MODIFIED GRAVITY in COSMOLOGY and FUNDAMENTAL PARTICLE PHYSICS by DE-CHANG DAI Submitted in Partial Fulfillment of the Requireme

Total Page:16

File Type:pdf, Size:1020Kb

MODIFIED GRAVITY in COSMOLOGY and FUNDAMENTAL PARTICLE PHYSICS by DE-CHANG DAI Submitted in Partial Fulfillment of the Requireme MODIFIED GRAVITY IN COSMOLOGY AND FUNDAMENTAL PARTICLE PHYSICS by DE-CHANG DAI Submitted in partial fulfillment of the requirements For the degree of Doctor of Philosophy Thesis Adviser: Dr. Glenn Starkman Department of Physics CASE WESTERN RESERVE UNUVERSITY May, 2008 CASE WESTERN RESERVE UNIVERSITY SCHOOL OF GRADUATE STUDIES We hereby approve the dissertation of De-Chang Dai candidate for the Doctor of Philosophy degree * (signed)Dr. Glenn D. Starkman (chair of the committee) Dr. Lawrence M. Krauss Dr. Harsh Mathur Dr. Colin McLarty (date) Mar 2008 *We also certify that written approval has been obtained for any proprietary material contained therein. Table of Contents 1 Introduction 1 1.1TheStandardModelofParticlePhysics................ 1 1.1.1 ParticlesandInteractionoftheStandardModel........ 2 1.2TheoryBeyondtheStandardModel................... 3 1.2.1 HierarchyProblem........................ 3 1.2.2 Supersymmetry(SUSY)..................... 4 1.2.3 Extra-Dimensions......................... 5 1.3ModifiedGravityinCosmology..................... 7 2 BlackMax: A Black-Hole Generator for the LHC 9 2.1Introduction................................ 9 2.2Black-holeproduction.......................... 13 2.2.1 Black-HoleFormationinBlackMax............... 24 2.3Gray-bodyFactors............................ 26 2.4Black-HoleEvolution .......................... 28 2.4.1 Electric and Color Charge Suppression ............. 31 2.4.2 MovementoftheBlack-HoleduringEvaporation........ 32 2.4.3 Rotation.............................. 34 2.5FinalBurst................................ 38 2.6 Input and Output . ............................ 39 2.7Results................................... 43 2.7.1 MassoftheInitialBlack-Holes................. 45 2.7.2 MovementofBlack-HolesintheBulk.............. 45 2.7.3 InitialBlack-HoleChargeDistribution............. 46 2.7.4 InitialBlack-HoleColorDistribution.............. 46 2.7.5 Evolution of Black-Hole Color and Charge during the Hawking RadiationPhase......................... 47 2.7.6 Numberofemittedparticles................... 57 2.7.7 EnergyDistributionsoftheEmittedParticles......... 58 2.7.8 PseudorapidityDistributionsoftheEmittedParticles..... 65 2.7.9 EmittedParticleTypes...................... 66 2.8Conclusion................................. 67 3 Birkhoff’s Theorem (BT) 72 3.1Introduction................................ 72 3.2Spacetimegeometry........................... 74 iii 3.2.1 Vacuumsolution......................... 76 3.2.2 Weaksourceonthebrane.................... 77 3.3Gravitationaleffectsofmassshells................... 80 3.3.1 Modeling............................. 80 3.3.2 Multipleshells........................... 81 3.4Conclusions................................ 84 4Conclusion 86 A Particle Emission Spectra 88 iv List of Tables A.1Literaturesourcesforparticleemissionspectra............. 93 A.2 Degrees of freedom of Standard-Model particles which are emitted from a black hole. For gravitons, the table shows 1, because the appropriate growth in the number of degrees of freedom is included explicitly in the graviton emission spectrum. ns is the number of extra dimensions in which vector and scalar fields can propagate. ............ 93 A.3 The fraction of emitted particles of different types (including final burst particles) in a variety of extra dimension scenarios. ∗Note that the ab- sence of gravitons in the case of a rotating black hole is due exclusively toourcurrentignoranceofthecorrectgray-bodyfactor........ 94 v List of Figures 1.1SomequadraticallydivergentHiggsself-energies............. 4 1.2 Split fermion model: Different fermions are constrained on different branes and gauge bosons are moving between different brances. 6 2.1 Horizon radius (in GeV−1) of a non-rotating black-hole as a function ofmassfor4-10spatialdimensions.................... 16 2.2 Hawking temperature(in GeV) of a non-rotating black-hole as a func- tionofmassfor4-10spatialdimensions................. 16 2.3 Horizon radius (in GeV−1) of a black-hole as a function of mass for differentBind=5spatialdimensions. ................. 17 2.4 Hawking temperature(in GeV) of a black-hole as a function of mass fordifferentBind=5spatialdimensions................. 18 2.5 Horizon radius (in GeV−1) of a rotating black-hole as a function of mass for different angular momentum in d=5 spatial dimensions. Angular momentum J is in units of ........................ 18 2.6 Hawking temperature(in GeV) of a rotating black-hole as a function of mass for different angular momentum in d=5 spatial dimensions. Angular momentum J is in units of ................... 