A Survey of Quaternionic Analysis
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Galaxies 2013, 1, 1-5; Doi:10.3390/Galaxies1010001
Galaxies 2013, 1, 1-5; doi:10.3390/galaxies1010001 OPEN ACCESS galaxies ISSN 2075-4434 www.mdpi.com/journal/galaxies Editorial Galaxies: An International Multidisciplinary Open Access Journal Emilio Elizalde Consejo Superior de Investigaciones Científicas, Instituto de Ciencias del Espacio & Institut d’Estudis Espacials de Catalunya, Faculty of Sciences, Campus Universitat Autònoma de Barcelona, Torre C5-Parell-2a planta, Bellaterra (Barcelona) 08193, Spain; E-Mail: [email protected]; Tel.: +34-93-581-4355 Received: 23 October 2012 / Accepted: 1 November 2012 / Published: 8 November 2012 The knowledge of the universe as a whole, its origin, size and shape, its evolution and future, has always intrigued the human mind. Galileo wrote: “Nature’s great book is written in mathematical language.” This new journal will be devoted to both aspects of knowledge: the direct investigation of our universe and its deeper understanding, from fundamental laws of nature which are translated into mathematical equations, as Galileo and Newton—to name just two representatives of a plethora of past and present researchers—already showed us how to do. Those physical laws, when brought to their most extreme consequences—to their limits in their respective domains of applicability—are even able to give us a plausible idea of how the origin of our universe came about and also of how we can expect its future to evolve and, eventually, how its end will take place. These laws also condense the important interplay between mathematics and physics as just one first example of the interdisciplinarity that will be promoted in the Galaxies Journal. Although already predicted by the great philosopher Immanuel Kant and others before him, galaxies and the existence of an “Island Universe” were only discovered a mere century ago, a fact too often forgotten nowadays when we deal with multiverses and the like. -
Frame Covariance and Fine Tuning in Inflationary Cosmology
FRAME COVARIANCE AND FINE TUNING IN INFLATIONARY COSMOLOGY A thesis submitted to the University of Manchester for the degree of Doctor of Philosophy in the Faculty of Science and Engineering 2019 By Sotirios Karamitsos School of Physics and Astronomy Contents Abstract 8 Declaration 9 Copyright Statement 10 Acknowledgements 11 1 Introduction 13 1.1 Frames in Cosmology: A Historical Overview . 13 1.2 Modern Cosmology: Frames and Fine Tuning . 15 1.3 Outline . 17 2 Standard Cosmology and the Inflationary Paradigm 20 2.1 General Relativity . 20 2.2 The Hot Big Bang Model . 25 2.2.1 The Expanding Universe . 26 2.2.2 The Friedmann Equations . 29 2.2.3 Horizons and Distances in Cosmology . 33 2.3 Problems in Standard Cosmology . 34 2.3.1 The Flatness Problem . 35 2.3.2 The Horizon Problem . 36 2 2.4 An Accelerating Universe . 37 2.5 Inflation: More Questions Than Answers? . 40 2.5.1 The Frame Problem . 41 2.5.2 Fine Tuning and Initial Conditions . 45 3 Classical Frame Covariance 48 3.1 Conformal and Weyl Transformations . 48 3.2 Conformal Transformations and Unit Changes . 51 3.3 Frames in Multifield Scalar-Tensor Theories . 55 3.4 Dynamics of Multifield Inflation . 63 4 Quantum Perturbations in Field Space 70 4.1 Gauge Invariant Perturbations . 71 4.2 The Field Space in Multifield Inflation . 74 4.3 Frame-Covariant Observable Quantities . 78 4.3.1 The Potential Slow-Roll Hierarchy . 81 4.3.2 Isocurvature Effects in Two-Field Models . 83 5 Fine Tuning in Inflation 88 5.1 Initial Conditions Fine Tuning . -
A Mathematical Derivation of the General Relativistic Schwarzschild
