arXiv subjects

Yoav Peleg

Publications and source records attributed to Yoav Peleg.

14 recordsLinked to original sources

arXiv1997

Lorentzian Approach to Black Hole Thermodynamics in the Hamiltonian Formulation

In this work, we extend the analysis of Brown and York to find the quasilocal energy in a spherical box in the Schwarzschild spacetime. Quasilocal energy is the value of the Hamiltonian that generates unit magnitude proper-time translations on the box orthogonal to the spatial hypersurfaces foliating the Schwarzschild spacetime. We call this Hamiltonian the Brown-York Hamiltonian. We find different classes of foliations that correspond to time-evolution by the Brown-York Hamiltonian. We show that although the Brown-York expression for the quasilocal energy is correct, one needs to supplement their derivation with an extra set of boundary conditions on the interior end of the spatial hypersurfaces inside the hole in order to obtain it from an action principle. Replacing this set of boundary conditions with another set yields the Louko-Whiting Hamiltonian, which corresponds to time-evolution of spatial hypersurfaces in a different foliation of the Schwarzschild spacetime. We argue that in the thermodynamical picture, the Brown-York Hamiltonian corresponds to the internal energy whereas the Louko-Whiting Hamiltonian corresponds to the Helmholtz free energy of the system. Unlike what has been the usual route to black hole thermodynamics in the past, this observation immediately allows us to obtain the partition function of such a system without resorting to any kind of Euclideanization of either the Hamiltonian or the action. In the process, we obtain some interesting insights into the geometrical nature of black hole thermodynamics.

gr-qc↗

arXiv1996

Choptuik Scaling and Quantum Effects in 2D Dilaton Gravity

We study numerically the collapse of massless scalar fields in two-dimensional dilaton gravity, both classically and semiclassically. At the classical level, we find that the black hole mass scales at threshold like $M_{\rm bh} \propto |p-p^*|^γ$, where $γ\simeq 0.53$. At the semiclassical level, we find that in general $M_{\rm bh}$ approaches a non-zero constant as $p \rightarrow p^*$. Thus, quantum effects produce a mass gap not present classically at the onset of black hole formation.

gr-qc↗

arXiv1996

Predictability and Semiclassical Approximation at the onset of Black Hole formation

We combine analytical and numerical techniques to study the collapse of conformally coupled massless scalar fields in semiclassical 2D dilaton gravity, with emphasis on solutions just below criticality when a black hole almost forms. We study classical information and quantum correlations. We show explicitly how recovery of information encoded in the classical initial data from the outgoing classical radiation becomes more difficult as criticality is approached. The outgoing quantum radiation consists of a positive-energy flux, which is essentially the standard Hawking radiation, followed by a negative-energy flux which ensures energy conservation and guarantees unitary evolution through strong correlations with the positive-energy Hawking radiation. As one reaches the critical solution there is a breakdown of unitarity. We show that this breakdown of predictability is intimately related to a breakdown of the semiclassical approximation.

hep-th↗

arXiv1996

Hamiltonian thermodynamics of two-dimensional vacuum dilatonic black holes

We consider the Hamiltonian dynamics and thermodynamics of the two-dimensional vacuum dilatonic black hole in the presence of a timelike boundary with a fixed value of the dilaton field. A~canonical transformation, previously developed by Varadarajan and Lau, allows a reduction of the classical dynamics into an unconstrained Hamiltonian system with one canonical pair of degrees of freedom. The reduced theory is quantized, and a partition function of a canonical ensemble is obtained as the trace of the analytically continued time evolution operator. The partition function exists for any values of the dilaton field and the temperature at the boundary, and the heat capacity is always positive. For temperatures higher than $β_c^{-1} = \hbarλ/(2π)$, the partition function is dominated by a classical black hole solution, and the dominant contribution to the entropy is the two-dimensional Bekenstein-Hawking entropy. For temperatures lower than~$β_c^{-1}$, the partition function remains well-behaved and the heat capacity is positive in the asymptotically flat space limit, in contrast to the corresponding limit in four-dimensional spherically symmetric Einstein gravity; however, in this limit, the partition function is not dominated by a classical black hole solution.

gr-qc↗

arXiv1996

Validity of the Semiclassical Approximation and Back=reaction

Studying two-dimensional evaporating dilatonic black holes, we show that the semiclassical approximation, based on the background field approach, is valid everywhere in regions of weak curvature (including the horizon), as long as one takes into account the effects of back-reaction of the Hawking radiation on the background geometry.

gr-qc↗

arXiv1995

Hawking Radiation and Unitary evolution

We find a family of exact solutions to the semi-classical equations (including back-reaction) of two-dimensional dilaton gravity, describing infalling null matter that becomes outgoing and returns to infinity without forming a black hole. When a black hole almost forms, the radiation reaching infinity in advance of the original outgoing null matter has the properties of Hawking radiation. The radiation reaching infinity after the null matter consists of a brief burst of negative energy that preserves unitarity and transfers information faster than the theoretical bound for positive energy.

gr-qc↗

arXiv1995

Self-Adjoint Wheeler-DeWitt Operators, the Problem of Time and the Wave Function of the Universe

