Study of the Thermodynamics of Charged Rotating Black Holes in Five-Dimensional Anti-De Sitter Spacetimes
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Aspects of Black Hole Physics
Aspects of Black Hole Physics Andreas Vigand Pedersen The Niels Bohr Institute Academic Advisor: Niels Obers e-mail: [email protected] Abstract: This project examines some of the exact solutions to Einstein’s theory, the theory of linearized gravity, the Komar definition of mass and angular momentum in general relativity and some aspects of (four dimen- sional) black hole physics. The project assumes familiarity with the basics of general relativity and differential geometry, but is otherwise intended to be self contained. The project was written as a ”self-study project” under the supervision of Niels Obers in the summer of 2008. Contents Contents ..................................... 1 Contents ..................................... 1 Preface and acknowledgement ......................... 2 Units, conventions and notation ........................ 3 1 Stationary solutions to Einstein’s equation ............ 4 1.1 Introduction .............................. 4 1.2 The Schwarzschild solution ...................... 6 1.3 The Reissner-Nordstr¨om solution .................. 18 1.4 The Kerr solution ........................... 24 1.5 The Kerr-Newman solution ..................... 28 2 Mass, charge and angular momentum (stationary spacetimes) 30 2.1 Introduction .............................. 30 2.2 Linearized Gravity .......................... 30 2.3 The weak field approximation .................... 35 2.3.1 The effect of a mass distribution on spacetime ....... 37 2.3.2 The effect of a charged mass distribution on spacetime .. 39 2.3.3 The effect of a rotating mass distribution on spacetime .. 40 2.4 Conserved currents in general relativity ............... 43 2.4.1 Komar integrals ........................ 49 2.5 Energy conditions ........................... 53 3 Black holes ................................ 57 3.1 Introduction .............................. 57 3.2 Event horizons ............................ 57 3.2.1 The no-hair theorem and Hawking’s area theorem .... -
Some Aspects in Cosmological Perturbation Theory and F (R) Gravity
Some Aspects in Cosmological Perturbation Theory and f (R) Gravity Dissertation zur Erlangung des Doktorgrades (Dr. rer. nat.) der Mathematisch-Naturwissenschaftlichen Fakultät der Rheinischen Friedrich-Wilhelms-Universität Bonn von Leonardo Castañeda C aus Tabio,Cundinamarca,Kolumbien Bonn, 2016 Dieser Forschungsbericht wurde als Dissertation von der Mathematisch-Naturwissenschaftlichen Fakultät der Universität Bonn angenommen und ist auf dem Hochschulschriftenserver der ULB Bonn http://hss.ulb.uni-bonn.de/diss_online elektronisch publiziert. 1. Gutachter: Prof. Dr. Peter Schneider 2. Gutachter: Prof. Dr. Cristiano Porciani Tag der Promotion: 31.08.2016 Erscheinungsjahr: 2016 In memoriam: My father Ruperto and my sister Cecilia Abstract General Relativity, the currently accepted theory of gravity, has not been thoroughly tested on very large scales. Therefore, alternative or extended models provide a viable alternative to Einstein’s theory. In this thesis I present the results of my research projects together with the Grupo de Gravitación y Cosmología at Universidad Nacional de Colombia; such projects were motivated by my time at Bonn University. In the first part, we address the topics related with the metric f (R) gravity, including the study of the boundary term for the action in this theory. The Geodesic Deviation Equation (GDE) in metric f (R) gravity is also studied. Finally, the results are applied to the Friedmann-Lemaitre-Robertson-Walker (FLRW) spacetime metric and some perspectives on use the of GDE as a cosmological tool are com- mented. The second part discusses a proposal of using second order cosmological perturbation theory to explore the evolution of cosmic magnetic fields. The main result is a dynamo-like cosmological equation for the evolution of the magnetic fields. -
Gravitational Multi-NUT Solitons, Komar Masses and Charges
