Relevant bibliographies by topics / Black hole physics

Contents

  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers
  6. Reports

Academic literature on the topic 'Black hole physics'

Author: Grafiati
Published: 4 June 2021
Last updated: 7 September 2023

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Journal articles on the topic "Black hole physics"

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Zakharov, Aleksandr F. "Black hole physics." Physics-Uspekhi 42, no. 9 (September 30, 1999): 947–51. http://dx.doi.org/10.1070/pu1999v042n09abeh000651.

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Zakharov, A. F. "Black hole physics." Uspekhi Fizicheskih Nauk 169, no. 9 (1999): 1041. http://dx.doi.org/10.3367/ufnr.0169.199909h.1041.

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Voss, D. "PHYSICS: Black Hole Encryption." Science 311, no. 5767 (March 17, 2006): 1525a. http://dx.doi.org/10.1126/science.311.5767.1525a.

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VISSER, MATT. "HAWKING RADIATION: A PARTICLE PHYSICS PERSPECTIVE." Modern Physics Letters A 08, no. 18 (June 14, 1993): 1661–70. http://dx.doi.org/10.1142/s0217732393001409.

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It has recently become fashionable to regard black holes as elementary particles. By taking this suggestion reasonably seriously it is possible to cobble together an elementary particle physics based on estimate for the decay rate (black hole) i → (black hole) f+ (massless quantum) . This estimate of the spontaneous emission rate contains two free parameters which may be fixed by demanding that the high energy end of the spectrum of emitted quanta match a black body spectrum at the Hawking temperature. The calculation, though technically trivial, has important conceptual implications: (1) The existence of Hawking radiation from black holes seems ultimately dependent only on the fact that massless quanta (and all other forms of matter) couple to gravity. (2) The essentially thermal nature of the Hawking spectrum seems to depend only on the fact that the number of internal states of a large mass black hole is enormous. (3) Remarkably, the resulting formula for the decay rate gives meaningful answers even when extrapolated to low mass black holes. The analysis seems to support the scenario of complete evaporation as the end point of the Hawking radiation process (no naked singularity, no stable massive remnant).
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Abramovsky. "Abramovsky—Gribov—Kancheli Theorem in the Physics of Black Holes." Physics 1, no. 2 (August 1, 2019): 253–70. http://dx.doi.org/10.3390/physics1020020.

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The proof of the Abramovsky—Gribov—Kancheli (AGK) theorem for black hole physics is given. Based on the AGK relations, a formula for the luminosity of a black hole as a function of the mass of the black hole is derived. The correspondence to experimental data is considered. It is shown that the black holes of the galaxies NGC3842 and NGC4889 do not differ from those of the other galaxies.
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Sims, Christopher. "Analogous Black Holes in Type-III Dirac Semimetal Ni3In2X2 (X = S, Se)." Crystals 13, no. 5 (May 20, 2023): 847. http://dx.doi.org/10.3390/cryst13050847.

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Black holes are objects that have a large mass and curve space time, characterized by their event horizon and singularity. Recently, an interesting concept of analogous black holes has emerged in the field of condensed matter physics. In this work, the possibility of realizing analogous black holes in topological material is Ni3In2X2 (X = S, Se) discussed. This work shows that the type-III Dirac cones of the material can lead to the emergence of an event horizon and the formation of a black hole-like region near the Dirac point. In addition, the possible experimental signatures of such a system are discussed and the potential implications of an analogous black hole for the study of black hole physics in condensed matter systems.
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Altas, E., and B. Tekin. "Basics of Apparent horizons in black hole physics." Journal of Physics: Conference Series 2191, no. 1 (February 1, 2022): 012002. http://dx.doi.org/10.1088/1742-6596/2191/1/012002.

