Lagrangians for Spinor Fields
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An Introduction to Quantum Field Theory
AN INTRODUCTION TO QUANTUM FIELD THEORY By Dr M Dasgupta University of Manchester Lecture presented at the School for Experimental High Energy Physics Students Somerville College, Oxford, September 2009 - 1 - - 2 - Contents 0 Prologue....................................................................................................... 5 1 Introduction ................................................................................................ 6 1.1 Lagrangian formalism in classical mechanics......................................... 6 1.2 Quantum mechanics................................................................................... 8 1.3 The Schrödinger picture........................................................................... 10 1.4 The Heisenberg picture............................................................................ 11 1.5 The quantum mechanical harmonic oscillator ..................................... 12 Problems .............................................................................................................. 13 2 Classical Field Theory............................................................................. 14 2.1 From N-point mechanics to field theory ............................................... 14 2.2 Relativistic field theory ............................................................................ 15 2.3 Action for a scalar field ............................................................................ 15 2.4 Plane wave solution to the Klein-Gordon equation ........................... -
Arxiv:Math/0212058V2 [Math.DG] 18 Nov 2003 Nosbrusof Subgroups Into Rdc C.[Oc 00 Et .].Eape O Uhsae a Spaces Such for Examples 3.2])
THE SPINOR BUNDLE OF RIEMANNIAN PRODUCTS FRANK KLINKER Abstract. In this note we compare the spinor bundle of a Riemannian mani- fold (M = M1 ×···×MN ,g) with the spinor bundles of the Riemannian factors (Mi,gi). We show that - without any holonomy conditions - the spinor bundle of (M,g) for a special class of metrics is isomorphic to a bundle obtained by tensoring the spinor bundles of (Mi,gi) in an appropriate way. For N = 2 and an one dimensional factor this construction was developed in [Baum 1989a]. Although the fact for general factors is frequently used in (at least physics) literature, a proof was missing. I would like to thank Shahram Biglari, Mario Listing, Marc Nardmann and Hans-Bert Rademacher for helpful comments. Special thanks go to Helga Baum, who pointed out some difficulties arising in the pseudo-Riemannian case. We consider a Riemannian manifold (M = M MN ,g), which is a product 1 ×···× of Riemannian spin manifolds (Mi,gi) and denote the projections on the respective factors by pi. Furthermore the dimension of Mi is Di such that the dimension of N M is given by D = i=1 Di. The tangent bundle of M is decomposed as P ∗ ∗ (1) T M = p Tx1 M p Tx MN . (x0,...,xN ) 1 1 ⊕···⊕ N N N We omit the projections and write TM = i=1 TMi. The metric g of M need not be the product metric of the metrics g on M , but L i i is assumed to be of the form c d (2) gab(x) = Ai (x)gi (xi)Ai (x), T Mi a cd b for D1 + + Di−1 +1 a,b D1 + + Di, 1 i N ··· ≤ ≤ ··· ≤ ≤ In particular, for those metrics the splitting (1) is orthogonal, i.e. -
Exact Solutions to the Interacting Spinor and Scalar Field Equations in the Godel Universe
XJ9700082 E2-96-367 A.Herrera 1, G.N.Shikin2 EXACT SOLUTIONS TO fHE INTERACTING SPINOR AND SCALAR FIELD EQUATIONS IN THE GODEL UNIVERSE 1 E-mail: [email protected] ^Department of Theoretical Physics, Russian Peoples ’ Friendship University, 117198, 6 Mikluho-Maklaya str., Moscow, Russia ^8 as ^; 1996 © (XrbCAHHeHHuft HHCTtrryr McpHMX HCCJicAOB&Htift, fly 6na, 1996 1. INTRODUCTION Recently an increasing interest was expressed to the search of soliton-like solu tions because of the necessity to describe the elementary particles as extended objects [1]. In this work, the interacting spinor and scalar field system is considered in the external gravitational field of the Godel universe in order to study the influence of the global properties of space-time on the interaction of one dimensional fields, in other words, to observe what is the role of gravitation in the interaction of elementary particles. The Godel universe exhibits a number of unusual properties associated with the rotation of the universe [2]. It is ho mogeneous in space and time and is filled with a perfect fluid. The main role of rotation in this universe consists in the avoidance of the cosmological singu larity in the early universe, when the centrifugate forces of rotation dominate over gravitation and the collapse does not occur [3]. The paper is organized as follows: in Sec. 2 the interacting spinor and scalar field system with £jnt = | <ptp<p'PF(Is) in the Godel universe is considered and exact solutions to the corresponding field equations are obtained. In Sec. 3 the properties of the energy density are investigated. -