19 2.7 Cross section for production of a black-hole (rotating or non-rotating) as a function of the number of spatial dimensions, for a tensionless brane,withnofermionbrane-splitting.................. 22 2.8 Cross section for production of a non-rotating black-hole as a function of the deficit angle parameter for d =5andns =2........... 22 2.9 Cross section for production of a non-rotating black-hole as a function of the number of fermion brane-splitting dimensions for d = 10. 23 2.10 Cross section for formation of a black-hole (rotating or non-rotating) as function of the minimum mass of black-hole, for a zero-tension brane, with no fermion brane-splitting. The vertical lines are the error bars. 23 2.11 Cross section for the two-body final-state scenario as a function of number of spatial dimensions where Mmin = M∗ =1TeV,Mmin = M∗ =3TeVandMmin =5TeV...................... 24 2.12Angularmomentumtiltgeometry..................... 27 vi 2.13 The emitted fermion intensity (normalized to one) as a function of the distance between the black-hole and the center of the gaussian distribu- tion of a fermionic brane. As a black-hole increases the distance from a fermionic brane due to recoil the intensity of the emitted fermions of that type falls down quickly. The radius of black-hole is set to be −1 −1 2M∗ . The width of the fermionic brane is M∗ . The plot is for the caseofoneextradimension........................ 29 2.14 Parameter.txt is the input file containing the parameters that one can change. The words in parentheses are the parameters that are used in thepaper.................................. 49 2.15 Output.txt: There are three parts to this file. The first part is a copy of parameter.txt. The second part includes information about the black-hole and the emitted particles. The first column identifies the what type of information each row is supplying – parent is information about the two incoming partons; Pbh is information on the energy and momenta of the produced black-holes; trace describes the location of the black-holes; Pem characterizes the emitted particles in the lab frame; Pemc characterizes the emitted particles in the center-of-mass frame; Elast describes the final burst. The third part of the file is the black-hole production cross-section as inferred from the events in this generatorrun. .............................. 50 2.16 Lines in the output file headed by the ID = Parent contain information abouttheinitialpartonswhichformedtheblack-hole.......... 51 2.17 Lines in the output file headed by the ID = Pbh contain the energies and momenta of the black-holes for each emission step. In case of rotating black-holes, the last column in the line is the angular momentum. 51 2.18 Lines in the output file headed by the ID = trace contain the location oftheblack-holeforeachemissionstep.................. 51 2.19 Lines in the output file headed by the ID = Pem contain the types of the emitted particles, their energies and momenta in the lab frame and thetimesoftheiremission......................... 51 2.20 Lines in the output file headed by the ID = Elast contain the types, energiesandmomentaofparticlesofthefinalburst........... 52 2.21 Mass distribution of initial black-holes (rotating and non-rotating) on atensionlessbraneforvariousnumbersofextradimension. ..... 52 2.22 Mass distribution of initial (non-rotating) black-holes on a non-zero tension brane for B =1.0, B =0.8andB =0.6............. 52 2.23 Mass distribution of initial (non-rotating) black-holes on a tensionless brane for d =10anddifferentnumbersofsplit-fermionbranes..... 53 2.24 black-hole movement in the mini-bulk due to recoil. X1, Y1 are coordi- nates in two extra dimensions. The red circle indicates the width of the quark brane. The blue circle indicates the width of the lepton brane. The black lines are black-holes traces. The size of the mini-bulk is 10 TeV−1 ×10 TeV−1. black-holes with non-zero standard model gauge charges bounce back from the wall of the mini-bulk. black-holes with zeroStandardModelgaugechargescanleavethemini-bulk...... 53 vii 2.25Electromagneticchargedistributionoftheinitialblack-holes...... 54 2.26 Initial color distribution of the created black-holes. The vertical lines areerrorbar................................ 54 2.27 Cumulative color distribution for non-rotating black-holes on a ten- sionless brane with d = 4 and no fermion brane splitting. Histogram with the black squares (open circles) is with (without) color suppression. 54 2.28 Number of particles emitted by a non-rotating black-hole on a tension- less brane prior to the “final burst” as function of number of extra dimension. Here ns = 0. The error bars denote one standard deviation range.................................... 55 2.29 Number of particles emitted by a non-rotating black-hole in the split- fermion model prior to the “final burst” as a function of the number of brane-splitting dimensions, with d = 10. Error bars denote one standarddeviationrange........................
