DOCSLIB.ORG

Exploring Black Hole Coalesce

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Exploring Black Hole Coalesce The Pennsylvania State University The Graduate School Eberly College of Science RINGING IN UNISON: EXPLORING BLACK HOLE COALESCENCE WITH QUASINORMAL MODES A Dissertation in Physics by Eloisa Bentivegna c 2008 Eloisa Bentivegna Submitted in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy May 2008 The dissertation of Eloisa Bentivegna was reviewed and approved* by the following: Deirdre Shoemaker Assistant Professor of Physics Dissertation Adviser Chair of Committee Pablo Laguna Professor of Astronomy & Astrophysics Professor of Physics Lee Samuel Finn Professor of Physics Professor of Astronomy & Astrophysics Yousry Azmy Professor of Nuclear Engineering Jayanth Banavar Professor of Physics Head of the Department of Physics *Signatures are on file in the Graduate School. ii Abstract The computational modeling of systems in the strong-gravity regime of General Relativity and the extraction of a coherent physical picture from the numerical data is a crucial step in the process of detecting and recognizing the theory’s imprint on our universe. Obtained and consolidated over the past two years, full 3D simulations of binary black hole systems in vacuum constitute one of the first successful steps in this field, based on the synergy of theoretical modeling, numerical analysis and computer science efforts. This dissertation seeks to model the merger of two coalescing black holes, employing a novel technique consisting of the propagation of a massless scalar field on the spacetime where the coalescence is taking place: the field is evolved on a set of fixed backgrounds, each provided by a spatial hypersurface generated numerically during a binary black hole merger. The scalar field scattered from the merger region exhibits quasinormal ringing once a common apparent horizon surrounds the two black holes. This occurs earlier than the onset of the perturbative regime as measured by the start of the quasinormal ringing in the gravitational waveforms, indicating that previous semianalytical evidence on the early validity of perturbative methods during a black hole merger is indeed correct. The scalar quasinormal frequencies are also used to associate a mass and a spin with each hypersurface: this measure is, within our error bars, compatible with the horizon mass and spin computed from the dynamical horizon framework. The emerging physical picture indicates that the behavior of a scalar field propagating on the spacetime of two merged (i.e., surrounded by a common apparent horizon) black holes is very close to that expected on a Kerr spacetime with mass and spin parameters equal to Mf and jf , the mass and spin of the common apparent horizon at the end of the coalescence. Some of the results discussed in this dissertation have been published as: E. Bentivegna, P. Laguna, and D. Shoemaker, The effect of gauge conditions on waveforms from binary black hole coalescence, AIP Conf. Proc., 873:9498 (2006). E. Bentivegna, D. Shoemaker, I. Hinder, and F. Herrmann, Probing the binary black hole merger regime with scalar perturbations, arXiv:0801.3478 (2008). iii Contents List of Tables vii List of Figures viii Acknowledgements xv 1 Introduction 1 1.1 The black hole concept in mathematical, numerical, astrophysical and quan- tum Relativity ................................... 3 1.2 Two-black-hole solutions ............................. 5 2 General Relativity and the three-plus-one decomposition 7 2.1 Gravitation according to General Relativity .................. 8 2.1.1 Exact solutions in vacuum: static and stationary black holes ..... 9 2.2 The dynamics of General Relativity ....................... 10 2.3 The ADM formulation .............................. 11 2.3.1 The 3 + 1 decomposition ......................... 12 2.3.2 Projections of the Riemann tensor .................... 14 2.3.3 Projections of Einstein’s equation .................... 15 2.4 Decomposition of the scalar wave equation ................... 18 iv 3 Scalar field evolution on a black hole background 19 3.1 Quasinormal ringing: damped oscillatory modes in open systems ....... 21 3.2 The scalar wave equation on a static, spherically symmetric spacetime .... 22 3.2.1 Green’s function analysis ......................... 25 3.3 The scalar wave equation on a stationary, axisymmetric spacetime ...... 28 3.3.1 Green’s function analysis ......................... 31 4 General Relativity and numerical methods 33 4.1 Scientific computing in General Relativity ................... 34 4.2 Modelling ..................................... 34 4.2.1 Evolution schemes and constraint preservation ............. 35 4.2.2 Coordinate conditions .......................... 39 4.2.3 Initial data ................................ 