On the Spinor Representation
Eur. Phys. J. C (2017) 77:487 DOI 10.1140/epjc/s10052-017-5035-y Regular Article - Theoretical Physics On the spinor representation J. M. Hoff da Silva1,a, C. H. Coronado Villalobos1,2,b, Roldão da Rocha3,c, R. J. Bueno Rogerio1,d 1 Departamento de Física e Química, Universidade Estadual Paulista, Guaratinguetá, SP, Brazil 2 Instituto de Física, Universidade Federal Fluminense, Av. Gal. Milton Tavares de Souza s/n, Gragoatá, Niterói, RJ 24210-346, Brazil 3 Centro de Matemática, Computação e Cognição, Universidade Federal do ABC-UFABC, Santo André 09210-580, Brazil Received: 16 February 2017 / Accepted: 30 June 2017 / Published online: 21 July 2017 © The Author(s) 2017. This article is an open access publication Abstract A systematic study of the spinor representation at least in principle, related to a set of fermionic observ- by means of the fermionic physical space is accomplished ables. Our aim in this paper is to delineate the importance and implemented. The spinor representation space is shown of the representation space, by studying its properties, and to be constrained by the Fierz–Pauli–Kofink identities among then relating them to their physical consequences. As one the spinor bilinear covariants. A robust geometric and topo- will realize, the representation space is quite complicated due logical structure can be manifested from the spinor space, to the constraints coming out the Fierz–Pauli–Kofink iden- wherein the first and second homotopy groups play promi- tities. However, a systematic study of the space properties nent roles on the underlying physical properties, associated ends up being useful to relate different domains (subspaces) to fermionic fields. -
An Introduction to Supersymmetry
An Introduction to Supersymmetry Ulrich Theis Institute for Theoretical Physics, Friedrich-Schiller-University Jena, Max-Wien-Platz 1, D–07743 Jena, Germany [email protected] This is a write-up of a series of five introductory lectures on global supersymmetry in four dimensions given at the 13th “Saalburg” Summer School 2007 in Wolfersdorf, Germany. Contents 1 Why supersymmetry? 1 2 Weyl spinors in D=4 4 3 The supersymmetry algebra 6 4 Supersymmetry multiplets 6 5 Superspace and superfields 9 6 Superspace integration 11 7 Chiral superfields 13 8 Supersymmetric gauge theories 17 9 Supersymmetry breaking 22 10 Perturbative non-renormalization theorems 26 A Sigma matrices 29 1 Why supersymmetry? When the Large Hadron Collider at CERN takes up operations soon, its main objective, besides confirming the existence of the Higgs boson, will be to discover new physics beyond the standard model of the strong and electroweak interactions. It is widely believed that what will be found is a (at energies accessible to the LHC softly broken) supersymmetric extension of the standard model. What makes supersymmetry such an attractive feature that the majority of the theoretical physics community is convinced of its existence? 1 First of all, under plausible assumptions on the properties of relativistic quantum field theories, supersymmetry is the unique extension of the algebra of Poincar´eand internal symmtries of the S-matrix. If new physics is based on such an extension, it must be supersymmetric. Furthermore, the quantum properties of supersymmetric theories are much better under control than in non-supersymmetric ones, thanks to powerful non- renormalization theorems. -
Majorana Spinors
MAJORANA SPINORS JOSE´ FIGUEROA-O'FARRILL Contents 1. Complex, real and quaternionic representations 2 2. Some basis-dependent formulae 5 3. Clifford algebras and their spinors 6 4. Complex Clifford algebras and the Majorana condition 10 5. Examples 13 One dimension 13 Two dimensions 13 Three dimensions 14 Four dimensions 14 Six dimensions 15 Ten dimensions 16 Eleven dimensions 16 Twelve dimensions 16 ...and back! 16 Summary 19 References 19 These notes arose as an attempt to conceptualise the `symplectic Majorana{Weyl condition' in 5+1 dimensions; but have turned into a general discussion of spinors. Spinors play a crucial role in supersymmetry. Part of their versatility is that they come in many guises: `Dirac', `Majorana', `Weyl', `Majorana{Weyl', `symplectic Majorana', `symplectic Majorana{Weyl', and their `pseudo' counterparts. The tra- ditional physics approach to this topic is a mixed bag of tricks using disparate aspects of representation theory of finite groups. In these notes we will attempt to provide a uniform treatment based on the classification of Clifford algebras, a work dating back to the early 60s and all but ignored by the theoretical physics com- munity. Recent developments in superstring theory have made us re-examine the conditions for the existence of different kinds of spinors in spacetimes of arbitrary signature, and we believe that a discussion of this more uniform approach is timely and could be useful to the student meeting this topic for the first time or to the practitioner who has difficulty remembering the answer to questions like \when do symplectic Majorana{Weyl spinors exist?" The notes are organised as follows. -