Gen Relativ Gravit (2009) 41:1367–1379 DOI 10.1007/s10714-008-0720-7 RESEARCH ARTICLE Gravitational multi-NUT solitons, Komar masses and charges Guillaume Bossard · Hermann Nicolai · K. S. Stelle Received: 30 September 2008 / Accepted: 19 October 2008 / Published online: 12 December 2008 © The Author(s) 2008. This article is published with open access at Springerlink.com Abstract Generalising expressions given by Komar, we give precise definitions of gravitational mass and solitonic NUT charge and we apply these to the description of a class of Minkowski-signature multi-Taub–NUT solutions without rod singularities. A Wick rotation then yields the corresponding class of Euclidean-signature gravitational multi-instantons. Keywords Komar charges · Dualities · Exact solutions 1 Introduction In many respects, the Taub–NUT solution [1] appears to be dual to the Schwarzschild solution in a fashion similar to the way a magnetic monopole is the dual of an electric charge in Maxwell theory. The Taub–NUT space–time admits closed time-like geo- desics [2] and, moreover, its analytic extension beyond the horizon turns out to be non G. Bossard (B) · H. Nicolai · K. S. Stelle AEI, Max-Planck-Institut für Gravitationsphysik, Am Mühlenberg 1, 14476 Potsdam, Germany e-mail: [email protected] H. Nicolai e-mail: [email protected] K. S. Stelle Theoretical Physics Group, Imperial College London, Prince Consort Road, London SW7 2AZ, UK e-mail: [email protected] K. S. Stelle Theory Division, Physics Department, CERN, 1211 Geneva 23, Switzerland 123 1368 G. Bossard et al. Hausdorff [3]. The horizon covers an orbifold singularity which is homeomorphic to a two-sphere, although the Riemann tensor is bounded in its vicinity. -
Part 3 Black Holes
Part 3 Black Holes Harvey Reall Part 3 Black Holes March 13, 2015 ii H.S. Reall Contents Preface vii 1 Spherical stars 1 1.1 Cold stars . .1 1.2 Spherical symmetry . .2 1.3 Time-independence . .3 1.4 Static, spherically symmetric, spacetimes . .4 1.5 Tolman-Oppenheimer-Volkoff equations . .5 1.6 Outside the star: the Schwarzschild solution . .6 1.7 The interior solution . .7 1.8 Maximum mass of a cold star . .8 2 The Schwarzschild black hole 11 2.1 Birkhoff's theorem . 11 2.2 Gravitational redshift . 12 2.3 Geodesics of the Schwarzschild solution . 13 2.4 Eddington-Finkelstein coordinates . 14 2.5 Finkelstein diagram . 17 2.6 Gravitational collapse . 18 2.7 Black hole region . 19 2.8 Detecting black holes . 21 2.9 Orbits around a black hole . 22 2.10 White holes . 24 2.11 The Kruskal extension . 25 2.12 Einstein-Rosen bridge . 28 2.13 Extendibility . 29 2.14 Singularities . 29 3 The initial value problem 33 3.1 Predictability . 33 3.2 The initial value problem in GR . 35 iii CONTENTS 3.3 Asymptotically flat initial data . 38 3.4 Strong cosmic censorship . 38 4 The singularity theorem 41 4.1 Null hypersurfaces . 41 4.2 Geodesic deviation . 43 4.3 Geodesic congruences . 44 4.4 Null geodesic congruences . 45 4.5 Expansion, rotation and shear . 46 4.6 Expansion and shear of a null hypersurface . 47 4.7 Trapped surfaces . 48 4.8 Raychaudhuri's equation . 50 4.9 Energy conditions . 51 4.10 Conjugate points . -
Modified Theories of Relativistic Gravity
Modified Theories of Relativistic Gravity: Theoretical Foundations, Phenomenology, and Applications in Physical Cosmology by c David Wenjie Tian A thesis submitted to the School of Graduate Studies in partial fulfillment of the requirements for the degree of Doctor of Philosophy Department of Theoretical Physics (Interdisciplinary Program) Faculty of Science Date of graduation: October 2016 Memorial University of Newfoundland March 2016 St. John’s Newfoundland and Labrador Abstract This thesis studies the theories and phenomenology of modified gravity, along with their applications in cosmology, astrophysics, and effective dark energy. This thesis is organized as follows. Chapter 1 reviews the fundamentals of relativistic gravity and cosmology, and Chapter 2 provides the required Co-authorship 2 2 Statement for Chapters 3 ∼ 6. Chapter 3 develops the L = f (R; Rc; Rm; Lm) class of modified gravity 2 µν 2 µανβ that allows for nonminimal matter-curvature couplings (Rc B RµνR , Rm B RµανβR ), derives the “co- herence condition” f 2 = f 2 = − f 2 =4 for the smooth limit to f (R; G; ) generalized Gauss-Bonnet R Rm Rc Lm gravity, and examines stress-energy-momentum conservation in more generic f (R; R1;:::; Rn; Lm) grav- ity. Chapter 