DOCSLIB.ORG

Gr-Qc] 3 Nov 2014 I’Avzef O.9,Is ,(00 147–151

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Gr-Qc] 3 Nov 2014 I’Avzef O.9,Is ,(00 147–151 JETP Letters, 2010, Vol. 92, No. 3, pp. 125-129. On the collisions between particles in the vicinity of rotating black holes 1) A. A. Griba, Yu. V. Pavlovb aTheoretical Physics and Astronomy Department, The Herzen University, 48, Moika, St. Petersburg, 191186, Russia e-mail: andrei [email protected] bInstitute of Problems in Mechanical Engineering, RAS, 61 Bolshoy, V.O., St. Petersburg, 199178, Russia e-mail: [email protected] Submitted 9 June 2010 Scattering of particles in the gravitational field of rotating black holes is considered. It is shown that scat- tering energy of particles in the centre of mass system can obtain very large values not only for extremal black holes but also for nonextremal ones. Extraction of energy after the collision is investigated. It is shown that due to the Penrose process the energy of the particle escaping the hole at infinity can be large. Contradictions in the problem of getting high energetic particles escaping the black hole are resolved. In [1] we put the hypothesis that active galactic nu- the cases of multiple scattering. In the first part we cal- clei can be the sources of ultrahigh energy particles in culate this energy, reproduce the results of [9, 10, 11] cosmic rays observed recently by the AUGER group and show that in some cases (multiple scattering) the (see [2]) due to the processes of converting dark mat- results of [10, 11] on the limitations of the scattering ter formed by superheavy neutral particles into visible energy for nonextremal black holes are not valid. particles — quarks, leptons (neutrinos), photons. If ac- In the second part we obtain the results for the ex- tive galactic nuclei are rotating black holes then in [1] traction of the energy after collision in the field of the we discussed the idea that “This black hole acts as a cos- Kerr’s metric. It occurs that the Penrose process plays mic supercollider in which superheavy particles of dark important role for getting larger energies of particles matter are accelerated close to the horizon to the Grand at infinity. Our calculations show that the conclusion Unification energies and can be scattering in collisions.” of [11] about the impossibility of getting at infinity the It was also shown [3] that in Penrose process [4] dark energy larger than the initial one in particle collisions matter particle can decay on two particles, one with the close to the black hole is wrong. negative energy, the other with the positive one and par- The system of units G = c = 1 is used in the paper. ticles of very high energy of the Grand Unification or- der can escape the black hole. Then these particles due 1. THE ENERGY OF COLLISION IN THE to interaction with photons close to the black hole will FIELD OF BLACK HOLES loose energy analogously up to the Greisen-Zatsepin- Kuzmin limit in cosmology [5, 6]. Let us consider particles falling on the rotating First calculations of the scattering of particles in the chargeless black hole. The Kerr’s metric of the rotating ergosphere of the rotating black hole, taking into ac- arXiv:1004.0913v2 [gr-qc] 3 Nov 2014 black hole in Boyer–Lindquist coordinates has the form count the Penrose process, with the result that particles 2 2 with high energy can escape the black hole, were made 2 2 2Mr (dt a sin θ dϕ) ds = dt 2 − 2 2 in [7, 8]. Recently in [9] it was shown that for the ro- − r + a cos θ dr2 tating black hole (if it is the critical one) the energy of (r2 + a2 cos2θ) + dθ2 (r2 + a2) sin2θ dϕ2, (1) − ∆ − scattering is unlimited. The result of [9] was criticized in [10, 11] in the sense that it does not occur in nature. where The authors of [10, 11] claimed that if the black hole is ∆= r2 2Mr + a2, (2) − not a critical rotating black hole so that its dimension- M is the mass of the black hole, J = aM is angular less angular momentum A = 1 but A = 0.998 then the 6 momentum. In the case a = 0 the metric (1) describes energy is limited. the static chargeless black hole in Schwarzschild coor- In this paper we show that the energy of scattering dinates. The event horizon for the Kerr’s black hole in the centre of mass system can be