GEM: the User Manual Understanding Spacetime Splittings and Their Relationships1

Total Page:16

File Type:pdf, Size:1020Kb

GEM: the User Manual Understanding Spacetime Splittings and Their Relationships1 GEM: the User Manual Understanding Spacetime Splittings and Their Relationships1 Robert T. Jantzen Paolo Carini and Donato Bini June 15, 2021 1This manuscript is preliminary and incomplete and is made available with the understanding that it will not be cited or reproduced without the permission of the authors. Abstract A comprehensive review of the various approaches to splitting spacetime into space-plus-time, establishing a common framework based on test observer families which is best referred to as gravitoelectromagnetism. Contents Preface vi 1 Introduction 1 1.1 Motivation: Local Special Relativity plus Rotating Coordinates . 1 1.2 Why bother? . 4 1.3 Starting vocabulary . 6 1.4 Historical background . 8 1.5 Orthogonalization in the Lorentzian plane . 11 1.6 Notation and conventions . 14 2 The congruence point of view and the measurement process 17 2.1 Algebra . 17 2.1.1 Observer orthogonal decomposition . 18 2.1.2 Observer-adapted frames . 21 2.1.3 Relative kinematics: algebra . 23 2.1.4 Splitting along parametrized spacetime curves and test particle worldlines . 26 2.1.5 Addition of velocities and the aberration map . 28 2.2 Derivatives . 29 2.2.1 Natural derivatives . 29 2.2.2 Covariant derivatives . 30 2.2.3 Kinematical quantities . 31 2.2.4 Splitting the exterior derivative . 33 2.2.5 Splitting the differential form divergence operator . 35 2.2.6 Spatial vector analysis . 35 2.2.7 Ordinary and Co-rotating Fermi-Walker derivatives . 37 2.2.8 Relation between Lie and Fermi-Walker temporal derivatives . 39 2.2.9 Total spatial covariant derivatives . 43 2.2.10 Splitting the total covariant derivative . 46 2.3 Observer-adapted frame derivatives . 47 2.3.1 Natural frame derivatives . 47 2.3.2 Splitting the connection coefficients . 48 2.3.3 Observer-adapted connection components . 49 2.3.4 Splitting covariant derivatives . 50 2.3.5 Observer-adapted components of total spatial covariant derivatives . 52 2.4 Relative kinematics: applications . 55 2.4.1 Splitting the acceleration equation . 55 2.4.2 Analogy with electromagnetism: gravitoelectromagnetism . 57 2.4.3 Maxwell-like equations . 58 2.4.4 Splitting the spin transport equation . 60 2.4.5 Relative Fermi-Walker transport and gyro precession . 62 2.4.6 The Schiff Precession Formula . 65 2.4.7 The relative angular velocity as a boost derivative . 67 i 2.4.8 Relative kinematics: transformation of spatial gravitational fields . 68 2.5 Spatial curvature and torsion . 70 2.5.1 Definitions . 70 2.5.2 Algebraic symmetries . 70 2.5.3 Symmetry-obeying spatial curvature . 72 2.5.4 Spatial Ricci tensors and scalar curvatures . 73 2.5.5 Pair interchange symmetry . 73 2.5.6 Spatial covariant exterior derivative . 74 2.6 The symmetrized curl operator for symmetric spatial 2-tensors . 76 2.7 Splitting spacetime curvature . 77 2.7.1 Splitting definitions . 77 2.7.2 Spacetime duality and curvature . 78 2.7.3 Evaluation of splitting fields . 79 2.7.4 Maxwell-like equations . 81 2.8 Mixed commutation formulas . 82 2.8.1 Splitting the Ricci identities . 82 2.8.2 Commuting $(u)u and r(u) ................................ 83 2.9 Splitting the Bianchi identities of the second kind . 84 2.9.1 Spacetime identities . 84 2.9.2 Spatial identities . 87 2.10 \Time without space defines space without time" and vice versa . 88 3 The slicing and threading points of view 89 3.1 Introduction . 89 3.2 Algebra . 89 3.2.1 The nonlinear reference frame . 89 3.2.2 Measurement and the lapse function . 90 3.2.3 The Shift . 92 3.2.4 Computational frames and the reference decomposition . 93 3.2.5 Decomposing the metric . 94 3.2.6 Relationship between the reference and observer decompositions . 96 3.2.7 The slicing, threading and reference representations . 97 3.2.8 Transformation between slicing and threading points of view . 98 3.2.9 So far: . 99 3.3 Derivatives . 101 3.3.1 Evolution . 101 3.3.2 Natural time derivatives . 101 3.3.3 Natural spatial derivatives . 102 3.3.4 Gauge transformations of the nonlinear reference frame . 103 3.3.5 Observer-adapted frame structure functions and kinematical quantities . 105 3.3.6 Spatial covariant derivative . 106 3.3.7 Spatial vector analysis . 107 3.3.8 Partially-observer-adapted frames: connection components . 108 3.3.9 Total spatial covariant derivatives . 