43 4.2.4 Boundary conditions ........................... 45 4.3 Numerical analysis ................................ 46 4.3.1 Integration of partial differential equations ............... 46 4.3.1.1 Finite differencing schemes .................. 46 4.3.1.2 Convergence to the continuum solution ............ 48 4.3.2 Function minimization .......................... 50 4.4 Computer science ................................. 52 5 Gravitational and scalar field evolution codes 55 5.1 BSSN evolution code ............................... 56 5.1.1 Scope ................................... 56 5.1.2 Structure ................................. 56 5.2 Scalar field evolution code ............................ 59 v 5.2.1 Scope ................................... 59 5.2.2 Structure ................................. 59 5.2.3 Code verification ............................. 61 5.2.3.1 Flat space tests ......................... 62 5.2.3.2 Single black hole tests ..................... 64 6 Probing the binary black bole merger regime with scalar perturbations 66 6.1 Binary black hole background .......................... 68 6.1.1 Energy and angular momentum ..................... 72 6.2 Scalar field evolution ............................... 72 6.2.1 Initial data ................................ 78 6.2.2 Frequency extraction ........................... 78 6.2.3 Mass and spin extraction ......................... 100 6.2.4 Scalar field evolution before the first common apparent horizon . 109 6.3 Error analysis ................................... 109 6.4 Discussion and conclusions ............................ 115 References 118 A Gauge conditions and physical observables 130 A.1 Zerilli waveforms ................................. 131 A.2 Error budget ................................... 131 B Extraction of quasinormal frequencies via an evolutionary strategy 134 B.1 Algorithm ..................................... 135 B.2 Application to quasinormal ringing waveforms ................. 135 vi List of Tables 6.1 The residual q and the best-fit values of ω20, α20, A20 and φ20, along with the corresponding mass and dimensionless spin estimates. ............. 107 6.2 The residual q and the best-fit values of ω40, α40, A40 and φ40, along with the corresponding mass and dimensionless spin estimates. ............. 107 6.3 The residual q and the best-fit values of ω60, α60, A60 and φ60, along with the corresponding mass and dimensionless spin estimates. ............. 108 vii List of Figures 3.1 The contour integral used to calculate G(x, y; t). The contribution from the poles of G(x, y; ω) in the lower half plane are responsible for the quasinormal mode components of the field, while the half circle as ω -if present at | |→∞ all- generates the prompt response to the initial data and the portion of the contour around the branch cut results in the late-time power-law tails (picture reproduced from [1]). ............................... 27 3.2 The spectrum of quasinormal modes for a Schwarzschild black hole, for the modes ℓ = 2 (diamonds) and ℓ = 3 (crosses). The absolute value of the imaginary part grows in a roughly linear fashion with n, so that higher and higher overtones tend to be more and more suppressed as the field evolves in time (plot reproduced from [2]). ........................ 29 4.1 Evolution of the spatial grid (here collapsed to a 2D plane) during the numer- ical evolution. At each time coordinate, the lapse and the shift are calculated to determine where each grid point is going to be positioned in the next it- eration. In binary black hole simulations, the gauge choices proposed, for instance, in [3] guarantee that the grid points remain far enough from the puncture singularities even when the puncture locations are advected through the grid. ...................................... 40 viii 4.2 Lapse function for four gauge types, on the x-y plane, for a single boosted puncture. The λ and γ values refer to the constants in equations (4.2.36) and (4.2.37), while µ = 0 and η = 4. In the case when λ = 1 and γ = 0, the collapsed-lapse region does not track the puncture location efficiently, lagging behind in the evolution and generating the stretched contour shown in the top right panel. .................................. 44 5.1 Structure and interdependencies of the BSSN evolution code used in the runs of chapter 6 .................................... 58 5.2 Structure and interdependencies of the scalar evolution code used in the runs of chapter 6 .................................... 60 5.3 Convergence factor for the plane wave. After a rapid initial transient, the value of Q settles, as expected, to 15. ...................... 62 5.4 Pointwise convergence for the plane wave, at t/λ = 0, 0.8, 1.6, 2.4, 3.2, 4.0. The difference between the two highest resolution runs is multiplied by the appropriate factor for a
Load more
Loading...
