Zero Mass Limit of Kerr Spacetime Is a Wormhole
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Spacetimes with Singularities Ovidiu Cristinel Stoica
Spacetimes with Singularities Ovidiu Cristinel Stoica To cite this version: Ovidiu Cristinel Stoica. Spacetimes with Singularities. An. Stiint. Univ. Ovidius Constanta, Ser. Mat., 2012, pp.26. hal-00617027v2 HAL Id: hal-00617027 https://hal.archives-ouvertes.fr/hal-00617027v2 Submitted on 30 Nov 2014 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Spacetimes with Singularities ∗†‡ Ovidiu-Cristinel Stoica Abstract We report on some advances made in the problem of singularities in general relativity. First is introduced the singular semi-Riemannian geometry for met- rics which can change their signature (in particular be degenerate). The standard operations like covariant contraction, covariant derivative, and constructions like the Riemann curvature are usually prohibited by the fact that the metric is not invertible. The things become even worse at the points where the signature changes. We show that we can still do many of these operations, in a different framework which we propose. This allows the writing of an equivalent form of Einstein’s equation, which works for degenerate metric too. Once we make the singularities manageable from mathematical view- point, we can extend analytically the black hole solutions and then choose from the maximal extensions globally hyperbolic regions. -
BLACK HOLES: the OTHER SIDE of INFINITY General Information
BLACK HOLES: THE OTHER SIDE OF INFINITY General Information Deep in the middle of our Milky Way galaxy lies an object made famous by science fiction—a supermassive black hole. Scientists have long speculated about the existence of black holes. German astronomer Karl Schwarzschild theorized that black holes form when massive stars collapse. The resulting gravity from this collapse would be so strong that the matter would become more and more dense. The gravity would eventually become so strong that nothing, not even radiation moving at the speed of light, could escape. Schwarzschild’s theories were predicted by Einstein and then borne out mathematically in 1939 by American astrophysicists Robert Oppenheimer and Hartland Snyder. WHAT EXACTLY IS A BLACK HOLE? First, it’s not really a hole! A black hole is an extremely massive concentration of matter, created when the largest stars collapse at the end of their lives. Astronomers theorize that a point with infinite density—called a singularity—lies at the center of black holes. SO WHY IS IT CALLED A HOLE? Albert Einstein’s 1915 General Theory of Relativity deals largely with the effects of gravity, and in essence predicts the existence of black holes and singularities. Einstein hypothesized that gravity is a direct result of mass distorting space. He argued that space behaves like an invisible fabric with an elastic quality. Celestial bodies interact with this “fabric” of space-time, appearing to create depressions termed “gravity wells” and drawing nearby objects into orbit around them. Based on this principle, the more massive a body is in space, the deeper the gravity well it will create. -
Closed Timelike Curves, Singularities and Causality: a Survey from Gödel to Chronological Protection
Closed Timelike Curves, Singularities and Causality: A Survey from Gödel to Chronological Protection Jean-Pierre Luminet Aix-Marseille Université, CNRS, Laboratoire d’Astrophysique de Marseille , France; Centre de Physique Théorique de Marseille (France) Observatoire de Paris, LUTH (France) [email protected] Abstract: I give a historical survey of the discussions about the existence of closed timelike curves in general relativistic models of the universe, opening the physical possibility of time travel in the past, as first recognized by K. Gödel in his rotating universe model of 1949. I emphasize that journeying into the past is intimately linked to spacetime models devoid of timelike singularities. Since such singularities arise as an inevitable consequence of the equations of general relativity given physically reasonable assumptions, time travel in the past becomes possible only when one or another of these assumptions is violated. It is the case