-ion collisions. For these solutions, early-time longitudinal flow is initially negative (inward), sizable direct, elliptic, and quadrangular flow is generated, and the average vorticity of the system is tunable by a single parameter. Despite large vorticity and angular momentum, we show that the system does not complete a single rotation.

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“…Classical, it appears that the spacetime generated by the limit (26) reproduces, in a patch near the horizon, the locally flat spacetime given by (25). But in the case (25) we have a unique ground state; i.e., the number of states is N = 1 (27) while in the limit (26) the number of states goes to infinity…”

Section: A the State Around The Horizonmentioning

confidence: 99%

Resolving the black hole causality paradox

Mathur

2019

Gen Relativ Gravit

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The black hole information paradox is really a combination of two problems: the causality paradox and the entanglement problem. The causality paradox arises because in the semiclassical approximation infalling matter gets causally trapped inside its own horizon; it is therefore unable to send its information back to infinity if we disallow propagation outside the light cone. We show how the causality paradox is resolved in the fuzzball paradigm. One needs to distinguish between two kinds of Rindler spaces: (a) Rindler space obtained by choosing accelerating coordinates in Minkowski space and (b) 'pseudo-Rindler' space, which describes the region near the surface of a fuzzball. These two spaces differ in their vacuum fluctuations. While low energy waves propagate the same way on both spaces, infalling objects with energies E ≫ T suffer an 'entropy enhanced tunneling' in the pseudo-Rindler spacetime (b); this leads to the nucleation of a fuzzball before the infalling object gets trapped inside a horizon. I. BLACK HOLE PUZZLESConsider a spherical shell of mass M collapsing to form a black hole. In the semiclassical approximation we find that the shell passes through its horizon at r h = 2GM , and ends at a singularity at r = 0. Hawking found that the vacuum around the horizon is unstable, and leads to the creation of particle pairs [1]. One member of the pair (carrying a net negative energy) falls into the hole and reduces its mass, while the other escapes to infinity as 'Hawking radiation'. While overall energy is conserved, there are two fundamental problems with this evaporation process:(A) The causality paradox: After the shell passes through its horizon, light cones in the region between the shell and the horizon 'point inwards' as shown schematically in fig.1. If we assume that we do not have any 'faster than light' propagation in our theory, then the information in the shell is causally trapped inside the horizon. Thus this information cannot escape to infinity as the hole evaporates away. What happens to this information at the endpoint of evaporation? (B) The entanglement problem: The process of Hawking radiation creates entangled pairs at the horizon; thus we find a monotonically increasing entanglement between the radiation near infinity and the remaining hole. Hawking's original computation was done at leading order in the semiclassical approximation, but the small corrections theorem [2] shows that this monotonic increase cannot be overcome by any source of small corrections to the pair creation process. What happens to this large entanglement near the endpoint of evaporation?These two problems together make up the black hole information paradox.One proposal to resolve both of these problems is the idea of 'remnants': the evaporation process stops due to quantum gravity effects when the hole reaches planck (a) (b) FIG. 1. (a) A shell of mass M is collapsing towards its horizon. (b) If the shell passes through its horizon, then the information it carries is trapped inside the horizon due to the structure...

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Collisions with black holes and deconfined plasmas

Cited by 23 publications

References 61 publications

Exact event horizon of a black hole merger

Exact event horizon of a black hole merger

Holographic heavy-ion collisions: Analytic solutions with longitudinal flow, elliptic flow and vorticity

Resolving the black hole causality paradox

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