Relativity and Accelerator Engineering
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Accelerator and Beam Physics Research Goals and Opportunities
Accelerator and Beam Physics Research Goals and Opportunities Working group: S. Nagaitsev (Fermilab/U.Chicago) Chair, Z. Huang (SLAC/Stanford), J. Power (ANL), J.-L. Vay (LBNL), P. Piot (NIU/ANL), L. Spentzouris (IIT), and J. Rosenzweig (UCLA) Workshops conveners: Y. Cai (SLAC), S. Cousineau (ORNL/UT), M. Conde (ANL), M. Hogan (SLAC), A. Valishev (Fermilab), M. Minty (BNL), T. Zolkin (Fermilab), X. Huang (ANL), V. Shiltsev (Fermilab), J. Seeman (SLAC), J. Byrd (ANL), and Y. Hao (MSU/FRIB) Advisors: B. Dunham (SLAC), B. Carlsten (LANL), A. Seryi (JLab), and R. Patterson (Cornell) January 2021 Abbreviations and Acronyms 2D two-dimensional 3D three-dimensional 4D four-dimensional 6D six-dimensional AAC Advanced Accelerator Concepts ABP Accelerator and Beam Physics DOE Department of Energy FEL Free-Electron Laser GARD General Accelerator R&D GC Grand Challenge H- a negatively charged Hydrogen ion HEP High-Energy Physics HEPAP High-Energy Physics Advisory Panel HFM High-Field Magnets KV Kapchinsky-Vladimirsky (distribution) ML/AI Machine Learning/Artificial Intelligence NCRF Normal-Conducting Radio-Frequency NNSA National Nuclear Security Administration NSF National Science Foundation OHEP Office of High Energy Physics QED Quantum Electrodynamics rf radio-frequency RMS Root Mean Square SCRF Super-Conducting Radio-Frequency USPAS US Particle Accelerator School WG Working Group 1 Accelerator and Beam Physics 1. EXECUTIVE SUMMARY Accelerators are a key capability for enabling discoveries in many fields such as Elementary Particle Physics, Nuclear Physics, and Materials Sciences. While recognizing the past dramatic successes of accelerator-based particle physics research, the April 2015 report of the Accelerator Research and Development Subpanel of HEPAP [1] recommended the development of a long-term vision and a roadmap for accelerator science and technology to enable future DOE HEP capabilities. -
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. -
Accelerator Physics and Modeling
BNL-52379 CAP-94-93R ACCELERATOR PHYSICS AND MODELING ZOHREH PARSA, EDITOR PROCEEDINGS OF THE SYMPOSIUM ON ACCELERATOR PHYSICS AND MODELING Brookhaven National Laboratory UPTON, NEW YORK 11973 ASSOCIATED UNIVERSITIES, INC. UNDER CONTRACT NO. DE-AC02-76CH00016 WITH THE UNITED STATES DEPARTMENT OF ENERGY DISCLAIMER This report was prepared as an account of work sponsored by an agency of the Unite1 States Government Neither the United States Government nor any agency thereof, nor any of their employees, nor any of their contractors, subcontractors, or their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, doea not necessarily constitute or imply its endorsement, recomm.ndation, or favoring by the UnitedStates Government or any agency, contractor or subcontractor thereof. The views and opinions of authors expressed herein do not necessarily state or reflect those of the United States Government or any agency, contractor or subcontractor thereof- Printed in the United States of America Available from National Technical Information Service U.S. Department of Commerce 5285 Port Royal Road Springfieid, VA 22161 NTIS price codes: Am&mffi TABLE OF CONTENTS Topic, Author Page no. Forward, Z . Parsa, Brookhaven National Lab. i Physics of High Brightness Beams , 1 M. Reiser, University of Maryland . Radio Frequency Beam Conditioner For Fast-Wave 45 Free-Electron Generators of Coherent Radiation Li-Hua NSLS Dept., Brookhaven National Lab, and A. -
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. -
Accelerator Physics Third Edition
