Electron-Positron Pairs in Physics and Astrophysics
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A Study of the Effects of Pair Production and Axionlike Particle
Washington University in St. Louis Washington University Open Scholarship Arts & Sciences Electronic Theses and Dissertations Arts & Sciences Summer 8-15-2016 A Study of the Effects of Pair Production and Axionlike Particle Oscillations on Very High Energy Gamma Rays from the Crab Pulsar Avery Michael Archer Washington University in St. Louis Follow this and additional works at: https://openscholarship.wustl.edu/art_sci_etds Recommended Citation Archer, Avery Michael, "A Study of the Effects of Pair Production and Axionlike Particle Oscillations on Very High Energy Gamma Rays from the Crab Pulsar" (2016). Arts & Sciences Electronic Theses and Dissertations. 828. https://openscholarship.wustl.edu/art_sci_etds/828 This Dissertation is brought to you for free and open access by the Arts & Sciences at Washington University Open Scholarship. It has been accepted for inclusion in Arts & Sciences Electronic Theses and Dissertations by an authorized administrator of Washington University Open Scholarship. For more information, please contact [email protected]. WASHINGTON UNIVERSITY IN ST. LOUIS Department of Physics Dissertation Examination Committee: James Buckley, Chair Francesc Ferrer Viktor Gruev Henric Krawzcynski Michael Ogilvie A Study of the Effects of Pair Production and Axionlike Particle Oscillations on Very High Energy Gamma Rays from the Crab Pulsar by Avery Michael Archer A dissertation presented to the Graduate School of Arts and Sciences of Washington University in partial fulfillment of the requirements for the degree of Doctor of Philosophy August 2016 Saint Louis, Missouri copyright by Avery Michael Archer 2016 Contents List of Tablesv List of Figures vi Acknowledgments xvi Abstract xix 1 Introduction1 1.1 Gamma-Ray Astronomy............................. 1 1.2 Pulsars...................................... -
7. Gamma and X-Ray Interactions in Matter
Photon interactions in matter Gamma- and X-Ray • Compton effect • Photoelectric effect Interactions in Matter • Pair production • Rayleigh (coherent) scattering Chapter 7 • Photonuclear interactions F.A. Attix, Introduction to Radiological Kinematics Physics and Radiation Dosimetry Interaction cross sections Energy-transfer cross sections Mass attenuation coefficients 1 2 Compton interaction A.H. Compton • Inelastic photon scattering by an electron • Arthur Holly Compton (September 10, 1892 – March 15, 1962) • Main assumption: the electron struck by the • Received Nobel prize in physics 1927 for incoming photon is unbound and stationary his discovery of the Compton effect – The largest contribution from binding is under • Was a key figure in the Manhattan Project, condition of high Z, low energy and creation of first nuclear reactor, which went critical in December 1942 – Under these conditions photoelectric effect is dominant Born and buried in • Consider two aspects: kinematics and cross Wooster, OH http://en.wikipedia.org/wiki/Arthur_Compton sections http://www.findagrave.com/cgi-bin/fg.cgi?page=gr&GRid=22551 3 4 Compton interaction: Kinematics Compton interaction: Kinematics • An earlier theory of -ray scattering by Thomson, based on observations only at low energies, predicted that the scattered photon should always have the same energy as the incident one, regardless of h or • The failure of the Thomson theory to describe high-energy photon scattering necessitated the • Inelastic collision • After the collision the electron departs -
Arxiv:1809.04815V2 [Physics.Hist-Ph] 28 Jan 2020