with wormhole-type solutions. S. Hawking and other authors have tried to save the paradoxical consequences of time travel in the past by advocating physical mechanisms of chronological protection; however, such mechanisms remain presently unknown, even when quantum fluctuations near horizons are taken into account. I close the survey by a brief and pedestrian discussion of Causal Dynamical Triangulations, an approach to quantum gravity in which causality plays a seminal role. Keywords: time travel; closed timelike curves; singularities; wormholes; Gödel’s universe; chronological protection; causal dynamical triangulations 1. Introduction In 1949, the mathematician and logician Kurt Gödel, who had previously demonstrated the incompleteness theorems that broke ground in logic, mathematics, and philosophy, became interested in the theory of general relativity of Albert Einstein, of which he became a close colleague at the Institute for Advanced Study at Princeton. -
Generalizations of the Kerr-Newman Solution
Generalizations of the Kerr-Newman solution Contents 1 Topics 1035 1.1 ICRANetParticipants. 1035 1.2 Ongoingcollaborations. 1035 1.3 Students ............................... 1035 2 Brief description 1037 3 Introduction 1039 4 Thegeneralstaticvacuumsolution 1041 4.1 Line element and field equations . 1041 4.2 Staticsolution ............................ 1043 5 Stationary generalization 1045 5.1 Ernst representation . 1045 5.2 Representation as a nonlinear sigma model . 1046 5.3 Representation as a generalized harmonic map . 1048 5.4 Dimensional extension . 1052 5.5 Thegeneralsolution . 1055 6 Tidal indicators in the spacetime of a rotating deformed mass 1059 6.1 Introduction ............................. 1059 6.2 The gravitational field of a rotating deformed mass . 1060 6.2.1 Limitingcases. 1062 6.3 Circularorbitsonthesymmetryplane . 1064 6.4 Tidalindicators ........................... 1065 6.4.1 Super-energy density and super-Poynting vector . 1067 6.4.2 Discussion.......................... 1068 6.4.3 Limit of slow rotation and small deformation . 1069 6.5 Multipole moments, tidal Love numbers and Post-Newtonian theory................................. 1076 6.6 Concludingremarks . 1077 7 Neutrino oscillations in the field of a rotating deformed mass 1081 7.1 Introduction ............................. 1081 7.2 Stationary axisymmetric spacetimes and neutrino oscillation . 1082 7.2.1 Geodesics .......................... 1083 1033 Contents 7.2.2 Neutrinooscillations . 1084 7.3 Neutrino oscillations in the Hartle-Thorne metric . 1085 7.4 Concludingremarks . 1088 8 Gravitational field of compact objects in general relativity 1091 8.1 Introduction ............................. 1091 8.2 The Hartle-Thorne metrics . 1094 8.2.1 The interior solution . 1094 8.2.2 The Exterior Solution . 1096 8.3 The Fock’s approach . 1097 8.3.1 The interior solution . -
Light Rays, Singularities, and All That
Light Rays, Singularities, and All That Edward Witten School of Natural Sciences, Institute for Advanced Study Einstein Drive, Princeton, NJ 08540 USA Abstract This article is an introduction to causal properties of General Relativity. Topics include the Raychaudhuri equation, singularity theorems of Penrose and Hawking, the black hole area theorem, topological censorship, and the Gao-Wald theorem. The article is based on lectures at the 2018 summer program Prospects in Theoretical Physics at the Institute for Advanced Study, and also at the 2020 New Zealand Mathematical Research Institute summer school in Nelson, New Zealand. Contents 1 Introduction 3 2 Causal Paths 4 3 Globally Hyperbolic Spacetimes 11 3.1 Definition . 11 3.2 Some Properties of Globally Hyperbolic Spacetimes . 15 3.3 More On Compactness . 18 3.4 Cauchy Horizons . 21 3.5 Causality Conditions . 23 3.6 Maximal Extensions . 24 4 Geodesics and Focal Points 25 4.1 The Riemannian Case . 25 4.2 Lorentz Signature Analog . 28 4.3 Raychaudhuri’s Equation . 31 4.4 Hawking’s Big Bang Singularity Theorem . 35 5 Null Geodesics and Penrose’s Theorem 37 5.1 Promptness . 37 5.2 Promptness And Focal Points . 40 5.3 More On The Boundary Of The Future . 46 1 5.4 The Null Raychaudhuri Equation . 47 5.5 Trapped Surfaces . 52 5.6 Penrose’s Theorem . 54 6 Black Holes 58 6.1 Cosmic Censorship . 58 6.2 The Black Hole Region . 60 6.3 The Horizon And Its Generators . 63 7 Some Additional Topics 66 7.1 Topological Censorship . 67 7.2 The Averaged Null Energy Condition . -