Loading...
Loading...
Loading...
Loading...

151 pages remaining, click to load more.

Recommended publications
  • Universal Thermodynamics in the Context of Dynamical Black Hole
    universe Article Universal Thermodynamics in the Context of Dynamical Black Hole Sudipto Bhattacharjee and Subenoy Chakraborty * Department of Mathematics, Jadavpur University, Kolkata 700032, West Bengal, India; slg00sudipto@gmail.com * Correspondence: schakraborty.math@gmail.com Received: 27 April 2018; Accepted: 22 June 2018; Published: 1 July 2018 Abstract: The present work is a brief review of the development of dynamical black holes from the geometric point view. Furthermore, in this context, universal thermodynamics in the FLRW model has been analyzed using the notion of the Kodama vector. Finally, some general conclusions have been drawn. Keywords: dynamical black hole; trapped surfaces; universal thermodynamics; unified first law 1. Introduction A black hole is a region of space-time from which all future directed null geodesics fail to reach the future null infinity I+. More specifically, the black hole region B of the space-time manifold M is the set of all events P that do not belong to the causal past of future null infinity, i.e., B = M − J−(I+). (1) Here, J−(I+) denotes the causal past of I+, i.e., it is the set of all points that causally precede I+. The boundary of the black hole region is termed as the event horizon (H), H = ¶B = ¶(J−(I+)). (2) A cross-section of the horizon is a 2D surface H(S) obtained by intersecting the event horizon with a space-like hypersurface S. As event the horizon is a causal boundary, it must be a null hypersurface generated by null geodesics that have no future end points. In the black hole region, there are trapped surfaces that are closed 2-surfaces (S) such that both ingoing and outgoing congruences of null geodesics are orthogonal to S, and the expansion scalar is negative everywhere on S.
    [Show full text]
  • The First Law for Slowly Evolving Horizons
    PHYSICAL REVIEW LETTERS week ending VOLUME 92, NUMBER 1 9JANUARY2004 The First Law for Slowly Evolving Horizons Ivan Booth* Department of Mathematics and Statistics, Memorial University of Newfoundland, St. John’s, Newfoundland and Labrador, Canada A1C 5S7 Stephen Fairhurst† Theoretical Physics Institute, Department of Physics, University of Alberta, Edmonton, Alberta, Canada T6G 2J1 (Received 5 August 2003; published 6 January 2004) We study the mechanics of Hayward’s trapping horizons, taking isolated horizons as equilibrium states. Zeroth and second laws of dynamic horizon mechanics come from the isolated and trapping horizon formalisms, respectively. We derive a dynamical first law by introducing a new perturbative formulation for dynamic horizons in which ‘‘slowly evolving’’ trapping horizons may be viewed as perturbatively nonisolated. DOI: 10.1103/PhysRevLett.92.011102 PACS numbers: 04.70.Bw, 04.25.Dm, 04.25.Nx The laws of black hole mechanics are one of the most Hv, with future-directed null normals ‘ and n. The ex- remarkable results to emerge from classical general rela- pansion ‘ of the null normal ‘ vanishes. Further, both tivity. Recently, they have been generalized to locally the expansion n of n and L n ‘ are negative. defined isolated horizons [1]. However, since no matter This definition captures the local conditions by which or radiation can cross an isolated horizon, the first and we would hope to distinguish a black hole. Specifically, second laws cannot be treated in full generality. Instead, the expansion of the outgoing light rays is zero on the the first law arises as a relation on the phase space of horizon, positive outside, and negative inside.