Arxiv:2004.02090V2 [Math.NT]
ON INDEFINITE AND POTENTIALLY UNIVERSAL QUADRATIC FORMS OVER NUMBER FIELDS FEI XU AND YANG ZHANG Abstract. A number field k admits a binary integral quadratic form which represents all integers locally but not globally if and only if the class number of k is bigger than one. In this case, there are only finitely many classes of such binary integral quadratic forms over k. A number field k admits a ternary integral quadratic form which represents all integers locally but not globally if and only if the class number of k is even. In this case, there are infinitely many classes of such ternary integral quadratic forms over k. An integral quadratic form over a number field k with more than one variables represents all integers of k over the ring of integers of a finite extension of k if and only if this quadratic form represents 1 over the ring of integers of a finite extension of k. 1. Introduction Universal integral quadratic forms over Z have been studied extensively by Dickson [7] and Ross [24] for both positive definite and indefinite cases in the 1930s. A positive definite integral quadratic form is called universal if it represents all positive integers. Ross pointed out that there is no ternary positive definite universal form over Z in [24] (see a more conceptual proof in [9, Lemma 3]). However, this result is not true over totally real number fields. In [20], Maass proved that x2 + y2 + z2 is a positive definite universal quadratic form over the ring of integers of Q(√5). -
5 the Dirac Equation and Spinors
5 The Dirac Equation and Spinors In this section we develop the appropriate wavefunctions for fundamental fermions and bosons. 5.1 Notation Review The three dimension differential operator is : ∂ ∂ ∂ = , , (5.1) ∂x ∂y ∂z We can generalise this to four dimensions ∂µ: 1 ∂ ∂ ∂ ∂ ∂ = , , , (5.2) µ c ∂t ∂x ∂y ∂z 5.2 The Schr¨odinger Equation First consider a classical non-relativistic particle of mass m in a potential U. The energy-momentum relationship is: p2 E = + U (5.3) 2m we can substitute the differential operators: ∂ Eˆ i pˆ i (5.4) → ∂t →− to obtain the non-relativistic Schr¨odinger Equation (with = 1): ∂ψ 1 i = 2 + U ψ (5.5) ∂t −2m For U = 0, the free particle solutions are: iEt ψ(x, t) e− ψ(x) (5.6) ∝ and the probability density ρ and current j are given by: 2 i ρ = ψ(x) j = ψ∗ ψ ψ ψ∗ (5.7) | | −2m − with conservation of probability giving the continuity equation: ∂ρ + j =0, (5.8) ∂t · Or in Covariant notation: µ µ ∂µj = 0 with j =(ρ,j) (5.9) The Schr¨odinger equation is 1st order in ∂/∂t but second order in ∂/∂x. However, as we are going to be dealing with relativistic particles, space and time should be treated equally. 25 5.3 The Klein-Gordon Equation For a relativistic particle the energy-momentum relationship is: p p = p pµ = E2 p 2 = m2 (5.10) · µ − | | Substituting the equation (5.4), leads to the relativistic Klein-Gordon equation: ∂2 + 2 ψ = m2ψ (5.11) −∂t2 The free particle solutions are plane waves: ip x i(Et p x) ψ e− · = e− − · (5.12) ∝ The Klein-Gordon equation successfully describes spin 0 particles in relativistic quan- tum field theory. -
Vector Fields
Vector Calculus Independent Study Unit 5: Vector Fields A vector field is a function which associates a vector to every point in space. Vector fields are everywhere in nature, from the wind (which has a velocity vector at every point) to gravity (which, in the simplest interpretation, would exert a vector force at on a mass at every point) to the gradient of any scalar field (for example, the gradient of the temperature field assigns to each point a vector which says which direction to travel if you want to get hotter fastest). In this section, you will learn the following techniques and topics: • How to graph a vector field by picking lots of points, evaluating the field at those points, and then drawing the resulting vector with its tail at the point. • A flow line for a velocity vector field is a path ~σ(t) that satisfies ~σ0(t)=F~(~σ(t)) For example, a tiny speck of dust in the wind follows a flow line. If you have an acceleration vector field, a flow line path satisfies ~σ00(t)=F~(~σ(t)) [For example, a tiny comet being acted on by gravity.] • Any vector field F~ which is equal to ∇f for some f is called a con- servative vector field, and f its potential. The terminology comes from physics; by the fundamental theorem of calculus for work in- tegrals, the work done by moving from one point to another in a conservative vector field doesn’t depend on the path and is simply the difference in potential at the two points. -