Singularities, Black Holes, and Cosmic Censorship: a Tribute to Roger Penrose
Foundations of Physics (2021) 51:42 https://doi.org/10.1007/s10701-021-00432-1 INVITED REVIEW Singularities, Black Holes, and Cosmic Censorship: A Tribute to Roger Penrose Klaas Landsman1 Received: 8 January 2021 / Accepted: 25 January 2021 © The Author(s) 2021 Abstract In the light of his recent (and fully deserved) Nobel Prize, this pedagogical paper draws attention to a fundamental tension that drove Penrose’s work on general rela- tivity. His 1965 singularity theorem (for which he got the prize) does not in fact imply the existence of black holes (even if its assumptions are met). Similarly, his versatile defnition of a singular space–time does not match the generally accepted defnition of a black hole (derived from his concept of null infnity). To overcome this, Penrose launched his cosmic censorship conjecture(s), whose evolution we discuss. In particular, we review both his own (mature) formulation and its later, inequivalent reformulation in the PDE literature. As a compromise, one might say that in “generic” or “physically reasonable” space–times, weak cosmic censorship postulates the appearance and stability of event horizons, whereas strong cosmic censorship asks for the instability and ensuing disappearance of Cauchy horizons. As an encore, an “Appendix” by Erik Curiel reviews the early history of the defni- tion of a black hole. Keywords General relativity · Roger Penrose · Black holes · Ccosmic censorship * Klaas Landsman [email protected] 1 Department of Mathematics, Radboud University, Nijmegen, The Netherlands Vol.:(0123456789)1 3 42 Page 2 of 38 Foundations of Physics (2021) 51:42 Conformal diagram [146, p. 208, Fig. -
Generalizations of the Kerr-Newman Solution
Generalizations of the Kerr-Newman solution Contents 1 Topics 663 1.1 ICRANetParticipants. 663 1.2 Ongoingcollaborations. 663 1.3 Students ............................... 663 2 Brief description 665 3 Introduction 667 4 Thegeneralstaticvacuumsolution 669 4.1 Line element and field equations . 669 4.2 Staticsolution ............................ 671 5 Stationary generalization 673 5.1 Ernst representation . 673 5.2 Representation as a nonlinear sigma model . 674 5.3 Representation as a generalized harmonic map . 676 5.4 Dimensional extension . 680 5.5 Thegeneralsolution ........................ 683 6 Static and slowly rotating stars in the weak-field approximation 687 6.1 Introduction ............................. 687 6.2 Slowly rotating stars in Newtonian gravity . 689 6.2.1 Coordinates ......................... 690 6.2.2 Spherical harmonics . 692 6.3 Physical properties of the model . 694 6.3.1 Mass and Central Density . 695 6.3.2 The Shape of the Star and Numerical Integration . 697 6.3.3 Ellipticity .......................... 699 6.3.4 Quadrupole Moment . 700 6.3.5 MomentofInertia . 700 6.4 Summary............................... 701 6.4.1 Thestaticcase........................ 702 6.4.2 The rotating case: l = 0Equations ............ 702 6.4.3 The rotating case: l = 2Equations ............ 703 6.5 Anexample:Whitedwarfs. 704 6.6 Conclusions ............................. 708 659 Contents 7 PropertiesoftheergoregionintheKerrspacetime 711 7.1 Introduction ............................. 711 7.2 Generalproperties ......................... 712 7.2.1 The black hole case (0 < a < M) ............. 713 7.2.2 The extreme black hole case (a = M) .......... 714 7.2.3 The naked singularity case (a > M) ........... 714 7.2.4 The equatorial plane . 714 7.2.5 Symmetries and Killing vectors . 715 7.2.6 The energetic inside the Kerr ergoregion . -
Stable Wormholes in the Background of an Exponential F (R) Gravity