Recommended publications
  • Quantum Black Holes
    Quantum Black Holes Xavier Calmet Physics & Astronomy University of Sussex Standard Model of particle physics It is described by a quantum field theory. Like athletes, coupling constants run (with energy)…. fast or slow When does gravity become important? The Planck mass is the energy scale A grand unification? at which quantum Is there actually only gravitational effects one fundamental interaction? become important. Doing quantum gravity is challenging • We do not know how to do calculations in quantum gravity. • Unifying gravity and quantum mechanics is difficult. • One can however show a few features such a theory should have, most notably: there is a minimal length in nature (e.g. XC, M. Graesser and S. Hsu) which corresponds to the size of the quantum fluctuations of spacetime itself. • New tools/theories are needed: string theory, loop quantum gravity, noncommutative geometry, nonperturbative quantum gravity… maybe something completely different. Quantization of gravity is an issue in the high energy regime which is tough to probe experimentally Dimensional analysis: 19 MP ~10 GeV but we shall see that it does not need to be the case. Since we do not have data: thought experiments can give us some clues. Why gravity do we need to quantize gravity? One example: linearized gravity coupled to matter (described by a quantum field theory) is problematic: See talk of Claus Kiefer We actually do not even know at what energy scale quantum gravity becomes strong! Let me give you two examples TeV gravity extra-dimensions where MP is the effective Planck scale in 4-dim ADD brane world RS warped extra-dimension Running of Newton’s constant XC, Hsu & Reeb (2008) • Consider GR with a massive scalar field • Let me consider the renormalization of the Planck mass: Like any other coupling constant: Newton’s constant runs! Theoretical physics can lead to anything… even business ideas! A large hidden sector! • Gravity can be strong at 1 TeV if Newton’s constant runs fast somewhere between eV range and 1 TeV.
    [Show full text]
  • HOMOGENEOUS EINSTEIN METRICS on SU(N) MANIFOLDS, HOOP CONJECTURE for BLACK RINGS, and ERGOREGIONS in MAGNETISED BLACK HOLE SPACE
    HOMOGENEOUS EINSTEIN METRICS ON SU(n) MANIFOLDS, HOOP CONJECTURE FOR BLACK RINGS, AND ERGOREGIONS IN MAGNETISED BLACK HOLE SPACETIMES A Dissertation by ABID HASAN MUJTABA Submitted to the Office of Graduate Studies of Texas A&M University in partial fulfillment of the requirements for the degree of DOCTOR OF PHILOSOPHY Approved by: Chair of Committee, Christopher Pope Committee Members, Bhaskar Dutta Stephen Fulling Ergin Sezgin Head of Department, George R. Welch May 2013 Major Subject: Physics Copyright 2013 Abid Hasan Mujtaba ABSTRACT This Dissertation covers three aspects of General Relativity: inequivalent Einstein metrics on Lie Group Manifolds, proving the Hoop Conjecture for Black Rings, and investigating ergoregions in magnetised black hole spacetimes. A number of analytical and numerical techniques are employed to that end. It is known that every compact simple Lie Group admits a bi-invariant homogeneous Ein- stein metric. We use two ans¨atzeto probe the existence of additional inequivalent Einstein metrics on the Lie Group SU(n). We provide an explicit construction of 2k + 1 and 2k inequivalent Einstein metrics on SU(2k) and SU(2k + 1) respectively. We prove the Hoop Conjecture for neutral and charged, singly and doubly rotating black rings. This allows one to determine whether a rotating mass distribution has an event horizon, that it is in fact a black ring. We investigate ergoregions in magnetised black hole spacetimes. We show that, in general, rotating charged black holes (Kerr-Newman) immersed in an external magnetic field have ergoregions that extend to infinity near the central axis unless we restrict the charge to q = amB and keep B below a maximal value.