Who discovered positron annihilation? Tim Dunker∗ (Dated: 29 January 2020) In the early 1930s, the positron, pair production, and, at last, positron annihila- tion were discovered. Over the years, several scientists have been credited with the discovery of the annihilation radiation. Commonly, Thibaud and Joliot have received credit for the discovery of positron annihilation. A conversation between Werner Heisenberg and Theodor Heiting prompted me to examine relevant publi- cations, when these were submitted and published, and how experimental results were interpreted in the relevant articles. I argue that it was Theodor Heiting— usually not mentioned at all in relevant publications—who discovered positron annihilation, and that he should receive proper credit. arXiv:1809.04815v2 [physics.hist-ph] 28 Jan 2020 ∗ tdu {at} justervesenet {dot} no 2 I. INTRODUCTION There is no doubt that the positron was discovered by Carl D. Anderson (e.g. Anderson, 1932; Hanson, 1961; Leone and Robotti, 2012) after its theoretical prediction by Paul A. M. Dirac (Dirac, 1928, 1931). Further, it is undoubted that Patrick M. S. Blackett and Giovanni P. S. Occhialini discovered pair production by taking photographs of electrons and positrons created from cosmic rays in a Wilson cloud chamber (Blackett and Occhialini, 1933). The answer to the question who experimentally discovered the reverse process—positron annihilation—has been less clear. Usually, Frédéric Joliot and Jean Thibaud receive credit for its discovery (e.g., Roqué, 1997, p. 110). Several of their contemporaries were enganged in similar research. In a letter correspondence with Werner Heisenberg Heiting and Heisenberg (1952), Theodor Heiting (see Appendix A for a rudimentary biography) claimed that it was he who discovered positron annihilation. -
Pkoduction of RELATIVISTIC ANTIHYDROGEN ATOMS by PAIR PRODUCTION with POSITRON CAPTURE*
SLAC-PUB-5850 May 1993 (T/E) PkODUCTION OF RELATIVISTIC ANTIHYDROGEN ATOMS BY PAIR PRODUCTION WITH POSITRON CAPTURE* Charles T. Munger and Stanley J. Brodsky Stanford Linear Accelerator Center, Stanford University, Stanford, California 94309 .~ and _- Ivan Schmidt _ _.._ Universidad Federico Santa Maria _. - .Casilla. 11 O-V, Valparaiso, Chile . ABSTRACT A beam of relativistic antihydrogen atoms-the bound state (Fe+)-can be created by circulating the beam of an antiproton storage ring through an internal gas target . An antiproton that passes through the Coulomb field of a nucleus of charge 2 will create e+e- pairs, and antihydrogen will form when a positron is created in a bound rather than a continuum state about the antiproton. The - cross section for this process is calculated to be N 4Z2 pb for antiproton momenta above 6 GeV/c. The gas target of Fermilab Accumulator experiment E760 has already produced an unobserved N 34 antihydrogen atoms, and a sample of _ N 760 is expected in 1995 from the successor experiment E835. No other source of antihydrogen exists. A simple method for detecting relativistic antihydrogen , - is -proposed and a method outlined of measuring the antihydrogen Lamb shift .g- ‘,. to N 1%. Submitted to Physical Review D *Work supported in part by Department of Energy contract DE-AC03-76SF00515 fSLAC’1 and in Dart bv Fondo National de InvestiPaci6n Cientifica v TecnoMcica. Chile. I. INTRODUCTION Antihydrogen, the simplest atomic bound state of antimatter, rf =, (e+$, has never. been observed. A 1on g- sought goal of atomic physics is to produce sufficient numbers of antihydrogen atoms to confirm the CPT invariance of bound states in quantum electrodynamics; for example, by verifying the equivalence of the+&/2 - 2.Py2 Lamb shifts of H and I?. -
1.3.4 Atoms and Molecules Name Symbol Definition SI Unit
1.3.4 Atoms and molecules Name Symbol Definition SI unit Notes nucleon number, A 1 mass number proton number, Z 1 atomic number neutron number N N = A - Z 1 electron rest mass me kg (1) mass of atom, ma, m kg atomic mass 12 atomic mass constant mu mu = ma( C)/12 kg (1), (2) mass excess ∆ ∆ = ma - Amu kg elementary charge, e C proton charage Planck constant h J s Planck constant/2π h h = h/2π J s 2 2 Bohr radius a0 a0 = 4πε0 h /mee m -1 Rydberg constant R∞ R∞ = Eh/2hc m 2 fine structure constant α α = e /4πε0 h c 1 ionization energy Ei J electron affinity Eea J (1) Analogous symbols are used for other particles with subscripts: p for proton, n for neutron, a for atom, N for nucleus, etc. (2) mu is equal to the unified atomic mass unit, with symbol u, i.e. mu = 1 u. In biochemistry the name dalton, with symbol Da, is used for the unified atomic mass unit, although the name and symbols have not been accepted by CGPM. Chapter 1 - 1 Name Symbol Definition SI unit Notes electronegativity χ χ = ½(Ei +Eea) J (3) dissociation energy Ed, D J from the ground state D0 J (4) from the potential De J (4) minimum principal quantum n E = -hcR/n2 1 number (H atom) angular momentum see under Spectroscopy, section 3.5. quantum numbers -1 magnetic dipole m, µ Ep = -m⋅⋅⋅B J T (5) moment of a molecule magnetizability ξ m = ξB J T-2 of a molecule -1 Bohr magneton µB µB = eh/2me J T (3) The concept of electronegativity was intoduced by L. -