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Abstract 1Event Horizon, a null hypersurface defining the boundary of the black hole region of a spacetime, is not particularly useful for evolving black holes since it is non-local in time. Instead, one uses the more tangible concept of Apparent Horizon for dynamical black holes out there in the sky that do all sorts of things: evolve, merge and feed on the environment. Event Horizon, being a gauge-independent, global property of the total spacetime is easy to define and locate in the stationary case; on the other hand, Apparent Horizon depends on the embedding of the surface in spacetime and hence it is somewhat tricky to define. But for numerical simulations in General Relativity, locating the Apparent Horizon helps one to excise the black hole region and the singularity to have a stable computation. Moreover, for stationary solutions cross-sections of these horizons match. Here we give a detailed pedagogical exposition of the subject and work out the non-trivial case of a slowly moving and spinning black hole.
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Poudel, Parashu Ram. "The Black Hole." Himalayan Physics 3 (December 26, 2012): 50–55. http://dx.doi.org/10.3126/hj.v3i0.7277.

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Black holes are the cold remnants of former stars. They are so dense that no matter -not even light - is able to escape their powerful gravitational pull. These are interesting objects from a fundamental physics point of view and play an important role in astrophysics. The knowledge of phenomenon of origin of black hole may lead to new understanding of the nature of the real universe. The Himalayan PhysicsVol. 3, No. 32012Page : 50-55
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Kubizňák, David, and Robert B. Mann. "Black hole chemistry." Canadian Journal of Physics 93, no. 9 (September 2015): 999–1002. http://dx.doi.org/10.1139/cjp-2014-0465.

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The mass of a black hole has traditionally been identified with its energy. We describe a new perspective on black hole thermodynamics, one that identifies the mass of a black hole with chemical enthalpy, and the cosmological constant as thermodynamic pressure. This leads to an understanding of black holes from the viewpoint of chemistry, in terms of concepts such as Van der Waals fluids, reentrant phase transitions, and triple points. Both charged and rotating black holes exhibit novel chemical-type phase behaviour, hitherto unseen.
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Frolov, Valery P. "Two-dimensional black hole physics." Physical Review D 46, no. 12 (December 15, 1992): 5383–94. http://dx.doi.org/10.1103/physrevd.46.5383.

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Dissertations / Theses on the topic "Black hole physics"

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Ahmadi, Morteza, and University of Lethbridge Faculty of Arts and Science. "Aspects of black hole physics." Thesis, Lethbridge, Alta. : University of Lethbridge, Faculty of Arts and Science, 2006, 2006. http://hdl.handle.net/10133/386.

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In this thesis, aspects of the physics of black holes are reviewed and new results in black hole thermodynamics are presented. First, general black hole solutions of Einstein’s equations of general relativity are mentioned and a proof of conservation law of energy and momentum in general relativity is presented. Aspects of the laws of black hole mechanics and Hawking radiation are then studied. Two proposals which attempt to explain the origin of black hole entropy (the brick wall model and entanglement entropy) are then discussed. Finally, some recent work related to the possible production and detection of black holes in colliders is presented.
viii, 141 leaves ; 29 cm.
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Chung, Hyeyoun. "Exploring Black Hole Dynamics." Thesis, Harvard University, 2014. http://nrs.harvard.edu/urn-3:HUL.InstRepos:14226081.