    [Show full text]
  • Spacetime Geometry from Graviton Condensation: a New Perspective on Black Holes
    Spacetime Geometry from Graviton Condensation: A new Perspective on Black Holes Sophia Zielinski née Müller München 2015 Spacetime Geometry from Graviton Condensation: A new Perspective on Black Holes Sophia Zielinski née Müller Dissertation an der Fakultät für Physik der Ludwig–Maximilians–Universität München vorgelegt von Sophia Zielinski geb. Müller aus Stuttgart München, den 18. Dezember 2015 Erstgutachter: Prof. Dr. Stefan Hofmann Zweitgutachter: Prof. Dr. Georgi Dvali Tag der mündlichen Prüfung: 13. April 2016 Contents Zusammenfassung ix Abstract xi Introduction 1 Naturalness problems . .1 The hierarchy problem . .1 The strong CP problem . .2 The cosmological constant problem . .3 Problems of gravity ... .3 ... in the UV . .4 ... in the IR and in general . .5 Outline . .7 I The classical description of spacetime geometry 9 1 The problem of singularities 11 1.1 Singularities in GR vs. other gauge theories . 11 1.2 Defining spacetime singularities . 12 1.3 On the singularity theorems . 13 1.3.1 Energy conditions and the Raychaudhuri equation . 13 1.3.2 Causality conditions . 15 1.3.3 Initial and boundary conditions . 16 1.3.4 Outlining the proof of the Hawking-Penrose theorem . 16 1.3.5 Discussion on the Hawking-Penrose theorem . 17 1.4 Limitations of singularity forecasts . 17 2 Towards a quantum theoretical probing of classical black holes 19 2.1 Defining quantum mechanical singularities . 19 2.1.1 Checking for quantum mechanical singularities in an example spacetime . 21 2.2 Extending the singularity analysis to quantum field theory . 22 2.2.1 Schrödinger representation of quantum field theory . 23 2.2.2 Quantum field probes of black hole singularities .
    [Show full text]
  • Geometrical Inequalities Bounding Angular Momentum and Charges in General Relativity
    Living Rev Relativ (2018) 21:5 https://doi.org/10.1007/s41114-018-0014-7 REVIEW ARTICLE Geometrical inequalities bounding angular momentum and charges in General Relativity Sergio Dain1 · María Eugenia Gabach-Clement1 Received: 10 October 2017 / Accepted: 1 June 2018 © The Author(s) 2018 Abstract Geometrical inequalities show how certain parameters of a physical system set restrictions on other parameters. For instance, a black hole of given mass can not rotate too fast, or an ordinary object of given size can not have too much electric charge. In this article, we are interested in bounds on the angular momentum and electromagnetic charges, in terms of total mass and size. We are mainly concerned with inequalities for black holes and ordinary objects. The former are the most studied systems in this context in General Relativity, and where most results have been found. Ordinary objects, on the other hand, present numerous challenges and many basic questions concerning geometrical estimates for them are still unanswered. We present the many results in these areas. We make emphasis in identifying the mathematical conditions that lead to such estimates, both for black holes and ordinary objects. Keywords Geometrical inequalities · Black holes · Ordinary objects The important moments in life are the ones we share with others. Sergio Dain This article is dedicated to the memory of Sergio Dain and Marcus Ansorg. Sergio Dain: Deceased. B María Eugenia Gabach-Clement [email protected] 1 Facultad de Matemática, Astronomía y Física, Universidad Nacional de Córdoba, Instituto de Física Enrique Gaviola, Consejo Nacional de Investigaciones Científicas y Técnicas, Córdoba, Argentina 123 5 Page 2 of 74 S.
