Showing papers on "Black hole thermodynamics published in 1984"
TL;DR: In this paper, a systematic development is given of the view that in the case of systems with long-range forces and which are therefore nonextensive (in some sense) some thermodynamic results do not hold.
Abstract: A systematic development is given of the view that in the case of systems with long-range forces and which are therefore nonextensive (in some sense) some thermodynamic results do not hold. Among these is the relationU − TS + pΝ = ΜN and the Gibbs-Duhem equation. If a search for an equilibrium state is made by maximization of the entropy one may obtain misleading results because superadditivity may be violated. The considerations are worked out for a simple gas model, but they are relevant to black hole thermodynamics. Rather general conclusions can be drawn which transcend special systems.
128 citations
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TL;DR: In this article, the Unruh-Wald scenario for mining quantum black holes is applied to de Sitter space and the following questions are addressed: will the generalized second law of thermodynamics be maintained for deSitter horizons?
Abstract: The Unruh-Wald scenario for mining quantum black holes is applied to de Sitter space. The following questions are addressed: Will the generalized second law of thermodynamics be maintained for de Sitter horizons. Does the mining process allow the recovery of unlimited energy from the cosmological gravitational field. The evaporation of a black hole in de Sitter space is also investigated in the context of the second law.
61 citations
TL;DR: There are two inequivalent ways in which the laws of physics in a gravitational field can be related to the laws in an inertial frame, when quantum mechanical effects are taken into account as mentioned in this paper.
53 citations
TL;DR: In this paper, a singular family of solutions of the Tolman-Oppenheimer-Volkoff (TOV) equation is described to represent a self-gravitating perfect fluid (i.e., photon gas) of temperature T_(BH) =(8πM)^(−1) in equilibrium with a Schwarzschild black hole.
Abstract: Thermodynamic equilibrium of a self-gravitating perfect fluid for a spherically symmetric system containing a black hole of mass M is investigated by means of the Tolman-Oppenheimer-Volkoff (TOV) equation. A singular family of solutions of the TOV equation is described. At r≫2M these solutions can be used to represent a perfect fluid (i.e., photon gas) of temperature T_(BH) =(8πM)^(−1) in equilibrium with a Schwarzschild black hole. The energy density is positive at all r>0. A singular negative point mass resides at r=0.
37 citations
TL;DR: In this paper, a method of constructing an analytical expression for the renormalized vacuum expectation value of the stress tensor and the mean-square field for a conformally invariant scalar field propagating on static space-times is presented.
Abstract: A method of constructing an analytical expression for the renormalized vacuum expectation value of the stress tensor and the mean-square field for a conformally invariant scalar field propagating on static space-times is presented. Particular emphasis is given to the case where the background geometry corresponds to a general spherically symmetric black hole, and explicit results are given for an extremal Reissner-Nordstroem black hole. In the special case of a Schwarzschild black hole, Page's results are recovered. Possible extensions of the method to cover stationary black holes are briefly discussed.
27 citations
TL;DR: In this paper, the back reaction equations for a spherically symmetric evaporating black hole space-time were investigated and a solution which reproduces Hawking's formula for the evaporation rate was shown to exist.
Abstract: The back reaction equations for a spherically symmetric evaporating black hole space-time are investigated. A solution which reproduces Hawking's formula for the evaporation rate is shown to exist.
22 citations
TL;DR: In this article, a theory of black holes under the assumption of weak cosmic censorship is developed, which includes the theory of Black Holes in the future asymptotically predictable spacetimes as a special case but it also applies to the cosmological situations including models with nonzero cosmologically constant of both signs.
Abstract: A theory of black holes is developed under the assumption of the weak cosmic censorship. It includes Hawking's theory of black holes in the future asymptotically predictable spacetimes as a special case but it also applies to the cosmological situations including models with nonzero cosmological constant of both signs.
12 citations
TL;DR: In this paper, the stability of thermodynamical equilibrium between a Schwarzschild black hole and its own radiation is refined by the use of Page's expression for the renormalized stress energy tensor.
Abstract: The Hawking criterion for the stability of thermodynamical equilibrium between a Schwarzschild black hole and its own radiation is refined by the use of Page's expression for the renormalized stress-energy tensor.
12 citations
TL;DR: The theory of black holes developed by Hawking in asymptotically flat space-times is generalized so that black holes in the cosmological situations are included as mentioned in this paper, assuming that the strong version of the Penrose cosmic censorship hypothesis holds.
Abstract: The theory of black holes developed by Hawking in asymptotically flat space-times is generalized so that black holes in the cosmological situations are included. It is assumed that the strong version of the Penrose cosmic censorship hypothesis holds.
9 citations
TL;DR: An upper bound for entropy is derived that is slightly stricter than that obtained by Bekenstein and is independent of black-hole thermodynamics.
Abstract: An upper bound for entropy is derived This bound is slightly stricter than that obtained by Bekenstein and is independent of black-hole thermodynamics
TL;DR: In this paper, it was argued that the scalar field needed by Agnese and La Camera for their demonstration that black holes do not exist is due to quantum effects, and it was further argued that quantum effects are responsible for the existence of black holes.
Abstract: It is argued that the scalar field, needed by Agnese and La Camera for their demonstration that black holes do not exist, is due to quantum effects.
TL;DR: This article treated a black hole as a relativistic gas of micro-black holes (planckions) which have fermionic character and derived expressions for some thermodynamic quantities.
Abstract: Treating a black hole as a relativistic gas of microblack holes (planckions) which have fermionic character, expressions for some thermodynamic quantities are obtained These have the same structure as those obtained by Hawking by other considerations
TL;DR: The case of placing a Schwarzschild black hole inside an ideal reflecting box, thereby setting up an equilibrium state, has been studied in this article, where the authors discuss the thennodynamical properties of such a system.
01 Jan 1984
01 Jan 1984
01 Jan 1984
TL;DR: In this paper, it was shown that using black holes does not work in the generalised second law case, and that the reason for this is due to the physical consequences of the thermal radiation seen in the vacuum by an accelerated observer.
Abstract: This note will give a brief report of some work which R. Wald and I1 have done recently. We have discovered that at least one possible technique for violating the generalised second law by using black holes does not work. The reason it does not work is rather surprising in that it makes fundamental use of the physical consequences of the thermal radiation seen in the vacuum by an accelerated observer.
01 Jan 1984
TL;DR: The work of Bekenstein and Hawking as discussed by the authors indicates that one may assign an entropy to the spacetime structure represented by the hole, given in the Schwarzschild case by Sbh = 1/4 A/G= 4 GM2 (1) where A is the event horizon area, M the mass, and I have used units with K = c = k = 1.
Abstract: One of the most enduring and persuasive results of one-loop quantum gravity calculations is the unexpected connection between black holes and thermodynamics. The work of Bekenstein1 and Hawking2 indicates that one may assign an entropy to the spacetime structure represented by the hole, given in the Schwarzschild case by Sbh = 1/4 A/G= 4 GM2 (1) where A is the event horizon area, M the mass, and I have used units with K = c = k = 1.
01 Jan 1984