4 proposes a unified formulation to derive the Friedmann equations from (non)equilibrium (eff) thermodynamics for modified gravities Rµν − Rgµν=2 = 8πGeffTµν , and applies this formulation to the Friedman-Robertson-Walker Universe governed by f (R), generalized Brans-Dicke, scalar-tensor-chameleon, quadratic, f (R; G) generalized Gauss-Bonnet and dynamical Chern-Simons gravities. Chapter 5 systemati- cally restudies the thermodynamics of the Universe in ΛCDM and modified gravities by requiring its com- patibility with the holographic-style gravitational equations, where possible solutions to the long-standing confusions regarding the temperature of the cosmological apparent horizon and the failure of the second law of thermodynamics are proposed. -
Extended General Relativity for a Curved Universe
Preprints (www.preprints.org) | NOT PEER-REVIEWED | Posted: 4 January 2021 doi:10.20944/preprints202010.0320.v4 Extended General Relativity for a Curved Universe Mohammed. B. Al-Fadhli1* 1College of Science, University of Lincoln, Lincoln, LN6 7TS, UK. Abstract: The recent Planck Legacy release revealed the presence of an enhanced lensing amplitude in the cosmic microwave background (CMB). Notably, this amplitude is higher than that estimated by the lambda cold dark matter model (ΛCDM), which endorses the positive curvature of the early Universe with a confidence level greater than 99%. Although General Relativity (GR) performs accurately in the local/present Universe where spacetime is almost flat, its lost boundary term, incompatibility with quantum mechanics and the necessity of dark matter and dark energy might indicate its incompleteness. By utilising the Einstein–Hilbert action, this study presents extended field equations considering the pre-existing/background curvature and the boundary contribution. The extended field equations consist of Einstein field equations with a conformal transformation feature in addition to the boundary term, which could remove singularities from the theory and facilitate its quantisation. The extended equations have been utilised to derive the evolution of the Universe with reference to the scale factor of the early Universe and its radius of curvature. Keywords: Astrometry, General Relativity, Boundary Term. 1. INTRODUCTION Considerable efforts have been devoted to Recent evidence by Planck Legacy recent release modifying gravity in form of Conformal Gravity, (PL18) indicated the presence of an enhanced lensing Loop Quantum Gravity, MOND, ADS-CFT, String amplitude in the cosmic microwave background theory, 퐹(푅) Gravity, etc. -
Quasilocal Mass in General Relativity
Quasi-local Mass in General Relativity Shing-Tung Yau Harvard University For the 60th birthday of Gary Horowtiz U. C. Santa Barbara, May. 1, 2015 This talk is based on joint work with Po-Ning Chen and Mu-Tao Wang. As is well known, it is not possible to find mass density of gravity in general relativity. The mass density would have to be first derivative of the metric tensor which is zero in suitable chosen coordinate at a point. 1 But we still desire to measure the total mass in a space like region bounded by a closed surface. The mass due to gravity should be computable from the intrinsic and the extrinsic geometry of the surface. It has been important question to find the right definition. Penrose gave a talk on this question in my seminar in the Institute for Advances Study in 1979, the year before Gary and Andy came to be postdocts. The quantity is called quasilocal mass. 2 Penrose listed it as the first major problem in his list of open problems. Many people, including Penrose, Hawking-Horowitz, Brown-York and others worked on this problem and various definitions were given. I thought about this problem and attempted to look at it from point of view of mathematician. 3 I list properties that the definition should satisfy : 1. It should be nonnegative and zero for any closed surfaces in flat Minkowski spacetime 2. It should converge to the familiar ADM mass for asymptotically flat spacetime if we have a sequence of coordinate spheres that approaches the spatial infinity of an asymptotic flat slice. -
Quasi-Local Conserved Quantities in General Relativity
