Stretching-Based Diagnostics in a Differential Geometry Setting

Total Page:16

File Type:pdf, Size:1020Kb

Stretching-Based Diagnostics in a Differential Geometry Setting Stretching-Based Diagnostics in a Differential Geometry Setting Johannes Poppe∗, Dirk Lebiedz∗ ∗Institute for Numerical Mathematics, Ulm University, Germany Abstract— It is a prominent challenge to analytically char- points on the trajectory with regard to the chosen metric. acterize slow invariant manifolds for dynamical systems with An evident choice for the connection is the so-called Levi- multiple time-scales. To this end, we transfer the system Civita connection. In this setting, solutions of the extended into a differential-geometric framework. This setting enables to formulate stretching-based diagnostics in a new context, system can be interpreted in analogy to free falling particles coinciding with the intrinsic differential-geometric property in a graviational field within the framework of general of sectional curvature. relativity. In the context of chemical reaction mechanisms, the gravitational field correlates to an abstract chemical I. INTRODUCTION force. A suitable choice for a metric g can be derived The identification of slow invariant manifolds (SIMs) and expressed by its components regarding the standard is an essential part in model-order reduction for reac- coordinates x1; ··· ; xn; τ: tive systems. The mathematical definition of the SIM by Id −f(x) g = n : Fenichel can be considered unsatisfactory, because it is ij −f(x)T 1 + f(x)T f(x) only applicable to so-called slow-fast system and does not provide the uniqueness of the SIM. Observing the phase The bundling trajectories of the extended system (1) be- space of the dynamical system (not necessarily a slow- comes a set of geodesics which bundle alongside a specific fast system), the SIM becomes a geometric object which subset/submanifold of geodesics - the SIM in space time. attracts trajectories, resulting in a bundling behavior. We Hence, the SIM is supposed to be characterized by some aim to find a more general definition of the SIM, guided differential geometric property representing this bundling by the prior observations in phase space within the field behavior. of differential geometry. This setting provides one major III. GEODESIC STRETCHING benefit: All quantities are formulated covariantly, i.e. they are independent of the coordinate choice. A recent work by In general relativity, bundling behavior is related to Heiter and Lebiedz [1] translates the invariance property to geodesic deviation, neighboring geodesics experience rel- vanishing sectional curvatures in the extended phase space. ative accelerations towards each other. II. GEODESICS IN SPACETIME A. Geodesic Deviation p 2 M ` :(−"; ") ! M Let x_ = f(x) with x 2 n and f : n ! n be For , each geodesic passing R R R p t = 0 sufficiently smooth. We consider the extended state space, through at defines the tangent vector i.e., the original state space is extended by an additional d` f(x) T := (0) 2 T M; here: T = time-axis τ. In order to clarify that τ is part of the extended dt p 1; state space, we call τ ”explicit time”. In contrast, t is called arXiv:1905.02311v1 [math.DG] 6 May 2019 because we plug-in solution trajectories of (1). Geodesic implicit time. The resulting curves in the extended system are the solutions of d x f(x) Geod. deviation Rdev,p(s) = 2 n+1: (1) tangent vector T dt τ 1 R Bundling behavior of trajectories of the original system geodesics separation vector s corresponds to bundling of the solutions of (1). The space M := Rn+1 is trivially a manifold. By defining a metric tensor g (a family of inner products that varies smoothly from point to point), the tuple (M; g) becomes a Rieman- Fig. 1. Visualization of geodesic deviation nian manifold. The core idea is to couple the dynamics of (1) with a metric such that every trajectory becomes deviation is formally defined as the endomorphism Rdev;p : a geodesic - a shortest connection path for each tuple of TpM ! TpM formed by inserting the tangent vector T into the first and third argument of the Riemann curvature D. Geometrical Interpretation tensor R :(T M)3 ! T M, p p p One can show that !g;v has an intrinsic differential geometric meaning: It represents the sectional curvature R (s) := R (T; s)T: (2) dev;p p K(~v; w) of the expanded vector v~ with tangent vector T The intuitive concept of geodesic deviation is shown in of each space time trajectory from above: Fig. 1. The input vector s is the so-called ”separation g(R (~v); v~) g(R(T; v~)T; v~) dev;p = := K(~v; T ): vector” representing a small difference between two points g(~v; v~) g(~v; v~)g(T;T ) − g(~v; T )2 on the paths of two neighboring geodesics. The output Sectional curvature depends on the given metric g. Hence, vector represents the relative acceleration between both there is no direct connection to the utilized sectional curva- geodesics. ture in [1] which is based on a different metric. B. Stretching-Based Diagnostics E. Results In [2], Adrover et al. study SIMs by comparing so-called We test our ansatz by considering the well-known non- stretching rates !v(x) of solution trajectories of a given linear Davis-Skodje (DS) system: dynamic system x_ = F (x) for different vectors v(x) 2 dx n n = −x (3a) R = TxR . Each stretching rate is defined by dt hJ v; vi dy (γ − 1)x + γx2 ! (x) := F ; = −γy + (3b) v hv; vi dt (1 + x)2 where γ > 1 is a fixed parameter and x > 0. This where JF represents the Jacobian matrix of F . For a given n n system has a one-dimensional SIM given by the graph sub-manifold U ⊂ R and p 2 U, the tangent space TpR representation y = h(x) = x : Fig. 2 shows geodesic is decomposed into the direct sum of tangent space TpU and 1+x stretching ratios near the SIM for system (3) with γ = 3. normal space NpU. Adrover et al. argue that on the SIM, stretching in normal directions is supposed to dominate Setting x as RPV and maximizing the ratio with respect to tangent directions. Hence - in case of a one-dimensional y yields points near the SIM. SIM in a two-dimensional system, with vt and vo being tangent and normal to the trajectory respectively - the so- called stretching ratio geod. stretching ratio SIM ! (x) r(x) := vo 9.5 !v (x) t 9.0 is supposed to be larger than one at the SIM. Bundling of trajectories is directly correlated to the stretching ratio. It 8.5 appears evident that r(x) is particularly large on the SIM, 8.0 making its maximization on the phase space for a fixed choice of reaction progress variables (RPVs) a viable option 0.450 0.950 to approximate the SIM. 0.475 0.975 0.500 1.000 y value 0.525 1.025 C. Adapting the Stretching-Based Approach 0.550 1.050 x value We integrate this stretching-based approach within the framework from subsection III-A in the following way: We Fig. 2. Surface plot of geodesic stretching ratio for the Davis-Skodje replace the euclidean metric h·; ·i with the metric g defined system near the SIM. Black curve is stretching ratio on SIM. n above and expand each v 2 TpR by an additional explicit time component (which is set to 0): ACKNOWLEDGEMENT v Special thanks goes to the Klaus-Tschira foundation for n 3 v 7! :=v ~ 2 n+1: R 0 R financial funding of the project. REFERENCES Instead of the Jacobian matrix acting on each tangent vector representing an infinitesimal acceleration, we apply the [1] P. Heiter and D. Lebiedz, “Towards Differential Geometric Char- acterization of Slow Invariant Manifolds in Extended Phase Space: geodesic deviation endomorphism defined in (2). The result Sectional Curvature and Flow Invariance”, in SIAM J. Applied is the notion of so-called geodesic stretching Dynamical Systems Vol. 17 (2018), No. 1, pp. 732–753 [2] A. Adrover, F. Creta, M. Giona, M. Valorani, “Stretching-based g(R (~v); v~) diagnostics and reduction of chemical kinetic models with diffusion”, ! := dev;p : g;v~ g(~v; v~) in Journal of Computational Physics 225 (2007) 1442–1471.