A Mathematical Derivation of the General Relativistic Schwarzschild Metric An Honors thesis presented to the faculty of the Departments of Physics and Mathematics East Tennessee State University In partial fulfillment of the requirements for the Honors Scholar and Honors-in-Discipline Programs for a Bachelor of Science in Physics and Mathematics by David Simpson April 2007 Robert Gardner, Ph.D. Mark Giroux, Ph.D. Keywords: differential geometry, general relativity, Schwarzschild metric, black holes ABSTRACT The Mathematical Derivation of the General Relativistic Schwarzschild Metric by David Simpson We briefly discuss some underlying principles of special and general relativity with the focus on a more geometric interpretation. We outline Einstein’s Equations which describes the geometry of spacetime due to the influence of mass, and from there derive the Schwarzschild metric. The metric relies on the curvature of spacetime to provide a means of measuring invariant spacetime intervals around an isolated, static, and spherically symmetric mass M, which could represent a star or a black hole. In the derivation, we suggest a concise mathematical line of reasoning to evaluate the large number of cumbersome equations involved which was not found elsewhere in our survey of the literature. 2 CONTENTS ABSTRACT ................................. 2 1 Introduction to Relativity ...................... 4 1.1 Minkowski Space ....................... 6 1.2 What is a black hole? ..................... 11 1.3 Geodesics and Christoffel Symbols ............. 14 2 Einstein’s Field Equations and Requirements for a Solution .17 2.1 Einstein’s Field Equations .................. 20 3 Derivation of the Schwarzschild Metric .............. 21 3.1 Evaluation of the Christoffel Symbols .......... 25 3.2 Ricci Tensor Components ................. -
PDF Solutions
Solutions to exercises Solutions to exercises Exercise 1.1 A‘stationary’ particle in anylaboratory on theEarth is actually subject to gravitationalforcesdue to theEarth andthe Sun. Thesehelp to ensure that theparticle moveswith thelaboratory.Ifstepsweretaken to counterbalance theseforcessothatthe particle wasreally not subject to anynet force, then the rotation of theEarth andthe Earth’sorbital motionaround theSun would carry thelaboratory away from theparticle, causing theforce-free particle to followacurving path through thelaboratory.Thiswouldclearly show that the particle didnot have constantvelocity in the laboratory (i.e.constantspeed in a fixed direction) andhence that aframe fixed in the laboratory is not an inertial frame.More realistically,anexperimentperformed usingthe kind of long, freely suspendedpendulum known as a Foucaultpendulum couldreveal the fact that a frame fixed on theEarth is rotating andthereforecannot be an inertial frame of reference. An even more practical demonstrationisprovidedbythe winds,which do not flowdirectly from areas of high pressure to areas of lowpressure because of theEarth’srotation. - Exercise 1.2 TheLorentzfactor is γ(V )=1/ 1−V2/c2. (a) If V =0.1c,then 1 γ = - =1.01 (to 3s.f.). 1 − (0.1c)2/c2 (b) If V =0.9c,then 1 γ = - =2.29 (to 3s.f.). 1 − (0.9c)2/c2 Notethatitisoften convenient to write speedsinterms of c instead of writingthe values in ms−1,because of thecancellation between factorsofc. ? @ AB Exercise 1.3 2 × 2 M = Theinverse of a matrix CDis ? @ 1 D −B M −1 = AD − BC −CA. Taking A = γ(V ), B = −γ(V )V/c, C = −γ(V)V/c and D = γ(V ),and noting that AD − BC =[γ(V)]2(1 − V 2/c2)=1,wehave ? @ γ(V )+γ(V)V/c [Λ]−1 = . -
Subgroups of Division Rings in Characteristic Zero Are Characterized