universe Article Stable Wormholes in the Background of an Exponential f (R) Gravity Ghulam Mustafa 1, Ibrar Hussain 2,* and M. Farasat Shamir 3 1 Department of Mathematics, Shanghai University, Shanghai 200444, China; [email protected] 2 School of Electrical Engineering and Computer Science, National University of Sciences and Technology, H-12, Islamabad 44000, Pakistan 3 National University of Computer and Emerging Sciences, Lahore Campus, Punjab 54000, Pakistan; [email protected] * Correspondence: [email protected] Received: 21 January 2020; Accepted: 3 March 2020; Published: 26 March 2020 Abstract: The current paper is devoted to investigating wormhole solutions with an exponential gravity model in the background of f (R) theory. Spherically symmetric static spacetime geometry is chosen to explore wormhole solutions with anisotropic fluid source. The behavior of the traceless matter is studied by employing a particular equation of state to describe the important properties of the shape-function of the wormhole geometry. Furthermore, the energy conditions and stability analysis are done for two specific shape-functions. It is seen that the energy condition are to be violated for both of the shape-functions chosen here. It is concluded that our results are stable and realistic. Keywords: wormholes; stability; f (R) gravity; energy conditions 1. Introduction The discussion on wormhole geometry is a very hot subject among the investigators of the different modified theories of gravity. The concept of wormhole was first expressed by Flamm [1] in 1916. After 20 years, Einstein and Rosen [2] calculated the wormhole geometry in a specific background. In fact, it was the second attempt to realize the basic structure of wormholes. -
Weyl Metrics and Wormholes
Prepared for submission to JCAP Weyl metrics and wormholes Gary W. Gibbons,a;b Mikhail S. Volkovb;c aDAMTP, University of Cambridge, Wilberforce Road, Cambridge CB3 0WA, UK bLaboratoire de Math´ematiqueset Physique Th´eorique,LMPT CNRS { UMR 7350, Universit´ede Tours, Parc de Grandmont, 37200 Tours, France cDepartment of General Relativity and Gravitation, Institute of Physics, Kazan Federal University, Kremlevskaya street 18, 420008 Kazan, Russia E-mail: [email protected], [email protected] Abstract. We study solutions obtained via applying dualities and complexifications to the vacuum Weyl metrics generated by massive rods and by point masses. Rescal- ing them and extending to complex parameter values yields axially symmetric vacuum solutions containing singularities along circles that can be viewed as singular mat- ter sources. These solutions have wormhole topology with several asymptotic regions interconnected by throats and their sources can be viewed as thin rings of negative tension encircling the throats. For a particular value of the ring tension the geometry becomes exactly flat although the topology remains non-trivial, so that the rings liter- ally produce holes in flat space. To create a single ring wormhole of one metre radius one needs a negative energy equivalent to the mass of Jupiter. Further duality trans- formations dress the rings with the scalar field, either conventional or phantom. This gives rise to large classes of static, axially symmetric solutions, presumably including all previously known solutions for a gravity-coupled massless scalar field, as for exam- ple the spherically symmetric Bronnikov-Ellis wormholes with phantom scalar. The multi-wormholes contain infinite struts everywhere at the symmetry axes, apart from arXiv:1701.05533v3 [hep-th] 25 May 2017 solutions with locally flat geometry. -
PHY390, the Kerr Metric and Black Holes
PHY390, The Kerr Metric and Black Holes James Lattimer Department of Physics & Astronomy 449 ESS Bldg. Stony Brook University April 1, 2021 Black Holes, Neutron Stars and Gravitational Radiation [email protected] James Lattimer PHY390, The Kerr Metric and Black Holes What Exactly is a Black Hole? Standard definition: A region of space from which nothing, not even light, can escape. I Where does the escape velocity equal the speed of light? r 2GMBH vesc = = c RSch This defines the Schwarzschild radius RSch to be 2GMBH M RSch = 2 ' 3 km c M I The event horizon marks the point of no return for any object. I A black hole is black because it absorbs everything incident on the event horizon and reflects nothing. I Black holes are hypothesized to form in three ways: I Gravitational collapse of a star I A high energy collision I Density fluctuations in the early universe I In general relativity, the black hole's mass is concentrated at the center in a singularity of infinite density. James Lattimer PHY390, The Kerr Metric and Black Holes John Michell and Black Holes The first reference is by the Anglican priest, John Michell (1724-1793), in a letter written to Henry Cavendish, of the Royal Society, in 1783. He reasoned, from observations of radiation pressure, that light, like mass, has inertia. If gravity affects light like its mass equivalent, light would be weakened. He argued that a Sun with 500 times its radius and the same density would be so massive that it's escape velocity would exceed light speed. -