2 Lecture 1: Spinors, Their Properties and Spinor Prodcuts
2 Lecture 1: spinors, their properties and spinor prodcuts Consider a theory of a single massless Dirac fermion . The Lagrangian is = ¯ i@ˆ . (2.1) L ⇣ ⌘ The Dirac equation is i@ˆ =0, (2.2) which, in momentum space becomes pUˆ (p)=0, pVˆ (p)=0, (2.3) depending on whether we take positive-energy(particle) or negative-energy (anti-particle) solutions of the Dirac equation. Therefore, in the massless case no di↵erence appears in equations for paprticles and anti-particles. Finding one solution is therefore sufficient. The algebra is simplified if we take γ matrices in Weyl repreentation where µ µ 0 σ γ = µ . (2.4) " σ¯ 0 # and σµ =(1,~σ) andσ ¯µ =(1, ~ ). The Pauli matrices are − 01 0 i 10 σ = ,σ= − ,σ= . (2.5) 1 10 2 i 0 3 0 1 " # " # " − # The matrix γ5 is taken to be 10 γ5 = − . (2.6) " 01# We can use the matrix γ5 to construct projection operators on to upper and lower parts of the four-component spinors U and V . The projection operators are 1 γ 1+γ Pˆ = − 5 , Pˆ = 5 . (2.7) L 2 R 2 Let us write u (p) U(p)= L , (2.8) uR(p) ! where uL(p) and uR(p) are two-component spinors. Since µ 0 pµσ pˆ = µ , (2.9) " pµσ¯ 0(p) # andpU ˆ (p) = 0, the two-component spinors satisfy the following (Weyl) equations µ µ pµσ uR(p)=0,pµσ¯ uL(p)=0. (2.10) –3– Suppose that we have a left handed spinor uL(p) that satisfies the Weyl equation. -
TASI 2008 Lectures: Introduction to Supersymmetry And
TASI 2008 Lectures: Introduction to Supersymmetry and Supersymmetry Breaking Yuri Shirman Department of Physics and Astronomy University of California, Irvine, CA 92697. [email protected] Abstract These lectures, presented at TASI 08 school, provide an introduction to supersymmetry and supersymmetry breaking. We present basic formalism of supersymmetry, super- symmetric non-renormalization theorems, and summarize non-perturbative dynamics of supersymmetric QCD. We then turn to discussion of tree level, non-perturbative, and metastable supersymmetry breaking. We introduce Minimal Supersymmetric Standard Model and discuss soft parameters in the Lagrangian. Finally we discuss several mech- anisms for communicating the supersymmetry breaking between the hidden and visible sectors. arXiv:0907.0039v1 [hep-ph] 1 Jul 2009 Contents 1 Introduction 2 1.1 Motivation..................................... 2 1.2 Weylfermions................................... 4 1.3 Afirstlookatsupersymmetry . .. 5 2 Constructing supersymmetric Lagrangians 6 2.1 Wess-ZuminoModel ............................... 6 2.2 Superfieldformalism .............................. 8 2.3 VectorSuperfield ................................. 12 2.4 Supersymmetric U(1)gaugetheory ....................... 13 2.5 Non-abeliangaugetheory . .. 15 3 Non-renormalization theorems 16 3.1 R-symmetry.................................... 17 3.2 Superpotentialterms . .. .. .. 17 3.3 Gaugecouplingrenormalization . ..... 19 3.4 D-termrenormalization. ... 20 4 Non-perturbative dynamics in SUSY QCD 20 4.1 Affleck-Dine-Seiberg -
13 the Dirac Equation
13 The Dirac Equation A two-component spinor a χ = b transforms under rotations as iθn J χ e− · χ; ! with the angular momentum operators, Ji given by: 1 Ji = σi; 2 where σ are the Pauli matrices, n is the unit vector along the axis of rotation and θ is the angle of rotation. For a relativistic description we must also describe Lorentz boosts generated by the operators Ki. Together Ji and Ki form the algebra (set of commutation relations) Ki;Kj = iεi jkJk − ε Ji;Kj = i i jkKk ε Ji;Jj = i i jkJk 1 For a spin- 2 particle Ki are represented as i Ki = σi; 2 giving us two inequivalent representations. 1 χ Starting with a spin- 2 particle at rest, described by a spinor (0), we can boost to give two possible spinors α=2n σ χR(p) = e · χ(0) = (cosh(α=2) + n σsinh(α=2))χ(0) · or α=2n σ χL(p) = e− · χ(0) = (cosh(α=2) n σsinh(α=2))χ(0) − · where p sinh(α) = j j m and Ep cosh(α) = m so that (Ep + m + σ p) χR(p) = · χ(0) 2m(Ep + m) σ (pEp + m p) χL(p) = − · χ(0) 2m(Ep + m) p 57 Under the parity operator the three-moment is reversed p p so that χL χR. Therefore if we 1 $ − $ require a Lorentz description of a spin- 2 particles to be a proper representation of parity, we must include both χL and χR in one spinor (note that for massive particles the transformation p p $ − can be achieved by a Lorentz boost).