    [Show full text]
  • The Violation of Cosmic Censorship
    VOLUME 66, NUMBER 8 PHYSICAL REVIEW LETTERS 25 FEBRUARY 1991 Formation of Naked Singularities: The Violation of Cosmic Censorship Stuart L. Shapiro and Saul A. Teukolsky Center for Radiophysics and Space Research and Departments of Astronomy and Physics, Cornell University, Ithaca, New York 14853 (Received 7 September 1990) We use a new numerical code to evolve collisionless gas spheroids in full general relativity. In all cases the spheroids collapse to singularities. When the spheroids are su%ciently compact, the singularities are hidden inside black holes. However, when the spheroids are su%ciently large, there are no apparent hor- izons. These results lend support to the hoop conjecture and appear to demonstrate that naked singulari- ties can form in asymptotically flat spacetimes. PACS numbers: 04.20.Jb, 95.30.Sf, 97.60.Lf It is well known that general relativity admits solu- nite. For collisionless matter, prolate evolution is forced tions with singularities, and that such solutions can be to terminate at the singular spindle state. For oblate produced by the gravitational collapse of nonsingular, evolution, the matter simply passes through the pancake asymptotically flat initial data. The cosmic censorship state, but then becomes prolate and also evolves to a hypothesis' states that such singularities will always be spindle singularity. clothed by event horizons and hence can never be visible Does this Newtonian example have any relevance to from the outside (no naked singularities). If cosmic cen- general relativity? We already know that inftnite cylin- sorship holds, then there is no problem with predicting ders do collapse to singularities in general relativity, and, the future evolution outside the event horizon.
    [Show full text]
  • Quantum Black Holes at the LHC
    Quantum black holes at the LHC Xavier Calmet Physics and Astronomy University of Sussex Frameworks for Quantum Black Holes (QBHs) at 1 TeV • Large extra-dimensions • Large hidden sector (and 4 dimensions) • Common feature: gravity becomes strong at 1 TeV and QBHs could be produced at colliders TeV gravity extra-dimensions where MP is the effective Planck scale in 4-dim ADD brane world RS warped extra-dimension Running of Newton’s constant • Consider GR with a massive scalar field • Let me consider the renormalization of the Planck mass: • Can be derived using the heat kernel method (regulator preserves symmetries!) • Gravity becomes strong if: A large hidden sector! XC, Hsu & Reeb (2008) • Gravity can be strong at 1 TeV if Newton’s constant runs fast somewhere between eV range and 1 TeV. 33 • Strong gravity at µ*=1 TeV takes N=10 fields. • We assume that these new fields only interact gravitationally with the standard model. • This will reproduce a lot of the phenomenology of models with large extra-dimensions A brief review on the formation of black holes When does a black hole form? This is well understood in general relativity with symmetrical distribution of matter: But, what happens in particle collisions at extremely high energies? Small black hole formation (in collisions of particles) • In trivial situations (spherical distribution of matter), one can solve explicitly Einstein’s equations e.g. Schwarzschild metric. • In more complicated cases one can’t solve Einstein equations exactly and one needs some other criteria. • Hoop conjecture (Kip Thorne): if an amount of energy E is confined to a ball of size R, where R < E, then that region will eventually evolve into a black hole.
    [Show full text]
  • Final Report (PDF)
    Geometric Analysis and General Relativity Greg Galloway (University of Miami), Daniel Pollack (University of Washington), David Maxwell (University of Alaska Fairbanks), Richard Schoen (University of California, Irvine) July 17 – 22, 2016 1 Overview of the Field General Relativity is one of the fundamental theories of modern physics. Since its formulation by Einstein in 1915, it has been a cornerstone of our understanding of the universe. Mathematical research on the prob- lems of general relativity brings together many important areas of research in partial differential equations, differential geometry, dynamical systems, analysis and numerical analysis. The fundamental mathematical questions which arise in general relativity have stimulated the development of substantial new tools in analysis and geometry. Conversely, the introduction of modern tools from these fields have recently led to significant developments in general relativity, shedding new light on a number of deep and far reaching conjectures. The rigorous mathematical study of Einstein’s theory began just over sixty years ago, with Yvonne Choquet-Bruhat’s proof that Einstein’s theory has a well-posed Cauchy problem. This describes the dy- namic evolution of space-time from a set of admissible initial data. The Cauchy problem is the cornerstone perspective of most modern mathematical approaches to the subject and has been the setting for many of the great accomplishments in the field. Notable subsequent developments include the Singularity Theorems of Hawking and Penrose during the late 1960’s, the proof of the the positive mass theorem in the early 1980’s by Schoen and Yau (and independently by Witten, in the case of spin manifolds) and the establishment of the non-linear stability of Minkowski space-time in the early 1990’s by Christodoulou and Klainerman.
