(Ebook) Modeling Black Hole Evaporation 1st Edition by Alessandro Fabbri, Jose Navarro Salas ISBN 1860945279 9781860945274

(Ebook) Modeling Black Hole Evaporation 1st Edition by Alessandro Fabbri, Jose Navarro Salas ISBN 1860945279 9781860945274

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ISBN 10: 1860945279 
ISBN 13: 9781860945274
Author: Alessandro Fabbri, Jose Navarro Salas

The scope of this book is two-fold: the first part gives a fully detailed and pedagogical presentation of the Hawking effect and its physical implications, and the second discusses the backreaction problem, especially in connection with exactly solvable semiclassical models that describe analytically the black hole evaporation process.The book aims to establish a link between the general relativistic viewpoint on black hole evaporation and the new CFT-type approaches to the subject. The detailed discussion on backreaction effects is also extremely valuable.

(Ebook) Modeling Black Hole Evaporation 1st Table of contents:

Chapter 1 Introduction
Chapter 2 Classical Black Holes
2.1 Modeling the Gravitational Collapse
2.1.1 The Oppenheimer–Snyder model
2.1.2 Non-spherical collapse
2.2 The Schwarzschild Black Hole
2.2.1 Eddington–Finkelstein coordinates
2.2.2 Kruskal coordinates
2.3 Causal Structure and Penrose Diagrams
2.3.1 Minkowski space
2.3.2 Schwarzschild spacetime
2.4 Kruskal and Locally Inertial Coordinates at the Horizons
2.4.1 Redshift factors and surface gravity
2.5 Charged Black Holes
2.6 The Extremal Reissner–Nordström Black Hole
2.7 Rotating Black Holes
2.7.1 Energy extraction from rotating black holes: the Penrose process
2.8 Trapped Surfaces, Apparent and Event Horizons
2.8.1 The area law theorem
2.9 The Laws of Black Hole Mechanics
2.10 Stringy Black Holes
Chapter 3 The Hawking Effect
3.1 Canonical Quantization in Minkowski Space
3.2 Quantization in Curved Spacetimes
3.2.1 Bogolubov transformations and particle production
3.3 Hawking Radiation in Vaidya Spacetime
3.3.1 Ingoing and outgoing modes
3.3.2 Wave packets
3.3.3 Wick rotation
3.3.4 Planck spectrum
3.3.5 Uncorrelated thermal radiation
3.3.6 Where are the correlations?
3.3.7 Thermal density matrix
3.4 Including the Backscattering
3.4.1 Waves in the Schwarzschild geometry
3.4.2 Late-time basis to accommodate backscattering
3.4.3 Thermal radiation and grey-body factors
3.4.4 Estimations for the luminosity
3.5 Importance of the Backreaction
3.6 Late-Time Independence on the Details of the Collapse
3.6.1 The example of two shock waves
3.6.2 Geometric optics approximation
3.6.3 General collapse
3.6.4 Adding angular momentum and charge
3.7 Black Hole Thermodynamics
3.8 Physical Implications of Black Hole Radiance and the Information Loss Paradox
3.8.1 Black hole evaporation
3.8.2 Breakdown of quantum predictability
3.8.3 Alternatives to restore quantum predictability
Chapter 4 Near-Horizon Approximation and Conformal Symmetry
4.1 Rindler Space
4.2 Conformal Symmetry, Stress Tensor and Particle Number
4.2.1 The normal ordered stress “tensor” operator
4.2.2 The SO(d,2) conformal group and Möbius transformations
4.2.3 The particle number operator
4.3 Radiation in Rindler Space: Hawking and Unruh Effects
4.3.1 The Hawking effect
4.3.2 Radiation through the horizon
4.3.3 The Unruh effect
4.3.4 Three different vacuum states
4.4 Anti-de Sitter Space as a Near-Horizon Geometry
4.4.1 Extremal black holes
4.4.2 Near-extremal black holes
4.5 Radiation in Anti-de Sitter Space: the Hawking Effect
4.5.1 Three vacuum states
4.6 The Moving-Mirror Analogy for the Hawking Effect
4.6.1 Exponential trajectory: thermal radiation
4.6.2 Radiationless trajectories
4.6.3 Asymptotically inertial trajectories and unitarity
Chapter 5 Stress Tensor, Anomalies and Effective Actions
5.1 Relating the Virasoro and Trace Anomalies via Locally Inertial Coordinates
5.2 The Polyakov Effective Action
5.2.1 The role of the Weyl-invariant effective action
5.3 Choice of the Quantum State
5.3.1 Boulware state
5.3.2 Hartle–Hawking state
5.3.3 The “in” and Unruh vacuum states: the Hawking flux
5.4 Including the Backscattering in the Stress Tensor: the s-wave
5.4.1 Two-dimensional symmetries
5.4.2 The normal ordered stress tensor
5.4.3 The covariant quantum stress tensor
5.4.4 Effective action
5.4.5 Quantum states and Hawking flux
5.5 Beyond the s-wave Approximation
5.6 The Problem of Backreaction
5.6.1 Backreaction equations from spherical reduction
5.6.2 The problem of determining the state-dependent functions
5.6.3 Returning to the near-horizon approximation
Chapter 6 Models for Evaporating Black Holes
6.1 The Near Horizon Approximation
6.1.1 Schwarzschild
6.1.2 Near-extremal Reissner–Nordström black holes: the JT model
6.1.3 Near-extremal dilaton black holes
6.2 The CGHS Model
6.2.1 The CGHS black hole
6.2.2 Including matter fields
6.2.3 Bogolubov coefficients and Hawking radiation
6.2.4 Quantum states for the CGHS black hole
6.3 The Problem of Backreaction in the CGHS Model
6.3.1 State-dependent functions for evaporating black holes
6.3.2 The RST model
6.3.3 Black hole evaporation in the RST model
6.4 The Semiclassical JT Model
6.4.1 Extremal solution
6.4.2 Semiclassical static solutions
6.4.3 General solutions
6.4.4 Black hole evaporation in the JT model
6.4.5 Beyond the near-horizon approximation and Hawking radiation
6.4.6 Information loss in the JT model

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Tags: Alessandro Fabbri, Jose Navarro Salas, Black, Evaporation