Subgroups of Division Rings Mark Lewis Murray Schacher June 27, 2018 Abstract We investigate the finite subgroups that occur in the Hamiltonian quaternion algebra over the real subfield of cyclotomic fields. When possible, we investigate their distribution among the maximal orders. MSC(2010): Primary: 16A39, 12E15; Secondary: 16U60 1 Introduction Let F be a field, and fix a and b to be non-0 elements of F . The symbol algebra A =(a, b) is the 4-dimensional algebra over F generated by elements i and j that satisfy the relations: i2 = a, j2 = b, ij = ji. (1) − One usually sets k = ij, which leads to the additional circular relations ij = k = ji, jk = i = kj, ki = j = ki. (2) − − − arXiv:1806.09654v1 [math.RA] 25 Jun 2018 The set 1, i, j, k forms a basis for A over F . It is not difficult to see that A is a central{ simple} algebra over F , and using Wedderburn’s theorem, we see that A is either a 4-dimensional division ring or the ring M2(F ) of2 2 matrices over F . It is known that A is split (i.e. is the ring of 2 2 matrices× over F ) if and only if b is a norm from the field F (√a). Note that×b is a norm over F (√a) if and only if there exist elements x, y F so that b = x2 y2a. This condition is symmetric in a and b. ∈ − More generally, we have the following isomorphism of algebras: (a, b) ∼= (a, ub) (3) 1 where u = x2 y2a is a norm from F (√a); see [4] or [6]. -
Some Aspects in Cosmological Perturbation Theory and F (R) Gravity
Some Aspects in Cosmological Perturbation Theory and f (R) Gravity Dissertation zur Erlangung des Doktorgrades (Dr. rer. nat.) der Mathematisch-Naturwissenschaftlichen Fakultät der Rheinischen Friedrich-Wilhelms-Universität Bonn von Leonardo Castañeda C aus Tabio,Cundinamarca,Kolumbien Bonn, 2016 Dieser Forschungsbericht wurde als Dissertation von der Mathematisch-Naturwissenschaftlichen Fakultät der Universität Bonn angenommen und ist auf dem Hochschulschriftenserver der ULB Bonn http://hss.ulb.uni-bonn.de/diss_online elektronisch publiziert. 1. Gutachter: Prof. Dr. Peter Schneider 2. Gutachter: Prof. Dr. Cristiano Porciani Tag der Promotion: 31.08.2016 Erscheinungsjahr: 2016 In memoriam: My father Ruperto and my sister Cecilia Abstract General Relativity, the currently accepted theory of gravity, has not been thoroughly tested on very large scales. Therefore, alternative or extended models provide a viable alternative to Einstein’s theory. In this thesis I present the results of my research projects together with the Grupo de Gravitación y Cosmología at Universidad Nacional de Colombia; such projects were motivated by my time at Bonn University. In the first part, we address the topics related with the metric f (R) gravity, including the study of the boundary term for the action in this theory. The Geodesic Deviation Equation (GDE) in metric f (R) gravity is also studied. Finally, the results are applied to the Friedmann-Lemaitre-Robertson-Walker (FLRW) spacetime metric and some perspectives on use the of GDE as a cosmological tool are com- mented. The second part discusses a proposal of using second order cosmological perturbation theory to explore the evolution of cosmic magnetic fields. The main result is a dynamo-like cosmological equation for the evolution of the magnetic fields. -
Schwarzschild Solution to Einstein's General Relativity
Schwarzschild Solution to Einstein's General Relativity Carson Blinn May 17, 2017 Contents 1 Introduction 1 1.1 Tensor Notations . .1 1.2 Manifolds . .2 2 Lorentz Transformations 4 2.1 Characteristic equations . .4 2.2 Minkowski Space . .6 3 Derivation of the Einstein Field Equations 7 3.1 Calculus of Variations . .7 3.2 Einstein-Hilbert Action . .9 3.3 Calculation of the Variation of the Ricci Tenosr and Scalar . 10 3.4 The Einstein Equations . 11 4 Derivation of Schwarzschild Metric 12 4.1 Assumptions . 12 4.2 Deriving the Christoffel Symbols . 12 4.3 The Ricci Tensor . 15 4.4 The Ricci Scalar . 19 4.5 Substituting into the Einstein Equations . 19 4.6 Solving and substituting into the metric . 20 5 Conclusion 21 References 22 Abstract This paper is intended as a very brief review of General Relativity for those who do not want to skimp on the details of the mathemat- ics behind how the theory works. This paper mainly uses [2], [3], [4], and [6] as a basis, and in addition contains short references to more in-depth references such as [1], [5], [7], and [8] when more depth was needed. With an introduction to manifolds and notation, special rel- ativity can be constructed which are the relativistic equations of flat space-time. After flat space-time, the Lagrangian and calculus of vari- ations will be introduced to construct the Einstein-Hilbert action to derive the Einstein field equations. With the field equations at hand the Schwarzschild equation will fall out with a few assumptions. -
