Moduli, Scalar Charges, and the First Law of Black Hole Thermodynamics

Gibbons, G. W.; Каллош, Рената; Kol, Barak

doi:10.1103/physrevlett.77.4992

Cited by 272 publications

(423 citation statements)

References 12 publications

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“…In [13] such calculations were extended (in 5 dimensions) to the case where the emitted energy is comparable to the appropriately defined left and right moving temperatures, which yields agreement for the greybody factor of the black hole in this domain. Such greybody factors agree also in 4 dimensions [14], and for the absorption of the non-minimally coupled 'fixed scalars' [15,16,17] in 5 dimensions [18] and in 4 dimensions [19].…”

Section: Introductionmentioning

confidence: 84%

Black hole greybody factors and absorption of scalars by effective strings

1997

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We compute the greybody factors for classical black holes in a domain where two kinds of charges and their anticharges are excited by the extra energy over extremality. We compare the result to the greybody factors expected from an effective string model which was earlier shown to give the correct entropy. In the regime where the left and right moving temperatures are much smaller than the square root of the effective string tension, we find a non-trivial greybody factor which agrees with the effective string model. However, if the temperatures are comparable with the square root of the effective string tension, the greybody factors agree only at the leading order in energy. Nevertheless, there are several interesting relations between the two results, suggesting that a modification of the effective string model might lead to better agreement.

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Section: Introductionmentioning

confidence: 84%

Black hole greybody factors and absorption of scalars by effective strings

1997

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“…It is known [5] that by eliminating the vector fields via their equations of motion this system may be reduced to the following set of field equations for the metric function U(τ ) and the scalar fields Φ r (τ ) in terms of the evolution parameter τ : 5) together with the constraint 6) where V BH (Φ, p, q) is a function of the scalars and of the electric and magnetic charges of the theory defined by:…”

Section: Jhep11(2007)032mentioning

confidence: 99%

“…For static, spherically symmetric black holes, the fixed values of the scalars at the horizon are determined in terms of the quantized electric and magnetic charges characterizing the solution, as extrema of an effective potential V BH [5]. This induces to expect the radial dependence of the scalar fields in each extremal solution to admit a description in terms of a system of first order equations:…”

Section: Introductionmentioning

confidence: 99%

First order description of black holes in moduli space

Andrianopoli¹,

D’Auria²,

Orazi³

et al. 2007

J. High Energy Phys.

104

250

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We show that the second order field equations characterizing extremal solutions for spherically symmetric, stationary black holes are in fact implied by a system of first order equations given in terms of a prepotential W . This confirms and generalizes the results in [14]. Moreover we prove that the squared prepotential function shares the same properties of a c-function and that it interpolates between M 2 ADM and M 2 BR , the parameter of the near-horizon Bertotti-Robinson geometry. When the black holes are solutions of extended supergravities we are able to find an explicit expression for the prepotentials, valid at any radial distance from the horizon, which reproduces all the attractors of the four dimensional N > 2 theories. Far from the horizon, however, for N -even, our ansatz poses a constraint on one of the U-duality invariants for the non-BPS solutions with Z = 0. We discuss a possible extension of our considerations to the non extremal case.

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“…The possibility of a thermodynamic geometry for extremal black holes was first alluded to in the context of Type II supergravities with special geometry of the moduli space [10]. In accordance with the first law of thermodynamics, the equilibrium state space for these black holes would now also involve the moduli fields at asymptotic infinity apart from the electric and the magnetic charges [22] as extensive thermodynamic variables. This, in general, leads to a curved equilibrium thermodynamic state space.…”

Section: Introductionmentioning

confidence: 99%

Thermodynamic geometry and extremal black holes in string theory

Sarkar

Sengupta

Tiwari

2008

J. High Energy Phys.

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We study a generalisation of thermodynamic geometry to degenerate quantum ground states at zero temperatures exemplified by charged extremal black holes in type II string theories. Several examples of extremal charged black holes with non degenerate thermodynamic geometries and finite but non zero state space scalar curvatures are established. These include black holes described by D1-D5-P and D2-D6-NS5-P brane systems and also two charged small black holes in Type II string theories. We also explore the modifications to the state space geometry and the scalar curvature due to the higher derivative contributions and string loop corrections as well as an exact entropy expression from quantum information theory. Our construction describes state space geometries arising out of a possible limiting thermodynamic characterisation of degenerate quantum ground states at zero temperatures.

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Moduli, Scalar Charges, and the First Law of Black Hole Thermodynamics

Cited by 272 publications

References 12 publications

Black hole greybody factors and absorption of scalars by effective strings

Black hole greybody factors and absorption of scalars by effective strings

First order description of black holes in moduli space

Thermodynamic geometry and extremal black holes in string theory

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