Preface Accelerator science took off in the 20th century. Accelerator scientists invent many in- novative technologies to produce and manipulate high energy and high quality beams that are instrumental to progresses in natural sciences. Many kinds of accelerators serve the need of research in natural and biomedical sciences, and the demand of applications in industry. In the 21st century, accelerators will become even more important in applications that include industrial processing and imaging, biomedical research, nuclear medicine, medical imaging, cancer therapy, energy research, etc. Accelerator research aims to produce beams in high power, high energy, and high brilliance frontiers. These beams addresses the needs of fundamental science research in particle and nuclear physics, condensed matter and biomedical sciences. High power beams may ignite many applications in industrial processing, energy production, and national security. Accelerator Physics studies the interaction between the charged particles and elec- tromagnetic field. Research topics in accelerator science include generation of elec- tromagnetic fields, material science, plasma, ion source, secondary beam production, nonlinear dynamics, collective instabilities, beam cooling, beam instrumentation, de- tection and analysis, beam manipulation, etc. The textbook is intended for graduate students who have completed their graduate core-courses including classical mechanics, electrodynamics, quantum mechanics, and statistical mechanics. I have tried to emphasize the fundamental physics behind each innovative idea with least amount of mathematical complication. The textbook may also be used by advanced undergraduate seniors who have completed courses on classical mechanics and electromagnetism. For beginners in accelerator physics, one begins with Secs. 2.I–2.IV in Chapter 2, and follows by Secs. -
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. -
Accelerator Physics Alid Engineering 3Rd Printing
Handbook of Accelerator Physics alid Engineering 3rd Printing edited by Alexander Wu Chao Stanford Linear Accelerator Center Maury Tigner Carneil University World Scientific lbh NEW JERSEY • LONDON • SINGAPORE • BEIJING • SHANGHAI • HONG KONG • TAIPEI • CHENNAI Table of Contents Preface 1 INTRODUCTION 1 1.1 HOW TO USE THIS BOOK 1 1.2 NOMENCLATURE 1 1.3 FUNDAMENTAL CONSTANTS 3 1.4 UNITS AND CONVERSIONS 4 1.4.1 Units A. W. Chao 4 1.4.2 Conversions M. Tigner 4 1.5 FUNDAMENTAL FORMULAE A. W. Chao 5 1.5.1 Special Functions 5 1.5.2 Curvilinear Coordinate Systems 6 1.5.3 Electromagnetism 6 1.5.4 Kinematical Relations 7 1.5.5 Vector Analysis 8 1.5.6 Relativity 8 1.6 GLOSSARY OF ACCELERATOR TYPES 8 1.6.1 Antiproton Sources J. Peoples, J.P. Marriner 8 1.6.2 Betatron M. Tigner 10 1.6.3 Colliders J. Rees 11 1.6.4 Cyclotron H. Blosser 13 1.6.5 Electrostatic Accelerator J. Ferry 16 1.6.6 FFAG Accelerators M.K. Craddock 18 1.6.7 Free-Electron Lasers C. Pellegrini 21 1.6.8 High Voltage Electrodynamic Accelerators M. Cleland 25 1.6.9 Induction Linacs R. Bangerter 28 1.6.10 Industrial Applications of Electrostatic Accelerators G. Norton, J.L. Duggan 30 1.6.11 Linear Accelerators for Electron G.A. Loew 31 1.6.12 Linear Accelerators for Protons S. Henderson, A. Aleksandrov 34 1.6.13 Livingston Chart J. Rees 38 1.6.14 Medical Applications of Accelerators J. Alonso 38 1.6.14.1 Radiation therapy 38 1.6.14.2 Radioisotopes 40 1.6.15 Microtron P.H. -
Accelerator Physics for Health Physicist by D. Cossairt
Accelerator Physics for Health Physicists J. Donald Cossairt Ph.D., C.H.P. Applied Scientist III Fermi National Accelerator Laboratory 1 Introduction • Goal is to improve knowledge and appreciation of the art of particle accelerator physics • Accelerator health physicists should understand how the machines work. • Accelerators have unique operational characteristics of importance to radiation protection. – For their own understanding – To promote communication with accelerator physicists, operators, and experimenters • This course will not make you an accelerator PHYSICIST! – Limitations of both time and level prescript that. – For those who want to learn more, academic courses and the U. S. Particle Accelerator School provide much comprehensive opportunities. • Much of the material is found in several of the references. – Particularly clear or unique descriptions are cited among these. 