Arxiv:1706.03391V2 [Astro-Ph.CO] 12 Sep 2017
Insights into neutrino decoupling gleaned from considerations of the role of electron mass E. Grohs∗ Department of Physics, University of Michigan, Ann Arbor, Michigan 48109, USA George M. Fuller Department of Physics, University of California, San Diego, La Jolla, California 92093, USA Abstract We present calculations showing how electron rest mass influences entropy flow, neutrino decoupling, and Big Bang Nucleosynthesis (BBN) in the early universe. To elucidate this physics and especially the sensitivity of BBN and related epochs to electron mass, we consider a parameter space of rest mass values larger and smaller than the accepted vacuum value. Electromagnetic equilibrium, coupled with the high entropy of the early universe, guarantees that significant numbers of electron-positron pairs are present, and dominate over the number of ionization electrons to temperatures much lower than the vacuum electron rest mass. Scattering between the electrons-positrons and the neutrinos largely controls the flow of entropy from the plasma into the neu- trino seas. Moreover, the number density of electron-positron-pair targets can be exponentially sensitive to the effective in-medium electron mass. This en- tropy flow influences the phasing of scale factor and temperature, the charged current weak-interaction-determined neutron-to-proton ratio, and the spectral distortions in the relic neutrino energy spectra. Our calculations show the sen- sitivity of the physics of this epoch to three separate effects: finite electron mass, finite-temperature quantum electrodynamic (QED) effects on the plasma equation of state, and Boltzmann neutrino energy transport. The ratio of neu- trino to plasma-component energy scales manifests in Cosmic Microwave Back- ground (CMB) observables, namely the baryon density and the radiation energy density, along with the primordial helium and deuterium abundances. -
Useful Constants
Appendix A Useful Constants A.1 Physical Constants Table A.1 Physical constants in SI units Symbol Constant Value c Speed of light 2.997925 × 108 m/s −19 e Elementary charge 1.602191 × 10 C −12 2 2 3 ε0 Permittivity 8.854 × 10 C s / kgm −7 2 μ0 Permeability 4π × 10 kgm/C −27 mH Atomic mass unit 1.660531 × 10 kg −31 me Electron mass 9.109558 × 10 kg −27 mp Proton mass 1.672614 × 10 kg −27 mn Neutron mass 1.674920 × 10 kg h Planck constant 6.626196 × 10−34 Js h¯ Planck constant 1.054591 × 10−34 Js R Gas constant 8.314510 × 103 J/(kgK) −23 k Boltzmann constant 1.380622 × 10 J/K −8 2 4 σ Stefan–Boltzmann constant 5.66961 × 10 W/ m K G Gravitational constant 6.6732 × 10−11 m3/ kgs2 M. Benacquista, An Introduction to the Evolution of Single and Binary Stars, 223 Undergraduate Lecture Notes in Physics, DOI 10.1007/978-1-4419-9991-7, © Springer Science+Business Media New York 2013 224 A Useful Constants Table A.2 Useful combinations and alternate units Symbol Constant Value 2 mHc Atomic mass unit 931.50MeV 2 mec Electron rest mass energy 511.00keV 2 mpc Proton rest mass energy 938.28MeV 2 mnc Neutron rest mass energy 939.57MeV h Planck constant 4.136 × 10−15 eVs h¯ Planck constant 6.582 × 10−16 eVs k Boltzmann constant 8.617 × 10−5 eV/K hc 1,240eVnm hc¯ 197.3eVnm 2 e /(4πε0) 1.440eVnm A.2 Astronomical Constants Table A.3 Astronomical units Symbol Constant Value AU Astronomical unit 1.4959787066 × 1011 m ly Light year 9.460730472 × 1015 m pc Parsec 2.0624806 × 105 AU 3.2615638ly 3.0856776 × 1016 m d Sidereal day 23h 56m 04.0905309s 8.61640905309 -
1 Drawing Feynman Diagrams
