Pkoduction of RELATIVISTIC ANTIHYDROGEN ATOMS by PAIR PRODUCTION with POSITRON CAPTURE*
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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. -
Electron-Positron Pairs in Physics and Astrophysics
Electron-positron pairs in physics and astrophysics: from heavy nuclei to black holes Remo Ruffini1,2,3, Gregory Vereshchagin1 and She-Sheng Xue1 1 ICRANet and ICRA, p.le della Repubblica 10, 65100 Pescara, Italy, 2 Dip. di Fisica, Universit`adi Roma “La Sapienza”, Piazzale Aldo Moro 5, I-00185 Roma, Italy, 3 ICRANet, Universit´ede Nice Sophia Antipolis, Grand Chˆateau, BP 2135, 28, avenue de Valrose, 06103 NICE CEDEX 2, France. Abstract Due to the interaction of physics and astrophysics we are witnessing in these years a splendid synthesis of theoretical, experimental and observational results originating from three fundamental physical processes. They were originally proposed by Dirac, by Breit and Wheeler and by Sauter, Heisenberg, Euler and Schwinger. For almost seventy years they have all three been followed by a continued effort of experimental verification on Earth-based experiments. The Dirac process, e+e 2γ, has been by − → far the most successful. It has obtained extremely accurate experimental verification and has led as well to an enormous number of new physics in possibly one of the most fruitful experimental avenues by introduction of storage rings in Frascati and followed by the largest accelerators worldwide: DESY, SLAC etc. The Breit–Wheeler process, 2γ e+e , although conceptually simple, being the inverse process of the Dirac one, → − has been by far one of the most difficult to be verified experimentally. Only recently, through the technology based on free electron X-ray laser and its numerous applications in Earth-based experiments, some first indications of its possible verification have been reached. The vacuum polarization process in strong electromagnetic field, pioneered by Sauter, Heisenberg, Euler and Schwinger, introduced the concept of critical electric 2 3 field Ec = mec /(e ). -
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. -
Gamma-Ray Pulsars: Models and Predictions
Gamma-Ray Pulsars: Models and Predictions Alice K. Harding NASA Goddard Space Flight Center, Greenbelt MD 20771, USA Abstract. Pulsed emission from γ-ray pulsars originates inside the magnetosphere, from radiation by charged particles accelerated near the magnetic poles or in the outer gaps. In polar cap models, the high energy spectrum is cut off by magnetic pair production above an energy that is dependent on the local magnetic field strength. While most young pulsars with surface fields in the range B =1012 1013 G are expected to have high energy cutoffs around several GeV, the gamma-ray− spectra of old pulsars having lower surface fields may extend to 50 GeV. Although the gamma- ray emission of older pulsars is weaker, detecting pulsed emission at high energies from nearby sources would be an important confirmation of polar cap models. Outer gap models predict more gradual high-energy turnovers at around 10 GeV, but also predict an inverse Compton component extending to TeV energies. Detection of pulsed TeV emission, which would not survive attenuation at the polar caps, is thus an important test of outer gap models. Next-generation gamma-ray telescopes sensitive to GeV-TeV emission will provide critical tests of pulsar acceleration and emission mechanisms. INTRODUCTION The last decade has seen a large increase in the number of detected γ-ray pulsars. At GeV energies, the number has grown from two to at least six (and possibly nine) pulsar detections by the EGRET telescope on the Compton Gamma Ray Obser- vatory (CGRO) (Thompson 2000). However, even with the advance of imaging Cherenkov telescopes in both northern and southern hemispheres, the number of detections of pulsed emission at energies above 20 GeV (Weekes et al. -
Charm Meson Molecules and the X(3872)
Charm Meson Molecules and the X(3872) DISSERTATION Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Masaoki Kusunoki, B.S. ***** The Ohio State University 2005 Dissertation Committee: Approved by Professor Eric Braaten, Adviser Professor Richard J. Furnstahl Adviser Professor Junko Shigemitsu Graduate Program in Professor Brian L. Winer Physics Abstract The recently discovered resonance X(3872) is interpreted as a loosely-bound S- wave charm meson molecule whose constituents are a superposition of the charm mesons D0D¯ ¤0 and D¤0D¯ 0. The unnaturally small binding energy of the molecule implies that it has some universal properties that depend only on its binding energy and its width. The existence of such a small energy