still unlimited in corresponds to the value 1)On particles collisions in the vicinity of rotating black holes, Pis’ma v ZhETF, vol. 92, iss. 3, (2010) 147–151. r = r M + M 2 a2 . (3) H ≡ − p 2 GRIB, PAVLOV The Cauchy horizon is For the extremal black hole A = xH = 1, lH = 2 and the expression (10) is divergent when the dimensionless r = r M M 2 a2 . (4) C ≡ − − angular momentum of one of the falling into the black p hole particles l 2. The scattering energy in the centre The surface called “the static limit” is defined by the → of mass system is increasing without limit [9]. expression Let’s note, that to get the collision with infinite en- 2 2 2 ergy one needs the infinite interval of as coordinate as r = r0 M + M a cos θ . (5) ≡ − proper time of the free falling particle. Really, from p The region of space-time between the horizon and the Eqs. (6), (8) for a particle with dimensionless angular static limit is ergosphere. momentum l and specific energy ε = 1 falling from some For equatorial (θ = π/2) geodesics in Kerr’s met- point r0 = x0M to the point rf = xf M > rH one ob- ric (1) one obtains ([12], 61): tains for the coordinate time (proper time of the ob- § server at rest far from the black hole) 2 dt 1 2 2 2Ma 2Ma = r + a + ε L , (6) x0 dτ ∆ r − r √x x3 + A2x +2A(A l) dx ∆t = M − . (x x )(x x ) 2x2 l2x + 2(A l)2 dϕ 1 2Ma 2M Z H C = ε + 1 L , (7) xf − − − − dτ ∆ r − r p (11) For the interval of proper time of the free falling to the dr 2 2M a2ε2 L2 ∆ = ε2 + (aε L)2 + − δ , (8) black hole particle one obtains from (8) dτ r3 − r2 − r2 1 x0 where δ1 = 1 for timelike geodesics (δ1 = 0 for isotropic x3/2 dx ∆τ = M . (12) geodesics), τ is the proper time of the moving particle, 2x2 l2x + 2(A l)2 ε = const is the specific energy: the particle with rest xZf − − mass m has the energy εm in the gravitational field (1); p Lm = const is the angular momentum of the particle In extremal case (A = 1, l = 2) the integrals (11), (12) diverges for x x = 1 and ∆t M2√2(x 1)−1, relative to the axis orthogonal to the plane of move- f → H ≈ f − ∆τ M ln(x 1) /√2 for x 1. ment. ≈ | f − | f → From (7), (8) for the angle of the particle falling in We denote x = r/M, xH = rH /M, xC = rC /M, A = a/M, l = L /M, ∆ = x2 2x + A2. For equatorial plane of the black hole one obtains n n x − the energy in the centre of mass frame of two colliding x0 √x (xl + 2(A l)) dx particles with angular momenta L1, L2, which are non- ∆ϕ = − . 2 2 2 relativistic at infinity (ε1 = ε2 = 1) and are moving in (x xH )(x xC ) 2x l x + 2(A l) xZf − − − − Kerr’s metric using (1), (6)–(8) one obtains [9]: p (13) 2 If A = 0, then integral (13) is divergent for xf xH . Ec.m. 1 2 6 → −1 In extremal case (A = 1, l = 2) ∆ϕ √2(xf 1) 2 = 2x (x 1)+ l1l2(2 x) 2 m x∆x − − ≈ − " for xf 1. So before collision with infinitely large en- 2 → +2A (x + 1) 2A(l1 + l2) (9) ergy the particle must commit infinitely large number − of rotations around the black hole. (2x2 + 2(l A)2 l2x) (2x2 + 2(l A)2 l2x) . Can one get the unlimited high energy of this scat- − 1 − − 1 2 − − 2 q # tering energy for the case of nonextremal black hole? Formula (8) leads to limitations on the possible values of To find the limit r rH for the black hole with → the angular momentum of falling particles: the massive a given angular momentum A one must take in (9) particle free falling in the black hole with dimensionless x = xH +α with α 0 and do calculations up to the or- 2 → 2 angular momentum A being nonrelativistic at infinity der α . Taking into account A = xH xC , xH + xC = 2, (ε = 1) to achieve the horizon of the black hole must after resolution of uncertainties in the limit α 0 one → have angular momentum from the interval obtains 2 2 1+ √1+ A = l l l =2 1+ √1 A . Ec.m.(r rH ) (l1 l2) − L ≤ ≤ R − → = 1+ − , (10) (14) 2m s 2xC (l1 lH )(l2 lH ) − − Putting the limiting values of angular momenta where lH =2xH /A. lL,lR into the formula (10) one obtains the maximal ONTHECOLLISIONSBETWEENPARTICLES 3 values of the collision energy of particles freely falling from the infinity but from some distance defined by (18) from infinity then due to the form of the potential it can have val- ues of l = lH δ large than lR and fall on the horizon. inf 2m − E (r rH )= (15) If the particle falling from infinity with l lR arrives c.m.
