Rotating Attractors

By D. Astefanesei, K. Goldstein, Rudra P. Jena, Ashoke Sen, S. Trivedi. 2006

269 citations recorded by the source corpus.

We prove that, in a general higher derivative theory of gravity coupled to abelian gauge ﬁelds and neutral scalar ﬁelds, the entropy and the near horizon background of a rotating extremal black hole is obtained by extremizing an entropy function which depends only on the parameters labeling the near horizon background and the electric and magnetic charges and angular momentum carried by the black hole. If the entropy function has a unique extremum then this extremum must be independent of the asymptotic values of the moduli scalar ﬁelds and the solution exhibits attractor behaviour. If the entropy function has ﬂat directions then the near horizon background is not uniquely determined by the extremization equations and could depend on the asymptotic data on the moduli ﬁelds, but the value of the entropy is still independent of this asymptotic data. We illustrate these results in the context of two derivative theories of gravity in several examples. These include Kerr black hole, Kerr-Newman black hole, black holes in Kaluza-Klein theory, and black holes in toroidally compactiﬁed heterotic string theory.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/649868aa1ed769aea5dbc960315bb38b32f8cba9

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

Central charges in extreme black hole/CFT correspondence (2009, unknown): “The near horizon geometry has the enhanced isometry SL(2, R) × U(1), as was observed earlier using the attractor mechanism [27, 28], and the scalar and vector fields are also invariant under this symmetry.”
Black hole entropy function, attractors and precision counting of microstates (2007, methodology): “If we denote by f (i) mn and fmn the field strengths associated with the three dimensional gauge fields a (i) m and am respectively, (7)Our convention for α differs from the one used in [24] by a minus sign.”
Quantum Entropy Function from AdS(2)/CFT(1) Correspondence (2008, unknown): “Contents”
A classification of near-horizon geometries of extremal vacuum black holes (2008, background): “In the case of extremal but non-supersymmetric black holes, the attractor mechanism was established upon the assumption that the near-horizon geometry of an extremal black hole must have an SO(2, 1) symmetry [21].”
Logarithmic corrections to rotating extremal black hole entropy in four and five dimensions (2011, background): “Some examples of such metrics can be found in [62] (in a different coordinate system for labelling AdS2 metric).”
Black hole microstates and attractor without supersymmetry (2006, background): “Extremal spinning black holes also display attractor behavior which can be understood from the existence of the underlying entropy function [67].”
Non-supersymmetric attractors (2005, methodology): “5) and then following [51], the entropy function is”
Large rotating AdS black holes from fluid mechanics (2007, background): “In particular, Astefanesei, Goldstein, Jena, Sen and Trivedi [33] have recently argued that the attractor mechanism applies to rotating extremal black holes, and have derived a differential equation that determines the attractor geometry (and gauge field distribution, etc.”
Arithmetic of quantum entropy function (2009, background): “Now QEF computes the degeneracy of states of a fixed angular momentum, just as it computes the degeneracy of states of a fixed charge, since from the point of view of the two dimensional string theory living on AdS2 the angular momentum can be regarded as a component of the electric charge vector [3”
Near extremal black hole entropy as entanglement entropy via AdS 2 / CFT 1 (2007, background): “Recently, it has been shown that extremal (rotating) black holes always have the SO(2, 1) symmetry in the near horizon limit [2, 3, 4].”
The Lovelock Black Holes (2008, background): “oles, and it was explicitly shown that (32) is recovered by analyzing the near horizon geometry. A rather general analysis was presented in Ref. [137]. Very interesting discussions are those of Refs. [138, 139]. The thermodynamic properties of topological black holes are also very interesting; see f”
Near-horizon symmetries of extremal black holes (2007, background): “ to a symmetry of the full metric, so the full isometry group is O(2,1)×U(1) where the U(1) arises from the axisymmetry of the black hole (generated by ∂/∂φ) [20]. Other 4d examples are considered in [18], with the conclusion that they also have O(2,1)×U(1) isometry group in the near-horizon limit. ”
Entropy function and AdS2/CFT1 correspondence (2008, background): “For an extremal black hole whose near horizon geometry has an AdS2 factor, this formula may be encoded in the entropy function formlism that reduces the problem of computing the entropy into a purely algebraic problem for spherically symmetric black holes [5] and a problem involving solution of simp”