Asymptotically flat, stable black hole solutions in Einstein--Yang-Mills--Chern-Simons theory

D. H. Tchrakian; Eugen Radu; Yves Brihaye

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Asymptotically flat, stable black hole solutions in Einstein--Yang-Mills--Chern-Simons theory

Yves Brihaye, Eugen Radu, D. H. Tchrakian

High Energy Physics - Theory · Submitted 7 Nov 2010

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The authors' main claim We construct finite mass, asymptotically flat black hole solutions in d=5 Einstein--Yang-Mills--Chern-Simons theory.

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arXiv ID1011.1624 (version 1)

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CitationD. H. Tchrakian, Eugen Radu, Yves Brihaye. "Asymptotically flat, stable black hole solutions in Einstein--Yang-Mills--Chern-Simons theory." arXiv:1011.1624 (2010). https://pith.science/paper/NAUBOMT7

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What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.42 · human participants 0.01 · controlled comparison 0.16 · randomized assignment 0.01 · states quantitative result 0.31 · compares with prior results 0.51 · mentions code or data availability 0.02.

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We construct finite mass, asymptotically flat black hole solutions in d=5 Einstein--Yang-Mills--Chern-Simons theory. Our results indicate the existence of a second order phase transition between Reissner-Nordstrom solutions and the non-Abelian black holes which generically are thermodynamically preferred. Some of the non-Abelian configurations are also stable under linear, spherically symmetric perturbations. In addition a solution in closed form describing an extremal black hole with non-Abelian hair is found for a special value of the Chern-Simons coupling constant.

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#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We construct finite mass, asymptotically flat black hole solutions in d=5 Einstein--Yang-Mills--Chern-Simons theory.	contribution 0.94	0.97	0.39	asserted 1.00
s1	Our results indicate the existence of a second order phase transition between Reissner-Nordstrom solutions and the non-Abelian black holes which generically are thermodynamically preferred.	interpretation 0.59	0.86	0.46	hedged possibility 1.00
s2	Some of the non-Abelian configurations are also stable under linear, spherically symmetric perturbations.	result 0.99	0.87	0.11	asserted 0.73
s3	In addition a solution in closed form describing an extremal black hole with non-Abelian hair is found for a special value of the Chern-Simons coupling constant.	result 0.87	0.97	0.11	asserted 1.00

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Original abstract

We construct finite mass, asymptotically flat black hole solutions in d=5 Einstein--Yang-Mills--Chern-Simons theory. Our results indicate the existence of a second order phase transition between Reissner-Nordstrom solutions and the non-Abelian black holes which generically are thermodynamically preferred. Some of the non-Abelian configurations are also stable under linear, spherically symmetric perturbations. In addition a solution in closed form describing an extremal black hole with non-Abelian hair is found for a special value of the Chern-Simons coupling constant.

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8 arXiv papers cite this in 13 sentences

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Moreover, for the same values of the mass and electric charge, the RN solution typically has a smaller event horizon radius (and thus a smaller entropy), than the nA black hole [ref] .

Einstein-Yang-Mills-Chern-Simons solutions in D=2n+1 dimensions · The thermodynamics of solutions · 0.81
We remark that, for $d=5$, a rather similar picture is found when considering instead solutions in a Einstein–Yang-Mills–Chern-Simons model [ref] , the Chern-Simons term providing an alternative to the higher order curvature terms of the YM hierarchy employed here.

Reissner-Nordstr\"om black holes with non-Abelian hair · Further remarks · 0.96

Cites it as background 1 paper

More details on the properties of the $Λ=0$ configurations togheter with typical profiles can be found in [ref] , [ref] .

An instability of the Reissner-Nordstrom solution and new hairy black holes in d=5 dimensions · The cases $Λ≤0$ · 0.85

What it cites · 9 sentences without a confident label

Builds on 1 paper

This configuration describes a non-Abelian deformation of the extremal RN-de Sitter black holes in [ref] .

Cosmological Multi-Black Hole Solutions · Introduction · 0.84

Uses the method or tool of 4 papers

We note only that, by using the approach in [ref] we have found that the EYMCS solutions with one node in $w(r)$ we have constructed are indeed unstable.

Instability of Gravitating Sphalerons · Introduction · 0.91
In the special case $κ=1/8$, following the approach in [ref] , one finds the following exact solution of the EYMCS equations within the general Ansatz ([ref]), ([ref]): [equation] where $Q≥2$ and $J$ are arbitrary parameters.

Supersymmetric Self-Gravitating Solitons · Introduction · 0.88
By using the methods in [ref] , [ref] , one finds that ([ref]) shares the basic features of the $J=0$ Abelian configuration.

Reissner-Nordstrom-de Sitter black hole, planar coordinates and dS/CFT · Introduction · 0.91

Compares with 2 papers

However, given the presence of several branches, the picture is more complicated for asymptotically flat solutions and we could not find so far simple universal relations between the relevant parameters as those found in [ref] in the AdS case.

Colorful horizons with charge in anti-de Sitter space · Introduction · 0.98
One should note that, despite the different asymptotic structure of spacetime and the different horizon topology, the solutions in this work have some similarities with the colorful black holes with charge in Anti-de Sitter (AdS) space [ref] , which provide a model of holographic superconductors.

New AdS non Abelian black holes with superconducting horizons · Introduction · 1.00

Cites as background 1 paper

In the Abelian case this leads to some new features for rotating black holes only [ref] .

Black Holes of D=5 Supergravity · Introduction · 0.88

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