Quasi-Local Conserved Quantities in General Relativity Dissertation by Henk Bart Quasi-Local Conserved Quantities in General Relativity Dissertation an der Fakult¨atf¨urPhysik der Ludwig{Maximilians{Universit¨at M¨unchen vorgelegt von Henk Bart aus Rotterdam, Niederlande M¨unchen,den 17. September 2019 Dissertation Submitted to the faculty of physics of the Ludwig{Maximilians{Universit¨atM¨unchen by Henk Bart Supervised by Prof. Dr. Dieter L¨ust Max-Planck-Institut f¨urPhysik, M¨unchen 1st Referee: prof. dr. Dieter L¨ust 2nd Referee: prof. dr. Johanna Erdmenger Date of submission: September 17th 2019 Date of oral examination: October 28th 2019 Zusammenfassung Aufgrund des Aquivalenzprinzips¨ existiert in der Allgemeinen Relativit¨atstheorie keine lokale Definition eines Energiebegriffs. Wenngleich Aussicht auf eine m¨ogliche quasi-lokale Definition der Energie bestand, existiert jedoch kein allgemeines Rah- menkonzept innerhalb dessen eine solche Definition einer quasi-lokalen Energie aus- reichend verstanden ist. In dieser Arbeit wird versucht ein solches Rahmenkonzept zu schaffen. Im ersten Teil dieser Arbeit schlagen wir ein allgemeines Rezept zur Definition quasi- lokaler Erhaltungsgr¨oenin der Allgemeinen Relativit¨atstheorievor. Unser Startpunkt ist die Konstruktion von Erhaltungsgr¨oßenauf einer Hyperfl¨ache unendlicher lichtar- tiger Entfernung (\null infinity") durch Wald und Zoupas. Wir zeigen warum ihre Kon- struktion im Inneren der Raumzeit nicht einsetzbar ist und deshalb nicht zur Definition quasi-lokaler Erhaltungsgren verwendet werden kann. Dann f¨uhrenwir eine Modifika- tion ihrer Konstruktion ein, sodass die Erhaltungsgr¨oenallgemeiner und insbesondere im Inneren der Raumzeit definiert sind. Wir fahren fort unsere Konstruktion auf BMS- Symmetrien anzuwenden. Dies sind asymptotische Symmetrien asymptotisch flacher Raumzeiten, welche bei \null infinity" BMS-Ladungen definieren, welche wiederum die Bondi-Masse beinhalten. -
Thin Disks As Sources of Stationary Axisymmetric Electrovacuum
Thin disks as sources of stationary axisymmetric electrovacuum spacetimes TOMAS LEDVINKA Department of Theoretical Physics Faculty of Mathematics and Physics Charles University V Holesovickach Praha Czech Republic A disertation submitted to the Faculty of Mathematics and Physics Charles University in accordance with the regulations for admission to the degree of Do ctor of Physics Branch of the do ctoral study F Theoretical physics astronomy and astrophysics Praha Octob er Acknowledgements I would like to thank professor Jir Bicak for his help He prop osed an inter esting problem encouraged me in my work and he has always had the time to discuss my work with me and has made valuable comments on the content of the thesis Contents Intro duction Relativistic disks as sources of the Kerr metric Thin layers as sources of the stationary axisymmetric spacetimes Total mass angular momentum and charge Energy conditions and the interpretation of the surface stressenergy tensor of the disk Disks formed of counterrotating surface streams of charged particles KerrNewman disks Schwarzschild disks Extreme Reissner Nordstrom disks Kerr disks Charged KerrNewman disks TomimatsuSato spacetimes Concluding remarks App endix A Radial prop erties of Kerr disks App endix B Radial prop erties of KerrNewman disks App endix C Radial prop erties of TomimatsuSato disks Intro duction Unlike in Newtonian gravity there is a lack of complete -
The Hawking Mass for Ellipsoidal 2-Surfaces in Minkowski and Schwarzschild Spacetimes Daniel Hansevi
Examensarbete The Hawking mass for ellipsoidal 2-surfaces in Minkowski and Schwarzschild spacetimes Daniel Hansevi LiTH - MAT - EX - - 08/14 - - SE The Hawking mass for ellipsoidal 2-surfaces in Minkowski and Schwarzschild spacetimes Applied Mathematics, Link¨opings Universitet Daniel Hansevi LiTH - MAT - EX - - 08/14 - - SE Examensarbete: 30 hp Level: D Supervisor: G¨oranBergqvist, Applied Mathematics, Link¨opings Universitet Examiner: G¨oranBergqvist, Applied Mathematics, Link¨opings Universitet Link¨oping: June 2008 Datum Avdelning, Institution Date Division, Department Matematiska Institutionen June 2008 581 83 LINKOPING¨ SWEDEN Spr˚ak Rapporttyp ISBN Language Report category ISRN Svenska/Swedish Licentiatavhandling LiTH - MAT - EX - - 08/14 - - SE x Engelska/English x