The Physics of Tachyons II. Tachyon Dynamics*
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Limits on New Physics from Black Holes Arxiv:1309.0530V1
Limits on New Physics from Black Holes Clifford Cheung and Stefan Leichenauer California Institute of Technology, Pasadena, CA 91125 Abstract Black holes emit high energy particles which induce a finite density potential for any scalar field φ coupling to the emitted quanta. Due to energetic considerations, φ evolves locally to minimize the effective masses of the outgoing states. In theories where φ resides at a metastable minimum, this effect can drive φ over its potential barrier and classically catalyze the decay of the vacuum. Because this is not a tunneling process, the decay rate is not exponentially suppressed and a single black hole in our past light cone may be sufficient to activate the decay. Moreover, decaying black holes radiate at ever higher temperatures, so they eventually probe the full spectrum of particles coupling to φ. We present a detailed analysis of vacuum decay catalyzed by a single particle, as well as by a black hole. The former is possible provided large couplings or a weak potential barrier. In contrast, the latter occurs much more easily and places new stringent limits on theories with hierarchical spectra. Finally, we comment on how these constraints apply to the standard model and its extensions, e.g. metastable supersymmetry breaking. arXiv:1309.0530v1 [hep-ph] 2 Sep 2013 1 Contents 1 Introduction3 2 Finite Density Potential4 2.1 Hawking Radiation Distribution . .4 2.2 Classical Derivation . .6 2.3 Quantum Derivation . .8 3 Catalyzed Vacuum Decay9 3.1 Scalar Potential . .9 3.2 Point Particle Instability . 10 3.3 Black Hole Instability . 11 3.3.1 Tadpole Instability . -
Tachyon-Dilaton Inflation As an Α'-Non Perturbative Solution in First
Anna Kostouki Work in progress with J. Alexandre and N. Mavromatos TachyonTachyon --DilatonDilaton InflationInflation asas anan αα''--nonnon perturbativeperturbative solutionsolution inin firstfirst quantizedquantized StringString CosmologyCosmology Oxford, 23 September 2008 A. Kostouki 2 nd UniverseNet School, Oxford, 23/09/08 1 OutlineOutline • Motivation : String Inflation in 4 dimensions • Closed Bosonic String in Graviton, Dilaton and Tachyon Backgrounds; a non – perturbative configuration • Conformal Invariance of this model • Cosmological Implications of this model: FRW universe & inflation (under conditions) • Open Issues: Exit from the inflationary phase; reheating A. Kostouki 2 nd UniverseNet School, Oxford, 23/09/08 2 MotivationMotivation Inflation : • elegant & simple idea • explains many cosmological observations (e.g. “horizon problem”, large - scale structure) Inflation in String Theory: • effective theory • in traditional string theories: compactification of extra dimensions of space-time is needed • other models exist too, but no longer “simple & elegant” A. Kostouki 2 nd UniverseNet School, Oxford, 23/09/08 3 ProposalProposal • Closed Bosonic String • graviton, dilaton and tachyon background • field configuration non-perturbative in Does it satisfy conformal invariance conditions? A. Kostouki 2 nd UniverseNet School, Oxford, 23/09/08 4 ConformalConformal propertiesproperties ofof thethe configurationconfiguration General field redefinition: • Theory is invariant • The Weyl anomaly coefficients transform : ( ) A. Kostouki 2 nd UniverseNet School, Oxford, 23/09/08 5 ConformalConformal propertiesproperties ofof thethe configurationconfiguration • 1-loop beta-functions: homogeneous dependence on X0, besides one term in the tachyon beta-function • Power counting → Every other term that appears at higher loops in the beta-functions is homogeneous A. Kostouki 2 nd UniverseNet School, Oxford, 23/09/08 6 ConformalConformal propertiesproperties ofof thethe configurationconfiguration One can find a general field redefinition , that: 1. -
Simulating Gamma-Ray Binaries with a Relativistic Extension of RAMSES? A
