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UC Berkeley UC Berkeley Electronic Theses and Dissertations
UC Berkeley UC Berkeley Electronic Theses and Dissertations Title Discoverable Matter: an Optimist’s View of Dark Matter and How to Find It Permalink https://escholarship.org/uc/item/2sv8b4x5 Author Mcgehee Jr., Robert Stephen Publication Date 2020 Peer reviewed|Thesis/dissertation eScholarship.org Powered by the California Digital Library University of California Discoverable Matter: an Optimist’s View of Dark Matter and How to Find It by Robert Stephen Mcgehee Jr. A dissertation submitted in partial satisfaction of the requirements for the degree of Doctor of Philosophy in Physics in the Graduate Division of the University of California, Berkeley Committee in charge: Professor Hitoshi Murayama, Chair Professor Alexander Givental Professor Yasunori Nomura Summer 2020 Discoverable Matter: an Optimist’s View of Dark Matter and How to Find It Copyright 2020 by Robert Stephen Mcgehee Jr. 1 Abstract Discoverable Matter: an Optimist’s View of Dark Matter and How to Find It by Robert Stephen Mcgehee Jr. Doctor of Philosophy in Physics University of California, Berkeley Professor Hitoshi Murayama, Chair An abundance of evidence from diverse cosmological times and scales demonstrates that 85% of the matter in the Universe is comprised of nonluminous, non-baryonic dark matter. Discovering its fundamental nature has become one of the greatest outstanding problems in modern science. Other persistent problems in physics have lingered for decades, among them the electroweak hierarchy and origin of the baryon asymmetry. Little is known about the solutions to these problems except that they must lie beyond the Standard Model. The first half of this dissertation explores dark matter models motivated by their solution to not only the dark matter conundrum but other issues such as electroweak naturalness and baryon asymmetry. -
Update on the Combined Analysis of Muon Measurements from Nine Air Shower Experiments
ICRC 2021 THE ASTROPARTICLE PHYSICS CONFERENCE ONLINE ICRC 2021Berlin | Germany THE ASTROPARTICLE PHYSICS CONFERENCE th Berlin37 International| Germany Cosmic Ray Conference 12–23 July 2021 Update on the Combined Analysis of Muon Measurements from Nine Air Shower Experiments Dennis Soldin0,∗ for the EAS-MSU, IceCube, KASCADE-Grande, NEVOD-DECOR, Pierre Auger, SUGAR, Telescope Array, and Yakutsk EAS Array Collaborations (a complete list of authors can be found at the end of the proceedings) 0Bartol Research Institute, Dept. of Physics and Astronomy University of Delaware, Newark, DE 19716, USA E-mail: [email protected] Over the last two decades, various experiments have measured muon densities in extensive air showers over several orders of magnitude in primary energy. While some experiments observed differences in the muon densities between simulated and experimentally measured air showers, others reported no discrepancies. We will present an update of the meta-analysis of muon measurements from nine air shower experiments, covering shower energies between a few PeV and tens of EeV and muon threshold energies from a few 100 MeV to about 10 GeV. In order to compare measurements from different experiments, their energy scale was cross-calibrated and the experimental data has been compared using a universal reference scale based on air shower simulations. Above 10 PeV, we find a muon excess with respect to simulations for all hadronic interaction models, which is increasing with shower energy. For EPOS-LHC and QGSJet-II.04 the significance of the slope of the increase is analyzed in detail under different assumptions of the individual experimental uncertainties. arXiv:2108.08341v2 [astro-ph.HE] 20 Aug 2021 37th International Cosmic Ray Conference (ICRC 2021) July 12th – 23rd, 2021 Online – Berlin, Germany ∗Presenter © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). -
Future Experimental Programs
Future Experimental Programs Hitoshi Murayama Department of Physics, University of California, Berkeley, California 94720, USA Theoretical Physics Group, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, University of Tokyo, Kashiwa 277-8583, Japan E-mail: [email protected], [email protected], [email protected] Abstract. I was asked to discuss future experimental programs even though I'm a theorist. As a result, I present my own personal views on where the field is, and where it is going, based on what I myself have been working on. In particular, I discuss why we need expeditions into high energies to find clues to where the relevant energy scale is for dark matter, baryon asymmetry, and neutrino mass. I also argue that the next energy frontier machine should be justified on the basis of what we know, namely the mass of the Higgs boson, so that we will learn what energy we should aim at once we nail the Higgs sector. Finally I make remarks on dark energy. arXiv:1401.0966v1 [hep-ph] 6 Jan 2014 Future Experimental Programs Murayama 2 1. Introduction The discovery of a \Higgs-like particle" on July 4, 2012 was a truly historic moment in the history of science [1, 2]. Many of us in the United States watched the seminar at CERN over webcast in the midnight hours. Given that it was announced on the Independence Day of the United States, we celebrated the Higgsdependence Day in the early morning. -