    [Show full text]
  • Arxiv:2006.03939V1 [Gr-Qc] 6 Jun 2020 in flat Spacetime Regions
    Horizons in a binary black hole merger I: Geometry and area increase Daniel Pook-Kolb,1, 2 Ofek Birnholtz,3 Jos´eLuis Jaramillo,4 Badri Krishnan,1, 2 and Erik Schnetter5, 6, 7 1Max-Planck-Institut f¨urGravitationsphysik (Albert Einstein Institute), Callinstr. 38, 30167 Hannover, Germany 2Leibniz Universit¨atHannover, 30167 Hannover, Germany 3Department of Physics, Bar-Ilan University, Ramat-Gan 5290002, Israel 4Institut de Math´ematiquesde Bourgogne (IMB), UMR 5584, CNRS, Universit´ede Bourgogne Franche-Comt´e,F-21000 Dijon, France 5Perimeter Institute for Theoretical Physics, Waterloo, ON N2L 2Y5, Canada 6Physics & Astronomy Department, University of Waterloo, Waterloo, ON N2L 3G1, Canada 7Center for Computation & Technology, Louisiana State University, Baton Rouge, LA 70803, USA Recent advances in numerical relativity have revealed how marginally trapped surfaces behave when black holes merge. It is now known that interesting topological features emerge during the merger, and marginally trapped surfaces can have self-intersections. This paper presents the most detailed study yet of the physical and geometric aspects of this scenario. For the case of a head-on collision of non-spinning black holes, we study in detail the world tube formed by the evolution of marginally trapped surfaces. In the first of this two-part study, we focus on geometrical properties of the dynamical horizons, i.e. the world tube traced out by the time evolution of marginally outer trapped surfaces. We show that even the simple case of a head-on collision of non-spinning black holes contains a rich variety of geometric and topological properties and is generally more complex than considered previously in the literature.
    [Show full text]
  • Arxiv:Gr-Qc/0511017 V3 20 Jan 2006 Xml,I a Ugse Yerly[] Hta MTS an That [6], Eardley by for Suggested Spacetimes
    AEI-2005-161 Non-symmetric trapped surfaces in the Schwarzschild and Vaidya spacetimes Erik Schnetter1,2, ∗ and Badri Krishnan2,† 1Center for Computation and Technology, 302 Johnston Hall, Louisiana State University, Baton Rouge, LA 70803, USA 2Max-Planck-Institut für Gravitationsphysik, Albert-Einstein-Institut, Am Mühlenberg 1, D-14476 Golm, Germany (Dated: January 2, 2006) Marginally trapped surfaces (MTSs) are commonly used in numerical relativity to locate black holes. For dynamical black holes, it is not known generally if this procedure is sufficiently reliable. Even for Schwarzschild black holes, Wald and Iyer constructed foliations which come arbitrarily close to the singularity but do not contain any MTSs. In this paper, we review the Wald–Iyer construction, discuss some implications for numerical relativity, and generalize to the well known Vaidya space- time describing spherically symmetric collapse of null dust. In the Vaidya spacetime, we numerically locate non-spherically symmetric trapped surfaces which extend outside the standard spherically symmetric trapping horizon. This shows that MTSs are common in this spacetime and that the event horizon is the most likely candidate for the boundary of the trapped region. PACS numbers: 04.25.Dm, 04.70.Bw Introduction: In stationary black hole spacetimes, there can be locally perturbed in an arbitrary spacelike direc- is a strong correspondence between marginally trapped tion to yield a 1-parameter family of MTSs. A precise surfaces (MTSs) and event horizons (EHs) because cross formulation of this idea and its proof follows from re- sections of stationary EHs are MTSs. MTSs also feature cent results of Andersson et al. [7].
    [Show full text]
  • Black Holes and Black Hole Thermodynamics Without Event Horizons
    General Relativity and Gravitation (2011) DOI 10.1007/s10714-008-0739-9 RESEARCHARTICLE Alex B. Nielsen Black holes and black hole thermodynamics without event horizons Received: 18 June 2008 / Accepted: 22 November 2008 c Springer Science+Business Media, LLC 2009 Abstract We investigate whether black holes can be defined without using event horizons. In particular we focus on the thermodynamic properties of event hori- zons and the alternative, locally defined horizons. We discuss the assumptions and limitations of the proofs of the zeroth, first and second laws of black hole mechan- ics for both event horizons and trapping horizons. This leads to the possibility that black holes may be more usefully defined in terms of trapping horizons. We also review how Hawking radiation may be seen to arise from trapping horizons and discuss which horizon area should be associated with the gravitational entropy. Keywords Black holes, Black hole thermodynamics, Hawking radiation, Trapping horizons Contents 1 Introduction . 2 2 Event horizons . 4 3 Local horizons . 8 4 Thermodynamics of black holes . 14 5 Area increase law . 17 6 Gravitational entropy . 19 7 The zeroth law . 22 8 The first law . 25 9 Hawking radiation for trapping horizons . 34 10 Fluid flow analogies . 36 11 Uniqueness . 37 12 Conclusion . 39 A. B. Nielsen Center for Theoretical Physics and School of Physics College of Natural Sciences, Seoul National University Seoul 151-742, Korea eujin@phya.snu.ac.kr 2 A. B. Nielsen 1 Introduction Black holes play a central role in physics. In astrophysics, they represent the end point of stellar collapse for sufficiently large stars.