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This thesis explores the evolution of different types of black holes, and the ways in which black hole dynamics can be used to answer questions about other physical systems. We first investigate the differences in observable gravitational effects between a four-dimensional Randall-Sundrum (RS) braneworld universe compared to a universe without the extra dimension, by considering a black hole solution to the braneworld model that is localized on the brane. When the brane has a negative cosmological constant, then for a certain range of parameters for the black hole, the intersection of the black hole with the brane approximates a Banados-Teitelboim-Zanelli (BTZ) black hole on the brane with corrections that fall off exponentially outside the horizon. We compute the quasinormal modes of the braneworld black hole, and compare them to the known quasinormal modes of the three-dimensional BTZ black hole. We find that there are two distinct regions for the braneworld black hole solutions that are reflected in the dependence of the quasinormal modes on the black hole mass. The imaginary parts of the quasinormal modes display phenomenological similarities to the quasinormal modes of the three-dimensional BTZ black hole, indicating that nonlinear gravitational effects may not be enough to distinguish between a lower-dimensional theory and a theory derived from a higher-dimensional braneworld. Secondly, we consider the evolution of non-extremal black holes in N=4, d=2 supergravity, and investigate how such black holes might evolve over time if perturbed away from extremality. We study this problem in the probe limit by finding tunneling amplitudes for a Dirac field in a single-centered background, which gives the decay rates for the emission of charged probe black holes from the central black hole. We find that there is no minimum to the potential for the probe particles at a finite distance from the central black hole, so any probes that are emitted escape to infinity. If the central black hole is BPS in the extremal limit, then the potential is flat and so there is no barrier to the emission of probes. If the central black hole is non-BPS in the extremal limit, then there is a barrier to emission and we compute the decay rate, which depends both on the charge of the central black hole and the charges of the emitted black holes. Finally, we consider the possibility that an extremal black hole, the end-point of the evolution of a non-extremal black hole through evaporation, may itself split into a multi-centered black hole solution through quantum tunneling, via a gravitational instanton analogous to the instanton for the symmetric double well in elementary quantum mechanics. We find a gravitational instanton that connects two vacuum states: one state corresponding to a single-centered extremal Reissner-Nordstrom (ERN) black hole configuration, and another state corresponding to a multi-centered ERN configuration. We evaluate the Euclidean action for this instanton and find that the amplitude for the tunneling process is equal to half the difference in entropy between the initial and final configurations.
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Luna, Raimon. "New Strategies for Black Hole Physics." Doctoral thesis, Universitat de Barcelona, 2020. http://hdl.handle.net/10803/669583.

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In this thesis we apply new approaches and develop new techniques to address various issues related to fundamental aspects of modern gravitational theory and black holes. We study the behavior of black branes in the large D approximation, that is, we consider a space with a very large number of dimensions. This approach allows us to obtain a set of very simple equations that capture many of the physical phenomena of gravity. This technique uses the fact that the gravitational field around a massive object decays faster the higher the dimension, so when you take the very large D limit it becomes concentrated in a very thin region of size 1/D around the horizon of the black hole. In this way, the horizon can be viewed as a membrane suspended in an essentially flat background geometry. The region where the black hole lives is, in some sense, excluded from the background space. We use the large D effective equations to investigate the phases and stability of black strings at different values of the dimension D and the compactification length L. In some cases, the Gregory-Laflamme instability of the uniform black strings can lead to stable non-uniform black strings. The transition type changes at a certain critical value of D ~ 13.5. We use 1/D corrections to estimate the value of the critical dimension, which turns out to be very accurate. Possible violations of Weak Cosmic Censorship in black hole collisions at D > 4 are also explored. The large D technique, through the effective equations, provides a powerful tool for analyzing such scenarios that would otherwise be very difficult to tackle using numerical simulations at finite D. It has recently been shown that rotating black holes can be described as Gaussian lumps on a black brane. The Strong Cosmic Censorship conjecture for highly charged Reissner-Nordström black holes has recently been called into question in asymptotically de Sitter spacetimes. To go beyond previous studies, this thesis includes the results of nearly extremal Reissner-Nordström nonlinear simulations. In order to perform the nonlinear (spherically symmetric) integrations, a new spectral code has been developed in double-null coordinates. Any continuous system that can be described as a quantum field theory will react to a change in the geometry where it is located. It will do so by changing its distribution of energy density, pressure and stresses. That is, the system is polarized, and its stress-energy tensor acquires a non-trivial quantum expectation value. In this context, the holographic duality, also known as AdS/CFT correspondence, is extremely useful for extracting valuable qualitative information from the system. Perturbations of the geometry of the AdS boundary will produce tidal deformations in the geometry of the bulk. To calculate this deformations, we solve the equations for a linearized perturbation of the geometry that satisfies suitable boundary conditions. Finally, we study a subset of Horndeski's theories whose equations of motion are locally well posed. However, it is necessary to determine whether global solutions exist and whether they are sufficiently well behaved. A worrisome possibility (which has been confirmed by numerical simulations) is a change in the character of the equation of motion, from hyperbolic to parabolic and finally to elliptical. This causes a change in the causal structure of the geometry.
En aquesta tesi aplicarem nous enfocaments i desenvoluparem noves tècniques per tractar diversos temes relacionats amb aspectes fonamentals de la teoria gravitacional moderna i els forats negres. Estudiem el comportament de les branes negres en l’aproximació large D, és a dir, considerem un espaitemps amb un nombre molt gran de dimensions. Aquest enfocament ens permet obtenir un conjunt d’equacions molt simples que recullen molts dels fenòmens físics de la gravetat. En alguns casos, la inestabilitat de Gregory-Laflamme de les cordes negres uniformes pot conduir a cordes negres no uniformes estables. S’exploren també possibles esdeveniments de violació de la Censura Còsmica Feble en col·lisions de forats negres a D > 4. La tècnica de large D, mitjançant les equacions efectives, proporciona una eina potent per analitzar aquest tipus d’escenaris que d’altra manera serien molt complicats d’abordar mitjançant simulacions numèriques a D finita. Recentment s’ha posat en dubte la conjectura de Censura Còsmica Forta per a forats negres de Reissner-Nordström altament carregats en espaitemps asimptòticament de Sitter. Per anar més enllà dels estudis anteriors, en aquesta tesi s’inclouen els resultats de simulacions completament no lineals de Reissner-Nordström altament carregats. Qualsevol sistema continu que es pugui descriure com una teoria quàntica de camps reaccionarà davant un canvi en la geometria on està situat. En aquest context, la correspondència AdS/CFT és extremadament útil per extreure informació qualitativa i valuosa del sistema. Les pertorbacions en la geometria de la frontera d’AdS produiran deformacions de marea en la geometria de l’interior. Per calcular aquesta deformació, resolem les equacions per a una pertorbació linealitzada de la geometria que satisfà una condició de contorn adequada a l’infinit. Finalment, s’estudia un subconjunt de les teories de Horndeski les equacions del moviment de les quals són localment ben plantejades. Tot i això, cal determinar si existeixen solucions globals i si aquestes solucions són prou ben comportades. Una possibilitat preocupant (que s’ha confirmat amb simulacions numèriques), és un canvi del caràcter de l’equació de moviment, d’hiperbòlica a parabòlica i finalment a el·líptica.
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Pidokrajt, Narit. "Information geometries in black hole physics." Doctoral thesis, Stockholms universitet, Fysikum, 2009. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-29365.