Quantum Fluctuations and Thermodynamic Processes in The
Quantum fluctuations and thermodynamic processes in the presence of closed timelike curves by Tsunefumi Tanaka A thesis submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Physics Montana State University © Copyright by Tsunefumi Tanaka (1997) Abstract: A closed timelike curve (CTC) is a closed loop in spacetime whose tangent vector is everywhere timelike. A spacetime which contains CTC’s will allow time travel. One of these spacetimes is Grant space. It can be constructed from Minkowski space by imposing periodic boundary conditions in spatial directions and making the boundaries move toward each other. If Hawking’s chronology protection conjecture is correct, there must be a physical mechanism preventing the formation of CTC’s. Currently the most promising candidate for the chronology protection mechanism is the back reaction of the metric to quantum vacuum fluctuations. In this thesis the quantum fluctuations for a massive scalar field, a self-interacting field, and for a field at nonzero temperature are calculated in Grant space. The stress-energy tensor is found to remain finite everywhere in Grant space for the massive scalar field with sufficiently large field mass. Otherwise it diverges on chronology horizons like the stress-energy tensor for a massless scalar field. If CTC’s exist they will have profound effects on physical processes. Causality can be protected even in the presence of CTC’s if the self-consistency condition is imposed on all processes. Simple classical thermodynamic processes of a box filled with ideal gas in the presence of CTC’s are studied. If a system of boxes is closed, its state does not change as it travels through a region of spacetime with CTC’s. -
Complex Structures in the Dynamics of Kerr Black Holes
Complex structures in the dynamics of Kerr black holes Ben Maybee [email protected] Higgs Centre for Theoretical Physics, The University of Edinburgh YTF 20, e-Durham In a certain film… Help! I need to precisely scatter off a spinning black hole and reach a life supporting planet… Spinning black holes are very special…maybe some insight will simplify things? Christopher Nolan and Warner Bros Pictures, 2013 In a certain film… Okay, you’re good with spin; what should I try? Black holes are easy; the spin vector 푎휇 determines all multipoles. Try using the Newman- Janis shift… Hansen, 1974 Outline 1. The Newman-Janis shift 2. Kerr black holes as elementary particles? 3. Effective actions and complex worldsheets 4. Spinor equations of motion 5. Discussion The Newman-Janis shift Simple statement: Kerr metric, with spin parameter 푎, can be Newman & obtained from Schwarzschild by complex Janis, 1965 transformation 푧 → 푧 + 푖푎 Kerr and Schwarzschild are both exact Kerr-Schild solutions to GR: Kerr & Schild, 1965 Background metric Null vector, Scalar function Classical double copy: ∃ gauge theory solution Monteiro, O’Connell & White, 2014 → EM analogue of Kerr: Kerr! The Newman-Janis shift Metrics: Under 푧 → 푧 + 푖푎, 푟2 → 푟ǁ + 푖푎 cos 휃 2. Why did that just happen??? Scattering amplitudes and spin No hair theorem → all black hole multipoles specified by Hansen, 1974 mass and spin vector. Wigner classification → single particle Wigner, states specified by mass and spin s. 1939 Little group irreps Any state in a little group irrep can be represented using chiral spinor- helicity variables: Distinct spinor reps Arkani-Hamed, Huang & Huang, 2017 Little group metric Massless: 푈(1) → 훿푖푗 2-spinors Massive: 푆푈 2 → 휖푗푖 3-point exponentiation Use to calculate amplitudes for any spin s: Chiral Spin = parameter e.g.