A&A 560, A79 (2013) Astronomy DOI: 10.1051/0004-6361/201322266 & c ESO 2013 Astrophysics Simulating gamma-ray binaries with a relativistic extension of RAMSES? A. Lamberts1;2, S. Fromang3, G. Dubus1, and R. Teyssier3;4 1 UJF-Grenoble 1 / CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG) UMR 5274, 38041 Grenoble, France e-mail: [email protected] 2 Physics Department, University of Wisconsin-Milwaukee, Milwaukee WI 53211, USA 3 Laboratoire AIM, CEA/DSM - CNRS - Université Paris 7, Irfu/Service d’Astrophysique, CEA-Saclay, 91191 Gif-sur-Yvette, France 4 Institute for Theoretical Physics, University of Zürich, Winterthurestrasse 190, 8057 Zürich, Switzerland Received 11 July 2013 / Accepted 29 September 2013 ABSTRACT Context. Gamma-ray binaries are composed of a massive star and a rotation-powered pulsar with a highly relativistic wind. The collision between the winds from both objects creates a shock structure where particles are accelerated, which results in the observed high-energy emission. Aims. We want to understand the impact of the relativistic nature of the pulsar wind on the structure and stability of the colliding wind region and highlight the differences with colliding winds from massive stars. We focus on how the structure evolves with increasing values of the Lorentz factor of the pulsar wind, keeping in mind that current simulations are unable to reach the expected values of pulsar wind Lorentz factors by orders of magnitude. Methods. We use high-resolution numerical simulations with a relativistic extension to the hydrodynamics code RAMSES we have developed. We perform two-dimensional simulations, and focus on the region close to the binary, where orbital motion can be ne- glected. -
Important Remarks on the Problem of Neutrino Passing Through the Matter Бештоев X
E2-2011-20 Kh.M. Beshtoev IMPORTANT REMARKS ON THE PROBLEM OF NEUTRINO PASSING THROUGH THE MATTER Бештоев X. М. E2-2011-20 Важные замечания к проблеме прохождения нейтрино через вещество Считается, что при прохождении нейтрино через вещество возникает ре- зонансное усиление осцилляций нейтрино. Показано, что уравнение Вольфен- штейна, описывающее прохождение нейтрино через вещество, имеет недоста- ток (не учитывает закон сохранения импульса, т. е. предполагается, что энер- гия нейтрино в веществе изменяется, а импульс остается неизменным). Это приводит, например, к изменению эффективной массы нейтрино на величину 0,87 • 10-2 эВ, которая возникает от мизерной энергии поляризации вещества, равной 5 • 10-12 эВ. После устранения этого недостатка, т.е. после учета из- менения импульса нейтрино в веществе, получены решения данного уравнения. В этих решениях возникают очень маленькие усиления осцилляции нейтрино в солнечном веществе из-за маленького значения энергии поляризации вещества при прохождении нейтрино. Также получены решения этого уравнения для двух предельных случаев. Работа выполнена в Лаборатории физики высоких энергий им. В. И. Векслера и А. М. Балдина ОИЯИ. Сообщение Объединенного института ядерных исследований. Дубна, 2011 Beshtoev Kh. M. E2-2011-20 Important Remarks on the Problem of Neutrino Passing through the Matter It is supposed that resonance enhancement of neutrino oscillations in the matter appears while a neutrino is passing through the matter. It is shown that Wolfenstein's equation, for a neutrino passing through the matter, has a disadvantage (it does not take into account the law of momentum conservation; i.e., it is supposed that in the matter the neutrino energy changes, but its momentum does not). It leads, for example, to changing the effective mass of the neutrino by the value 0.87 • 10-2 eV from a very small value of energy polarization of the matter caused by the neutrino, which is equal to 5 • 10-12 eV. -
Tachyonic Dark Matter
Tachyonic dark matter P.C.W. Davies Australian Centre for Astrobiology Macquarie University, New South Wales, Australia 2109 [email protected] Abstract Recent attempts to explain the dark matter and energy content of the universe have involved some radical extensions of standard physics, including quintessence, phantom energy, additional space dimensions and variations in the speed of light. In this paper I consider the possibility that some dark matter might be in the form of tachyons. I show that, subject to some reasonable assumptions, a tachyonic cosmological fluid would produce distinctive effects, such as a surge in quantum vacuum energy and particle creation, and a change in the conventional temperature-time relation for the normal cosmological material. Possible observational consequences are discussed. Keywords: tachyons, cosmological models, dark matter 1 1. Tachyons in an expanding universe In this section I consider the behaviour of a tachyon in an expanding universe, following the treatment in Davies (1975). A tachyon is a particle with imaginary mass iµ (µ real and positive), velocity v > c and momentum and energy given in a local inertial frame by p = µv(v2 – 1)-1/2 (1.1) E = µ(v2 – 1)-1/2 (1.2) where here and henceforth I choose units with c = ħ =1. Consider such a particle moving in a Friedmann-Roberston-Walker (FRW) universe with scale factor a(t), t being the cosmic time. In a short time dt, the particle will have moved a distance vdt to a point where the local comoving frame is retreating at a speed dv = (a′/a)vdt, where a′ = da/dt. -