Recommended publications
  • Local Flatness and Geodesic Deviation of Causal Geodesics
    UTM 724, July 2008 Local flatness and geodesic deviation of causal geodesics. Valter Moretti1,2, Roberto Di Criscienzo3, 1 Dipartimento di Matematica, Universit`adi Trento and Istituto Nazionale di Fisica Nucleare – Gruppo Collegato di Trento, via Sommarive 14 I-38050 Povo (TN), Italy. 2 Istituto Nazionale di Alta Matematica “F.Severi”– GNFM 3 Department of Physics, University of Toronto, 60 St. George Street, Toronto, ON, M5S 1A7, Canada. E-mail: [email protected], [email protected] Abstract. We analyze the interplay of local flatness and geodesic deviation measured for causal geodesics starting from the remark that, form a physical viewpoint, the geodesic deviation can be measured for causal geodesic, observing the motion of (infinitesimal) falling bodies, but it can hardly be evaluated on spacelike geodesics. We establish that a generic spacetime is (locally) flat if and only if there is no geodesic deviation for timelike geodesics or, equivalently, there is no geodesic deviation for null geodesics. 1 Introduction The presence of tidal forces, i.e. geodesic deviation for causal geodesics, can be adopted to give a notion of gravitation valid in the general relativistic context, as the geodesic deviation is not affected by the equivalence principle and thus it cannot be canceled out by an appropriate choice of the reference frame. By direct inspection (see [MTW03]), one sees that the absence of geodesic deviation referred to all type of geodesics is equivalent the fact that the Riemann tensor vanishes everywhere in a spacetime (M, g). The latter fact, in turn, is equivalent to the locally flatness of the spacetime, i.e.
    [Show full text]
  • General Relativity Fall 2019 Lecture 13: Geodesic Deviation; Einstein field Equations
    General Relativity Fall 2019 Lecture 13: Geodesic deviation; Einstein field equations Yacine Ali-Ha¨ımoud October 11th, 2019 GEODESIC DEVIATION The principle of equivalence states that one cannot distinguish a uniform gravitational field from being in an accelerated frame. However, tidal fields, i.e. gradients of gravitational fields, are indeed measurable. Here we will show that the Riemann tensor encodes tidal fields. Consider a fiducial free-falling observer, thus moving along a geodesic G. We set up Fermi normal coordinates in µ the vicinity of this geodesic, i.e. coordinates in which gµν = ηµν jG and ΓνσjG = 0. Events along the geodesic have coordinates (x0; xi) = (t; 0), where we denote by t the proper time of the fiducial observer. Now consider another free-falling observer, close enough from the fiducial observer that we can describe its position with the Fermi normal coordinates. We denote by τ the proper time of that second observer. In the Fermi normal coordinates, the spatial components of the geodesic equation for the second observer can be written as d2xi d dxi d2xi dxi d2t dxi dxµ dxν = (dt/dτ)−1 (dt/dτ)−1 = (dt/dτ)−2 − (dt/dτ)−3 = − Γi − Γ0 : (1) dt2 dτ dτ dτ 2 dτ dτ 2 µν µν dt dt dt The Christoffel symbols have to be evaluated along the geodesic of the second observer. If the second observer is close µ µ λ λ µ enough to the fiducial geodesic, we may Taylor-expand Γνσ around G, where they vanish: Γνσ(x ) ≈ x @λΓνσjG + 2 µ 0 µ O(x ).
    [Show full text]
  • 3. Introducing Riemannian Geometry
    3. Introducing Riemannian Geometry We have yet to meet the star of the show. There is one object that we can place on a manifold whose importance dwarfs all others, at least when it comes to understanding gravity. This is the metric. The existence of a metric brings a whole host of new concepts to the table which, collectively, are called Riemannian geometry.Infact,strictlyspeakingwewillneeda slightly di↵erent kind of metric for our study of gravity, one which, like the Minkowski metric, has some strange minus signs. This is referred to as Lorentzian Geometry and a slightly better name for this section would be “Introducing Riemannian and Lorentzian Geometry”. However, for our immediate purposes the di↵erences are minor. The novelties of Lorentzian geometry will become more pronounced later in the course when we explore some of the physical consequences such as horizons. 3.1 The Metric In Section 1, we informally introduced the metric as a way to measure distances between points. It does, indeed, provide this service but it is not its initial purpose. Instead, the metric is an inner product on each vector space Tp(M). Definition:Ametric g is a (0, 2) tensor field that is: Symmetric: g(X, Y )=g(Y,X). • Non-Degenerate: If, for any p M, g(X, Y ) =0forallY T (M)thenX =0. • 2 p 2 p p With a choice of coordinates, we can write the metric as g = g (x) dxµ dx⌫ µ⌫ ⌦ The object g is often written as a line element ds2 and this expression is abbreviated as 2 µ ⌫ ds = gµ⌫(x) dx dx This is the form that we saw previously in (1.4).