Load more

Recommended publications
  • Arxiv:2010.09481V1 [Gr-Qc] 19 Oct 2020 Ally Neutral Plasma Start to Be Relevant
    Radiative Penrose process: Energy Gain by a Single Radiating Charged Particle in the Ergosphere of Rotating Black Hole Martin Koloˇs, Arman Tursunov, and ZdenˇekStuchl´ık Research Centre for Theoretical Physics and Astrophysics, Institute of Physics, Silesian University in Opava, Bezruˇcovon´am.13,CZ-74601 Opava, Czech Republic∗ We demonstrate an extraordinary effect of energy gain by a single radiating charged particle inside the ergosphere of a Kerr black hole in presence of magnetic field. We solve numerically the covariant form of the Lorentz-Dirac equation reduced from the DeWitt-Brehme equation and analyze energy evolution of the radiating charged particle inside the ergosphere, where the energy of emitted radiation can be negative with respect to a distant observer in dependence on the relative orientation of the magnetic field, black hole spin and the direction of the charged particle motion. Consequently, the charged particle can leave the ergosphere with energy greater than initial in expense of black hole's rotational energy. In contrast to the original Penrose process and its various modification, the new process does not require the interactions (collisions or decay) with other particles and consequent restrictions on the relative velocities between fragments. We show that such a Radiative Penrose effect is potentially observable and discuss its possible relevance in formation of relativistic jets and in similar high-energy astrophysical settings. INTRODUCTION KERR SPACETIME AND EXTERNAL MAGNETIC FIELD The fundamental role of combined strong gravitational The Kerr metric in the Boyer{Lindquist coordinates and magnetic fields for processes around BH has been and geometric units (G = 1 = c) reads proposed in [1, 2].
    [Show full text]
  • Energetics of the Kerr-Newman Black Hole by the Penrose Process
    J. Astrophys. Astr. (1985) 6, 85 –100 Energetics of the Kerr-Newman Black Hole by the Penrose Process Manjiri Bhat, Sanjeev Dhurandhar & Naresh Dadhich Department of Mathematics, University of Poona, Pune 411 007 Received 1984 September 20; accepted 1985 January 10 Abstract. We have studied in detail the energetics of Kerr–Newman black hole by the Penrose process using charged particles. It turns out that the presence of electromagnetic field offers very favourable conditions for energy extraction by allowing for a region with enlarged negative energy states much beyond r = 2M, and higher negative values for energy. However, when uncharged particles are involved, the efficiency of the process (defined as the gain in energy/input energy) gets reduced by the presence of charge on the black hole in comparison with the maximum efficiency limit of 20.7 per cent for the Kerr black hole. This fact is overwhelmingly compensated when charged particles are involved as there exists virtually no upper bound on the efficiency. A specific example of over 100 per cent efficiency is given. Key words: black hole energetics—Kerr-Newman black hole—Penrose process—energy extraction 1. Introduction The problem of powering active galactic nuclei, X-raybinaries and quasars is one of the most important problems today in high energy astrophysics. Several mechanisms have been proposed by various authors (Abramowicz, Calvani & Nobili 1983; Rees et al., 1982; Koztowski, Jaroszynski & Abramowicz 1978; Shakura & Sunyaev 1973; for an excellent review see Pringle 1981). Rees et al. (1982) argue that the electromagnetic extraction of black hole’s rotational energy can be achieved by appropriately putting charged particles in negative energy orbits.