    [Show full text]
  • Dynamical Black Holes and Expanding Plasmas
    DCPT-09/13 NSF-KITP-09-20 Dynamical black holes & expanding plasmas Pau Figuerasa,∗ Veronika E. Hubenya;b,y Mukund Rangamania;b,z and Simon F. Rossax aCentre for Particle Theory & Department of Mathematical Sciences, Science Laboratories, South Road, Durham DH1 3LE, United Kingdom. b Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93015, USA. November 13, 2018 Abstract We analyse the global structure of time-dependent geometries dual to expanding plasmas, considering two examples: the boost invariant Bjorken flow, and the con- formal soliton flow. While the geometry dual to the Bjorken flow is constructed in a perturbation expansion at late proper time, the conformal soliton flow has an exact dual (which corresponds to a Poincar´epatch of Schwarzschild-AdS). In particular, we discuss the position and area of event and apparent horizons in the two geometries. The conformal soliton geometry offers a sharp distinction between event and apparent horizon; whereas the area of the event horizon diverges, that of the apparent horizon stays finite and constant. This suggests that the entropy of the corresponding CFT state is related to the apparent horizon rather than the event horizon. arXiv:0902.4696v2 [hep-th] 23 Mar 2009 ∗pau.figueras@durham.ac.uk yveronika.hubeny@durham.ac.uk zmukund.rangamani@durham.ac.uk xS.F.Ross@durham.ac.uk Contents 1 Introduction1 2 Boost invariant flow5 2.1 Bjorken hydrodynamics . .5 2.2 The gravity dual to Bjorken flow . .6 2.3 Apparent horizon for the BF spacetime . .9 2.4 Event horizon for the BF spacetime . 10 3 The Conformal Soliton flow 13 3.1 The BTZ spacetime as a conformal soliton .
    [Show full text]
  • Arxiv:2106.02595V2 [Gr-Qc] 26 Jun 2021 Ments – Fully Characterize the Horizon Geometry
    Tidal deformation of dynamical horizons in binary black hole mergers Vaishak Prasad,1 Anshu Gupta,1 Sukanta Bose,1, 2 and Badri Krishnan3, 4, 5 1Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune 411 007, India 2Department of Physics and Astronomy, Washington State University, 1245 Webster, Pullman, WA 99164-2814, U.S.A 3Max-Planck-Institut f¨urGravitationsphysik (Albert Einstein Institute), Callinstr. 38, 30167 Hannover, Germany 4Leibniz Universit¨atHannover, Welfengarten 1-A, D-30167 Hannover, Germany 5Institute for Mathematics, Astrophysics and Particle Physics, Radboud University, Heyendaalseweg 135, 6525 AJ Nijmegen, The Netherlands (Dated: June 29, 2021) An important physical phenomenon that manifests itself during the inspiral of two orbiting com- pact objects is the tidal deformation of each under the gravitational influence of its companion. In the case of binary neutron star mergers, this tidal deformation and the associated Love numbers have been used to probe properties of dense matter and the nuclear equation of state. Non-spinning black holes on the other hand have a vanishing (field) tidal Love number in General Relativity. This pertains to the deformation of the asymptotic gravitational field. In certain cases, especially in the late stages of the inspiral phase when the black holes get close to each other, the source multipole moments might be more relevant in probing their properties and the No-Hair theorem; contrast- ingly, these Love numbers do not vanish. In this paper, we track the source multipole moments in simulations of several binary black hole mergers and calculate these Love numbers. We present evidence that, at least for modest mass ratios, the behavior of the source multipole moments is universal.