A Journey Into the Quantum Universe
Dr. Hitoshi Murayama is a professor in the Department of Physics at the University of California, Berkeley as well as Why are we here? the founding director of the Kavli Institute for the Physics and Mathematics of the Universe at the University of Tokyo. A Journey Into In October 2014, he gave a speech at the United Nations headquarters in New York about how science unites people the Quantum and brings peace. He received the Yukawa Commemoration Prize in Theoretical Physics and is a Fellow of the American Physical Society and the American Academy of Arts and Universe Sciences. In this interview, we discuss Dr. Murayama’s work at the intersection of theoretical particle physics, string theory, and cosmology. Interview with Dr. Hitoshi Murayama : How did your early experiences in Japan shape your career BSJand motivations? What led you to practice physics in both the United States and Japan? : It started when I was a little kid. I had really bad asthma, HMso every year, I missed quite a few days of school. When I was at home, I did not have anything to do but watch TV, and on TV, there were some very interesting educational programs. These programs are what got me interested in science and math. Then, throughout university, I had a very keen interest in the area of physics that I am working in right now, namely at the interface of theoretical particle physics and cosmology. It turned out that, back in those days, this was not a very active area of physics in Japan, so I did not really get to further my studies in this area. -
Spinning Test Particle in Four-Dimensional Einstein–Gauss–Bonnet Black Holes
universe Communication Spinning Test Particle in Four-Dimensional Einstein–Gauss–Bonnet Black Holes Yu-Peng Zhang 1,2, Shao-Wen Wei 1,2 and Yu-Xiao Liu 1,2,3* 1 Joint Research Center for Physics, Lanzhou University and Qinghai Normal University, Lanzhou 730000 and Xining 810000, China; [email protected] (Y.-P.Z.); [email protected] (S.-W.W.) 2 Institute of Theoretical Physics & Research Center of Gravitation, Lanzhou University, Lanzhou 730000, China 3 Key Laboratory for Magnetism and Magnetic of the Ministry of Education, Lanzhou University, Lanzhou 730000, China * Correspondence: [email protected] Received: 27 June 2020; Accepted: 27 July 2020; Published: 28 July 2020 Abstract: In this paper, we investigate the motion of a classical spinning test particle in a background of a spherically symmetric black hole based on the novel four-dimensional Einstein–Gauss–Bonnet gravity [D. Glavan and C. Lin, Phys. Rev. Lett. 124, 081301 (2020)]. We find that the effective potential of a spinning test particle in this background could have two minima when the Gauss–Bonnet coupling parameter a is nearly in a special range −8 < a/M2 < −2 (M is the mass of the black hole), which means a particle can be in two separate orbits with the same spin-angular momentum and orbital angular momentum, and the accretion disc could have discrete structures. We also investigate the innermost stable circular orbits of the spinning test particle and find that the corresponding radius could be smaller than the cases in general relativity. Keywords: Gauss–Bonnet; innermost stable circular orbits; spinning test particle 1. -
Cherenkov Light Imaging in Astroparticle Physics
Cherenkov light imaging in astroparticle physics U. F. Katz Erlangen Centre for Astroparticle Physics, Friedrich-Alexander University Erlangen-N¨urnberg, Erwin-Rommel-Str. 1, 91058 Erlangen, Germany Abstract Cherenkov light induced by fast charged particles in transparent dielectric media such as air or water is exploited by a variety of experimental techniques to detect and measure extraterrestrial particles impinging on Earth. A selection of detection principles is discussed and corresponding experiments are presented together with breakthrough-results they achieved. Some future develop- ments are highlighted. Keywords: Astroparticle physics, Cherenkov detectors, neutrino telescopes, gamma-ray telescopes, cosmic-ray detectors 1. Introduction Photomultiplier tubes (PMTs) and, more recently, silicon pho- tomultipliers (SiPMs) [3,4] are the standard sensor types. They In 2018, we commemorate the 60th anniversary of the award are provided by specialised companies who cooperate with the of the Nobel Prize to Pavel Alexeyewich Cherenkov, Ilya experiments in developing and optimising sensors according to Mikhailovich Frank and Igor Yevgenyevich Tamm for the dis- the respective specific needs (see e.g. [5,6]). covery and the interpretation of the Cherenkov effect [1,2]. In the following, the detection principles of different types of The impact of this discovery on astroparticle physics is enor- Cherenkov experiments in astroparticle physics are presented mous and persistent. Cherenkov detection techniques were ins- together with selected technical details and outstanding results. tumental for the dicovery of neutrino oscillations; the detection of high-energy cosmic neutrinos; the establishment of ground- based gamma-ray astronomy; and important for the progress in 2. Ground-based gamma-ray detectors cosmic-ray physics. -
A620 Dynamics 2017 L