    [Show full text]
  • Gravitational Collapse and Cosmic Censorship
    Gravitational Collapse and Cosmic Censorship Robert M. Wald Enrico Fermi Institute and Department of Physics University of Chicago 5640 S. Ellis Avenue Chicago, Illinois 60637-1433 February 5, 2008 Abstract We review the status of the weak cosmic censorship conjecture, which asserts, in essence, that all singularities of gravitational collapse are hidden within black holes. Although little progress has been made toward a general proof (or disproof) of this conjecture, there has been some notable recent progress in the study of some examples and special cases related to the conjecture. These results support the view that naked singularities cannot arise generically. arXiv:gr-qc/9710068v3 6 Nov 1997 1 1 Introduction It has long been known that under a wide variety of circumstances, solutions to Einstein’s equation with physically reasonable matter must develop singu- larities [1]. In particular, if a sufficiently large amount of mass is contained in a sufficiently small region, trapped surfaces must form [2] or future light cone reconvergence should occur [3], in which case gravitational collapse to a singularity must result. One of the key outstanding issues in classical general relativity is the determination of the nature of the singularities that result from gravitational collapse. A key aspect of this issue is whether the singularities produced by gravi- tational collapse must always be hidden in a black hole—so that no “naked singularities”, visible to a distant observer, can ever occur. The conjecture that, generically, the singularities of gravitational collapse are contained in black holes is known as the weak cosmic censorship conjecture [4]. (A much more precise statement of this conjecture will be given in Sec.
    [Show full text]
  • Kip Stephen Thorne Becoming One of the Youngest Full Professors in the History of the California Institute of Technology
    IRAQI JOURNAL OF APPLIED PHYSICS Vol. 13, No. 4, October-December 2017, 9-12 Thorne rapidly excelled at academics early in life, Kip Stephen Thorne becoming one of the youngest full professors in the history of the California Institute of Technology. He received his B.S. degree from Caltech in 1962, and Ph.D. degree from Princeton University in 1965. He wrote his doctoral thesis, Geometrodynamics of Cylindrical Systems, under the supervision of relativist John Wheeler. Thorne returned to Caltech as an associate professor in 1967 and became a professor of theoretical physics in 1970, the William R. Kenan, Jr. Professor in 1981, and the Feynman Professor of Theoretical Physics in 1991. He was an adjunct professor at the University of Utah from 1971 to 1998 and Andrew D. White Professor at Large at Cornell University from 1986 to 1992. In June 2009 he resigned his Feynman Professorship (he is now the Feynman Professor of Theoretical Physics, Emeritus) to pursue a career of writing and movie making. His first film project was Interstellar, working with Christopher Nolan. Throughout the years, Thorne has served as a mentor and thesis advisor for many leading theorists who now work on observational, experimental, or astrophysical aspects of general relativity. Approximately 50 physicists have received Ph.D.s at Caltech under Thorne's personal mentorship. Thorne is known for his ability to convey the Kip Stephen Thorne (born June 1, 1940) is an excitement and significance of discoveries in American theoretical physicist and Nobel laureate, gravitation and astrophysics to both professional and known for his contributions in gravitational lay audiences.