    [Show full text]
  • Geodesic Deviation Equation in Locally De Sitter Spacetimes
    Instituto de Física Teórica Universidade Estadual Paulista MSc Thesis IFT-D-007/18 Geodesic Deviation Equation in Locally de Sitter Spacetimes Johan Renzo Salazar Malpartida Supervisor José Geraldo Pereira August 2018 Salazar Malpartida, Johan Renzo S161g Geodesic deviation equation in locally de sitter spacetimes / Johan Renzo Salazar Malpartida. -- São Paulo, 2018 37 f. : il. Dissertação (mestrado) - Universidade Estadual Paulista (Unesp), Instituto de Física Teórica (IFT), São Paulo Orientador: Jose Geraldo Pereira 1. Relatividade (Física). 2. Relatividade especial (Física). 3. Gravitação. I. Título. Sistema de geração automática de fichas catalográficas da Unesp. Biblioteca do Instituto de Física Teórica (IFT), São Paulo. Dados fornecidos pelo autor(a). Agradecimientos Quero agradecer meu orientador, Prof. José Geraldo Pereira, pelo apoio e paciência que teve comigo. Seus ensinamentos me ajudaram a ter novas idéias sobre a Física, muito obrigado pela oportunidade que me foi concedida de fazer um Mestrado, e conhecer o Brasil. A mi familia por el apoyo siempre brindado. À CAPES, pelo apoio financeiro. iii Resumo Como é bem conhecido, a relatividade especial de Einstein, cuja cinemática é governada pelo grupo de Poincaré, deixa de valer na escala de Planck devido à existência de uma escala de comprimento invariante, dada pelo comprimento de Planck. Por essa razão, ela é incapaz de descrever a cinemática naquela escala. Uma solução possível para esse problema, a qual preserva a simetria de Lorentz — e consequentemente a causalidade — é substituir a relatividade espe- cial de Einstein por uma relatividade especial na qual a cinemática é governada pelo grupo de de Sitter. Claro que uma mudança na relatividade especial irá pruduzir mudanças concomitantes na relatividade geral, a qual se torna o que chamamos de relatividade geral modificada por de Sit- ter.
    [Show full text]
  • THE RIEMANN CURVATURE TENSOR, JACOBI FIELDS and GRAPHS 1. Geodesic Deviation
    THE RIEMANN CURVATURE TENSOR, JACOBI FIELDS and GRAPHS 1. Geodesic deviation: the curvature tensor and Jacobi fields. Let (M; g) be a Riemannian manifold, p 2 M. Suppose we want to measure the \instantaneous spreading rate" of geodesic rays issuing from p. The natural way to do this is to consider a geodesic variation: 0 f(t; s) = expp(tv(s)); v(s) 2 TpM; v(0) = v; v (0) = w: Then the \spreading rate" is measured by the variation vector field V (t): @f V (t) = = d expp(tv)[tw]; @s js=0 a vector field along the geodesic γ(t) = expp(tv). Let's try to find a differ- ential equation satisfied by V . We have: DV D @f D @f D2V D D @f = = ; = ( ): @t @t @s @s @t @t2 @t @s @t Setting W = @tf (a vector field along f), we see that DW=@t ≡ 0: D @f D D ( ) = (d exp (tv(s))[v(s)] = γ_ (t) = 0; @t @t @t p @t s since γs(t) = expp(tv(s)) is a geodesic (γs(0) = p; γ_s(0) = v(s)). Thus we need to compute the vector field X(t) along f: D DW D DW X(t) := − ; @t @s @s @t for then, along γ(t): D2V = X(t): dt2 We compute in a coordinate chart: i n i f(s; t) = (x (s; t)) 2 R ;W (s; t) = a (s; t)@xi : Using the symmetry of the connection, we find: X = ai@ x @ x (r r @ − r r @ ): t k s j @xk @xj xi @xj @xk xi We now consider the linearity over smooth functions of this commutator of covariant derivatives.
