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Books on the topic 'Radiation de Hawking acoustique'

Author: Grafiati

Published: 25 January 2025

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1

Andie, Roman. Hawking Radiation 3. Lighthouse Books for Translation and Publishing, 2017.

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Andie, Roman. Hawking Radiation 4. Lighthouse Books for Translation and Publishing, 2017.

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Andie, Roman. Hawking Radiation 5. by Lighthouse Books for Translation and Publishing, 2017.

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Andie, Roman. Hawking Radiation 1. Lighthouse Books for Translation and Publishing, 2017.

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5

Faccio, Daniele, Francesco D. Belgiorno, and Sergio L. Cacciatori. Hawking Radiation: From Astrophysical Black Holes to Analogous Systems in Lab. World Scientific Publishing Co Pte Ltd, 2018.

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6

Lyamshev, Leonid M. Radiation Acoustics. Taylor & Francis Group, 2014.

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7

Lyamshev, Leonid M. Radiation Acoustics. CRC, 2004.

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8

Lyamshev, Leonid M. Radiation Acoustics. Taylor & Francis Group, 2003.

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9

Lyamshev, Leonid M. Radiation Acoustics. Taylor & Francis Group, 2004.

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10

Radiation acoustics. Boca Raton, FL: CRC Press, 2003.

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11

Blundell, Katherine. 5. Entropy and thermodynamics of black holes. Oxford University Press, 2015. http://dx.doi.org/10.1093/actrade/9780199602667.003.0005.

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‘Entropy and thermodynamics of black holes’ considers how the laws of thermodynamics and entropy can be applied to black holes. It discusses the work of Roger Penrose, James Bardeen, Brandon Carter, and Stephen Hawking, which, using quantum mechanics and quantum field theory, has enabled these scientists to propose likely behaviour in and around black holes. The concepts of black hole evaporation and Hawking radiation are explained to show how black holes lose mass and eventually disappear. It concludes with the black hole information paradox: can the information stored in the matter that fell into the black hole ever be recovered?

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12

Kachelriess, Michael. Black holes. Oxford University Press, 2018. http://dx.doi.org/10.1093/oso/9780198802877.003.0025.

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Black holes are introduced as solutions of Einsteins equations contain-ing a physical singularity covered by an event horizon. The properties of Schwarzschild and of Kerr black holes are examined. It is demonstrated that the event horizon of a black hole can only increase within classical physics. However, the event horizon is an infinite redshift surface and emits in the semi-classical picture thermal radiation. This Hawking radiation leads in turn to the information paradox.

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Deruelle, Nathalie, and Jean-Philippe Uzan. The physics of black holes II. Oxford University Press, 2018. http://dx.doi.org/10.1093/oso/9780198786399.003.0050.

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This chapter gives a brief description of Hawking radiation, which involves a combination of general relativity and quantum field theory and leads to a thermodynamical interpretation of the laws governing the evolution of black holes. The study of the Penrose process near a Kerr black hole leads to the conclusion that its irreducible mass can only increase. A similar but more general conclusion was reached by Hawking, who showed that the sum of the areas of the horizons of black holes interacting with matter can only increase, with the condition that the cosmic censorship hypothesis is valid and that the matter obeys the so-called weak energy condition. The chapter concludes with the Israel theorem, which allows one to argue that if gravitation is described by general relativity, then not only do black holes exist, but all black holes are represented by the Kerr–Schwarzschild solution.

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14

Borodin, Alexei. Random matrix representations of critical statistics. Edited by Gernot Akemann, Jinho Baik, and Philippe Di Francesco. Oxford University Press, 2018. http://dx.doi.org/10.1093/oxfordhb/9780198744191.013.12.

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This article examines two random matrix ensembles that are useful for describing critical spectral statistics in systems with multifractal eigenfunction statistics: the Gaussian non-invariant ensemble and the invariant random matrix ensemble. It first provides an overview of non-invariant Gaussian random matrix theory (RMT) with multifractal eigenvectors and invariant random matrix theory (RMT) with log-square confinement before discussing self-unfolding and not self-unfolding in invariant RMT. It then considers a non-trivial unfolding and how it changes the form of the spectral correlations, along with the appearance of a ghost correlation dip in RMT and Hawking radiation. It also describes the correspondence between invariant and non-invariant ensembles and concludes by introducing a simple field theory in 1+1 dimensions which reproduces level statistics of both of the two random matrix models and the classical Wigner-Dyson spectral statistics in the framework of the unified formalism of Luttinger liquid.

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15

Steane, Andrew M. Relativity Made Relatively Easy Volume 2. Oxford University Press, 2021. http://dx.doi.org/10.1093/oso/9780192895646.001.0001.

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This is a textbook on general relativity and cosmology for a physics undergraduate or an entry-level graduate course. General relativity is the main subject; cosmology is also discussed in considerable detail (enough for a complete introductory course). Part 1 introduces concepts and deals with weak-field applications such as gravitation around ordinary stars, gravimagnetic effects and low-amplitude gravitational waves. The theory is derived in detail and the physical meaning explained. Sources, energy and detection of gravitational radiation are discussed. Part 2 develops the mathematics of differential geometry, along with physical applications, and discusses the exact treatment of curvature and the field equations. The electromagnetic field and fluid flow are treated, as well as geodesics, redshift, and so on. Part 3 then shows how the field equation is solved in standard cases such as Schwarzschild-Droste, Reissner-Nordstrom, Kerr, and internal stellar structure. Orbits and related phenomena are obtained. Black holes are described in detail, including horizons, wormholes, Penrose process and Hawking radiation. Part 4 covers cosmology, first in terms of metric, then dynamics, structure formation and observational methods. The meaning of cosmic expansion is explained at length. Recombination and last scattering are calculated, and the quantitative analysis of the CMB is sketched. Inflation is introduced briefly but quantitatively. Part 5 is a brief introduction to classical field theory, including spinors and the Dirac equation, proceeding as far as the Einstein-Hilbert action. Throughout the book the emphasis is on making the mathematics as clear as possible, and keeping in touch with physical observations.

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