    [Show full text]
  • Schwarzschild Black Hole Can Also Produce Super-Radiation Phenomena
    Schwarzschild black hole can also produce super-radiation phenomena Wen-Xiang Chen∗ Department of Astronomy, School of Physics and Materials Science, GuangZhou University According to traditional theory, the Schwarzschild black hole does not produce super radiation. If the boundary conditions are set in advance, the possibility is combined with the wave function of the coupling of the boson in the Schwarzschild black hole, and the mass of the incident boson acts as a mirror, so even if the Schwarzschild black hole can also produce super-radiation phenomena. Keywords: Schwarzschild black hole, superradiance, Wronskian determinant I. INTRODUCTION In a closely related study in 1962, Roger Penrose proposed a theory that by using point particles, it is possible to extract rotational energy from black holes. The Penrose process describes the fact that the Kerr black hole energy layer region may have negative energy relative to the observer outside the horizon. When a particle falls into the energy layer region, such a process may occur: the particle from the black hole To escape, its energy is greater than the initial state. It can also show that in Reissner-Nordstrom (charged, static) and rotating black holes, a generalized ergoregion and similar energy extraction process is possible. The Penrose process is a process inferred by Roger Penrose that can extract energy from a rotating black hole. Because the rotating energy is at the position of the black hole, not in the event horizon, but in the area called the energy layer in Kerr space-time, where the particles must be like a propelling locomotive, rotating with space-time, so it is possible to extract energy .
    [Show full text]
  • Arxiv:1605.04629V2 [Gr-Qc]
    Implementing black hole as efficient power plant Shao-Wen Wei ∗, Yu-Xiao Liu† Institute of Theoretical Physics & Research Center of Gravitation, Lanzhou University, Lanzhou 730000, People’s Republic of China Abstract Treating the black hole molecules as working substance and considering its phase structure, we study the black hole heat engine by a charged anti-de Sitter black hole. In the reduced temperature- entropy chart, it is found that the work, heat, and efficiency of the engine are free of the black hole charge. Applying the Rankine cycle with or without a back pressure mechanism to the black hole heat engine, the compact formula for the efficiency is obtained. And the heat, work and efficiency are worked out. The result shows that the black hole engine working along the Rankine cycle with a back pressure mechanism has a higher efficiency. This provides a novel and efficient mechanism to produce the useful mechanical work, and such black hole heat engine may act as a possible energy source for the high energy astrophysical phenomena near the black hole. PACS numbers: 04.70.Dy, 05.70.Ce, 07.20.Pe Keywords: Black hole, heat engine, phase transition arXiv:1605.04629v2 [gr-qc] 7 Jun 2019 ∗ [email protected] † [email protected] 1 I. INTRODUCTION Black hole has been a fascinating object since general relativity predicted its existence. Compared with other stars, a black hole has sufficient density and a huge amount of energy. Near a black hole, there are many high energy astrophysical phenomena related to the energy flow, such as the power jet and black holes merging.