    [Show full text]
  • Lecture 8: Geodesic Deviation Etc
    – 1 – Orthonormal Tetrads, continued Here’s another example, that combines local frame calculations with more global anal- ysis. Suppose you have a particle at rest at infinity, and you drop it radially into a Schwarzschild black hole. What is the radial velocity as seen by a local static observer at radius r? The particle being at rest at infinity means that its total energy is ut = −1. Radial motion has θ and φ components zero, so u2 = −1 means r t u ur + u ut = −1 g (ur)2 + gttu2 = −1 rr t (1) (ur)2/(1 − 2M/r) − 1/(1 − 2M/r) = −1 (ur)2 =2M/r . Therefore, ur = dr/dτ = p2M/r. The radial velocity seen by a local static observer is vrˆ = urˆ/utˆ rˆ = −u /utˆ − rˆ r t = e ru /(e tˆut) (2) −1/2 r −1/2 = −(1 − 2M/r) u /[(1 − 2M/r) ut] = p2M/r . Therefore, the locally measured radial velocity is just the same as the Newtonian expression, when Schwarzschild coordinates are used. By comparison, the radial velocity as measured at infinity is dr vr = = ur/ut = ur/(gttu )=(1 − 2M/r)ur = (1 − 2M/r)p2M/r . (3) dt t This drops to zero at the horizon. Note that there is one factor of (1 − 2M/r)1/2 from the redshift and one from the change in the radial coordinate. Geodesic Deviation and Spacetime Curvature Previously we talked about geodesics, the paths of freely falling particles. We also indicated early on that the only “force” that gravity can exert on a particle is a tidal force.
    [Show full text]
  • Arxiv:1804.11106V2 [Gr-Qc] 2 Jun 2018 Oe Yscinii Nwihw Ou Nteproperties the on Focus Fol- We Is Which This in III, Equation
    Deviation equation in Riemann-Cartan spacetime Dirk Puetzfeld∗ University of Bremen, Center of Applied Space Technology and Microgravity (ZARM), 28359 Bremen, Germany Yuri N. Obukhov† Theoretical Physics Laboratory, Nuclear Safety Institute, Russian Academy of Sciences, B.Tulskaya 52, 115191 Moscow, Russia (Dated: June 5, 2018) We derive a generalized deviation equation in Riemann-Cartan spacetime. The equation describes the dynamics of the connecting vector which links events on two general adjacent world lines. Our result is valid for any theory in a Riemann-Cartan background, in particular, it is applicable to a large class of gravitational theories which go beyond the general relativistic framework. PACS numbers: 04.50.-h; 04.20.Cv; 04.25.-g Keywords: Deviation equation; Approximation methods; Equations of motion; Riemann-Cartan spacetime I. INTRODUCTION of a world function based on autoparallels in a Riemann- Cartan background. These results are then applied in Within the theory of General Relativity, the rela- section IV to arrive at an expanded approximate ver- tive motion of test bodies is described by means of the sion of the deviation equation. In section V we discuss geodesic deviation (Jacobi) equation [1–4]. This equa- how different coordinate choices, depending on the un- tion only holds under certain assumptions and can be derlying gravity theory, affect the interpretation and the used only for the description of structureless neutral test operational value of the deviation equation. We conclude bodies. our paper in section VI with a discussion of the results In a previous work [5], we have worked out generalized obtained and with an outlook of their possible applica- versions of the deviation equation, see also [6–28] for al- tions.
