Stationary BPS Solutions in N=2 Supergravity with R^2-Interactions

By G. Cardoso, B. Wit, J. Käppeli, T. Mohaupt. 2000

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We analyze a broad class of stationary solutions with residual N = 1 supersymmetry of four-dimensional N = 2 supergravity theories with terms quadratic in the Weyl tensor. These terms are encoded in a holomorphic function, which determines the most relevant part of the action and which plays a central role in our analysis. The solutions include extremal black holes and rotating field configurations, and may have multiple centers. We prove that they are expressed in terms of harmonic functions associated with the electric and magnetic charges carried by the solutions by a proper generalization of the so-called stabilization equations. Electric/magnetic duality is manifest throughout the analysis. We also prove that spacetimes with unbroken supersymmetry are fully determined by electric and magnetic charges. This result establishes the so-called fixed-point behavior according to which the moduli fields must flow towards certain prescribed values on a fully supersymmetric horizon, but now in a more general context with higher-order curvature interactions. We briefly comment on the implications of our results for the metric on the moduli space of extremal black hole solutions.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/0cb62275b0a3b59462eb8524b546f80a53db4855

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Citations in the corpus

Precision Counting of Small Black Holes (2005, background): “the one-loop topological amplitude F 1), it was shown recently that the black hole develops a smooth horizon, with a similar geometry AdS 2 × S2 × X as found in the large black hole case [36,37] (see [13,38,39] for earlier work on this subject). Moreover, the Bekenstein-Hawking-Wald entropy, taking ”
Split states, entropy enigmas, holes and halos (2007, background): “We neglect R(2) corrections [62], which is justified in the large charge limit”
Black hole microstates and attractor without supersymmetry (2006, background): “) cases supersymmetry will prevent lifting of these ﬂat directions by higher derivative terms and associated runaway behavior, especially if the near horizon geometry has enhanced supersymmetry as in [5, 6, 45, 8]. Hence the entropy of such black holes remains well-deﬁned. For non-BPS black holes th”
Exact solutions for supersymmetric stationary black hole composites (2003, unknown): “Type IIB string theory on Xτ is mirror (or T-dual 3) to IIA on Y = E ′τ ×E ′τ ×E ′τ , with E ′τ the 2-torus with area a = Im τ and B-field flux b = Re τ (which together determine the complexified Kähler class of Y ).”
Exact and Asymptotic Degeneracies of Small Black Holes (2005, methodology): “Indeed, for a subclass of higher derivative terms that are determined by the topological string amplitudes, the corrected black hole solution can be determined using the generalized attractor equations [5,6,7,8,30].”
Black hole entropy function, attractors and precision counting of microstates (2007, methodology): “13) gives the expression for the entropy of these black holes as written down in [84,85,86,72,87,83,88,89,2].”
Near-horizon symmetries of extremal black holes (2007, background): “ depend on any moduli of the theory. It was initially discovered for supersymmetric black holes [1, 2, 3], then realized that it still applies in the presence of certain higher-derivative corrections [4, 5, 6], and most recently extended to non-supersymmetric black holes [7, 8, 9]. This has led to a”