Examensarbete C-uppsats Serietitel och serienummer ISSN D-uppsats Title of series, numbering 0348-2960 Ovrig¨ rapport URL f¨orelektronisk version Titel The Hawking mass for ellipsoidal 2-surfaces in Minkowski and Schwarzschild space- Title times F¨orfattare Daniel Hansevi Author Sammanfattning Abstract In general relativity, the nature of mass is non-local. However, an appropriate def- inition of mass at a quasi-local level could give a more detailed characterization of the gravitational field around massive bodies. Several attempts have been made to find such a definition. One of the candidates is the Hawking mass. This thesis presents a method for calculating the spin coefficients used in the expression for the Hawking mass, and gives a closed-form expression for the Hawking mass of ellipsoidal 2-surfaces in Minkowski spacetime. Furthermore, the Hawking mass is shown to have the correct limits, both in Minkowski and Schwarzschild, along particular foliations of leaves approaching a metric 2-sphere. -
Energy in General Relativity: a Comparison Between Quasilocal Definitions
Energy in general relativity: A comparison between quasilocal definitions Diogo Pinto Leite de Bragan¸ca A thesis submitted to obtain the Master of Science degree in Engineering Physics Supervisor: Professor Doutor Jos´ePizarro de Sande e Lemos Examination committee Chairperson: Prof. Ana Maria Vergueiro Monteiro Cidade Mour~ao Supervisor: Prof. Jos´ePizarro de Sande e Lemos Member of the Committee: Dr. Andrea Nerozzi September 2016 The most incomprehensible thing about the world is that it is comprehensible. Albert Einstein Acknowledgements I thank Professor Jos´eSande Lemos for having had the courage to accept me as his student, for interesting and insightful discussions on the nature of gravitational energy in general relativity, for helping me finding a problem to solve for my thesis, among many other things. I also thank my fellow student colleagues and friends for all the work we did together that constantly increased my skills, in many different dimensions. I would like to specially thank all the participants of the C´ırculo de Reflex˜aodo IST, of the Miss~aoPa´ıs project, of the Peregrina¸c~aodo IST project, and of the Portal da Sabedoria learning project. Of course, I would also like to thank all my family for continuous support during all my life and for fruitful physics discussions too. Finally, I want to thank Mary for all the help and orientation. iii Abstract Using a 3+1 spacetime decomposition, we derive Brown-York's and Lynden-Bell-Katz's quasilocal energy definitions. Then, we analyse the properties of the two definitions in specific spacetimes and derive what laws of black hole mechanics come from each definition. -
Fundamental Equations for Hypersurfaces
Appendix A Fundamental Equations for Hypersurfaces In this appendix we consider submanifolds with codimension 1 of a pseudo- Riemannian manifold and derive, among other things, the important equations of Gauss and Codazzi–Mainardi. These have many useful applications, in particular for 3 + 1 splittings of Einstein’s equations (see Sect. 3.9). For definiteness, we consider a spacelike hypersurface Σ of a Lorentz manifold (M, g). Other situations, e.g., timelike hypersurfaces can be treated in the same way, with sign changes here and there. The formulation can also be generalized to sub- manifolds of codimension larger than 1 of arbitrary pseudo-Riemannian manifolds (see, for instance, [51]), a situation that occurs for instance in string theory. Let ι : Σ −→ M denote the embedding and let g¯ = ι∗g be the induced metric on Σ. The pair (Σ, g)¯ is a three-dimensional Riemannian manifold. Other quanti- ties which belong to Σ will often be indicated by a bar. The basic results of this appendix are most efficiently derived with the help of adapted moving frames and the structure equations of Cartan. So let {eμ} be an orthonormal frame on an open region of M, with the property that the ei ,fori = 1, 2, 3, at points of Σ are tangent μ to Σ. The dual basis of {eμ} is denoted by {θ }.OnΣ the {ei} can be regarded as a triad of Σ that is dual to the restrictions θ¯i := θ j |TΣ(i.e., the restrictions to tangent vectors of Σ). Indices for objects on Σ always refer to this pair of dual basis.