1 Drawing Feynman Diagrams 1. A fermion (quark, lepton, neutrino) is drawn by a straight line with an arrow pointing to the left: f f 2. An antifermion is drawn by a straight line with an arrow pointing to the right: f f 3. A photon or W ±, Z0 boson is drawn by a wavy line: γ W ±;Z0 4. A gluon is drawn by a curled line: g 5. The emission of a photon from a lepton or a quark doesn’t change the fermion: γ l; q l; q But a photon cannot be emitted from a neutrino: γ ν ν 6. The emission of a W ± from a fermion changes the flavour of the fermion in the following way: − − − 2 Q = −1 e µ τ u c t Q = + 3 1 Q = 0 νe νµ ντ d s b Q = − 3 But for quarks, we have an additional mixing between families: u c t d s b This means that when emitting a W ±, an u quark for example will mostly change into a d quark, but it has a small chance to change into a s quark instead, and an even smaller chance to change into a b quark. Similarly, a c will mostly change into a s quark, but has small chances of changing into an u or b. Note that there is no horizontal mixing, i.e. an u never changes into a c quark! In practice, we will limit ourselves to the light quarks (u; d; s): 1 DRAWING FEYNMAN DIAGRAMS 2 u d s Some examples for diagrams emitting a W ±: W − W + e− νe u d And using quark mixing: W + u s To know the sign of the W -boson, we use charge conservation: the sum of the charges at the left hand side must equal the sum of the charges at the right hand side. -
Symmetric Tensor Gauge Theories on Curved Spaces
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Caltech Authors Symmetric Tensor Gauge Theories on Curved Spaces Kevin Slagle Department of Physics, University of Toronto Toronto, Ontario M5S 1A7, Canada Department of Physics and Institute for Quantum Information and Matter California Institute of Technology, Pasadena, California 91125, USA Abhinav Prem, Michael Pretko Department of Physics and Center for Theory of Quantum Matter University of Colorado, Boulder, CO 80309 Abstract Fractons and other subdimensional particles are an exotic class of emergent quasi-particle excitations with severely restricted mobility. A wide class of models featuring these quasi-particles have a natural description in the language of symmetric tensor gauge theories, which feature conservation laws restricting the motion of particles to lower-dimensional sub-spaces, such as lines or points. In this work, we investigate the fate of symmetric tensor gauge theories in the presence of spatial curvature. We find that weak curvature can induce small (exponentially suppressed) violations on the mobility restrictions of charges, leaving a sense of asymptotic fractonic/sub-dimensional behavior on generic manifolds. Nevertheless, we show that certain symmetric tensor gauge theories maintain sharp mobility restrictions and gauge invariance on certain special curved spaces, such as Einstein manifolds or spaces of constant curvature. Contents 1 Introduction 2 2 Review of Symmetric Tensor Gauge Theories3 2.1 Scalar Charge Theory . .3 2.2 Traceless Scalar Charge Theory . .4 2.3 Vector Charge Theory . .4 2.4 Traceless Vector Charge Theory . .5 3 Curvature-Induced Violation of Mobility Restrictions6 4 Robustness of Fractons on Einstein Manifolds8 4.1 Traceless Scalar Charge Theory . -
Worldline Sphaleron for Thermal Schwinger Pair Production
IMPERIAL-TP-2018-OG-1 HIP-2018-17-TH Worldline sphaleron for thermal Schwinger pair production Oliver Gould,1, 2, ∗ Arttu Rajantie,1, y and Cheng Xie1, z 1Department of Physics, Imperial College London, SW7 2AZ, UK 2Helsinki Institute of Physics, University of Helsinki, FI-00014, Finland (Dated: August 24, 2018) With increasing temperatures, Schwinger pair production changes from a quantum tunnelling to a classical, thermal process, determined by a worldline sphaleron. We show this and calculate the corresponding rate of pair production for both spinor and scalar quantum electrodynamics, including the semiclassical prefactor. For electron-positron pair production from a thermal bath of photons and in the presence of an electric field, the rate we derive is faster than both perturbative photon fusion and the zero temperature Schwinger process. We work to all-orders in the coupling and hence our results are also relevant to the pair production of (strongly coupled) magnetic monopoles in heavy-ion collisions. I. INTRODUCTION Schwinger rate, Γ(E; T ), takes the form, 1 In non-Abelian gauge theories, sphaleron processes, X Γ(E; T ) = c h(J · A)ni; (1) or thermal over-barrier transitions, have long been un- n derstood to dominate over quantum tunnelling transi- n=0 1 tions at high enough temperatures [1{4] . The same is where E is the magnitude of the electric field and T is true, for example, in gravitational theories [5]. On the the temperature. The leading term, c0, gives the one loop other hand, sphalerons have been conspicuously absent result, that of Schwinger [6], at zero temperature. -
