Resonances in Subatomic Physics
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Quantum Phase Space in Relativistic Theory: the Case of Charge-Invariant Observables
Proceedings of Institute of Mathematics of NAS of Ukraine 2004, Vol. 50, Part 3, 1448–1453 Quantum Phase Space in Relativistic Theory: the Case of Charge-Invariant Observables A.A. SEMENOV †, B.I. LEV † and C.V. USENKO ‡ † Institute of Physics of NAS of Ukraine, 46 Nauky Ave., 03028 Kyiv, Ukraine E-mail: [email protected], [email protected] ‡ Physics Department, Taras Shevchenko Kyiv University, 6 Academician Glushkov Ave., 03127 Kyiv, Ukraine E-mail: [email protected] Mathematical method of quantum phase space is very useful in physical applications like quantum optics and non-relativistic quantum mechanics. However, attempts to generalize it for the relativistic case lead to some difficulties. One of problems is band structure of energy spectrum for a relativistic particle. This corresponds to an internal degree of freedom, so- called charge variable. In physical problems we often deal with such dynamical variables that do not depend on this degree of freedom. These are position, momentum, and any combination of them. Restricting our consideration to this kind of observables we propose the relativistic Weyl–Wigner–Moyal formalism that contains some surprising differences from its non-relativistic counterpart. This paper is devoted to the phase space formalism that is specific representation of quan- tum mechanics. This representation is very close to classical mechanics and its basic idea is a description of quantum observables by means of functions in phase space (symbols) instead of operators in the Hilbert space of states. The first idea about this representation has been proposed in the early days of quantum mechanics in the well-known Weyl work [1]. -
Spacetime Diagrams(1D in Space)
PH300 Modern Physics SP11 Last time: • Time dilation and length contraction Today: • Spacetime • Addition of velocities • Lorentz transformations Thursday: • Relativistic momentum and energy “The only reason for time is so that HW03 due, beginning of class; HW04 assigned everything doesn’t happen at once.” 2/1 Day 6: Next week: - Albert Einstein Questions? Intro to quantum Spacetime Thursday: Exam I (in class) Addition of Velocities Relativistic Momentum & Energy Lorentz Transformations 1 2 Spacetime Diagrams (1D in space) Spacetime Diagrams (1D in space) c · t In PHYS I: v In PH300: x x x x Δx Δx v = /Δt Δt t t Recall: Lucy plays with a fire cracker in the train. (1D in space) Spacetime Diagrams Ricky watches the scene from the track. c· t In PH300: object moving with 0<v<c. ‘Worldline’ of the object L R -2 -1 0 1 2 x object moving with 0>v>-c v c·t c·t Lucy object at rest object moving with v = -c. at x=1 x=0 at time t=0 -2 -1 0 1 2 x -2 -1 0 1 2 x Ricky 1 Example: Ricky on the tracks Example: Lucy in the train ct ct Light reaches both walls at the same time. Light travels to both walls Ricky concludes: Light reaches left side first. x x L R L R Lucy concludes: Light reaches both sides at the same time In Ricky’s frame: Walls are in motion In Lucy’s frame: Walls are at rest S Frame S’ as viewed from S ... -3 -2 -1 0 1 2 3 .. -
Reflection Invariant and Symmetry Detection
1 Reflection Invariant and Symmetry Detection Erbo Li and Hua Li Abstract—Symmetry detection and discrimination are of fundamental meaning in science, technology, and engineering. This paper introduces reflection invariants and defines the directional moments(DMs) to detect symmetry for shape analysis and object recognition. And it demonstrates that detection of reflection symmetry can be done in a simple way by solving a trigonometric system derived from the DMs, and discrimination of reflection symmetry can be achieved by application of the reflection invariants in 2D and 3D. Rotation symmetry can also be determined based on that. Also, if none of reflection invariants is equal to zero, then there is no symmetry. And the experiments in 2D and 3D show that all the reflection lines or planes can be deterministically found using DMs up to order six. This result can be used to simplify the efforts of symmetry detection in research areas,such as protein structure, model retrieval, reverse engineering, and machine vision etc. Index Terms—symmetry detection, shape analysis, object recognition, directional moment, moment invariant, isometry, congruent, reflection, chirality, rotation F 1 INTRODUCTION Kazhdan et al. [1] developed a continuous measure and dis- The essence of geometric symmetry is self-evident, which cussed the properties of the reflective symmetry descriptor, can be found everywhere in nature and social lives, as which was expanded to 3D by [2] and was augmented in shown in Figure 1. It is true that we are living in a spatial distribution of the objects asymmetry by [3] . For symmetric world. Pursuing the explanation of symmetry symmetry discrimination [4] defined a symmetry distance will provide better understanding to the surrounding world of shapes. -