Non-Tachyonic Semi-Realistic Non-Supersymmetric Heterotic-String Vacua
Eur. Phys. J. C (2016) 76:208 DOI 10.1140/epjc/s10052-016-4056-2 Regular Article - Theoretical Physics Non-tachyonic semi-realistic non-supersymmetric heterotic-string vacua Johar M. Ashfaquea, Panos Athanasopoulosb, Alon E. Faraggic, Hasan Sonmezd Department of Mathematical Sciences, University of Liverpool, Liverpool L69 7ZL, UK Received: 1 December 2015 / Accepted: 31 March 2016 / Published online: 15 April 2016 © The Author(s) 2016. This article is published with open access at Springerlink.com Abstract The heterotic-string models in the free fermionic 1 Introduction formulation gave rise to some of the most realistic-string models to date, which possess N = 1 spacetime supersym- The discovery of the agent of electroweak symmetry break- metry. Lack of evidence for supersymmetry at the LHC insti- ing at the LHC [1,2] is a pivotal moment in particle physics. gated recent interest in non-supersymmetric heterotic-string While confirmation of this agent as the Standard Model vacua. We explore what may be learned in this context from electroweak doublet representation will require experimental the quasi-realistic free fermionic models. We show that con- scrutiny in the decades to come, the data to date seems to vin- structions with a low number of families give rise to pro- dicate this possibility. Substantiation of this interpretation of liferation of a priori tachyon producing sectors, compared to the data will reinforce the view that the electroweak symme- the non-realistic examples, which typically may contain only try breaking mechanism is intrinsically perturbative, and that one such sector. The reason being that in the realistic cases the SM provides a viable perturbative parameterisation up to the internal six dimensional space is fragmented into smaller the Planck scale. -
Lorentz Invariant Relative Velocity and Relativistic Binary Collisions
Lorentz invariant relative velocity and relativistic binary collisions Mirco Cannoni∗ Departamento de F´ısica Aplicada, Facultad de Ciencias Experimentales, Universidad de Huelva, 21071 Huelva, Spain (Dated: May 2, 2016) This article reviews the concept of Lorentz invariant relative velocity that is often misunderstood or unknown in high energy physics literature. The properties of the relative velocity allow to formulate the invariant flux and cross section without recurring to non–physical velocities or any assumption about the reference frame. Applications such as the luminosity of a collider, the use as kinematic variable, and the statistical theory of collisions in a relativistic classical gas are reviewed. It is emphasized how the hyperbolic properties of the velocity space explain the peculiarities of relativistic scattering. CONTENTS section. To fix the ideas we consider the total cross sec- tion for binary collisions 1 + 2 f where f is a final → I. Introduction 1 state with 2 or more particles. The basic quantity that is measured in experiments is II. The definition of invariant cross section: three the reaction rate, that is the number of events with the problems and a solution 2 final state f per unit volume per unit of time, A. Why collinear velocities? 2 dN dN The Møller’s flux 3 f f f = = 4 . (1) B. ‘Who’ is the relative velocity? 3 R dV dt d x C. Transformation of densities 4 The value of the reaction rate is proportional to the num- D. The Landau-Lifschitz solution 4 ber density of particles n1 and n2 that approach each other with a certain relative velocity, for example an in- III. -
Stability of a Tachyon Braneworld