109 3.3.10 Spatial gravitational forces . 111 3.3.11 Second-order acceleration equation . 112 3.3.12 The spin transport equation . 113 3.3.13 Transformation of spatial gravitational fields . 114 3.4 Spatial curvature . 115 3.5 Initial value problem? . 115 3.5.1 Hypersurface and slicing points of view . 115 3.5.2 Thin sandwich problem . 116 3.5.3 Congruence and threading points of view . 116 ii 3.5.4 Perfect fluids . 117 4 Maxwell's equations 118 4.1 Introduction . 118 4.2 Splitting the electromagnetic field . 118 4.2.1 Congruence point of view . 118 4.2.2 Slicing and threading points of view . 119 4.2.3 Observer Boost . 120 4.2.4 Reference representation (Landau-Lifshitz-Hanni) . 120 4.3 Splitting the 4-current . 122 4.4 Splitting Maxwell's equations . ..
Recommended publications
  • Aspects of Black Hole Physics
    Aspects of Black Hole Physics Andreas Vigand Pedersen The Niels Bohr Institute Academic Advisor: Niels Obers e-mail: [email protected] Abstract: This project examines some of the exact solutions to Einstein’s theory, the theory of linearized gravity, the Komar definition of mass and angular momentum in general relativity and some aspects of (four dimen- sional) black hole physics. The project assumes familiarity with the basics of general relativity and differential geometry, but is otherwise intended to be self contained. The project was written as a ”self-study project” under the supervision of Niels Obers in the summer of 2008. Contents Contents ..................................... 1 Contents ..................................... 1 Preface and acknowledgement ......................... 2 Units, conventions and notation ........................ 3 1 Stationary solutions to Einstein’s equation ............ 4 1.1 Introduction .............................. 4 1.2 The Schwarzschild solution ...................... 6 1.3 The Reissner-Nordstr¨om solution .................. 18 1.4 The Kerr solution ........................... 24 1.5 The Kerr-Newman solution ..................... 28 2 Mass, charge and angular momentum (stationary spacetimes) 30 2.1 Introduction .............................. 30 2.2 Linearized Gravity .......................... 30 2.3 The weak field approximation .................... 35 2.3.1 The effect of a mass distribution on spacetime ....... 37 2.3.2 The effect of a charged mass distribution on spacetime .. 39 2.3.3 The effect of a rotating mass distribution on spacetime .. 40 2.4 Conserved currents in general relativity ............... 43 2.4.1 Komar integrals ........................ 49 2.5 Energy conditions ........................... 53 3 Black holes ................................ 57 3.1 Introduction .............................. 57 3.2 Event horizons ............................ 57 3.2.1 The no-hair theorem and Hawking’s area theorem ....
    [Show full text]
  • The Schwarzschild Metric and Applications 1
    The Schwarzschild Metric and Applications 1 Analytic solutions of Einstein©s equations are hard to come by. It©s easier in situations that exhibit symmetries. 1916: Karl Schwarzschild sought the metric describing the static, spherically symmetric spacetime surrounding a spherically symmetric mass distribution. A static spacetime is one for which there exists a time coordinate t such that i) all the components of g are independent of t ii) the line element ds2 is invariant under the transformation t -t A spacetime that satisfies (i) but not (ii) is called stationary. An example is a rotating azimuthally symmetric mass distribution. The metric for a static spacetime has the form where xi are the spatial coordinates and dl2 is a time-independent spatial metric. Cross-terms dt dxi are missing because their presence would violate condition (ii). [Note: The Kerr metric, which describes the spacetime outside a rotating 2 axisymmetric mass distribution, contains a term ∝ dt d.] To preserve spherical symmetry, dl2 can be distorted from the flat-space metric only in the radial direction. In flat space, (1) r is the distance from the origin and (2) 4r2 is the area of a sphere. Let©s define r such that (2) remains true but (1) can be violated. Then, A(xi) A(r) in cases of spherical symmetry. The Ricci tensor for this metric is diagonal, with components SP 10.1 Primes denote differentiation with respect to r. The region outside the spherically symmetric mass distribution is empty. 3 The vacuum Einstein equations are R = 0. To find A(r) and B(r): 2.