    [Show full text]
  • Dynamical Horizons and Super-Translation Transitions of the Horizon
    USTC-ICTS/PCFT-20-31 Dynamical horizons and Super-Translation transitions of the horizon Ayan Chatterjee∗ Department of Physics and Astronomical Science, Central University of Himachal Pradesh, Dharamshala -176215, India. Avirup Ghoshy Interdisciplinary Center for Theoretical Study, University of Science and Technology of China, and Peng Huanwu Center for Fundamental Theory, Hefei, Anhui 230026, China A condition is defined which determines if a supertranslation is induced in the course of a general evolution from one isolated horizon phase to another via a dy- namical horizon. This condition fixes preferred slices on an isolated horizon and is preserved along an Isolated Horizon. If it is not preserved, in the course of a general evolution, then a supertranslation will be said to have been induced. A sim- ple example of spherically symmetric dynamical horizons is studied to illustrate the conditions for inducing supertranslations. I. INTRODUCTION The notion of supertranslation and superrotation symmetries at the past and future null infinity have gained importance with the realisation that they reproduce Weinberg's soft graviton theorem [1{5] These fascinating results along with the proposal for resolving the information loss paradox by utilising the notion of supertranslations and interpreting them arXiv:2009.09270v1 [gr-qc] 19 Sep 2020 as additional hair for black holes [6,7], led to a renewed interest in the study of near horizon symmetries [8{16]. The main aim has been to explore the near horizon structure of black hole horizons and seek symmetries which are similar in spirit to the asymptotic symmetries at null infinity. While it is far from clear whether these indeed resolve the paradox it is also important that we explore these from a wider perspective.
    [Show full text]
  • For Publisher's Use HOW BLACK HOLES GROW∗ ABHAY
    For Publisher's use HOW BLACK HOLES GROW∗ ABHAY ASHTEKAR Center for Gravitational Physics and Geometry Physics Department, Penn State University, University Park, PA 16802, USA; Kavli Institute of Theoretical Physics University of California, Santa Barbara, CA 93106-4030, USA A summary of on how black holes grow in full, non-linear general relativity is presented. Specifically, a notion of dynamical horizons is introduced and expressions of fluxes of energy and angular momentum carried by gravitational waves across these horizons are obtained. Fluxes are local and the energy flux is positive. Change in the horizon area is related to these fluxes. The flux formulae also give rise to balance laws analogous to the ones obtained by Bondi and Sachs at null infinity and provide generalizations of the first and second laws of black hole mechanics. 1 Introduction Black holes are perhaps the most fascinating manifestations of the curvature of space and time predicted by general relativity. Properties of isolated black holes in equilibrium have been well-understood for quite some time. However, in Nature, black holes are rarely in equilibrium. They grow by swallowing stars and galactic debris as well as electromagnetic and gravitational radiation. For such dynamical black holes, the only known major result in exact general relativity has been a celebrated area theorem, proved by Stephen Hawking in the early seventies: if matter satisfies the dominant energy condition, the area of the black hole event horizon can never decrease. This theorem has been extremely influential because of its similarity with the second law of thermodynamics. However, it is a `qualitative' result; it does not provide an explicit formula for the amount by which the area increases in any given physical situation.
    [Show full text]
  • Deformation of Codimension-2 Surfaces and Horizon Thermodynamics
    Horizons Deformation of submanifolds Quasi-local horizons Horizon thermodynamics Cosmology Conclusion Deformation of Codimension-2 Surfaces and Horizon Thermodynamics ù|² (Li-Ming Cao) FCOÆÔnX 2011c7 Horizons Deformation of submanifolds Quasi-local horizons Horizon thermodynamics Cosmology Conclusion ÌSN Horizons Deformation of submanifolds Submanifold theory The definition of deformation Deformation equation The case with an arbitrary codimension Example: Codimension-1 Example: Codimension-2 Quasi-local horizons Horizon thermodynamics The method with quasi-local energy The method without quasi-local energy Slowly evolving horizon Cosmology Conclusion Horizons Deformation of submanifolds Quasi-local horizons Horizon thermodynamics Cosmology Conclusion Event horizon Black hole region, B, of an asymptotically flat spacetime is defined as B = M − I−(I+) . • The event horizon H is defined as the boundary of B. So H is the boundary of the past of I+. • Other spacetimes with different asymptotical behavior. For example, asymptotically AdS spacetime • We do not know how to define the event horizon if we can not get the information of the future infinity of a spacetime. Horizons Deformation of submanifolds Quasi-local horizons Horizon thermodynamics Cosmology Conclusion The definition of event Horizon Figure: The definition of event horizon Horizons Deformation of submanifolds Quasi-local horizons Horizon thermodynamics Cosmology Conclusion Fail to describe strong gravity property A special Vaidya spacetime (Ashtekar and Krishnan 2004): 2 2 2 g = −f(v, r)dv + 2dvdr + r dΩ2 , (1) with 1 v < 0; f(v, r) = 1 − m(v)/r 0 ≤ v < 0 ≤ v0, m˙ > 0; 1 − m0/r v > v0, m0 is a constant. Figure: Event horizon can exist in flat region of spacetime Horizons Deformation of submanifolds Quasi-local horizons Horizon thermodynamics Cosmology Conclusion Killing horizon A null hypersurface K is a Killing horizon of a Killing vector field ξ if, on K, ξ is normal to K.
