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Author: Jose Navarro-salas
Publisher: World Scientific
ISBN: 1783260386
Category : Science
Languages : en
Pages : 350
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Book Description
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./a
Author: Jose Navarro-salas
Publisher: World Scientific
ISBN: 1783260386
Category : Science
Languages : en
Pages : 350
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Book Description
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./a
Author: Daniel Grumiller
Publisher: Springer Nature
ISBN: 3031103432
Category : Science
Languages : en
Pages : 431
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Book Description
This textbook gradually introduces the reader to several topics related to black hole physics with a didactic approach. It starts with the most basic black hole solution, the Schwarzschild metric, and discusses the basic classical properties of black hole solutions as seen by different probes. Then it reviews various theorems about black hole properties as solutions to Einstein gravity coupled to matter fields, conserved charges associated with black holes, and laws of black hole thermodynamics. Next, it elucidates semiclassical and quantum aspects of black holes, which are relevant in ongoing and future research. The book is enriched with many exercises and solutions to assist in the learning. The textbook is designed for physics graduate students who want to start their research career in the field of black holes; postdocs who recently changed their research focus towards black holes and want to get up-to-date on recent and current research topics; advanced researchers intending to teach (or learn) basic and advanced aspects of black hole physics and the associated mathematical tools. Besides general relativity, the reader needs to be familiar with standard undergraduate physics, like thermodynamics, quantum mechanics, and statistical mechanics. Moreover, familiarity with basic quantum field theory in Minkowski space is assumed. The book covers the rest of the needed background material in the main text or the appendices.
Author: Shintaro Sawayama
Publisher: Shintaro Sawayama
ISBN: 4907170033
Category : Science
Languages : en
Pages : 58
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Book Description
We consider how the mass of the black hole decreases by the Hawking radiation in the Vaidya spacetime, using the concept of dynamical horizon equation, proposed by Ashtekar and Krishnan. Using the formula for the change of the dynamical horizon, we derive an equation for the mass incorporating the Hawking radiation. It is shown that the final state is the Minkowski spacetime in our particular model. We finally solved the equation which describes how black hole mass decreases. The back-reaction problem of the Hawking radiation has not been solved by the conventional method by solving the Einstein equation. While we can solve this problem using the following three ideas. First idea is to use the dynamical horizon equation which only needs information of the horizon surface. Then we calculate usual field equation as the integration equation. Second we taken negative energy into account near the black hole horizon. Using the negative energy we can enlarge the dynamical horizon to the timelike case. Third, we use the Vaidya metric. Usually the Einstein equation and the dynamical horizon equation are not compatible. However, using the Vaidya metric as a background we can use the dynamical horizon equation in place of the Einstein equation.
Author: Mario Novello
Publisher: World Scientific
ISBN: 9814489603
Category : Science
Languages : en
Pages : 415
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Book Description
Physicists are pondering on the possibility of simulating black holes in the laboratory by means of various “analog models”. These analog models, typically based on condensed matter physics, can be used to help us understand general relativity (Einstein's gravity); conversely, abstract techniques developed in general relativity can sometimes be used to help us understand certain aspects of condensed matter physics. This book contains 13 chapters — written by experts in general relativity, particle physics, and condensed matter physics — that explore various aspects of this two-way traffic.
Author: 陳冠宇
Publisher:
ISBN:
Category :
Languages : en
Pages :
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Book Description
Author: Karthik Shankar
Publisher:
ISBN:
Category :
Languages : en
Pages :
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Book Description
ABSTRACT: Hawking's discovery that a black hole quantum mechanically radiates energy like a black body suggests that its mass should decrease, leading to a process known as black hole evaporation. Solving for the evaporating black hole geometry (that is, its metric) exactly doesn't seem possible because it involves many complications. The most serious complication is that we do not have an analytic functional form for the quantum stress energy tensor in terms of the unknown metric. One approach to solving this problem is to use a Quasi-static approximation, which assumes that the evaporating black hole at every instant can be approximated by a stationary black hole. Effectively, it assumes that the luminosity of the black hole at any instant goes as 1/M2, where M is the mass of the black hole at that instant. In this dissertation, the validity of this approximation is examined in the context of a simple model where exact numerical calculations can be performed. In this model, we assume an analytic form for the quantum stress energy tensor in terms of the unknown metric. This model is a four dimensional extension of the two dimensional black hole geometry originally investigated by Unruh, Fulling and Davies. We explicitly compare the results obtained from the quasi-static approximation and the exact numerical calculation performed in this model. We observe that there is a significant difference between the quasi-static approximation and the exact calculation whenever the quantum effects are large. When the quantum effects are very small, as in astrophysical black holes, the quasi-static approximation matches the exact calculations very closely.