    [Show full text]
  • The Schwarzschild Metric and Applications 1
    The Schwarzschild Metric and Applications 1 Analytic solutions of Einstein's equations are hard to come by. It's easier in situations that e hibit symmetries. 1916: Karl Schwarzschild sought the metric describing the static, spherically symmetric spacetime surrounding a spherically symmetric mass distribution. A static spacetime is one for which there exists a time coordinate t such that i' all the components of g are independent of t ii' the line element ds( is invariant under the transformation t -t A spacetime that satis+es (i) but not (ii' is called stationary. An example is a rotating azimuthally symmetric mass distribution. The metric for a static spacetime has the form where xi are the spatial coordinates and dl( is a time*independent spatial metric. -ross-terms dt dxi are missing because their presence would violate condition (ii'. 23ote: The Kerr metric, which describes the spacetime outside a rotating ( axisymmetric mass distribution, contains a term ∝ dt d.] To preser)e spherical symmetry& dl( can be distorted from the flat-space metric only in the radial direction. In 5at space, (1) r is the distance from the origin and (2) 6r( is the area of a sphere. Let's de+ne r such that (2) remains true but (1) can be violated. Then, A,xi' A,r) in cases of spherical symmetry. The Ricci tensor for this metric is diagonal, with components S/ 10.1 /rimes denote differentiation with respect to r. The region outside the spherically symmetric mass distribution is empty. 9 The vacuum Einstein equations are R = 0. To find A,r' and B,r'# (.
    [Show full text]
  • General Relativity
    GENERAL RELATIVITY IAN LIM LAST UPDATED JANUARY 25, 2019 These notes were taken for the General Relativity course taught by Malcolm Perry at the University of Cambridge as part of the Mathematical Tripos Part III in Michaelmas Term 2018. I live-TEXed them using TeXworks, and as such there may be typos; please send questions, comments, complaints, and corrections to [email protected]. Many thanks to Arun Debray for the LATEX template for these lecture notes: as of the time of writing, you can find him at https://web.ma.utexas.edu/users/a.debray/. Contents 1. Friday, October 5, 2018 1 2. Monday, October 8, 2018 4 3. Wednesday, October 10, 20186 4. Friday, October 12, 2018 10 5. Wednesday, October 17, 2018 12 6. Friday, October 19, 2018 15 7. Monday, October 22, 2018 17 8. Wednesday, October 24, 2018 22 9. Friday, October 26, 2018 26 10. Monday, October 29, 2018 28 11. Wednesday, October 31, 2018 32 12. Friday, November 2, 2018 34 13. Monday, November 5, 2018 38 14. Wednesday, November 7, 2018 40 15. Friday, November 9, 2018 44 16. Monday, November 12, 2018 48 17. Wednesday, November 14, 2018 52 18. Friday, November 16, 2018 55 19. Monday, November 19, 2018 57 20. Wednesday, November 21, 2018 62 21. Friday, November 23, 2018 64 22. Monday, November 26, 2018 67 23. Wednesday, November 28, 2018 70 Lecture 1. Friday, October 5, 2018 Unlike in previous years, this course is intended to be a stand-alone course on general relativity, building up the mathematical formalism needed to construct the full theory and explore some examples of interesting spacetime metrics.