    [Show full text]
  • Approximate Universal Relations for Neutron Stars and Quark Stars
    Approximate universal relations for neutron stars and quark stars Authors: Kent Yagi and Nicolas Yunes NOTICE: this is the author’s version of a work that was accepted for publication in Physics Reports. Changes resulting from the publishing process, such as peer review, editing, corrections, structural formatting, and other quality control mechanisms may not be reflected in this document. Changes may have been made to this work since it was submitted for publication. A definitive version was subsequently published in Physics Reports, VOL# 681, (March 2017). DOI# 10.1016/j.physrep.2017.03.002 Yagi, Kent , and Nicolas Yunes. "Approximate universal relations for neutron stars and quark stars." Physics Reports (March 2017). DOI: 10.1016/j.physrep.2017.03.002. Made available through Montana State University’s ScholarWorks scholarworks.montana.edu Approximate universal relations for neutron stars and quark stars Kent Yagi a,b,*, Nicolás Yunes b a Department of Physics, Princeton University, Princeton, NJ 08544, USA b eXtreme Gravity Institute, Department of Physics, Montana State University, Bozeman, MT 59717, USA Abstract Neutron stars and quark stars are ideal laboratories to study fundamental physics at supra nuclear densities and strong gravitational fields. Astrophysical observables, however, depend strongly on the star's internal structure, which is currently unknown due to uncertainties in the equation of state. Universal relations, however, exist among certain stellar observables that do not depend sensitively on the star's internal structure. One such set of relations is between the star's moment of inertia (I), its tidal Love number (Love) and its quadrupole moment (Q ), the so-called I–Love–Q relations.
    [Show full text]
  • Shape of Black Holes but Are Absent in the Shape of ’Newtonian’ Objects
    Gravitation, Relativistic Astrophysics and Cosmology Second Argentinian-Brazilian Meeting, 2014 G. S. Vila, F. L. Vieyro and J. Fabris, eds. Shape of black holes María Eugenia Gabach Clement FaMAF-UNC, IFEG CONICET, Córdoba, Argentina Abstract. It is well known that celestial bodies tend to be spherical due to gravity and that rotation produces deviations from this sphericity. We discuss what is known and expected about the shape of black holes’ horizons from their formation to their final, stationary state. We present some recent results showing that black hole rotation indeed manifests in the widening of their central regions, limits their global shapes and enforces their whole geometry to be close to the extreme Kerr horizon geometry at almost maximal rotation speed. The results depend only on the horizon area and angular momentum. In particular they are entirely independent of the surrounding geometry of the spacetime and of the presence of matter satisfying the strong energy condition. We also discuss the the relation of this result with the Hoop conjecture. 1. Introduction This article is inspired by and based on a recent article [Gab2013] by MEGC and Martin Reiris. We refer the reader to [Gab2013] for further discussions and technical details. The problem we wish to address is how to describe and characterize the shape of black holes. By this we mean the shape of their horizons, how we can measure it, what the restrictions on it are, if there are any, and how some physical parameters affect and determine this shape. This problem has three important roots that we would like to refer to: The first one is the connection between the shape of a black hole and the shape of arXiv:1503.01928v2 [gr-qc] 10 Mar 2015 the matter configuration that collapsed to form it.
    [Show full text]
  • Bekenstein Bounds, Penrose Inequalities, and Black Hole Formation
    PHYSICAL REVIEW D 97, 124026 (2018) Bekenstein bounds, Penrose inequalities, and black hole formation Jaroslaw S. Jaracz* and Marcus A. Khuri† Department of Mathematics, Stony Brook University, Stony Brook, New York 11794, USA (Received 14 February 2018; published 12 June 2018) A universal geometric inequality for bodies relating energy, size, angular momentum, and charge is naturally implied by Bekenstein’s entropy bounds. We establish versions of this inequality for axisymmetric bodies satisfying appropriate energy conditions, thus lending credence to the most general form of Bekenstein’s bound. Similar techniques are then used to prove a Penrose-like inequality in which the ADM energy is bounded from below in terms of horizon area, angular momentum, and charge. Lastly, new criteria for the formation of black holes is presented involving concentration of angular momentum, charge, and nonelectromagnetic matter energy. DOI: 10.1103/PhysRevD.97.124026 I. INTRODUCTION setting of asymptotically flat, maximal initial data. The inequality produced in [10] is not quite in the form of In [1], Bekenstein utilized heuristic arguments involving (1.2), and it is not clear if one implies the other. Both results black holes to derive an upper bound for the entropy of [9,10] are based on monotonicity of the Hawking mass along macroscopic bodies, in terms of the total energy and radius inverse mean curvature flow (IMCF), which is valid in the of the smallest sphere that encloses the object. This inequal- maximal case assuming the dominant energy condition holds. ity was later generalized [2–5] to include contributions from The purpose of the present article is threefold.
    [Show full text]