We discuss minisuperspace aspects a non empty Robertson-Walker universe containing scalar matter field. The requirement that the Wheeler-DeWitt (WDW) operator be self adjoint is a key ingredient in constructing the physical Hilbert space and has non-trivial cosmological implications since it is related with the problem of time in quantum cosmology. Namely, if time is parametrized by matter fields we find two types of domains for the self adjoint WDW operator: a non trivial domain is comprised of zero current (Hartle-Hawking type) wave functions and is parametrized by two new parameters, whereas the domain of a self adjoint WDW operator acting on tunneling (Vilenkin type) wave functions is a {\em single} ray. On the other hand, if time is parametrized by the scale factor both types of wave functions give rise to non trivial domains for the self adjoint WDW operators, and no new parameters appear in them.

hep-th↗

arXiv1995

Semi-infinite Throat as the End-state Geometry of two-dimensional Black Hole Evaporation

We study a modified two-dimensional dilaton gravity theory which is exactly solvable in the semiclassical approximation including back-reaction. The vacuum solutions of this modified theory are asymptotically flat static space-times. Infalling matter forms a black hole if its energy is above a certain threshold. The black hole singularity is initially hidden behind a timelike apparent horizon. As the black hole evaporates by emitting Hawking radiation, the singularity meets the shrinking horizon in finite retarded time to become naked. A natural boundary condition exists at the naked singularity such that for general infalling matter-configuration the evaporating black hole geometries can be matched continuously to a unique static end-state geometry. This end-state geometry is asymptotically flat at its right spatial infinity, while its left spatial infinity is a semi-infinite throat extending into the strong coupling region.

hep-th↗

arXiv1995

Phase Transition for Gravitationally Collapsing Dust Shells in 2+1 Dimensions

The collapse of thin dust shells in 2+1 dimensional gravity with and without a cosmological constant in analyzed. A critical value of the shell's mass as a function of its radius and position is derived. For $Λ< 0$, a naked singularity or black hole forms depending on whether the shell's mass is below or just above this value. The solution space is divided into four different regions by three critical surfaces. For $Λ< 0$, two surfaces separate regions of black hole solutions and solutions with naked singularities, while the other surface separates regions of open and closed spaces. Near the transition between black hole and naked singularity, we find ${\cal M} \sim c_{p}(p-p^*)^β$, where $β=1/2$ and ${\cal M}$ is a naturally defined order parameter. We find no phase transition in crossing from an open to closed space. The critical solutions are analogous to higher dimensional extremal black holes. All four phases coexist at one point in solution space correspondiong to the static extremal solution.

gr-qc↗

arXiv1994

Singularity Free Quasi-Classical Schwarzschild Space-Times

Using canonical (Schrodinger) quantization of spherically symetric gravitational dust systems, we find the quasi-classical (coherent) state, |α^{(s)}>, that corresponds to the classical Schwarzschild solution. We calculate the ``quasi-classical Schwarzschild mertic", which is the expectation value of the quantized metric in thhis quasi-classical state. Depending on the quantization scheme that we use, we study three different quasi- classical geometries, all of which turn out to be singularity free. Their maximal extensions are complete manifolds with no singularities, describing a tower of asymptotically flat universes connected through Planck size wormholes.

gr-qc↗

arXiv1994

Avoidance of Classical Singularities in Quantized Gravitational Dust Systems

We use the canonical quantization of spherically symetric dust universes, and calculate the expectation value of the quantized metric, $<Ψ|\hat{g}|Ψ>$. Though the classical solutions are singular, and the wave functions have no zero support on singular geometries, the expectation values are everywhere regular. For a quasi-classical (coherent) state, the metric expectation value describes a universe (or star) that collapses to a minimum radius, the Planck radius, and re-expands again.

hep-th↗

arXiv1993

Quantum Dust Black Holes

By analysing the infinite dimensional midisuperspace of spherically symmetric dust universes, and aply it to collapsing dust stars, one finds that the general quantum state is a bound state. This leads to discrete spectrum. In the case of a Schwarzschild black hole, the discrete spectrum implies Bekenstein area quantization: the area of the horizon is an integer multiple of the Planck area. Knowing the microscopic (quantum) states, we suggest a microscopic interpretation of the thermodynamics of black holes: the degeneracy of the quantum states forming a black hole, gives the Bekenstein- Hawking entropy. All other thermodynamical quantities can be derived by using the standard definitions.

hep-th↗

arXiv1993

The Wave Function of a Collapsing Star and Quantization Conditions

A very simple minisuperspace describing the Oppenheimer-Snyder collapsing star is found. The semiclasical wave function of that model turn out to describe a bound state. For fixed initial radius of the collapsing star, the corrssponding Bohr-Sommerfeld quantization condition implies mass quantization. An extension of this model, and some consequences, are considered.

hep-th↗

arXiv1993

4D and 2D Evaporating Dilatonic Black Holes

The picture of S-wave scatering from a 4D extremal dilatonic black hole is examined. Classically, a small matter shock wave will form a non-extremal black hole. In the "throat region" the r-t geometry is exactly that of a collapsing 2D black hole. The 4D Hawking radiation (in this classical background) gives the 2D Hawking radiation exactly in the throat region. Inclusion of the back-reaction changes this picture: the 4D solution can then be matched to the 2D one only if the Hawking radiation is very small and only at the beginning of the radiation. We give that 4D solution. When the total radiating energy approaches the energy carried by the shock wave, the 4D picture breaks down. This happens even before an apparent horizon is formed, which suggests that the 4D semi-classical solution is quite different from the 2D one.

hep-th↗