Basic Four-Momentum Kinematics As
L4:1 Basic four-momentum kinematics Rindler: Ch5: sec. 25-30, 32 Last time we intruduced the contravariant 4-vector HUB, (II.6-)II.7, p142-146 +part of I.9-1.10, 154-162 vector The world is inconsistent! and the covariant 4-vector component as implicit sum over We also introduced the scalar product For a 4-vector square we have thus spacelike timelike lightlike Today we will introduce some useful 4-vectors, but rst we introduce the proper time, which is simply the time percieved in an intertial frame (i.e. time by a clock moving with observer) If the observer is at rest, then only the time component changes but all observers agree on ✁S, therefore we have for an observer at constant speed L4:2 For a general world line, corresponding to an accelerating observer, we have Using this it makes sense to de ne the 4-velocity As transforms as a contravariant 4-vector and as a scalar indeed transforms as a contravariant 4-vector, so the notation makes sense! We also introduce the 4-acceleration Let's calculate the 4-velocity: and the 4-velocity square Multiplying the 4-velocity with the mass we get the 4-momentum Note: In Rindler m is called m and Rindler's I will always mean with . which transforms as, i.e. is, a contravariant 4-vector. Remark: in some (old) literature the factor is referred to as the relativistic mass or relativistic inertial mass. L4:3 The spatial components of the 4-momentum is the relativistic 3-momentum or simply relativistic momentum and the 0-component turns out to give the energy: Remark: Taylor expanding for small v we get: rest energy nonrelativistic kinetic energy for v=0 nonrelativistic momentum For the 4-momentum square we have: As you may expect we have conservation of 4-momentum, i.e. -
Newton's Laws
Newton’s Laws First Law A body moves with constant velocity unless a net force acts on the body. Second Law The rate of change of momentum of a body is equal to the net force applied to the body. Third Law If object A exerts a force on object B, then object B exerts a force on object A. These have equal magnitude but opposite direction. Newton’s second law The second law should be familiar: F = ma where m is the inertial mass (a scalar) and a is the acceleration (a vector). Note that a is the rate of change of velocity, which is in turn the rate of change of displacement. So d d2 a = v = r dt dt2 which, in simplied notation is a = v_ = r¨ The principle of relativity The principle of relativity The laws of nature are identical in all inertial frames of reference An inertial frame of reference is one in which a freely moving body proceeds with uniform velocity. The Galilean transformation - In Newtonian mechanics, the concepts of space and time are completely separable. - Time is considered an absolute quantity which is independent of the frame of reference: t0 = t. - The laws of mechanics are invariant under a transformation of the coordinate system. u y y 0 S S 0 x x0 Consider two inertial reference frames S and S0. The frame S0 moves at a velocity u relative to the frame S along the x axis. The trans- formation of the coordinates of a point is, therefore x0 = x − ut y 0 = y z0 = z The above equations constitute a Galilean transformation u y y 0 S S 0 x x0 These equations are linear (as we would hope), so we can write the same equations for changes in each of the coordinates: ∆x0 = ∆x − u∆t ∆y 0 = ∆y ∆z0 = ∆z u y y 0 S S 0 x x0 For moving particles, we need to know how to transform velocity, v, and acceleration, a, between frames. -
The Velocity and Momentum Four-Vectors
Physics 171 Fall 2015 The velocity and momentum four-vectors 1. The four-velocity vector The velocity four-vector of a particle is defined by: dxµ U µ = =(γc ; γ~v ) , (1) dτ where xµ = (ct ; ~x) is the four-position vector and dτ is the differential proper time. To derive eq. (1), we must express dτ in terms of dt, where t is the time coordinate. Consider the infinitesimal invariant spacetime separation, 2 2 2 µ ν ds = −c dτ = ηµν dx dx , (2) in a convention where ηµν = diag(−1 , 1 , 1 , 1) . In eq. (2), there is an implicit sum over the repeated indices as dictated by the Einstein summation convention. Dividing by −c2 yields 3 1 c2 − v2 v2 dτ 2 = c2dt2 − dxidxi = dt2 = 1 − dt2 = γ−2dt2 , c2 c2 c2 i=1 ! X i i 2 i i where we have employed the three-velocity v = dx /dt and v ≡ i v v . In the last step we have introduced γ ≡ (1 − v2/c2)−1/2. It follows that P dτ = γ−1 dt . (3) Using eq. (3) and the definition of the three-velocity, ~v = d~x/dt, we easily obtain eq. (1). Note that the squared magnitude of the four-velocity vector, 2 µ ν 2 U ≡ ηµνU U = −c (4) is a Lorentz invariant, which is most easily evaluated in the rest frame of the particle where ~v = 0, in which case U µ = c (1 ; ~0). 2. The relativistic law of addition of velocities Let us now consider the following question. -