Quaternion Zernike Spherical Polynomials
MATHEMATICS OF COMPUTATION Volume 84, Number 293, May 2015, Pages 1317–1337 S 0025-5718(2014)02888-3 Article electronically published on August 29, 2014 QUATERNION ZERNIKE SPHERICAL POLYNOMIALS J. MORAIS AND I. CAC¸ AO˜ Abstract. Over the past few years considerable attention has been given to the role played by the Zernike polynomials (ZPs) in many different fields of geometrical optics, optical engineering, and astronomy. The ZPs and their applications to corneal surface modeling played a key role in this develop- ment. These polynomials are a complete set of orthogonal functions over the unit circle and are commonly used to describe balanced aberrations. In the present paper we introduce the Zernike spherical polynomials within quater- nionic analysis ((R)QZSPs), which refine and extend the Zernike moments (defined through their polynomial counterparts). In particular, the underlying functions are of three real variables and take on either values in the reduced and full quaternions (identified, respectively, with R3 and R4). (R)QZSPs are orthonormal in the unit ball. The representation of these functions in terms of spherical monogenics over the unit sphere are explicitly given, from which several recurrence formulae for fast computer implementations can be derived. A summary of their fundamental properties and a further second or- der homogeneous differential equation are also discussed. As an application, we provide the reader with plot simulations that demonstrate the effectiveness of our approach. (R)QZSPs are new in literature and have some consequences that are now under investigation. 1. Introduction 1.1. The Zernike spherical polynomials. The complex Zernike polynomials (ZPs) have long been successfully used in many different fields of optics. -
Einstein's Mistakes
Einstein’s Mistakes Einstein was the greatest genius of the Twentieth Century, but his discoveries were blighted with mistakes. The Human Failing of Genius. 1 PART 1 An evaluation of the man Here, Einstein grows up, his thinking evolves, and many quotations from him are listed. Albert Einstein (1879-1955) Einstein at 14 Einstein at 26 Einstein at 42 3 Albert Einstein (1879-1955) Einstein at age 61 (1940) 4 Albert Einstein (1879-1955) Born in Ulm, Swabian region of Southern Germany. From a Jewish merchant family. Had a sister Maja. Family rejected Jewish customs. Did not inherit any mathematical talent. Inherited stubbornness, Inherited a roguish sense of humor, An inclination to mysticism, And a habit of grüblen or protracted, agonizing “brooding” over whatever was on its mind. Leading to the thought experiment. 5 Portrait in 1947 – age 68, and his habit of agonizing brooding over whatever was on its mind. He was in Princeton, NJ, USA. 6 Einstein the mystic •“Everyone who is seriously involved in pursuit of science becomes convinced that a spirit is manifest in the laws of the universe, one that is vastly superior to that of man..” •“When I assess a theory, I ask myself, if I was God, would I have arranged the universe that way?” •His roguish sense of humor was always there. •When asked what will be his reactions to observational evidence against the bending of light predicted by his general theory of relativity, he said: •”Then I would feel sorry for the Good Lord. The theory is correct anyway.” 7 Einstein: Mathematics •More quotations from Einstein: •“How it is possible that mathematics, a product of human thought that is independent of experience, fits so excellently the objects of physical reality?” •Questions asked by many people and Einstein: •“Is God a mathematician?” •His conclusion: •“ The Lord is cunning, but not malicious.” 8 Einstein the Stubborn Mystic “What interests me is whether God had any choice in the creation of the world” Some broadcasters expunged the comment from the soundtrack because they thought it was blasphemous. -