    [Show full text]
  • Horizons As Boundary Conditions in Spherical Symmetry
    Horizons as boundary conditions in spherical symmetry Sharmila Gunasekaran∗ and Ivan Boothy Department of Mathematics and Statistics Memorial University of Newfoundland St. John's, Newfoundland and Labrador, A1C 5S7, Canada (Dated: March 31, 2021) We initiate the development of a horizon-based initial (or rather final) value formalism to describe the geometry and physics of the near-horizon spacetime: data specified on the horizon and a future ingoing null boundary determine the near-horizon geometry. In this initial paper we restrict our attention to spherically symmetric spacetimes made dynamic by matter fields. We illustrate the for- malism by considering a black hole interacting with a) inward-falling, null matter (with no outward flux) and b) a massless scalar field. The inward-falling case can be exactly solved from horizon data. For the more involved case of the scalar field we analytically investigate the near slowly evolving horizon regime and propose a numerical integration for the general case. I. INTRODUCTION This paper begins an investigation into what horizon dynamics can tell us about external black hole physics. At first thought this might seem obvious: if one watches a numerical simulation of a black hole merger and sees a post-merger horizon ringdown (see for example [1]) then it is natural to think of that oscillation as a source of emitted gravitational waves. However this cannot be the case. Neither event nor apparent horizons can actually (a)Future and past domains of dependence for send signals to infinity: apparent horizons lie inside event H : standard (3+1) IVP horizons which in turn are the boundary for signals that dynamic can reach infinity[2].
    [Show full text]
  • Horizon Energy and Angular Momentum from a Hamiltonian
    Horizon energy and angular momentum from a Hamiltonian perspective Ivan Booth1,2∗ and Stephen Fairhurst1,3† 1. Theoretical Physics Institute, Department of Physics, University of Alberta, Edmonton, Alberta, T6G 2J1, Canada 2. Department of Mathematics and Statistics, Memorial University of Newfoundland, St. John’s, Newfoundland and Labrador, A1C 5S7, Canada 3. Department of Physics, University of Wisconsin – Milwaukee, P.O. Box 413, Wisconsin, 53201, U.S.A. Abstract Classical black holes and event horizons are highly non-local objects, defined in terms of the causal past of future null infinity. Alternative, (quasi)local definitions are often used in mathemat- ical, quantum, and numerical relativity. These include apparent, trapping, isolated, and dynamical horizons, all of which are closely associated to two-surfaces of zero outward null expansion. In this paper we show that three-surfaces which can be foliated with such two-surfaces are suitable bound- aries in both a quasilocal action and a phase space formulation of general relativity. The resulting formalism provides expressions for the quasilocal energy and angular momentum associated with the horizon. The values of the energy and angular momentum are in agreement with those derived from the isolated and dynamical horizon frameworks. arXiv:gr-qc/0505049v2 20 Oct 2005 ∗Electronic address: ibooth@math.mun.ca †Electronic address: sfairhur@gravity.phys.uwm.edu 1 I. INTRODUCTION The basic ideas of black hole physics are well-known. These foundations, including the singularity, uniqueness, and area increase theorems [1], the laws of black hole mechanics [2], and the identity between those laws and the laws of thermodynamics [3, 4], have been understood for several decades.
    [Show full text]