    [Show full text]
  • 1 Electromagnetic Fields and Charges In
    Electromagnetic fields and charges in ‘3+1’ spacetime derived from symmetry in ‘3+3’ spacetime J.E.Carroll Dept. of Engineering, University of Cambridge, CB2 1PZ E-mail: [email protected] PACS 11.10.Kk Field theories in dimensions other than 4 03.50.De Classical electromagnetism, Maxwell equations 41.20Jb Electromagnetic wave propagation 14.80.Hv Magnetic monopoles 14.70.Bh Photons 11.30.Rd Chiral Symmetries Abstract: Maxwell’s classic equations with fields, potentials, positive and negative charges in ‘3+1’ spacetime are derived solely from the symmetry that is required by the Geometric Algebra of a ‘3+3’ spacetime. The observed direction of time is augmented by two additional orthogonal temporal dimensions forming a complex plane where i is the bi-vector determining this plane. Variations in the ‘transverse’ time determine a zero rest mass. Real fields and sources arise from averaging over a contour in transverse time. Positive and negative charges are linked with poles and zeros generating traditional plane waves with ‘right-handed’ E, B, with a direction of propagation k. Conjugation and space-reversal give ‘left-handed’ plane waves without any net change in the chirality of ‘3+3’ spacetime. Resonant wave-packets of left- and right- handed waves can be formed with eigen frequencies equal to the characteristic frequencies (N+½)fO that are observed for photons. 1 1. Introduction There are many and varied starting points for derivations of Maxwell’s equations. For example Kobe uses the gauge invariance of the Schrödinger equation [1] while Feynman, as reported by Dyson, starts with Newton’s classical laws along with quantum non- commutation rules of position and momentum [2].
    [Show full text]
  • Transverse Geometry and Physical Observers
    Transverse geometry and physical observers D. H. Delphenich 1 Abstract: It is proposed that the mathematical formalism that is most appropriate for the study of spatially non-integrable cosmological models is the transverse geometry of a one-dimensional foliation (congruence) defined by a physical observer. By that means, one can discuss the geometry of space, as viewed by that observer, without the necessity of introducing a complementary sub-bundle to the observer’s line bundle or a codimension-one foliation transverse to the observer’s foliation. The concept of groups of transverse isometries acting on such a spacetime and the relationship of transverse geometry to spacetime threadings (1+3 decompositions) is also discussed. MSC: 53C12, 53C50, 53C80 Keywords: transverse geometry, foliations, physical observers, 1+3 splittings of spacetime 1. Introduction. One of the most profound aspects of Einstein’s theory of relativity was the idea that physical phenomena were better modeled as taking place in a four-dimensional spacetime manifold M than by means of parameterized curves in a spatial three-manifold. However, the correspondence principle says that any new theory must duplicate the successes of the theory that it is replacing at some level of approximation. Hence, a fundamental problem of relativity theory is how to reduce the four-dimensional spacetime picture of physical phenomena back to the three-dimensional spatial picture of Newtonian gravitation and mechanics. The simplest approach is to assume that M is a product manifold of the form R×Σ, where Σ represents the spatial 3-manifold; indeed, most existing models of spacetime take this form.
    [Show full text]
  • Part 3 Black Holes
    Part 3 Black Holes Harvey Reall Part 3 Black Holes March 13, 2015 ii H.S. Reall Contents Preface vii 1 Spherical stars 1 1.1 Cold stars . .1 1.2 Spherical symmetry . .2 1.3 Time-independence . .3 1.4 Static, spherically symmetric, spacetimes . .4 1.5 Tolman-Oppenheimer-Volkoff equations . .5 1.6 Outside the star: the Schwarzschild solution . .6 1.7 The interior solution . .7 1.8 Maximum mass of a cold star . .8 2 The Schwarzschild black hole 11 2.1 Birkhoff's theorem . 11 2.2 Gravitational redshift . 12 2.3 Geodesics of the Schwarzschild solution . 13 2.4 Eddington-Finkelstein coordinates . 14 2.5 Finkelstein diagram . 17 2.6 Gravitational collapse . 18 2.7 Black hole region . 19 2.8 Detecting black holes . 21 2.9 Orbits around a black hole . 22 2.10 White holes . 24 2.11 The Kruskal extension . 25 2.12 Einstein-Rosen bridge . 28 2.13 Extendibility . 29 2.14 Singularities . 29 3 The initial value problem 33 3.1 Predictability . 33 3.2 The initial value problem in GR . 35 iii CONTENTS 3.3 Asymptotically flat initial data . 38 3.4 Strong cosmic censorship . 38 4 The singularity theorem 41 4.1 Null hypersurfaces . 41 4.2 Geodesic deviation . 43 4.3 Geodesic congruences . 44 4.4 Null geodesic congruences . 45 4.5 Expansion, rotation and shear . 46 4.6 Expansion and shear of a null hypersurface . 47 4.7 Trapped surfaces . 48 4.8 Raychaudhuri's equation . 50 4.9 Energy conditions . 51 4.10 Conjugate points .
