Black holes in static electrovac space-times

“…Here we review background material used in the following chapters and the main asymptotically flat black hole solutions of Einstein theory. According to the no-hair theorems [12,33,37,50,66,67], the Schwarzschild and Kerr spacetimes and their charged (Reissner-Nordström and Kerr-Newman) generalizations are the generic asymptotically flat electrovacuum black hole solutions of this theory. In General Relativity a black hole formed by gravitational collapse will settle down to a state determined by only three parameters: its mass M, angular momentum J, and electric charge Q, irrespective of the initial configuration, the nature of the collapsing matter, and the details of the collapse.…”

Section: Stationary Black Holes Of General Relativitymentioning

confidence: 99%

Stationary Black Holes in General Relativity

Faraoni

2015

Cosmological and Black Hole Apparent Horizons

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The noblest pleasure is the joy of understanding.-Leonardo da Vinci IntroductionBeginning with the Rindler horizons which appear for accelerated observers in Minkowski space without gravity, one comes quickly to acknowledge the presence of various types of horizons when gravity is introduced in spacetime: first one encounters black hole horizons and cosmological horizons. Then, studying classical and semiclassical black holes one is faced with inner, outer, Cauchy, and extremal horizons. The early literature on black holes and the works which developed black hole thermodynamics in the seventies had plenty to do with discussing stationary black holes and event horizons (e.g., [23,74,75]). Dynamical situations such as gravitational collapse, black hole evaporation due to Hawking radiation, and black holes interacting with non-trivial environments and exchanging mass-energy require that the concept of event horizon be generalized to some other construct with which it is possible to work. Conceivable dynamical situations include black holes accreting or expelling gravitating (i.e., non-test) matter; examples are Vaidya spacetimes, black holes immersed in a cosmological "background" other than de Sitter space, black holes emitting (and possibly also absorbing) Hawking radiation (which becomes significant in the last evolutionary stages with backreaction playing an important role), or black holes with variable mass because of other physical processes. If a black hole is placed in a non-trivial environment, its mass-energy should be also the internal energy which we need to account for in the first law of thermodynamics. This mass-energy must be defined carefully; usually it is identified with some quasi-local energy construct which is related to the notion of horizon. In these lectures we will use the Misner-Sharp-Hernandez mass in spherical symmetry and its generalization, the Hawking-Hayward quasi-local energy in the absence of spherical symmetry.Intuitively, an horizon is "a frontier between things observable and things unobservable" [64]. Inequivalent notions of black hole horizon abound in the technical literature and the terminology used features event,

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“…The developments in the uniqueness of static electro-vacuum black holes went in parallel to the developments in the vacuum case. Some remarkable works which played an important role in the general proof of the uniqueness of static electro-vacuum black holes are, 39,50,58,55,59,45,25,30 where again the doubling method played a fundamental role. Uniqueness of static black holes using the doubling method has also been proved for other matter models, as for instance the Einstein-Maxwell-dilaton model.…”

Section: Uniqueness Theorems For Black Holesmentioning

confidence: 99%

On Uniqueness Results for Static, Asymptotically Flat Initial Data Containing MOTS

Carrasco¹,

Mars²

2013

Black Holes

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Marginally outer trapped surfaces are widely believed to be useful quasi-local, dynamical replacements for black holes. It is also expected that in a stationary situation both concepts should essentially concide. In this contribution we explore this expectation by studying whether the uniqueness theorems for static black holes extend to static spacetimes contaning a spacelike hypersurface, possibly with boundary, which includes an asymptotically flat end and a marginally outer trapped surface (MOTS) which is bounding with respect to that end. We conclude that, under suitable conditions which involve no global-in-time assumptions, the answer to this question is affirmative. The matter model is arbitrary except for the condition that it satisfies the null energy condition and it admits a static black hole uniqueness proof using the doubling method of Bunting and Masoodul-Alam.

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Black holes in static electrovac space-times

Cited by 52 publications

References 6 publications

Matter outside a static higher-dimensional black hole

Matter outside a static higher-dimensional black hole

Stationary Black Holes in General Relativity

On Uniqueness Results for Static, Asymptotically Flat Initial Data Containing MOTS

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