Stability of a tachyon braneworld Gabriel Germán,a Alfredo Herrera-Aguilar,b;c André Martorano Kuerten,a;d Dagoberto Malagón–Morejón,a and Roldão da Rochae aInstituto de Ciencias Físicas, Universidad Nacional Autónoma de México, Apartado Postal 48-3, 62251, Cuernavaca, Morelos, México bInstituto de Física, Benemérita Universidad Autónoma de Puebla, Apartado Postal J-48, 72570, Puebla, Puebla, México cInstituto de Física y Matemáticas, Universidad Michoacana de San Nicolás de Hidalgo, Ciudad Universitaria, CP 58040, Morelia, Michoacán, México dCentro de Ciências Naturais e Humanas, Universidade Federal do ABC, 09210-580, Santo André, SP, Brazil eCentro de Matemática, Computação e Cognição, Universidade Federal do ABC, 09210-580, Santo André, SP, Brazil E-mail: gabriel@fis.unam.mx, malagon@fis.unam.mx, [email protected], [email protected], [email protected] Abstract. Within the braneworld paradigm the tachyonic scalar field has been used to gener- ate models that attempt to solve some of the open problems that physics faces nowadays, both in cosmology and high energy physics as well. When these field configurations are produced by the interplay of higher dimensional warped gravity with some matter content, braneworld models must prove to be stable under the whole set of small fluctuations of the gravitational and matter fields background, among other consistency tests. Here we present a complete proof of the stability under scalar perturbations of tachyonic thick braneworlds with an em- bedded maximally symmetric 4D space-time, revealing its physical consistency. This family of models contains a recently reported tachyonic de Sitter thick braneworld which possesses a series of appealing properties. -
Annulus Amplitudes and ZZ Branes in Minimal String Theory
EFI-04-19 PUPT-2121 Annulus Amplitudes and ZZ Branes in Minimal String Theory David Kutasov,1 Kazumi Okuyama,1 Jongwon Park,1 Nathan Seiberg2 and David Shih3 1Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA 2School of Natural Sciences, Institute for Advanced Study, Princeton, NJ 08540 USA 3Department of Physics, Princeton University, Princeton, NJ 08544 USA We study the annulus amplitudes of (p, q) minimal string theory. Focusing on the ZZ-FZZT annulus amplitude as a target-space probe of the ZZ brane, we use it to confirm that the ZZ branes are localized in the strong-coupling region. Along the way we learn that the ZZ-FZZT open strings are fermions, even though our theory is bosonic! We also provide arXiv:hep-th/0406030v2 22 Jun 2004 a geometrical interpretation of the annulus amplitudes in terms of the Riemann surface that emerges from the FZZT branes. The ZZ-FZZT annulus amplitude measures the Mp,q deformation of due to the presence of background ZZ branes; each kind of ZZ-brane Mp,q deforms only one A-period of the surface. Finally, we use the annulus amplitudes to argue that the ZZ branes can be regarded as “wrong-branch” tachyons which violate the bound α<Q/2. June, 2004 1. Introduction Minimal string theories are string theories based on the (p, q) minimal conformal field theories coupled to Liouville. They were first solved using their description in terms of matrix models [1-8] (for reviews, see e.g. [9,10]). This tractable description allows explicit calculations of many physical quantities of interest. -
The Physics of Tachyons I. Tachyon Kinematics
Aust. J. Phys., 1992, 45, 591-620 The Physics of Tachyons I. Tachyon Kinematics Ross L. Dawe A and Kenneth C. Hines School of Physics, University of Melbourne, Parkville, Vic. 3052, Australia. A Present address: Maritime Operations Division, Materials Research Laboratory, P.O. Box 1750, Salisbury, S.A. 5108, Australia. Abstract A new formulation of the theory of tachyons is developed using the same two postulates as in special relativity. Use is made of a 'switching principle' to show how tachyons automatically obey the laws of conservation of energy, momentum and electric charge. Tachyonic mechanics is further developed by a consideration of tachyonic rods and clocks. There follows a discussion of the conservation of electric charge and the apparent visual appearance of a tachyonic cube. 1. Introduction The question of whether or not tachyons can exist has been a subject of considerable theoretical interest in recent decades. The most notable formulations of a theory of tachyons at the classical relativistic level have been provided by Bilaniuk et al. (1962, 1969), Recami and Mignani (1974), Recami (1986)* and Corben (1975, 1976, 1978). Recami has built up a detailed formulation based on symmetry arguments within special relativity, while Corben takes a more rigorous approach but has not completed all of the details. Tachyon theories are prone to misinterpretation, and the resulting fallacies and paradoxes have often proved difficult to resolve. It is the purpose of this and subsequent papers to build upon the work by these authors by presenting a rigorous formulation of the theory of tachyons in which the particles are able to interact with ordinary matter via the laws of mechanics and electrodynamics. -