    [Show full text]
  • Chapter 13 Curvature in Riemannian Manifolds
    Chapter 13 Curvature in Riemannian Manifolds 13.1 The Curvature Tensor If (M, , )isaRiemannianmanifoldand is a connection on M (that is, a connection on TM−), we− saw in Section 11.2 (Proposition 11.8)∇ that the curvature induced by is given by ∇ R(X, Y )= , ∇X ◦∇Y −∇Y ◦∇X −∇[X,Y ] for all X, Y X(M), with R(X, Y ) Γ( om(TM,TM)) = Hom (Γ(TM), Γ(TM)). ∈ ∈ H ∼ C∞(M) Since sections of the tangent bundle are vector fields (Γ(TM)=X(M)), R defines a map R: X(M) X(M) X(M) X(M), × × −→ and, as we observed just after stating Proposition 11.8, R(X, Y )Z is C∞(M)-linear in X, Y, Z and skew-symmetric in X and Y .ItfollowsthatR defines a (1, 3)-tensor, also denoted R, with R : T M T M T M T M. p p × p × p −→ p Experience shows that it is useful to consider the (0, 4)-tensor, also denoted R,givenby R (x, y, z, w)= R (x, y)z,w p p p as well as the expression R(x, y, y, x), which, for an orthonormal pair, of vectors (x, y), is known as the sectional curvature, K(x, y). This last expression brings up a dilemma regarding the choice for the sign of R. With our present choice, the sectional curvature, K(x, y), is given by K(x, y)=R(x, y, y, x)but many authors define K as K(x, y)=R(x, y, x, y). Since R(x, y)isskew-symmetricinx, y, the latter choice corresponds to using R(x, y)insteadofR(x, y), that is, to define R(X, Y ) by − R(X, Y )= + .
    [Show full text]
  • Deformations with Maximal Supersymmetries Part 2: Off-Shell Formulation
    Deformations with maximal supersymmetries part 2: off-shell formulation The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Chang, Chi-Ming et al. “Deformations with Maximal Supersymmetries Part 2: Off-Shell Formulation.” Journal of High Energy Physics 2016.4 (2016): n. pag. As Published http://dx.doi.org/10.1007/JHEP04(2016)171 Publisher Springer Berlin Heidelberg Version Final published version Citable link http://hdl.handle.net/1721.1/103304 Terms of Use Creative Commons Attribution Detailed Terms http://creativecommons.org/licenses/by/4.0/ Published for SISSA by Springer Received: February 26, 2016 Accepted: April 23, 2016 Published: April 28, 2016 Deformations with maximal supersymmetries part 2: JHEP04(2016)171 off-shell formulation Chi-Ming Chang,a Ying-Hsuan Lin,a Yifan Wangb and Xi Yina aJefferson Physical Laboratory, Harvard University, Cambridge, MA 02138, U.S.A. bCenter for Theoretical Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, U.S.A. E-mail: [email protected], [email protected], [email protected], [email protected] Abstract: Continuing our exploration of maximally supersymmetric gauge theories (MSYM) deformed by higher dimensional operators, in this paper we consider an off- shell approach based on pure spinor superspace and focus on constructing supersymmetric deformations beyond the first order. In particular, we give a construction of the Batalin- Vilkovisky action of an all-order non-Abelian Born-Infeld deformation of MSYM in the non-minimal pure spinor formalism. We also discuss subtleties in the integration over the pure spinor superspace and the relevance of Berkovits-Nekrasov regularization.