2 A word about notation • Vector notation will be used extensively. – Vectors are printed in italic boldface (e.g., E) – Their corresponding magnitudes are shown in italics (e.g., E). • Variable names generally will follow the published literature. • Consistency has not been achieved. – This author cannot fix that by himself! – Chose to remain close to the literature – Watch the context! 3 Summary of relativistic relationships including Maxwell’s equations • Special theory of relativity is important. • Accelerators work because of Maxwell’s equations. •Therest energy of a particle Wo is connected to its rest mass mo by the speed of light c: 2 Wmcoo= (1) • Total energy W of a particle moving with velocity v is 2 22mco W 1 Wmc== =γ mco γ == , (2) 2 2 1− β , with Wo 1− β β = v/c, m is the relativistic mass, and γ is the relativistic parameter. -
Sarah M. Cousineau
Sarah M. Cousineau Section Head: Accelerator Science and Technology, Spallation Neutron Source Spallation Neutron Source Phone: +1 865 406 0294 PO Box 2008, MS 6461 [email protected] Oak Ridge, TN 37831-6461 Current Job Responsibilities: • Lead the Accelerator Science and Technology group at the Spallation Neutron Source (SNS) accelerator: § Lead the production, measurement, understanding and analysis of the SNS 1.4 MW H- linac and ring proton beams § Define and oversee a robust R&D program targeted at high intensity, high power beams § Define and oversee an effective mechanical engineering design program that supports both beam operations and accelerator R&D § Manage the beam study program aimed at identifying, understanding, and mitigating accelerator performance limitations § Guide and facilitate strategic plans for accelerator performance improvements, and software tools for efficient modeling and analysis of the beam § Manage the section budget and provide professional development opportunities for staff § Promote a strong culture of safety in all activities § Participate in outreach and professional community service roles Education: • 2003 Ph.D. (Accelerator Physics), Indiana University • 2000 M.S. (Accelerator Physics), Indiana University • 1998 B.S. (Physics, summa cum laude), University of North Dakota Research Interests: • Collective effects in high intensity beams, space charge and instabilities • Novel injection methods for proton drivers • Laser and ion beam interactions • Code development and simulation of high intensity beams • Novel beam diagnostics and measurement techniques • High power beam collimation • High current and duty factor H- ion sources Professional Experience: 07/2020 – present Section Head, Accelerator Science and Technology 01/2016 – 07/2020 Group Leader, Beam Science and Technology group, Spallation Neutron Source 02/2012 – 07/2020 Joint Faculty Professor, Department of Physics and Astronomy, University of Tennessee 1 Sarah M. -
Accelerator Physics of Colliders
1 31. Accelerator Physics of Colliders 31. Accelerator Physics of Colliders Revised August 2019 by M.J. Syphers (Northern Illinois U.; FNAL) and F. Zimmermann (CERN). This article provides background for the High-Energy Collider Parameter Tables that follow and some additional information. 31.1 Luminosity The number of events, Nexp, is the product of the cross section of interest, σexp, and the time integral over the instantaneous luminosity, L: Z Nexp = σexp × L(t)dt. (31.1) Today’s colliders all employ bunched beams. If two bunches containing n1 and n2 particles collide head-on with average collision frequency fcoll, a basic expression for the luminosity is n1n2 L = fcoll ∗ ∗ F (31.2) 4πσxσy ∗ ∗ where σx and σy characterize the rms transverse beam sizes in the horizontal (bend) and vertical directions at the interaction point, and F is a factor of order 1, that takes into account geometric effects such as a crossing angle and finite bunch length, and