    [Show full text]
  • Return of the Quantum Cosmic Censor
    Return of the quantum cosmic censor Shahar Hod The Ruppin Academic Center, Emeq Hefer 40250, Israel and The Hadassah Institute, Jerusalem 91010, Israel (Dated: November 8, 2018) The influential theorems of Hawking and Penrose demonstrate that spacetime singularities are ubiquitous features of general relativity, Einstein’s theory of gravity. The utility of classical general relativity in describing gravitational phenomena is maintained by the cosmic censorship principle. This conjecture, whose validity is still one of the most important open questions in general relativity, asserts that the undesirable spacetime singularities are always hidden inside of black holes. In this Letter we reanalyze extreme situations which have been considered as counterexamples to the cosmic censorship hypothesis. In particular, we consider the absorption of fermion particles by a spinning black hole. Ignoring quantum effects may lead one to conclude that an incident fermion wave may over spin the black hole, thereby exposing its inner singularity to distant observers. However, we show that when quantum effects are properly taken into account, the integrity of the black-hole event horizon is irrefutable. This observation suggests that the cosmic censorship principle is intrinsically a quantum phenomena. Spacetime singularities that arise in gravitational col- the relation lapse are always hidden inside of black holes, invisible to M 2 Q2 a2 0 , (1) distant observers. This is the essence of the weak cosmic − − ≥ censorship conjecture (WCCC), put forward by Penrose where a J/M is the specific angular momentum of forty years ago [1, 2, 3, 4]. The validity of this hypothesis the black≡ hole. Extreme black holes are the ones which is essential for preserving the predictability of Einstein’s saturate the relation (1).
    [Show full text]
  • The Collisional Penrose Process
    Noname manuscript No. (will be inserted by the editor) The Collisional Penrose Process Jeremy D. Schnittman Received: date / Accepted: date Abstract Shortly after the discovery of the Kerr metric in 1963, it was realized that a region existed outside of the black hole's event horizon where no time-like observer could remain stationary. In 1969, Roger Penrose showed that particles within this ergosphere region could possess negative energy, as measured by an observer at infinity. When captured by the horizon, these negative energy parti- cles essentially extract mass and angular momentum from the black hole. While the decay of a single particle within the ergosphere is not a particularly efficient means of energy extraction, the collision of multiple particles can reach arbitrar- ily high center-of-mass energy in the limit of extremal black hole spin. The re- sulting particles can escape with high efficiency, potentially erving as a probe of high-energy particle physics as well as general relativity. In this paper, we briefly review the history of the field and highlight a specific astrophysical application of the collisional Penrose process: the potential to enhance annihilation of dark matter particles in the vicinity of a supermassive black hole. Keywords black holes · ergosphere · Kerr metric 1 Introduction We begin with a brief overview of the Kerr metric for spinning, stationary black holes [1]. By far the most convenient, and thus most common form of the Kerr metric is the form derived by Boyer and Lindquist [2]. In standard spherical coor-
    [Show full text]
  • Conformal Field Theory and Black Hole Physics
    CONFORMAL FIELD THEORY AND BLACK HOLE PHYSICS Steve Sidhu Bachelor of Science, University of Northern British Columbia, 2009 A Thesis Submitted to the School of Graduate Studies of the University of Lethbridge in Partial Fulfilment of the Requirements for the Degree MASTER OF SCIENCE Department of Physics and Astronomy University of Lethbridge LETHBRIDGE, ALBERTA, CANADA c Steve Sidhu, 2012 Dedication To my parents, my sister, and Paige R. Ryan. iii Abstract 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) dimen- sions. 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. iv Acknowledgements I would like to thank my supervisors Mark Walton and Saurya Das. I would also like to thank Ali Nassar and Ahmed Farag Ali for the many discussions, the Theo- retical Physics Group, and the entire Department of Physics and Astronomy at the University of Lethbridge. v Table of Contents Approval/Signature Page ii Dedication iii Abstract iv Acknowledgements v Table of Contents vi 1 Introduction 1 2 Einstein’s field equations and black hole solutions 7 2.1 Conventions and notations . 7 2.2 Einstein’s field equations .