Dynamics and how to use the orbits of stars to do interesting things ! chapter 3 of S+G- parts of Ch 11 of MWB (Mo, van den Bosch, White)! READ S&G Ch 3 sec 3.1, 3.2, 3 .4! we are skipping over epicycles ! 1! A Guide to the Next Few Lectures ! •The geometry of gravitational potentials : methods to derive gravitational ! potentials from mass distributions, and visa versa.! •Potentials define how stars move ! consider stellar orbit shapes, and divide them into orbit classes.! •The gravitational field and stellar motion are interconnected : ! the Virial Theorem relates the global potential energy and kinetic energy of !the system. ! ! • Collisions?! • The Distribution Function (DF) : ! the DF specifies how stars are distributed throughout the system and ! !with what velocities.! For collisionless systems, the DF is constrained by a continuity equation :! ! the Collisionless Boltzmann Equation ! •This can be recast in more observational terms as the Jeans Equation. ! The Jeans Theorem helps us choose DFs which are solutions to the continuity equations! 2! A Reminder of Newtonian Physics sec 3.1 in S&G! eq 3.1! φ (x) is the potential! eq 3.2! eq 3.3! Gauss's thm ∫ !φ •ds2=4πGM! the Integral of the normal component! over a closed surface =4πG x mass within eq 3.4! that surface! ρ(x) is the mass density3! distribution! Conservation of Energy and Angular Momentum ! Angular momentum L! 4! Some Basics - M. Whittle! • The gravitational potential energy is a scalar field ! • its gradient gives the net gravitational force (per unit mass) which is a vector field : see S&G pg 113 ! Poissons eq inside the mass distribution ! Outside the mass dist ! 5! Poisson's Eq+ Definition of Potential Energy (W) ! ρ(x) is the density dist! S+G pg 112-113! Potential energy W ! 6! Derivation of Poisson's Eq ! see S+G pg112 for detailed derivation or web page 'Poisson's equation' ! 7! More Newton-Spherical Systems Newtons 1st theorem: a body inside a spherical shell has no net gravitational force from that shell; e.g. -
History of High-Energy Neutrino Astronomy
History of high-energy neutrino astronomy C. Spiering DESY, Platanenallee 6, D-15738 Zeuthen, Germany This talk sketches the main milestones of the path towards cubic kilometer neutrino telescopes. It starts with the first conceptual ideas in the late 1950s and describes the emergence of concepts for detectors with a realistic discovery potential in the 1970s and 1980s. After the pioneering project DUMAND close to Hawaii was terminated in 1995, the further development was carried by NT200 in Lake Baikal, AMANDA at the South Pole and ANTARES in the Mediterranean Sea. In 2013, more than half a century after the first concepts, IceCube has discovered extraterrestrial high-energy neutrinos and opened a new observational window to the cosmos { marking a milestone along a journey which is far from being finished. 1 From first concepts to the detection of atmospheric neutrinos The initial idea of neutrino astronomy beyond the solar system rested on two arguments: The first was the expectation that a supernova stellar collapse in our galaxy would be accompanied by an enormous burst of neutrinos in the 5-10 MeV range. The second was the expectation that fast rotating pulsars must accelerate charged particles in their Tera-Gauss magnetic fields. Either in the source or on their way to Earth they must hit matter, generate pions and neutrinos as decay products of the pions. The first ideas to detect cosmic high energy neutrinos underground or underwater date back to the late fifties (see 1 for a detailed history of cosmic neutrino detectors). In the 1960 Annual Review of Nuclear Science, K. -
Introduction. What Is a Classical Field Theory? Introduction This Course
Classical Field Theory Introduction. What is a classical field theory? Introduction. What is a classical field theory? Introduction This course was created to provide information that can be used in a variety of places in theoretical physics, principally in quantum field theory, particle physics, electromagnetic theory, fluid mechanics and general relativity. Indeed, it is usually in such courses that the techniques, tools, and results we shall develop here are introduced { if only in bits and pieces. As explained below, it seems better to give a unified, systematic development of the tools of classical field theory in one place. If you want to be a theoretical/mathematical physicist you must see this stuff at least once. If you are just interested in getting a deeper look at some fundamental/foundational physics and applied mathematics ideas, this is a good place to do it. The most familiar classical* field theories in physics are probably (i) the \Newtonian theory of gravity", based upon the Poisson equation for the gravitational potential and Newton's laws, and (ii) electromagnetic theory, based upon Maxwell's equations and the Lorentz force law. Both of these field theories are exhibited below. These theories are, as you know, pretty well worked over in their own right. Both of these field theories appear in introductory physics courses as well as in upper level courses. Einstein provided us with another important classical field theory { a relativistic gravitational theory { via his general theory of relativity. This subject takes some investment in geometrical technology to adequately explain. It does, however, also typically get a course of its own. -