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In this thesis we aim to develop new perspectives on the statistical mechanics of black holes using an information geometric approach (Ruppeiner and Weinhold geometry). The Ruppeiner metric is defined as a Hessian matrix on a Gibbs surface, and provides a geometric description of thermodynamic systems in equilibrium. This Ruppeiner geometry exhibits physically suggestive features; a flat Ruppeiner metric for systems with no interactions i.e. the ideal gas, and curvature singularities signaling critical behavior(s) of the system. We construct a flatness theorem based on the scaling property of the black holes, which proves to be useful in many cases. Another thermodynamic geometry known as the Weinhold geometry is defined as the Hessian of internal energy and is conformally related to the Ruppeiner metric with the system’s temperature as a conformal factor.  We investigate a number of black hole families in various gravity theories. Our findings are briefly summarized as follows: the Reissner-Nordström type, the Einstein-Maxwell-dilaton andBTZ black holes have flat Ruppeiner metrics that can be represented by a unique state space diagram. We conjecture that the state space diagram encodes extremality properties of the black hole solution. The Kerr type black holes have curved Ruppeiner metrics whose curvature singularities are meaningful in five dimensions and higher, signifying the onset of thermodynamic instabilities of the black hole in higher dimensions. All the three-parameter black hole families in our study have non-flat Ruppeiner and Weinhold metrics and their associated curvature singularities occur in the extremal limits. We also study two-dimensional black hole families whose thermodynamic geometries are dependent on parameters that determine the thermodynamics of the black hole in question. The tidal charged black hole which arises in the braneworld gravity is studied. Despite its similarity to the Reissner-Nordström type, its thermodynamic geometries are distinctive.
At the time of the doctoral defense, the following papers were unpublished and had a status as follows: Paper 2: Submitted.
Geometry and Physics
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Chambers, Chris M. "Classical aspects of black hole physics." Thesis, University of Newcastle Upon Tyne, 1995. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.294892.