    [Show full text]
  • General Relativity University of Cambridge Part III Mathematical Tripos
    Preprint typeset in JHEP style - HYPER VERSION Michaelmas Term, 2019 General Relativity University of Cambridge Part III Mathematical Tripos David Tong Department of Applied Mathematics and Theoretical Physics, Centre for Mathematical Sciences, Wilberforce Road, Cambridge, CB3 OBA, UK http://www.damtp.cam.ac.uk/user/tong/gr.html [email protected] –1– Recommended Books and Resources There are many decent text books on general relativity. Here are a handful that I like: Sean Carroll, “Spacetime and Geometry” • A straightforward and clear introduction to the subject. Bob Wald, “General Relativity” • The go-to relativity book for relativists. Steven Weinberg, “Gravitation and Cosmology” • The go-to relativity book for particle physicists. Misner, Thorne and Wheeler, “Gravitation” • Extraordinary and ridiculous in equal measure, this book covers an insane amount of material but with genuinely excellent explanations. Now, is that track 1 or track 2? Tony Zee, “Einstein Gravity in a Nutshell” • Professor Zee likes a bit of a chat. So settle down, prepare yourself for more tangents than Tp(M), and enjoy this entertaining, but not particularly concise, meander through the subject. Nakahara, “Geometry, Topology and Physics” • Areallyexcellentbookthatwillsatisfyyourgeometricalandtopologicalneedsforthis course and much beyond. It is particularly useful for Sections 2 and 3 of these lectures where we cover di↵erential geometry. Anumberofexcellentlecturenotesareavailableontheweb,includingan early version of Sean Carroll’s book. Links can be found
    [Show full text]
  • Geodesic Deviation Equation for Relativistic Tops and the Detection of Gravitational Waves
    REVISTA MEXICANA DE FISICA´ S 53 (2) 141–145 FEBRERO 2007 Geodesic deviation equation for relativistic tops and the detection of gravitational waves J.A. Nieto Escuela de Ciencias F´ısico-Matematicas,´ Universidad Autonoma´ de Sinaloa, 80010 Culiacan´ Sinaloa, Mexico.´ J. Saucedo Departamento de Investigacion´ en F´ısica de la Universidad de Sonora, 83000 Hermosillo Sonora, Mexico.´ V.M. Villanueva Instituto de F´ısica y Matematicas,´ Universidad Michoacana de San Nicolas´ de Hidalgo, 58040, Morelia, Michoacan,´ Mexico.´ Recibido el 18 de julio de 2005; aceptado el 14 de marzo de 2005 In this contribution, we review the derivation of the relativistic top geodesic deviation equation. This equation results in a generalization of the geodesic deviation equation for a pair of nearby point particles. This property is taken into account in investigating the detection of gravitational waves, and we show how our generalized formula for a relativistic top can be used to study the gravitational wave backgrounds. Besides of these facts, we argue that our formulation may be of special interest for detecting the inflationary gravitational waves via the polarization of the cosmic background radiation. Keywords: Geodesic equation; relativistic top; gravitational waves. En esta contribucion,´ revisamos la derivacion´ de la ecuacion´ de desviacion´ de geodesicas´ para trompos relativistas. Esta ecuacion´ es una generalizacion´ de la ecuacion´ de geodesicas´ para un par de objetos puntuales cercanos. Esta propiedad es tomada en cuenta para investigar la deteccion´ de ondas gravitacionales, y mostramos como´ nuestra formula´ generalizada para un trompo relativista puede ser usada para estudiar los fondos de ondas gravitacionales. Ademas´ de estos hechos, argumentamos que nuestra formulacion´ puede ser de especial interes´ para detectar las ondas gravitacionales inflacionarias a traves´ de la polarizacion´ en la radiacion´ cosmica´ de fondo.
    [Show full text]
  • Geodesic Deviation in the Ads Black String Spacetime H.Culetu Ovidius
    Geodesic Deviation in the AdS Black String Spacetime H.Culetu* Ovidius University, Department of Physics, B-dul Mamaia 124, 8700 Constanta, Romania Abstract. The equation of motion of test particles in the geometry of a black string embedded in a five dimensional AdS spacetime is studied. With an inversion transformation on the fifth coordinate “w”, we obtain a simple form of the geodesics and the geodesics deviation. α The equations for the separation vector ξ between two nearby geodesics are found, with ξ5(λ) = ξ 5 λ (0) sin( /l) independent of the Schwarzschild potential U(r) (l – the AdS radius). 1. Introduction The conjecture that our world would be a three-brane embedded in extra spatial dimensions has been considered as a solution to the weak scale hierarchy problem. The recent developments are based on the idea that ordinary matter fields are confined to a three – dimensional world while gravity could live in a higher dimensional space [1,2]. But the question is whether the model gives back standard four dimensional gravity in the brane assumed to represent our world. Randall and Sundrum (RS) [3] consider our Universe as a negative tension domain wall separated from a positive tension wall by a region of anti - de Sitter geometry. In a 2–nd work [4] RS have introduced a positive tension 3-brane (where we live) inside 5-dimensional anti-de Sitter (AdS) space. Chamblin et al. [5] studied a black hole formed by gravitational collapse in the RS models with the horizon extended into the directions transverse to the brane.