Investigation of a Micro- and Nano-Particle In-Space Electrostatic Propulsion Concept
Investigation of a Micro- and Nano-Particle In-Space Electrostatic Propulsion Concept by Louis D. Musinski A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy (Electrical Engineering) in The University of Michigan 2009 Doctoral Committee: Professor Brian E. Gilchrist, Co-Chair Professor Alec D. Gallimore, Co-Chair Professor Yogesh B. Gianchandani Associate Professor Michael J. Solomon Louis D. Musinski © ———————— 2009 All Rights Reserved Acknowledgements First, I would like to thank everyone who helped and supported me throughout my entire education. This work was made possible by everyone who has touched my life and includes people too numerous mention. To everyone who is not directly mentioned here, thank you! I would like to express gratitude for my advisor and co-chairman, Dr. Brian Gilchrist. His support over the last several years has been invaluable towards my development as an engineer and a person. The enthusiasm he exudes motivates people around him and I consider myself privileged to have worked with him. I look forward to future collaborations. I also thank my other co-chairman, Dr. Alec Gallimore, who has also provided significant guidance throughout my graduate school career. Dr. Michael Solomon and Dr. Yogesh Gianchandani, thank you for your help and guidance as members of my dissertation committee. I was fortunate to have been involved with a wonderful research group, nanoFET, which was composed of, not only excellent engineers, but also people that were a pleasure to work with. Thank you: Dr. Joanna Mirecki-Millunchick, Dr. Mark Burns, Dr. Michael Kiedar, Thomas Liu, Deshpremy Mukhija, Inkyu Eu, and David Liaw. -
A Second Order Differential Equation for a Point Charged Particle
A SECOND ORDER DIFFERENTIAL EQUATION FOR A POINT CHARGED PARTICLE Ricardo Gallego Torrom´e Departamento de Matem´atica Universidade Federal de S˜ao Carlos, Brazil Email: [email protected] Abstract. A model for the dynamics of a classical point charged particle interacting with higher order jet fields is introduced. In this model, the dy- namics of the charged particle is described by an implicit ordinary second order differential equation. Such equation is free of run-away and pre-accelerated so- lutions of Dirac’s type. The theory is Lorentz invariant, compatible with the first law of Newton and Larmor’s power radiation formula. Few implications of the new equation in the phenomenology of non-neutral plasmas is considered. 1. Introduction To find a consistent theory of classical electrodynamics of point charged particles interacting with its own radiation field is one of the most notable open problems in classical field theory. Historically, the investigation of the radiation reaction of point charged particles lead to the relativistic Abraham-Lorentz-Dirac equation [7] (in short, the ALD equation). However, the theoretical problems and paradoxes associated with ALD inclined many authors to support the view that the classical electrodynamics of point charged particles should not be based on the coupled sys- tem ALD /Maxwell system of equations. Attempts to find a consistent theory of classical electrodynamics of point particles include reduction of order schemes for the ALD equation [17], re-normalization group schemes [24], higher order deriva- tive field theories [2, 20], Feynman-Wheeler’s absorber theory of electrodynamics [9], models where the observable mass is variable with time [1, 18], non-linear elec- trodynamic theories [3] and dissipative force models [22, 14]. -
Physical Setting/Physics Core Curriculum Was Reviewed by Many Teachers and Administrators Across the State
PhysicalPhysical Setting/Setting/ PhysicsPhysics Core Curriculum THE UNIVERSITY OF THE STATE OF NEW YORK THE STATE EDUCATION DEPARTMENT http://www.emsc.nysed.gov THE UNIVERSITY OF THE STATE OF NEW YORK Regents of The University CARL T. HAYDEN, Chancellor, A.B., J.D. ............................................................................Elmira ADELAIDE L. SANFORD, Vice Chancellor, B.A., M.A., P.D. .................................................Hollis DIANE O’NEILL MCGIVERN, B.S.N., M.A., Ph.D. ..............................................................Staten Island SAUL B. COHEN, B.A., M.A., Ph.D. .....................................................................................New Rochelle JAMES C. DAWSON, A.A., B.A., M.S., Ph.D. .......................................................................Peru ROBERT M. BENNETT, B.A., M.S. ........................................................................................Tonawanda ROBERT M. JOHNSON, B.S., J.D. .........................................................................................Huntington ANTHONY S. BOTTAR, B.A., J.D. .........................................................................................North Syracuse MERRYL H. TISCH, B.A., M.A. ............................................................................................New York ENA L. FARLEY, B.A., M.A., Ph.D. .....................................................................................Brockport GERALDINE D. CHAPEY, B.A., M.A., Ed.D...........................................................................Belle