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Zhu, Yucong. "The Bright Side of Black Holes: Radiation From Black Hole Accretion Disks." Thesis, Harvard University, 2015. http://nrs.harvard.edu/urn-3:HUL.InstRepos:17463143.

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An understanding of radiation is paramount for connecting observations of accretion disks with the theory of black holes. In this thesis, we explore via radiative transfer postprocessing calculations the observational signatures of black holes. We investigate disk spectra by analyzing general relativistic magnetohydrodynamic (GRMHD) simulations of accretion disks. For the most part there are no surprises -- the resulting GRMHD spectrum is very close to the analytic Novikov & Thorne (1973) prediction from decades past, except for a small modification in the case of spinning black holes, which exhibit a high-energy power-law tail that is sourced by hot Comptonized gas from within the plunging region of the accretion flow. These conclusions are borne out by both 1D and 3D radiative transfer calculations of the disk. Significant effort was spent in developing from scratch the 3D radiative code that we used for the analysis. The code is named HERO (Hybrid Evaluator for Radiative Objects) and it is a new general purpose grid-based 3D general relativistic radiative solver.
Astronomy
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O'Sullivan, Stephen Gerard. "Making better binary models and modeling distorted black holes using black hole perturbation theory." Thesis, Massachusetts Institute of Technology, 2015. http://hdl.handle.net/1721.1/99297.

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Thesis: Ph. D., Massachusetts Institute of Technology, Department of Physics, 2015.
Cataloged from PDF version of thesis.
Includes bibliographical references.
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 < V/3/2. In analyzing how a Kerr black hole is distorted by a small body for a circular equatorial orbit, we find that Newtonian intuition is not applicable. We also apply these techniques to generic Kerr black hole orbits, which enables us to look at time-dependent phenomena on the horizon. In particular, we find significant offsets between the applied tide and the horizon's response, as well as small amplitude coherent wiggles in the horizon's shear response to the applied tide. These appear to arise from the teleological nature of the horizon's response to tides.
by Stephen Gerard O'Sullivan.
Ph. D.
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Sung, Shih-Ta. "Black hole entropy and models." Thesis, Durham University, 1997. http://etheses.dur.ac.uk/4677/.

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No universally accepted statistical explanation of black hole entropy exists up to now, therefore, it is worth another try. Admittedly, black hole entropy does not have to have a statistical origin. If the "black hole entropy" is called "black hole index" instead, someone might be lured to give it an economic explanation. Nonetheless, the only way to justify one's claim about the statistical origin of black hole entropy is to compute it statistically. This is the motivation for the construction of black hole models. In chapter 1, I first review the four laws of classical black hole mechanics which form the basis for the introduction of black hole thermodynamics. After observing the formal analogy between the four laws of the black hole mechanics and that of the ordinary thermodynamics, I further explore the thermodynamic properties of black holes in chapter 2 by reviewing the phenomenon of Hawking radiation and introducing the idea of black hole entropy. Three statistical explanations of black hole entropy are introduced in chapter 3. I will start with’t Hooft's brick wall model. Then, á la Brown and York, I review the approach based on the gravitational degrees of freedom via path integral. In the final part of this chapter, I present my own version of a quantum statistical explanation of black hole entropy by regarding a black hole as a cavity with thermal states inside. The final chapter will be devoted to the construction of black hole models to materialise the idea that a black hole, in some sense, can be regarded as a cavity where thermalised quantum states reside with quantised spectrum. These quantum states and the corresponding spectrum will then justify the statistical explanation of black hole entropy presented in the final section of chapter 3.
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Kolishetty, Kiran. "Quantum properties of black hole." Thesis, Lancaster University, 2014. http://eprints.lancs.ac.uk/71783/.

