A stringy cloak for a classical singularity
By A. Dabholkar, R. Kallosh, A. Maloney. 2004
214 citations recorded by the source corpus.
We consider a class of 4D supersymmetric black hole solutions, arising from string theory compactifications, which classically have vanishing horizon area and singular space-time geometry. String theory motivates the inclusion of higher derivative terms, which convert these singular classical solutions into regular black holes with finite horizon area. In particular, the supersymmetric attractor equations imply that the central charge, which determines the radius of the AdS2 × S2 near horizon geometry, acquires a non-vanishing value due to quantum effects. In this case quantum corrections to the Bekenstein-Hawking relation between entropy and area are large. This is the first explicit example where stringy quantum gravity effects replace a classical null singularity by a black hole with finite horizon area.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Statistical and Nonlinear Physics
View Paper: https://www.semanticscholar.org/paper/8dc68482b4617999132ff5d090e08b9eee5a25a0
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Citations in the corpus
- Wald's entropy is equal to a quarter of the horizon area in units of the effective gravitational coupling (2007, background): “(70) The factor of 2 difference between Wald’s entropy and the Bekenstein-Hawking entropy has been somewhat of a puzzle since its discovery in the context of N = 2 SUGRA [15].”
- Black hole microstates and attractor without supersymmetry (2006, methodology): “In fact in the case of small black holes the higher derivative corrections actually create the AdS2 × S near horizon geometry even though in the supergravity approximation the geometry is singular[10, 11].”
- Precision Counting of Small Black Holes (2005, methodology): “Moreover, the Bekenstein-Hawking-Wald entropy, taking into account this R(2) correction, matches the microscopic entropy in leading order, including the precise numerical coefficient [36, 37].”
- Microscopic black hole entropy in theories with higher derivatives (2005, unknown): “June, 2005 1 pkraus@physics.ucla.edu 2 larsenf@umich.edu”
- Rotating Attractors (2006, background): “These examples include non-supersymmetric theories, actions with higher derivative corrections, extremal black holes in higher dimensions etc.[4, 5, 6, 7, 8, 9, 10, 11, 12, 13, 14, 15, 16, 17, 18, 19, 20, 21, 22, 23, 24, 25, 26, 27, 28, 29, 30, 31, 32, 33, 34, 35, 36, 37, 38, 39].”
- Quantum Black Holes, Wall Crossing, and Mock Modular Forms (2012, background): “his expectation. This fact was indeed one of the early indications of a possible duality between heterotic and Type-II strings [120]. The DH-states correspond to the microstates of a small black hole [103, 28, 40] for large n. The macroscopic entropy S(n) of these black holes should equal the asympt”
- Exact and Asymptotic Degeneracies of Small Black Holes (2005, background): “The corrected solution has a smooth horizon with string scale area in the heterotic string metric [23,31,32,33,34].”
- Black hole entropy function, attractors and precision counting of microstates (2007, background): “As we have seen, this phenomenon can be demonstrated explicitly for purely electrically charged small black holes representing fundamental heterotic string [96, 98, 99, 100, 101, 174, 175, 176, 19] and hence also their S-dual purely magnetic states.”
- Lectures on black holes, topological strings and quantum attractors (2006, result): “This is in fact confirmed by a study of the corrected geometry [104, 105].”
- Black Holes, Qubits and Octonions (2008, unknown): “See also [142, 143, 144, 145, 146, 147].”