    [Show full text]
  • Geodesic Structure in Schwarzschild Geometry with Extensions in Higher Dimensional Spacetimes
    Virginia Commonwealth University VCU Scholars Compass Theses and Dissertations Graduate School 2018 GEODESIC STRUCTURE IN SCHWARZSCHILD GEOMETRY WITH EXTENSIONS IN HIGHER DIMENSIONAL SPACETIMES Ian M. Newsome Virginia Commonwealth University Follow this and additional works at: https://scholarscompass.vcu.edu/etd Part of the Elementary Particles and Fields and String Theory Commons, and the Other Physics Commons © Ian M Newsome Downloaded from https://scholarscompass.vcu.edu/etd/5414 This Thesis is brought to you for free and open access by the Graduate School at VCU Scholars Compass. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of VCU Scholars Compass. For more information, please contact [email protected]. c Ian Marshall Newsome, May 2018 All Rights Reserved. GEODESIC STRUCTURE IN SCHWARZSCHILD GEOMETRY WITH EXTENSIONS IN HIGHER DIMENSIONAL SPACETIMES A Thesis submitted in partial fulfillment of the requirements for the degree of Master of Science at Virginia Commonwealth University. by IAN MARSHALL NEWSOME August 2016 to May 2018 Director: Robert H. Gowdy, Associate Professor, Associate Chair, Department of Physics Virginia Commonwewalth University Richmond, Virginia May, 2018 i Acknowledgements I would like to thank Dr. Robert Gowdy for his guidance during the creation of this thesis. His patience and assistance have been paramount to my understanding of the fields of differential geometry and the theory of relativity. I would also like to thank my mother and father for their continuing support during my higher education, without which I may have faltered long ago. ii TABLE OF CONTENTS Chapter Page Acknowledgements :::::::::::::::::::::::::::::::: ii Table of Contents :::::::::::::::::::::::::::::::: iii List of Tables ::::::::::::::::::::::::::::::::::: iv List of Figures :::::::::::::::::::::::::::::::::: v Abstract ::::::::::::::::::::::::::::::::::::: ix 1 Introduction ::::::::::::::::::::::::::::::::: 1 1.1 Background .
    [Show full text]
  • Compendium of Useful Formulas
    Preprint typeset in JHEP style - HYPER VERSION Compendium of useful formulas Matthew Headrick Abstract: Almost everything I know. Contents 1. Miscellaneous math 3 1.1 A matrix identity 3 1.2 Campbell-Baker-Hausdorff 3 1.3 Pauli matrices 3 1.4 Level repulsion 3 1.5 The Legendre transform 3 1.6 Gaussian integrals 5 1.7 Saddle-point approximation 5 1.8 Cauchy principal value 6 1.9 A few Fourier transforms 7 2. Differential geometry 7 2.1 Diffeomorphisms vs. coordinate tranformations 7 2.2 Connection and curvatures 8 2.3 Geodesic deviation equation 9 2.4 Forms 10 2.5 Harmonic forms 11 2.6 Vielbein formalism 12 2.7 Lie derivatives and Killing fields 13 2.8 Weyl transformations 14 2.9 Metric perturbations 14 2.10 Warped products 14 2.11 Flat fibrations 15 2.12 Gauss-Bonnet theorems 16 2.13 Hypersurfaces 17 2.14 General submanifolds 21 2.15 K¨ahlergeometry 21 2.16 Poincar´eduality 23 2.17 Coordinates for S2 24 2.18 The Hopf fibration 25 2.19 Unit sphere 27 3. Classical mechanics 27 3.1 Lagrangian and Hamiltonian formulations 27 3.2 Symmetries 29 3.3 Noether's theorem for higher-order actions 31 3.4 Gauge symmetries 32 3.5 Hamilton-Jacobi theory 34 { 1 { 4. Gauge theories 36 4.1 Generalities 36 4.2 Standard Model 37 5. General relativity 40 5.1 Dimensions 40 5.2 Fundamentals 40 5.3 Spherically symmetric solutions 41 5.4 Cauchy problem 42 5.5 Gravitational waves 44 5.6 Israel junction condition 46 5.7 Boundary term 47 5.8 Dimensional reductions 49 6.
    [Show full text]