Author: Stephen Gerard O'Sullivan
Publisher:
ISBN:
Category :
Languages : en
Pages : 226
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Book Description
In this thesis, I discuss the application and development of black hole perturbation theory both from an observational standpoint via gravitational waves and also tidal distortions of black hole horizons. The promise of gravitational wave astronomy depends on our ability to accurately model gravitational wave signals from astrophysical sources. This requires large numbers of accurate theoretical template waveforms spanning large regions of parameter space to be cross-correlated against the output of gravitational-wave detectors. Numerical simulations of binary black-hole evolution are now possible but remain CPU costly. They also have problems with small mass ratios where perturbative analyses are efficient. This high computational cost has motivated the development of the effective-one-body (EOB) formalism, a framework which models the three phases of binary black hole coalescence - inspiral, plunge/merger, and ring down - by combining information from a variety of modeling techniques. In this thesis, we combine EOB with black hole perturbation theory to study the transition from inspiral to plunge-merger and ringdown. This allows us to tune and improve the accuracy of EOB. In Newtonian gravity, tidal coupling between members of a binary system has an influence on that binary's dynamics. There are also well-understood connections between the geometry of the binary's distorted members and the impact of tides on the orbit's evolution. In this thesis we develop tools for investigating the tidal distortion of black holes for tides arising from a body in a bound orbit. We also develop tools to visualize the horizon's distortion for black hole spin a/M
Author: Eric Poisson
Publisher: Cambridge University Press
ISBN: 1139451995
Category : Science
Languages : en
Pages : 253
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Book Description
This 2004 textbook fills a gap in the literature on general relativity by providing the advanced student with practical tools for the computation of many physically interesting quantities. The context is provided by the mathematical theory of black holes, one of the most elegant, successful, and relevant applications of general relativity. Among the topics discussed are congruencies of timelike and null geodesics, the embedding of spacelike, timelike and null hypersurfaces in spacetime, and the Lagrangian and Hamiltonian formulations of general relativity. Although the book is self-contained, it is not meant to serve as an introduction to general relativity. Instead, it is meant to help the reader acquire advanced skills and become a competent researcher in relativity and gravitational physics. The primary readership consists of graduate students in gravitational physics. It will also be a useful reference for more seasoned researchers working in this field.
Author: Dieter Lüst
Publisher: Springer
ISBN: 3030109194
Category : Science
Languages : en
Pages : 116
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Book Description
Based on Prof. Lüst's Masters course at the University of Munich, this book begins with a short introduction to general relativity. It then presents black hole solutions, and discusses Penrose diagrams, black hole thermodynamics and entropy, the Unruh effect, Hawking radiation, the black hole information problem, black holes in supergravity and string theory, the black hole microstate counting in string theory, asymptotic symmetries in general relativity, and a particular quantum model for black holes. The book offers an up-to-date summary of all the pertinent questions in this highly active field of physics, and is ideal reading for graduate students and young researchers.
Author: Zachary Lee Carson
Publisher:
ISBN:
Category :
Languages : en
Pages : 106
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Book Description
Several advancements in our understanding of fuzzball black have been made via the study of a dual Conformal Field Theory. In this approach, the full picture of black hole formation and eventual evaporation is expected to correspond to thermalization in the CFT dual. In other words, an initial set of high-energy wavepackets that 'break up' into a large quantity of low-energy excitations in the CFT should be the dual to an initial set of high-energy infalling particles forming a black hole that then evaporates via a large quantity of low-energy Hawking radiation in the gravity description. The nature of a fuzzball's CFT dual depends on particular parameters of the underlying gravity theory, its moduli space, and it is conjectured that some choice of parameters is dual to a particularly simple `orbifold' CFT. Calculations at this orbifold point match some semi-classical results, but it is also clear that the orbifold point is does not exactly match the behavior of gravity as we know it. It is thus necessary to move away from this orbifild point via the perturbative application of a deformation operator. A framework for studying deformations away from the orbifold point was developed some time ago, but its application was previously limited to the simplest of tree-level processes. My work extends this framework to all tree-level processes. At this stage, there is no clear indication of thermalization. In addition, analysis is muddied by a change in the Hilbert space of the CFT. This makes comparisons between initial and final states difficult to perform. To address this, the framework was further extended to include a simple one-loop process. This process maintains a consistent Hilbert space between in and out states, allowing a more straightforward search for thermalization effects. Furthermore, certain patterns occurred when comparing the one-loop results to the tree-level process that constitutes the loop's first half. It is thus natural to conjecture that some of these patterns may remain at even higher orders. In addition to this work, I also present detailed analysis of a simplifying regime known as the 'continuum limit.' In this limit, the energy of the system is taken to be much larger than the size of the individual quanta, so that excitation levels appear continuous rather than discrete. This is exactly the regime of black hole formation. It also greatly simplifies the results of our calculations, which is of particular importance when dealing with the otherwise intractable expressions found in even the simplest one-loop case. While my work has not by any means succeeded in completing the ideal picture of black hole formation and subsequent evaporation, it provides a solid foundation upon which one may continue the search. By maintaining a consistent Hilbert space, the new one-loop result is readily extendable via a method of repeated application, which is not the case for the tree-level calculations. For the same reason it provides a more accessible place to search for wave packet splitting. And while the analytic results are particularly messy, they are accessible enough to facilitate future numerical work. Furthermore, a large number of useful relations have been proven to all orders of the twist portion of the deformation.