Uniform Relativistic Acceleration
Uniform Relativistic Acceleration Benjamin Knorr June 19, 2010 Contents 1 Transformation of acceleration between two reference frames 1 2 Rindler Coordinates 4 2.1 Hyperbolic motion . .4 2.2 The uniformly accelerated reference frame - Rindler coordinates .5 3 Some applications of accelerated motion 8 3.1 Bell's spaceship . .8 3.2 Relation to the Schwarzschild metric . 11 3.3 Black hole thermodynamics . 12 1 Abstract This paper is based on a talk I gave by choice at 06/18/10 within the course Theoretical Physics II: Electrodynamics provided by PD Dr. A. Schiller at Uni- versity of Leipzig in the summer term of 2010. A basic knowledge in special relativity is necessary to be able to understand all argumentations and formulae. First I shortly will revise the transformation of velocities and accelerations. It follows some argumentation about the hyperbolic path a uniformly accelerated particle will take. After this I will introduce the Rindler coordinates. Lastly there will be some examples and (probably the most interesting part of this paper) an outlook of acceleration in GRT. The main sources I used for information are Rindler, W. Relativity, Oxford University Press, 2006, and arXiv:0906.1919v3. Chapter 1 Transformation of acceleration between two reference frames The Lorentz transformation is the basic tool when considering more than one reference frames in special relativity (SR) since it leaves the speed of light c invariant. Between two different reference frames1 it is given by x = γ(X − vT ) (1.1) v t = γ(T − X ) (1.2) c2 By the equivalence -
Decay Rates and Cross Section
Decay rates and Cross section Ashfaq Ahmad National Centre for Physics Outlines Introduction Basics variables used in Exp. HEP Analysis Decay rates and Cross section calculations Summary 11/17/2014 Ashfaq Ahmad 2 Standard Model With these particles we can explain the entire matter, from atoms to galaxies In fact all visible stable matter is made of the first family, So Simple! Many Nobel prizes have been awarded (both theory/Exp. side) 11/17/2014 Ashfaq Ahmad 3 Standard Model Why Higgs Particle, the only missing piece until July 2012? In Standard Model particles are massless =>To explain the non-zero mass of W and Z bosons and fermions masses are generated by the so called Higgs mechanism: Quarks and leptons acquire masses by interacting with the scalar Higgs field (amount coupling strength) 11/17/2014 Ashfaq Ahmad 4 Fundamental Fermions 1st generation 2nd generation 3rd generation Dynamics of fermions described by Dirac Equation 11/17/2014 Ashfaq Ahmad 5 Experiment and Theory It doesn’t matter how beautiful your theory is, it doesn’t matter how smart you are. If it doesn’t agree with experiment, it’s wrong. Richard P. Feynman A theory is something nobody believes except the person who made it, An experiment is something everybody believes except the person who made it. Albert Einstein 11/17/2014 Ashfaq Ahmad 6 Some Basics Mandelstam Variables In a two body scattering process of the form 1 + 2→ 3 + 4, there are 4 four-vectors involved, namely pi (i =1,2,3,4) = (Ei, pi) Three Lorentz Invariant variables namely s, t and u are defined. -
Introduction to General Relativity
Introduction to General Relativity Janos Polonyi University of Strasbourg, Strasbourg, France (Dated: September 21, 2021) Contents I. Introduction 5 A. Equivalence principle 5 B. Gravitation and geometry 6 C. Static gravitational field 8 D. Classical field theories 9 II. Gauge theories 12 A. Global symmetries 12 B. Local symmetries 13 C. Gauging 14 D. Covariant derivative 16 E. Parallel transport 17 F. Field strength tensor 19 G. Classical electrodynamics 21 III. Gravity 22 A. Classical field theory on curved space-time 22 B. Geometry 25 C. Gauge group 26 1. Space-time diffeomorphism 26 2. Internal Poincar´egroup 27 D. Gauge theory of diffeomorphism 29 1. Covariant derivative 29 2. Lie derivative 32 3. Field strength tensor 32 2 E. Metric admissibility 34 F. Invariant integral 36 G. Dynamics 39 IV. Coupling to matter 42 A. Point particle in an external gravitational field 42 1. Equivalence Principle 42 2. Spin precession 43 3. Variational equation of motion 44 4. Geodesic deviation 45 5. Newtonian limit 46 B. Interacting matter-gravity system 47 1. Point particle 47 2. Ideal fluid 48 3. Classical fields 49 V. Gravitational radiation 49 A. Linearization 50 B. Wave equation 51 C. Plane-waves 52 D. Polarization 52 VI. Schwarzschild solution 54 A. Metric 54 B. Geodesics 59 C. Space-like hyper-surfaces 61 D. Around the Schwarzschild-horizon 62 1. Falling through the horizon 62 2. Stretching the horizon 63 3. Szekeres-Kruskall coordinate system 64 4. Causal structure 67 VII. Homogeneous and isotropic cosmology 68 A. Maximally symmetric spaces 69 3 B. Robertson-Walker metric 70 C. -
Should Physical Laws Be Unit-Invariant?