    [Show full text]
  • Disser Shaymatov.Pdf
    UZBEKISTAN ACADEMY OF SCIENCES ASTRONOMICAL INSTITUTE INSTITUTE OF NUCLEAR PHYSICS УДК 530.12:531.51 SHAYMATOV SANJAR RUZIMUROTOVICH GENERAL RELATIVISTIC ASTROPHYSICAL PROCESSES IN THE VICINITY OF COMPACT GRAVITATIONAL OBJECTS IN THE PRESENCE OF EXTERNAL ELECTROMAGNETIC FIELD 01.03.01- ASTRONOMY DISSERTATION OF THE DOCTOR OF PHILOSOFY (PhD) ON PHYSICAL AND MATHEMATICAL SCIENCES Supervisor: Ahmedov Bobomurat Juraevich doctor of sciences in physics and mathematics, professor Tashkent- 2018 1 Contents INTRODUCTION ……………………………………………………………… 4 CHAPTER I. ASTROPHYSICAL AND OBSERVATIONAL PROPERTIES OF BLACK HOLES ……………………………………. 14 §1.1 Introduction .................................................................................................. 14 §1.2 Supermassive black hole candidates ….…. ................................................... 18 §1.3 Stellar mass black hole candidates .…………………………………….…...21 §1.4 Conclusion …………………………………………………………………..23 CHAPTER II. THE MOTION OF PARTICLES IN THE BOUND NON- GEODESIC ORBITS AROUND COMPACT GRAVITATING OBJECTS IMMERSED IN AN EXTERNAL MAGNETIC FIELD … 25 §2.1 Introduction ..................................................................................................... 25 §2.2 Influence of magnetic field on isofrequency orbits around Schwarzschild black hole .......................................................................................................................... 28 § 2.2.1 The non-geodesic equations of motion ............................................... 28 §2.2.2 Influence
    [Show full text]
  • Introduction to Black Hole Astrophysics, 2010 Gustavo E
    Lecture Notes Introduction to Black Hole Astrophysics, 2010 Gustavo E. Romero Introduction to black hole astrophysics Gustavo E. Romero Instituto Argentino de Radioastronomía, C.C. 5, Villa Elisa (1894), and Facultad de Cs. Astronómicas y Geofísicas, UNLP, Paseo del Bosque S/N, (1900) La Plata, Argentina, [email protected] Es cosa averiguada que no se sabe nada, y que todos son ignorantes; y aun esto no se sabe de cierto, que, a saberse, ya se supiera algo: sospéchase. Quevedo Abstract. Black holes are perhaps the most strange and fascinating objects in the universe. Our understanding of space and time is pushed to its limits by the extreme conditions found in these objects. They can be used as natural laboratories to test the behavior of matter in very strong gravitational fields. Black holes seem to play a key role in the universe, powering a wide variety of phenomena, from X-ray binaries to active galactic nuclei. In these lecture notes the basics of black hole physics and astrophysics are reviewed. 1. Introduction Strictly speaking, black holes do not exist. Moreover, holes, of any kind, do not exist. You can talk about holes of course. For instance you can say: “there is a hole in the wall”. You can give many details of the hole: it is big, it is round shaped, light comes in through it. Even, perhaps, the hole could be such that you can go through to the outside. But I am sure that you do not think that there is a thing made out of nothingness in the wall.
    [Show full text]
  • Magnetic Penrose Process and Blanford-Zanejk Mechanism: A
    Magnetic Penrose Process and Blanford-Zanejk mechanism: A clarification Naresh Dadhich Centre for Theoretical Physics, Jamia Millia Islamia, New Delhi 110 025 & IUCAA, Post Bag 4, Ganeshkhind, Pune 411 007, India [email protected] PACS numbers :04.20.-q, 04.70-s, 04.70.Dy, 95.30.Sf Abstract The Penrose process (PP) is an ingenious mechanism of extracting rotational energy from a rotating black hole, however it was soon realized that it was not very efficient for its astrophysical applications for powering the central engine of quasars and AGNs. The situation however changed dramatically in the presence of magnetic field produced by the accretion disk surrounding the hole in the equatorial plane. In 1985, Wagh, Dhurandhar and Dadhich [1] had for the first time considered the magnetic Penrose process (MPP) in which the magnetic field could now provide the energy required for a fragment to ride on negative energy orbit thereby overcoming the stringent velocity constraint of the original PP. Thus MPP turned very efficient and so much so that efficiency could now even exceed 100 percent. They had in principle established revival of PP for astrophysical applications in powering the high energy sources. MPP is however similar to the earlier discovered and well known Blandford-Znajeck (BZ) mechanism in which the rotational energy of the hole is extracted out through a purely electromagnetic process. Though both the processes use magnetic field as a device to extract rotational energy from the hole, yet their kernel is quite arXiv:1210.1041v1 [astro-ph.HE] 3 Oct 2012 different in spirit.