scale motivates the separation of scales that leads to factorization formulas for production rates and decay rates of the X(3872). Factorization formulas are applied to predict that the line shape of the X(3872) differs significantly from that of a Breit-Wigner resonance and that there should be a peak in the invariant mass distribution for B ! D0D¯ ¤0K near the D0D¯ ¤0 threshold. An analysis of data by the Babar collaboration on B ! D(¤)D¯ (¤)K is used to predict that the decay B0 ! XK0 should be suppressed compared to B+ ! XK+. The differential decay rates of the X(3872) into J=Ã and light hadrons are also calculated up to multiplicative constants. If the X(3872) is indeed an S-wave charm meson molecule, it will provide a beautiful example of the predictive power of universality. -
Antineutron Oscillation Theory
RecentRecent ProgressProgress inin Neutron-Neutron- AntineutronAntineutron OscillationOscillation TheoryTheory MichaelMichael WagmanWagman (UW/INT)(UW/INT) QuarkQuark ConfinementConfinement andand thethe HadronHadron SpectrumSpectrum XIIXII withwith MichaelMichael Buchoff,Buchoff, EnricoEnrico Rinaldi,Rinaldi, ChrisChris Schroeder,Schroeder, andand JoeJoe WasemWasem (LLNL),(LLNL), andand SergeySergey SyritsynSyritsyn (Jefferson(Jefferson Lab/StonyLab/Stony Brook)Brook) 1 Neutron-Antineutron Oscillations violates fundamental symmetries of baryon number and , sensitive to different physics than proton decay Testable signature of possible BSM baryogenesis mechanisms explaining matter-antimatter asymmetry 2 Neutron-Antineutron Phenomenology Similarities to kaon, neutrino oscillations Magnetic fields, nuclear interactions modify transition rate Mohapatra (2009) 3 Experimental Constraints 4 Experimental Outlook European Spallation Source could have 1000 times ILL sensitivity, probe 30 times higher within next decade 5 Neutron-Antineutron Theory: The Standard Model and Beyond Theory must make robust predictions for to reliably interpret the constraints from these experiments Lattice QCD Renormalization Group BSM QCD max lattice BSM strong resolution physics? 6 Baryogenesis Baryon asymmetry and produced by same interactions in several BSM theories Post-sphaleron baryogenesis in e.g. left-right symmetric theories predicts there is a theoretical upper bound on Babu, Dev, Fortes, and Mohapatra (2013) Planck Mohapatra and Marshak (1980) 7 Six-Quark -
Neutron-Antineutron Oscillations: Theoretical Status and Experimental Prospects
Neutron-Antineutron Oscillations: Theoretical Status and Experimental Prospects D. G. Phillips IIo,x, W. M. Snowe,b,∗, K. Babur, S. Banerjeeu, D. V. Baxtere,b, Z. Berezhianii,y, M. Bergevinz, S. Bhattacharyau, G. Brooijmansc, L. Castellanosaf, M-C. Chenaa, C. E. Coppolaag, R. Cowsikai, J. A. Crabtreeq, P. Dasah, E. B. Deeso,x, A. Dolgovg,p,ab, P. D. Fergusonq, M. Frostag, T. Gabrielag, A. Galt, F. Gallmeierq, K. Ganezera, E. Golubevaf, G. Greeneag, B. Hartfiela, A. Hawarin, L. Heilbronnaf, C. Johnsone, Y. Kamyshkovag, B. Kerbikovg,k, M. Kitaguchil, B. Z. Kopeliovichae, V. B. Kopeliovichf,k, V. A. Kuzminf, C-Y. Liue,b, P. McGaugheyj, M. Mockoj, R. Mohapatraac, N. Mokhovd, G. Muhrerj, H. P. Mummm, L. Okung, R. W. Pattie Jr.o,x, C. Quiggd, E. Rambergd, A. Rayah, A. Royh, A. Rugglesaf, U. Sarkars, A. Saundersj, A. P. Serebrovv, H. M. Shimizul, R. Shrockw, A. K. Sikdarah, S. Sjuej, S. Striganovd, L. W. Townsendaf, R. Tschirhartd, A. Vainshteinad, R. Van Kootene, Z. Wangj, A. R. Youngo,x aCalifornia State University, Dominguez Hills, Department of Physics, 1000 E. Victoria St., NSMB-202, Carson, CA 90747, USA bCenter for the Exploration of Energy and Matter, 2401 Milo B. Sampson Lane, Bloomington, IN 47408, USA cColumbia University, Department of Physics, 538 West 120th St., 704 Pupin Hall, MC 5255, New York, NY 10027, USA dFermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA eIndiana University, Department of Physics, 727 E. Third St., Swain Hall West, Room 117, Bloomington, IN 47405, USA fInstitute for Nuclear Research, Russian Academy of Sciences, Prospekt 60-letiya Oktyabrya 7a, Moscow 117312, Russia gInstitute of Theoretical and Experimental Physics, Bolshaya Cheremushkinskaya ul. -
A Pair Production Telescope for Medium-Energy Gamma-Ray Polarimetry