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In this research report I would like to present some of the results obtained based on the published research, it is on the analogue model of Bose Einstein condensate of gravitons. In my investigation with different approach I could reach similar conclusion for Schwarzschild radius which is derived for Bose Einstein condensate of N-gravitons . I could calculate the pressure inside the condensed black hole. It is found that the Bogoliubov dispersion relation for the elementary excitations of the weakly-interacting N-gravitons is shown to hold for the case of the weakly-interacting Graviton gas or N weakly interacting gravitons. where both the cases of attraction and repulsion is taken into consideration between the weakly coupled N-gravitons. It is interesting to notice that weakly interactions among gravitons have differences in attractive and repulsive case, additionally I will be looking into the possible way to understand the entropy of the N-graviton in a condensed Black hole. Finally I could derive the critical point for Black hole for N gravitons in case of weakly attractive interacting N gravitons , In attractive nature of N-gravitons I found that it has critical point at which black holes do not form the condensate , above this critical value k Black hole seems to form a condensate of N-gravitons. In this approach Black hole entropy is understood from condensed matter physics perspective as excited states of condensed matter of N-gravitons. Furthermore, this includes the literature review in order to support the results obtained in my calculations.
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Sidhu, Steve. "Conformal field theory and black hole physics." Thesis, Lethbridge, Alta. : University of Lethbridge, Dept. of Physics and Astronomy, c2012, 2012. http://hdl.handle.net/10133/3109.

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This thesis reviews the use of 2-dimensional conformal field theory applied to gravity, specifically calculating Bekenstein-Hawking entropy of black holes in (2+1) dimensions. A brief review of general relativity, Conformal Field Theory, energy extraction from black holes, and black hole thermodynamics will be given. The Cardy formula, which calculates the entropy of a black hole from the AdS/CFT duality, will be shown to calculate the correct Bekenstein-Hawking entropy of the static and rotating BTZ black holes. The first law of black hole thermodynamics of the static, rotating, and charged-rotating BTZ black holes will be verified.
vii, 119 leaves : ill. ; 29 cm
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Books on the topic "Black hole physics"

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Venzo, De Sabbata, Zhang Zhenjiu, North Atlantic Treaty Organization. Scientific Affairs Division., and NATO Advanced Study Institute on Black Hole Physics (1991 : Erice, Italy), eds. Black hole physics. Dordrecht: Kluwer Academic Publishers, 1992.

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Frolov, Valeri P., and Igor D. Novikov. Black Hole Physics. Dordrecht: Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-011-5139-9.

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Sabbata, Venzo, and Zhenjiu Zhang, eds. Black Hole Physics. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2420-1.

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Grumiller, Daniel, and Mohammad Mehdi Sheikh-Jabbari. Black Hole Physics. Cham: Springer International Publishing, 2022. http://dx.doi.org/10.1007/978-3-031-10343-8.

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Sabbata, Venzo. Black Hole Physics. Dordrecht: Springer Netherlands, 1992.

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service), SpringerLink (Online, ed. Black Hole Gravitohydromagnetics. Berlin, Heidelberg: Springer-Verlag Berlin Heidelberg, 2009.

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Andrei, Zelnikov, ed. Introduction to black hole physics. Oxford: Oxford University Press, USA, 2011.

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Punsly, Brian. Black Hole Gravitohydromagnetics. Berlin, Heidelberg: Springer Berlin Heidelberg, 2001.

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D, Novikov I., ed. Black hole physics: Basic concepts and new developments. Dordrecht: Kluwer, 1998.

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ill, Carroll Michael, ed. A black hole is not a hole. Watertown, MA: Charlesbridge, 2011.

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Book chapters on the topic "Black hole physics"

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Romero, Gustavo E., and Gabriela S. Vila. "Black Hole Physics." In Introduction to Black Hole Astrophysics, 73–97. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-642-39596-3_3.

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Lüst, Dieter, and Ward Vleeshouwers. "Rotating Black Holes and Black Hole Mechanics." In SpringerBriefs in Physics, 37–40. Cham: Springer International Publishing, 2019. http://dx.doi.org/10.1007/978-3-030-10919-6_10.

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Lüst, Dieter, and Ward Vleeshouwers. "Black Hole Thermodynamics." In SpringerBriefs in Physics, 45–47. Cham: Springer International Publishing, 2019. http://dx.doi.org/10.1007/978-3-030-10919-6_12.