Inhomogeneous Fragmentation of the Rolling Tachyon Gary Felder Smith College, [email protected]
Smith ScholarWorks Physics: Faculty Publications Physics 8-24-2004 Inhomogeneous Fragmentation of the Rolling Tachyon Gary Felder Smith College, [email protected] Lev Kofman University of Toronto Follow this and additional works at: https://scholarworks.smith.edu/phy_facpubs Part of the Physics Commons Recommended Citation Felder, Gary and Kofman, Lev, "Inhomogeneous Fragmentation of the Rolling Tachyon" (2004). Physics: Faculty Publications. 13. https://scholarworks.smith.edu/phy_facpubs/13 This Article has been accepted for inclusion in Physics: Faculty Publications by an authorized administrator of Smith ScholarWorks. For more information, please contact [email protected] PHYSICAL REVIEW D 70, 046004 ͑2004͒ Inhomogeneous fragmentation of the rolling tachyon Gary Felder* Smith College Physics Department, Northampton, Massachusetts 01063, USA Lev Kofman† CITA, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada ͑Received 19 April 2004; published 24 August 2004͒ Dirac-Born-Infeld type effective actions reproduce many aspects of string theory classical tachyon dynamics of unstable Dp-branes. The inhomogeneous tachyon field rolling from the top of its potential forms topological defects of lower codimensions. In between them, as we show, the tachyon energy density fragments into a p-dimensional web-like high density network evolving with time. We present an analytic asymptotic series solution of the nonlinear equations for the inhomogeneous tachyon and its stress energy. The generic solution for a tachyon field with a runaway potential in arbitrary dimensions is described by the free streaming of noninteracting massive particles whose initial velocities are defined by the gradients of the initial tachyon profile. Thus, relativistic particle mechanics is a dual picture of the tachyon field effective action. -
Cosmological Signature of Tachyon Condensation
Cosmological Signature of Tachyon Condensation Alexey Koshelev SIGRAV School, January 2009 Mainly based on JHEP 02 (2007) 041, hep-th/0605085 by I.Ya. Aref’eva, A. K., JHEP 04 (2007) 029, hep-th/0701103 by A. K. JHEP 0908 (2008) 068, arXiv:0804.3570, by I.Ya. Aref’eva, A. K. and work in progress by A. K. and S. Vernov Cosmological Signature of Tachyon Condensation Plan Plan • Overview of the problem • Open String Field Theory and Cosmology • Dilaton and open-closed strings coupling • Cosmological model • Perturbations • Summary and Outlook 1/14 Cosmological Signature of Tachyon Condensation Overview • Overview of the problem – Observational facts – Problems and challenges • Open String Field Theory and Cosmology • Dilaton and open-closed strings coupling • Cosmological model • Perturbations • Summary and Outlook 2/14 Cosmological Signature of Tachyon Condensation Overview/Facts Observational facts • Data on Ia supernovae • Galaxy clusters mea- Universe exhibits surements an accelerated expansion • WMAP Our universe is known to be homogeneous, isotropic and with high accuracy spatially flat. (1+3) dimensional spatially flat FRW universe ds2 = dt2 + a(t)2d~x2 − Equation of state: p = wρ, w< 0 — Dark Energy +0.14 Perlmutter et. al., 1999 w = 1 0.11 − − Riess et. al., 2004 Komatsu et. al., 2008 Spergel et. al., 2006 3/14 Cosmological Signature of Tachyon Condensation Overview/Problems Theoretical issues • w > 1 — Quintessence models − • w = 1 — Cosmological constant − • w < 1 — Phantom models − 4/14 Cosmological Signature of Tachyon Condensation Overview/Problems Theoretical issues • w > 1 — Quintessence models − • w = 1 — Cosmological constant − • w < 1 — Phantom models − • Just a cosmological constant has no theoretical explanation so far • A Phantom divide (w = 1) crossing is not excluded.