1 A Pair Production Telescope for Medium-Energy Gamma-Ray Polarimetry Stanley D. Hunter 1a, Peter F. Bloser b, Gerardo O. Depaola c, Michael P. Dion d, Georgia A. DeNolfo a, Andrei Hanu a, Marcos Iparraguirre c, Jason Legere b, Francesco Longo e, Mark L. McConnell b, Suzanne F. Nowicki a,f, James M. Ryan b, Seunghee Son a,f, and Floyd W. Stecker a a NASA/Goddard Space Flight Center, Greenbelt Road, Greenbelt, MD 20771 b Space Science Center, University of New Hampshire, Durham, NH 03824 c Facultad de Matemática, Astronomía y Fisica, Universidad de Córdoba, Córdoba 5008 Argentina d Pacific Northwest National Laboratory, Richland, WA 99352 e Dipartimento di fisica, Università Degli Studi de Trieste, Treste Italy f Department of Physics, University of Maryland Baltimore County, Baltimore, MD 21250 ABSTRACT We describe the science motivation and development of a pair production telescope for medium- energy (~5-200 MeV) gamma-ray polarimetry. Our instrument concept, the Advanced Energetic Pair Telescope (AdEPT), takes advantage of the Three-Dimensional Track Imager, a low-density gaseous time projection chamber, to achieve angular resolution within a factor of two of the pair production kinematics limit (~0.6 ° at 70 MeV), continuum sensitivity comparable with the Fermi-LAT front detector (<3 ×10 -6 MeV cm -2 s-1 at 70 MeV), and minimum detectable polarization less than 10% for a 10 mCrab source in 10 6 seconds. Keywords: gamma rays, telescope, pair production, angular resolution, polarimetry, sensitivity, time projection chamber, astrophysics 1Corresponding author at: NASA/GSFC, Code 661, Greenbelt, MD 20771, USA. Tel: +1 301 286-7280; fax +1 301 286-0677, E-mail address : [email protected] phone; 2 1. -
An Analysis Methodology for the Gamma-Ray Large Area Space Telescope
An Analysis Methodology for the Gamma-ray Large Area Space Telescope Robin D. Moms" and Johann Cohen-Tanugi' *RIACS,NASA Ames Research Centec MS 269-2, Moffett Field, CA 94035, USA, [email protected] ?Istituto Nazionale di Fisica Nucleare, Pisa, Italy, johann . cohengpi . infn . i t Abstract. The Large Area Telescope CAT) instrument on the Gama Ray Large Area Space Telescope (GLAST) has been designed to detect high-energy gamma rays and 'determine their direction of incidence and energy. We propose a reconstruction algorithmbased on recent advances in statistical methodology. This method, alternative to the standard event analysis inherited from high energy collider physics experiments, incorporates more accurately the physical processes occurring in the detector, and makes full use of the statistical information available. It could thus provide a better estimate of the direction and energy of the primary photon. INTRODUCTION Gamma rays are produced by some of the highest energy events in the universe, and their study is critical to understanding the source locations and production mechanisms of ultra-relativistic cosmic particles [ 1, and refs therein]. The LAT instrument on the Gamma Ray Large Area Space Telescope (GLAST) satellite is scheduled for launch in late 2006. Its goal is to observe the gamma ray sky in the energy range 20 MeV to 300 GeV. At these energies, the photon interacts with matter primarily by annihilating into an electron positron pair. As a consequence, its parameters of interest (direction and energy) can be estimated only through the subsequent interaction of the two charged tracks with the active material of the detector. -
Neutron-Antineutron Oscillations: Discrete Symmetries and Quark Operators
PACIFIC-2018.9 Gump Station, Moorea, French Polynesia Aug 31 — Sept 6, 2018 Neutron-Antineutron Oscillations: Discrete Symmetries and Quark Operators Arkady Vainshtein William Fine Theoretical Physics Institute University of Minnesota, KITP, University of California, Santa Barbara With Zurab Berezhiani Search for the neutron-antineutron oscillations was suggested by Vadim Kuzmin in 1970, and such experiments are under active discussion now, see D. G. Phillips, II et al., Phys. Rept. 612, 1 (2016) This is a transition where the baryon charge B is changed by two units. The observation of the transition besides demonstration of the baryon charge non-conservation could be also important for explanation of baryogengesis. Of course, following Sakharov conditions, it should be also accompanied by CP non-conservation. Thus, discrete symmetries associated with neutron-antineutron mixing are of real interest. C, P and T symmetries in | Δ B| =2 transitions In our 2015 text Zurab Berezhiani, AV, arXiv:1506.05096 we noted that the parity P , defined in such a way that P 2 =1 , is broken in n-nbar transition as well as CP .. Indeed, eigenvalues of parity P are ± 1 and opposite for neutron and antineutron. So, n-nbar mixing breaks P . We noted, however, that it does not automatically imply an existence of CP breaking in absence of interaction. In September of the same 2015 we presented at the INT workshop in Seattle a modified definition of parity P z , 2 such that P z = − 1 , and parities P z are i for both, neutron and antineutron. With this modification all discrete symmetries are preserved in n-nbar transition.