dynamic effects, such as the mutual focusing of the two beam during the collision. For a circular collider, fcoll equals the number of bunches per beam times the revolution frequency. In 31.2, it is assumed that the bunches are identical in transverse profile, that the profiles are Gaussian and independent of position along the bunch, and the particle distributions are not altered during bunch crossing. Nonzero beam crossing angles θc in the horizontal plane and long bunches (rms bunch length σz) will reduce the luminosity, 2 1/2 ∗ e.g., by a factor F ≈ 1/(1 + φ ) , where the parameter φ ≡ θcσz/(2σx) is known as the Piwinski angle. -
A Brief History and Review of Accelerators
A BRIEF HISTORY AND REVIEW OF ACCELERATORS P.J. Bryant CERN, Geneva, Switzerland ABSTRACT The history of accelerators is traced from three separate roots, through a rapid development to the present day. The well-known Livingston chart is used to illustrate how spectacular this development has been with, on average, an increase of one and a half orders of magnitude in energy per decade, since the early thirties. Several present-day accelerators are reviewed along with plans and hopes for the future. 1 . INTRODUCTION High-energy physics research has always been the driving force behind the development of particle accelerators. They started life in physics research laboratories in glass envelopes sealed with varnish and putty with shining electrodes and frequent discharges, but they have long since outgrown this environment to become large-scale facilities offering services to large communities. Although the particle physics community is still the main group, they have been joined by others of whom the synchrotron light users are the largest and fastest growing. There is also an increasing interest in radiation therapy in the medical world and industry has been a long-time user of ion implantation and many other applications. Consequently accelerators now constitute a field of activity in their own right with professional physicists and engineers dedicated to their study, construction and operation. This paper will describe the early history of accelerators, review the important milestones in their development up to the present day and take a preview of future plans and hopes. 2 . HISTORICAL ROOTS The early history of accelerators can be traced from three separate roots. -
Relativity, EM Forces - Historical Introduction
Accelerator Physics Alex Bogacz (Jefferson Lab) / [email protected] Geoff Krafft (Jefferson Lab/ODU) / [email protected] Timofey Zolkin (U. Chicago/Fermilab) / [email protected] Thomas Jefferson National Accelerator Facility Lecture 1Accelerator− Relativity, Physics EM Forces, Intro Operated by JSA for the U.S. Department of Energy USPAS, Fort Collins, CO, June 10-21, 2013 1 Introductions and Outline Syllabus Week 1 Week 2 Introduction Course logistics, Homework, Exam: http://casa/publications/USPAS_Summer_2013.shtml Relativistic mechanics review Relativistic E&M review, Cyclotrons Survey of accelerators and accelerator concepts Thomas Jefferson National Accelerator Facility Lecture 1Accelerator− Relativity, Physics EM Forces, Intro Operated by JSA for the U.S. Department of Energy 2 Syllabus – week 1 Mon 10 June 0900-1200 Lecture 1 ‘Relativity, EM Forces - Historical Introduction Mon 10 June 1330-1630 Lecture 2 ‘Weak focusing and Transverse Stability’ Tue 11 June 0900-1200 Lecture 3 ‘Linear Optics’ Tue 11 June 1330-1630 Lecture 4 ‘Phase Stability, Synchrotron Motion’ Wed 12 June 0900-1200 Lecture 5 ‘Magnetic Multipoles, Magnet Design’ Wed 12 June 1330-1630 Lecture 6 ‘Particle Acceleration’ Thu 13 June 0900-1200 Lecture 7 ‘Coupled Betatron Motion I’ Thu 13 June 1330-1630 Lecture 8 ‘Synchrotron Radiation’ Fri 14 June 0900-1200 Lecture 9 ‘Coupled Betatron Motion II’ Fri 14 June 1330-1530 Lecture 10 ‘Radiation Distributions’ Thomas Jefferson National Accelerator Facility Lecture 1Accelerator− Relativity, Physics EM Forces, Intro Operated