Black holes in general relativity

By Matt Visser. 2009

561 citations recorded by the source corpus.

What is going on (as of August 2008) at the interface between theoretical general relativity, string-inspired models, and observational astrophysics? Quite a lot. In this mini-survey I will make a personal choice and focus on four specific questions: Do black holes "exist"? (For selected values of the word "exist".) Is black hole formation and evaporation unitary? Can one mimic a black hole to arbitrary accuracy? Can one detect the presence of a horizon using local physics?

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/8252c6a2324feb661b79c61f6e148fa7a0d08459

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Citations in the corpus

The 1965 Penrose singularity theorem (2014, background): “The parallelism between MOTS and minimal hypersurfaces in Riemannian spaces can be explored further, and one can actually solve the Plateau problem for MOTS, that is, the existence of MOTS spanning a given, prescribed, boundary [95].”
Superradiance: Energy Extraction, Black-Hole Bombs and Implications for Astrophysics and Particle Physics (2015, background): “A special feature of vacuum stationary GR solutions is their axisymmetry [215].”
Holographic thermalization, quasinormal modes and superradiance in Kerr-AdS (2013, background): “However, it does not violate the rigidity theorems [36, 37, 38].”
Black holes with only one Killing field (2011, background): “This is not just due to the fact that finding analytic solutions of Einstein’s equation usually requires the assumption of symmetries, but also follows from theorems which say that stationary black holes must be axisymmetric [1, 2, 3].”
Uniqueness Theorem for 5-Dimensional Black Holes with Two Axial Killing Fields (2007, background): “In this regard, the situation in 5 dimensions is very different from the anal ogous situation in 4 dimensions: Here the original rigidity theorem [15, 16, 5, 30, 28, 8] also guarantees the existence of one axial Killing field.”
Energy conditions in general relativity and quantum field theory (2020, background): “For a four-dimensional stationary black hole, if Σ ∩ H is compact and if the DEC holds, Hawking has shown that each connected component of Σ ∩ H must be homeomorphic to a sphere [159].”
Born–Infeld inspired modifications of gravity (2017, methodology): “On the other hand, the very connection between Hawking’s radiation [199] and standard thermodynamic systems still calls for an understanding in terms of hypothetical black hole microscopic degrees of freedom, and the controversy about the potential existence of firewalls at the event horizon still g”
A Primer on Energy Conditions (2014, background): “Then the theorem, as first conjectured by Yau [214], is as follows: let (M , gab) be a timelike geodesically complete spacetime satisfying the SEC; if it contains a timelike line, then it is isometric erik@strangebeautiful.com 2. a stationary, asymptotically flat black hole is topologically S252 [10”
Present status of the Penrose inequality (2009, background): “Under this restriction, the Penrose heuristic argument implies [79],[52],”
Approximate Universal Relations for Neutron Stars and Quark Stars (2016, background): “Hawking proved that all stationary black holes must (i) have a horizon with a spherical topology and (ii) must be either static or axially symmetric [20, 21].”
Essentials of blackfold dynamics (2009, methodology): “17) The conditions that κ and Ωi must remain uniform over the blackfold worldvolume were referred to in [1] as the blackness conditions and were imposed, invoking general theorems for stationary black holes — zeroth law of black hole mechanics and horizon rigidity [31, 32, 33] —, as necessary condit”
Kerr black holes with Proca hair (2016, methodology): “For matter obeying the null energy condition, the rigidity theorem implies that the spacetime is also axi-symmetric [6].”
Radial pulsations and stability of anisotropic stars with a quasi-local equation of state (2010, methodology): “which is used as an example of a non-local variable in [24, 25] can, in fact, be understood as a quasi-local variable since ρ = 3m/4r(3)π = 3μ/8πr(2), where μ = 2m/r and r are acceptable quasi-local variables [4, 23].”
Stability of marginally outer trapped surfaces and existence of marginally outer trapped tubes (2007, background): “Hawking’s analysis was extended by Newman [20] who calculated the general variation δv of the expansion θ with respect to any transversal direction v.”
Colloquium: Stimulating uncertainty: Amplifying the quantum vacuum with superconducting circuits (2011, methodology): “This idea was used by (Hawking, 1972) to prove that any physical process necessarily increases the surface area of a black hole dABH ≥ 0.”
The Kerr metric (2014, background): “These ideas were synthesized and extended by Bardeen, Carter, and Hawking [41].”
Black hole chemistry: thermodynamics with Lambda (2016, background): “The first indication linking these two subjects came from Hawking’s area theorem [30], which states that the area of the event horizon of a black hole can never decrease5.”