    [Show full text]
  • The Symmetry of the Interior and Exterior of Schwarzschild and Reissner–Nordstrom Black Holes—Sphere Vs
    S S symmetry Article The Symmetry of the Interior and Exterior of Schwarzschild and Reissner–Nordstrom Black Holes—Sphere vs. Cylinder Andy T. Augousti 1,* , Andrzej Radosz 2, Pawel Gusin 2 and Aleksander Kaczmarek 2 1 Faculty of Science, Engineering and Computing, Kingston University London Roehampton Vale, London SW15 3DW, UK 2 Faculty of Basic Problems of Technology (Wroclaw), Wroclaw University of Science and Technology, 50-370 Wroclaw, Poland; [email protected] (A.R.); [email protected] (P.G.); [email protected] (A.K.) * Correspondence: [email protected] Received: 31 March 2020; Accepted: 6 May 2020; Published: 23 May 2020 Abstract: One can question the relationship between the symmetries of the exterior and interior of black holes with an isotropic and static exterior. This question is justified by the variety of recent findings indicating substantial or even dramatic differences in the properties of the exterior and interior of isotropic, static black holes. By invoking some of these findings related to a variety of the thought experiments with freely falling or uniformly accelerated test particles, one can establish the dynamic properties of the interior, which turn out to be equivalent to anisotropic cosmology, simultaneously expanding and contracting, albeit in different directions. In order to illustrate the comparison between the symmetry of the exterior vs. the interior, we apply conventional t, r, θ, ' coordinates to both of these ranges, although on the horizon(s) they display singular behavior. Using a simple approach based on co-moving and freely falling observers, the dynamics of the cylindrically shaped interior are explored.
    [Show full text]
  • Black Holes from a to Z
    Black Holes from A to Z Andrew Strominger Center for the Fundamental Laws of Nature, Harvard University, Cambridge, MA 02138, USA Last updated: July 15, 2015 Abstract These are the lecture notes from Professor Andrew Strominger's Physics 211r: Black Holes from A to Z course given in Spring 2015, at Harvard University. It is the first half of a survey of black holes focusing on the deep puzzles they present concerning the relations between general relativity, quantum mechanics and ther- modynamics. Topics include: causal structure, event horizons, Penrose diagrams, the Kerr geometry, the laws of black hole thermodynamics, Hawking radiation, the Bekenstein-Hawking entropy/area law, the information puzzle, microstate counting and holography. Parallel issues for cosmological and de Sitter event horizons are also discussed. These notes are prepared by Yichen Shi, Prahar Mitra, and Alex Lupsasca, with all illustrations by Prahar Mitra. 1 Contents 1 Introduction 3 2 Causal structure, event horizons and Penrose diagrams 4 2.1 Minkowski space . .4 2.2 de Sitter space . .6 2.3 Anti-de Sitter space . .9 3 Schwarzschild black holes 11 3.1 Near horizon limit . 11 3.2 Causal structure . 12 3.3 Vaidya metric . 15 4 Reissner-Nordstr¨omblack holes 18 4.1 m2 < Q2: a naked singularity . 18 4.2 m2 = Q2: the extremal case . 19 4.3 m2 > Q2: a regular black hole with two horizons . 22 5 Kerr and Kerr-Newman black holes 23 5.1 Kerr metric . 23 5.2 Singularity structure . 24 5.3 Ergosphere . 25 5.4 Near horizon extremal Kerr . 27 5.5 Penrose process .
    [Show full text]