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Novikov, Igor D., and Valery P. Frolov. "Rotating Black Hole." In Physics of Black Holes, 51–81. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-017-2651-1_4.

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Novikov, Igor D., and Valery P. Frolov. "Black-Hole Electrodynamics." In Physics of Black Holes, 135–55. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-017-2651-1_7.

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Frolov, Valeri P., and Igor D. Novikov. "Black hole Perturbations." In Fundamental Theories of Physics, 87–149. Dordrecht: Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-011-5139-9_4.

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Frolov, Valeri P., and Igor D. Novikov. "Black Hole Electrodynamics." In Fundamental Theories of Physics, 290–318. Dordrecht: Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-011-5139-9_8.

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Zhang, Zhenjiu. "Physics of Black Holes: Classical, Quantum and Astrophysical." In Black Hole Physics, 1–53. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2420-1_1.

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Ching, Chengrui, Tsohsiu Ho, Yiren Wang, and Jing Yao. "Possible Multi-Explosions of Supernovae and Induced Gravitational Collapse." In Black Hole Physics, 403–16. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2420-1_10.

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Bergmann, Peter G. "Concluding Remarks." In Black Hole Physics, 417–19. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2420-1_11.

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Conference papers on the topic "Black hole physics"

1

Bilic, Neven. "Black-Hole Phenomenology." In School on Particle Physics, Gravity and Cosmology. Trieste, Italy: Sissa Medialab, 2007. http://dx.doi.org/10.22323/1.034.0004.

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Matzner, Richard A. "Designing a 2 black hole code." In Computational quantum physics. AIP, 1992. http://dx.doi.org/10.1063/1.42616.

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Ben Achour, Jibril, and Karim Noui. "Analytical continuation of black hole entropy in Loop Quantum Gravity: Lessons from black hole thermodynamics." In Frontiers of Fundamental Physics 14. Trieste, Italy: Sissa Medialab, 2016. http://dx.doi.org/10.22323/1.224.0158.

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Tejeiro-Sarmiento, Juan Manuel. "Black Hole Entanglement Entropy." In A CENTURY OF RELATIVITY PHYSICS: ERE 2005; XXVIII Spanish Relativity Meeting. AIP, 2006. http://dx.doi.org/10.1063/1.2218196.

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Lambert, Pierre-Henry. "Introduction to Black Hole evaporation." In Ninth Modave Summer School in Mathematical Physics. Trieste, Italy: Sissa Medialab, 2014. http://dx.doi.org/10.22323/1.201.0001.

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Bianchi, Eugenio. "Last gasps of a black hole." In Frontiers of Fundamental Physics 14. Trieste, Italy: Sissa Medialab, 2016. http://dx.doi.org/10.22323/1.224.0035.

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Lemos, José P. S., Vilson T. Zanchin, Carlos Herdeiro, and Roger Picken. "New regular black hole solutions." In XIX INTERNATIONAL FALL WORKSHOP ON GEOMETRY AND PHYSICS. AIP, 2011. http://dx.doi.org/10.1063/1.3599140.

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Hooft, Gerard 't. "THE BLACK HOLE INFORMATION PROBLEM." In Proceedings of the International School of Subnuclear Physics. WORLD SCIENTIFIC, 2007. http://dx.doi.org/10.1142/9789812708427_0008.

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Marrani, Alessio. "Non-Linear Invariance of Black Hole Entropy." In The European Physical Society Conference on High Energy Physics. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.314.0543.

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Polchinski, Joseph. "The Black Hole Information Problem." In 2015 Theoretical Advanced Study Institute in Elementary Particle Physics. WORLD SCIENTIFIC, 2016. http://dx.doi.org/10.1142/9789813149441_0006.

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Reports on the topic "Black hole physics"

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Balachandran, A. P., A. Momen, and L. Chandar. Edge states in gravity and black hole physics. Office of Scientific and Technical Information (OSTI), September 1995. http://dx.doi.org/10.2172/176797.

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