International Centre for Theoretical Physics
IC/95/253 INTERNATIONAL CENTRE FOR THEORETICAL PHYSICS LOCALIZED STRUCTURES OF ELECTROMAGNETIC WAVES IN HOT ELECTRON-POSITRON PLASMA S. Kartal L.N. Tsintsadze and V.I. Berezhiani MIRAMARE-TRIESTE y s. - - INTERNATIONAL ATOMIC ENERGY £ ,. AGENCY .v ^^ ^ UNITED NATIONS T " ; . EDUCATIONAL, i r' * SCI ENTI FIC- * -- AND CULTURAL j * - ORGANIZATION VOL 2 7 Ni 0 6 IC/95/253 International Atomic Energy Agency and United Nations Educational Scientific and Cultural Organization INTERNATIONAL CENTRE FOR THEORETICAL PHYSICS LOCALIZED STRUCTURES OF ELECTROMAGNETIC WAVES IN HOT ELECTRON-POSITRON PLASMA ' S. K'urtaF, L.N. Tsiiitsacfzc'' ancf V./. fiercz/iiani International Centre for Theoretical Physics, Trieste, Italy. ABSTRACT The dynamics of relativistically strong electromagnetic (EM) wave propagation in hot electron-positron plasma is investigated. The possibility of finding localized stationary structures of EM waves is explored. It is shown that under certain conditions the EM wave forms a stable localized soliton-like structures where plasma is completely expelled from the region of EM field location. MIRAMARE TRIESTE August 1995 'Submitted to Physical Review E. 'Permanent address; University ofT ', inbul, Department of Physics, 34459, Vezneciler- Istanbul, Turkey. 3Present address: Faculty of Science, Hiroshima University, Hiroshima 739, Japan. Permanent address: Institute of Physics, The Georgian Academy of Science, Tbilisi 380077, Republic of Georgia. During the last few years a considerable amount of work has been de- voted to the analysis of nonlinear electromagnetic (EM) wave propagation in electron-positron (e-p) plasmas [I]. Electron- positron pairs are thought to be a major constituent of the plasma emanating both from the pulsars and from inner region of the accretion disks surrounding the central black holes in the active galactic nuclei (AGN) [2]. -
Chapter 6. Maxwell Equations, Macroscopic Electromagnetism, Conservation Laws
Chapter 6. Maxwell Equations, Macroscopic Electromagnetism, Conservation Laws 6.1 Displacement Current The magnetic field due to a current distribution satisfies Ampere’s law, (5.45) Using Stokes’s theorem we can transform this equation into an integral form: ∮ ∫ (5.47) We shall examine this law, show that it sometimes fails, and find a generalization that is always valid. Magnetic field near a charging capacitor loop C Fig 6.1 parallel plate capacitor Consider the circuit shown in Fig. 6.1, which consists of a parallel plate capacitor being charged by a constant current . Ampere’s law applied to the loop C and the surface leads to ∫ ∫ (6.1) If, on the other hand, Ampere’s law is applied to the loop C and the surface , we find (6.2) ∫ ∫ Equations 6.1 and 6.2 contradict each other and thus cannot both be correct. The origin of this contradiction is that Ampere’s law is a faulty equation, not consistent with charge conservation: (6.3) ∫ ∫ ∫ ∫ 1 Generalization of Ampere’s law by Maxwell Ampere’s law was derived for steady-state current phenomena with . Using the continuity equation for charge and current (6.4) and Coulombs law (6.5) we obtain ( ) (6.6) Ampere’s law is generalized by the replacement (6.7) i.e., (6.8) Maxwell equations Maxwell equations consist of Eq. 6.8 plus three equations with which we are already familiar: (6.9) 6.2 Vector and Scalar Potentials Definition of and Since , we can still define in terms of a vector potential: (6.10) Then Faradays law can be written ( ) The vanishing curl means that we can define a scalar potential satisfying (6.11) or (6.12) 2 Maxwell equations in terms of vector and scalar potentials and defined as Eqs.