    [Show full text]
  • On the Geometry of Null Congruences in General Relativity*
    Proc. Indian Acad. Sci., Vol. 85 A, No. 6, 1977, pp. 546-551. On the geometry of null congruences in general relativity* ZAFAR AHSAN AND NIKHAT PARVEEN MALIK Department of Mathematics, Aligarh Muslim University, Aligarh 202001 MS received 16 August 1976; in revised form 5 January 1977 ABSTRACT Some theorems for the null conguences within the framework of general theory of relativity are given. These theorems are important in themselves as they illustrate the geometric meaning of the spin coeffi- cients. The newly developed Geroch-Held-Penrose (GHP) formalism has been used throughout the investigations. The salient features of GHP formalism that are necessary for the present work are given, and these techniques are applied to a pair of null congruences C (1) and C(n). 1. REVIEW OF THE TECHNIQUES SUPPOSE that two future pointing null directions are assigned at each point of the space-time. We can choose, as two of our tetrad vectors, two null vectors la, na (a, b,. — 1, 2, 3, 4) which point in these two directions and lava = 1 and the remaining tetrad vectors may be taken as Xa and Ya ortho- gonal to each la and na and to each other and also ma = 1/A/2 (Xa + iYa) and •Q = 1/x/2 (Xa — iYa), where a bar denotes the complex conjugation. If the scalar 7), with respect to the tetrad (la, ma, nza, na), undergoes the transformations _P aq (1) whenever la, na, ma and ma transform according as la ^ rla na . t.-1 l a ma -^ e^ 0 ma lilya-io ma (2) * Partially supported by a Junior Research Fellowship of Council of Scientific and Indu-- trial Research (India) under grant No.
    [Show full text]
  • Eienstein Field Equations and Heisenberg's Principle Of
    International Journal of Scientific and Research Publications, Volume 2, Issue 9, September 2012 1 ISSN 2250-3153 EIENSTEIN FIELD EQUATIONS AND HEISENBERG’S PRINCIPLE OF UNCERTAINLY THE CONSUMMATION OF GTR AND UNCERTAINTY PRINCIPLE 1DR K N PRASANNA KUMAR, 2PROF B S KIRANAGI AND 3PROF C S BAGEWADI ABSTRACT: The Einstein field equations (EFE) or Einstein's equations are a set of 10 equations in Albert Einstein's general theory of relativity which describe the fundamental interaction (e&eb) of gravitation as a result of space time being curved by matter and energy. First published by Einstein in 1915 as a tensor equation, the EFE equate spacetime curvature (expressed by the Einstein tensor) with (=) the energy and momentum tensor within that spacetime (expressed by the stress–energy tensor).Both space time curvature tensor and energy and momentum tensor is classified in to various groups based on which objects they are attributed to. It is to be noted that the total amount of energy and mass in the Universe is zero. But as is said in different context, it is like the Bank Credits and Debits, with the individual debits and Credits being conserved, holistically, the conservation and preservation of Debits and Credits occur, and manifest in the form of General Ledger. Transformations of energy also take place individually in the same form and if all such transformations are classified and written as a Transfer Scroll, it should tally with the total, universalistic transformation. This is a very important factor to be borne in mind. Like accounts are classifiable based on rate of interest, balance standing or the age, we can classify the factors and parameters in the Universe, be it age, interaction ability, mass, energy content.
    [Show full text]
  • The Reissner-Nordström Metric
    The Reissner-Nordström metric Jonatan Nordebo March 16, 2016 Abstract A brief review of special and general relativity including some classi- cal electrodynamics is given. We then present a detailed derivation of the Reissner-Nordström metric. The derivation is done by solving the Einstein-Maxwell equations for a spherically symmetric electrically charged body. The physics of this spacetime is then studied. This includes gravitational time dilation and redshift, equations of motion for both massive and massless non-charged particles derived from the geodesic equation and equations of motion for a massive charged par- ticle derived with lagrangian formalism. Finally, a quick discussion of the properties of a Reissner-Nordström black hole is given. 1 Contents 1 Introduction 3 2 Review of Special Relativity 3 2.1 4-vectors . 6 2.2 Electrodynamics in Special Relativity . 8 3 Tensor Fields and Manifolds 11 3.1 Covariant Differentiation and Christoffel Symbols . 13 3.2 Riemann Tensor . 15 3.3 Parallel Transport and Geodesics . 18 4 Basics of General Relativity 19 4.1 The Equivalence Principle . 19 4.2 The Principle of General Covariance . 20 4.3 Electrodynamics in General Relativity . 21 4.4 Newtonian Limit of the Geodesic Equation . 22 4.5 Einstein’s Field Equations . 24 5 The Reissner-Nordström Metric 25 5.1 Gravitational Time Dilation and Redshift . 32 5.2 The Geodesic Equation . 34 5.2.1 Comparison to Newtonian Mechanics . 37 5.2.2 Circular Orbits of Photons . 38 5.3 Motion of a Charged Particle . 38 5.4 Event Horizons and Black Holes . 40 6 Summary and Conclusion 44 2 1 Introduction In 1915 Einstein completed his general theory of relativity.
    [Show full text]