Should physical laws be unit-invariant? 1. Introduction In a paper published in this journal in 2015, Sally Riordan reviews a recent debate about whether fundamental constants are really “constant”, or whether they may change over cosmological timescales. Her context is the impending redefinition of the kilogram and other units in terms of fundamental constants – a practice which is seen as more “objective” than defining units in terms of human artefacts. She focusses on one particular constant, the fine structure constant (α), for which some evidence of such a variation has been reported. Although α is not one of the fundamental constants involved in the proposed redefinitions, it is linked to some which are, so that there is a clear cause for concern. One of the authors she references is Michael Duff, who presents an argument supporting his assertion that dimensionless constants are more fundamental than dimensioned ones; this argument employs various systems of so-called “natural units”. [see Riordan (2015); Duff (2004)] An interesting feature of this discussion is that not only Riordan herself, but all the papers she cites, use a formula for α that is valid only in certain systems of units, and would not feature in a modern physics textbook. This violates another aspect of objectivity – namely, the idea that our physical laws should be expressed in such a way that they are independent of the particular units we choose to use; they should be unit-invariant. In this paper I investigate the place of unit-invariance in the history of physics, together with its converse, unit-dependence, which we will find is a common feature of some branches of physics, despite the fact that, as I will show in an analysis of Duff’s argument, unit-dependent formulae can lead to erroneous conclusions. -
Relativistic Kinematics & Dynamics Momentum and Energy
Physics 106a, Caltech | 3 December, 2019 Lecture 18 { Relativistic kinematics & dynamics Momentum and energy Our discussion of 4-vectors in general led us to the energy-momentum 4-vector p with components in some inertial frame (E; ~p) = (mγu; mγu~u) with ~u the velocity of the particle in that inertial 2 −1=2 1 2 frame and γu = (1 − u ) . The length-squared of the 4-vector is (since u = 1) p2 = m2 = E2 − p2 (1) where the last expression is the evaluation in some inertial frame and p = j~pj. In conventional units this is E2 = p2c2 + m2c4 : (2) For a light particle (photon) m = 0 and so E = p (going back to c = 1). Thus the energy-momentum 4-vector for a photon is E(1; n^) withn ^ the direction of propagation. This is consistent with the quantum expressions E = hν; ~p = (h/λ)^n with ν the frequency and λ the wave length, and νλ = 1 (the speed of light) We are led to the expression for the relativistic 3-momentum and energy m~u m ~p = p ;E = p : (3) 1 − u2 1 − u2 Note that ~u = ~p=E. The frame independent statement that the energy-momentum 4-vector is conserved leads to the conservation of this 3-momentum and energy in each inertial frame, with the new implication that mass can be converted to and from energy. Since (E; ~p) form the components of a 4-vector they transform between inertial frames in the same way as (t; ~x), i.e. in our standard configuration 0 px = γ(px − vE) (4) 0 py = py (5) 0 pz = pz (6) 0 E = γ(E − vpx) (7) and the inverse 0 0 px = γ(px + vE ) (8) 0 py = py (9) 0 pz = pz (10) 0 0 E = γ(E + vpx) (11) These reduce to the Galilean expressions for small particle speeds and small transformation speeds. -
Relativistic Kinematics of Particle Interactions Introduction
le kin rel.tex Relativistic Kinematics of Particle Interactions byW von Schlipp e, March2002 1. Notation; 4-vectors, covariant and contravariant comp onents, metric tensor, invariants. 2. Lorentz transformation; frequently used reference frames: Lab frame, centre-of-mass frame; Minkowski metric, rapidity. 3. Two-b o dy decays. 4. Three-b o dy decays. 5. Particle collisions. 6. Elastic collisions. 7. Inelastic collisions: quasi-elastic collisions, particle creation. 8. Deep inelastic scattering. 9. Phase space integrals. Intro duction These notes are intended to provide a summary of the essentials of relativistic kinematics of particle reactions. A basic familiarity with the sp ecial theory of relativity is assumed. Most derivations are omitted: it is assumed that the interested reader will b e able to verify the results, which usually requires no more than elementary algebra. Only the phase space calculations are done in some detail since we recognise that they are frequently a bit of a struggle. For a deep er study of this sub ject the reader should consult the monograph on particle kinematics byByckling and Ka jantie. Section 1 sets the scene with an intro duction of the notation used here. Although other notations and conventions are used elsewhere, I present only one version which I b elieveto b e the one most frequently encountered in the literature on particle physics, notably in such widely used textb o oks as Relativistic Quantum Mechanics by Bjorken and Drell and in the b o oks listed in the bibliography. This is followed in section 2 by a brief discussion of the Lorentz transformation.