Linearized Einstein Field Equations
General Relativity Fall 2019 Lecture 15: Linearized Einstein field equations Yacine Ali-Ha¨ımoud October 17th 2019 SUMMARY FROM PREVIOUS LECTURE We are considering nearly flat spacetimes with nearly globally Minkowski coordinates: gµν = ηµν + hµν , with jhµν j 1. Such coordinates are not unique. First, we can make Lorentz transformations and keep a µ ν globally-Minkowski coordinate system, with hµ0ν0 = Λ µ0 Λ ν0 hµν , so that hµν can be seen as a Lorentz tensor µ µ µ ν field on flat spacetime. Second, if we make small changes of coordinates, x ! x − ξ , with j@µξ j 1, the metric perturbation remains small and changes as hµν ! hµν + 2ξ(µ,ν). By analogy with electromagnetism, we can see these small coordinate changes as gauge transformations, leaving the Riemann tensor unchanged at linear order. Since we will linearize the relevant equations, we may work in Fourier space: each Fourier mode satisfies an independent equation. We denote by ~k the wavenumber and by k^ its direction and k its norm. We have decomposed the 10 independent components of the metric perturbation according to their transformation properties under spatial rotations: there are 4 independent \scalar" components, which can be taken, for instance, ^i ^i^j to be h00; k h0i; hii, and k k hij { or any 4 linearly independent combinations thereof. There are 2 independent ilm^ ilm^ ^j transverse \vector" components, each with 2 independent components: klh0m and klhmjk { these are proportional to the curl of h0i and to the curl of the divergence of hij, and are divergenceless (transverse to the ~ TT Fourier wavenumber k). -
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'# (. -
Open Sloan-Dissertation.Pdf
The Pennsylvania State University The Graduate School LOOP QUANTUM COSMOLOGY AND THE EARLY UNIVERSE A Dissertation in Physics by David Sloan c 2010 David Sloan Submitted in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy August 2010 The thesis of David Sloan was reviewed and approved∗ by the following: Abhay Ashtekar Eberly Professor of Physics Dissertation Advisor, Chair of Committee Martin Bojowald Professor of Physics Tyce De Young Professor of Physics Nigel Higson Professor of Mathematics Jayanth Banavar Professor of Physics Head of the Department of Physics ∗Signatures are on file in the Graduate School. Abstract In this dissertation we explore two issues relating to Loop Quantum Cosmology (LQC) and the early universe. The first is expressing the Belinkskii, Khalatnikov and Lifshitz (BKL) conjecture in a manner suitable for loop quantization. The BKL conjecture says that on approach to space-like singularities in general rela- tivity, time derivatives dominate over spatial derivatives so that the dynamics at any spatial point is well captured by a set of coupled ordinary differential equa- tions. A large body of numerical and analytical evidence has accumulated in favor of these ideas, mostly using a framework adapted to the partial differential equa- tions that result from analyzing Einstein's equations. By contrast we begin with a Hamiltonian framework so that we can provide a formulation of this conjecture in terms of variables that are tailored to non-perturbative quantization. We explore this system in some detail, establishing the role of `Mixmaster' dynamics and the nature of the resulting singularity. Our formulation serves as a first step in the analysis of the fate of generic space-like singularities in loop quantum gravity.