ELECTROMAGNETIC SHOWERS. Paolo Lipari. Lecture 2

Similar documents
Universality (and its limitations) in Cosmic Ray shower development

Interaction of Electron and Photons with Matter

Physics 663. Particle Physics Phenomenology. April 23, Physics 663, lecture 4 1

Passage of particles through matter

Tim Huege for the LOPES collaboration

remsstrahlung 1 Bremsstrahlung

The LHCf data hadronic interactions and UHECR showers. Paolo Lipari LHCf meeting Catania, 6th july 2011

Hadronic Showers. KIP Journal Club: Calorimetry and Jets 2009/10/28 A.Kaplan & A.Tadday

Validation of EM Part of Geant4

Electromagnetic and hadronic showers development. G. Gaudio, M. Livan The Art of Calorimetry Lecture II

> News < AMS-02 will be launched onboard the Shuttle Endeavour On May 2nd 2:33 P.M. from NASA Kennedy space center!

Synchrotron Radiation II

Particle-Matter Interactions

PHY492: Nuclear & Particle Physics. Lecture 24. Exam 2 Particle Detectors

2nd-Meeting. Ionization energy loss. Multiple Coulomb scattering (plural and single scattering, too) Tracking chambers

Physics 736. Experimental Methods in Nuclear-, Particle-, and Astrophysics. Lecture 3

Neutrino detection. Kate Scholberg, Duke University International Neutrino Summer School Sao Paulo, Brazil, August 2015

Particle Detectors. Summer Student Lectures 2010 Werner Riegler, CERN, History of Instrumentation History of Particle Physics

Nuclear Physics and Astrophysics

Calorimeter for detection of the high-energy photons

Synchrotron Radiation II

Calorimetry I Electromagnetic Calorimeters

CORSIKA: Extensive Air Shower Simulation

Emphasis on what happens to emitted particle (if no nuclear reaction and MEDIUM (i.e., atomic effects)

2. Passage of Radiation Through Matter

Physics Lecture 6

Air Shower Simulations for NAHSA

99 Years from Discovery : What is our current picture on Cosmic Rays? #6 How cosmic rays travel to Earth? Presented by Nahee Park

energy loss Ionization + excitation of atomic energy levels Mean energy loss rate de /dx proportional to (electric charge) 2 of incident particle

arxiv: v1 [astro-ph.im] 14 Sep 2017

CHARGED PARTICLE INTERACTIONS

Study of Number of photons at axis Shower with different de/dx and Fluorescence Yield

Selected "Phacts" for the Physics Regents Exam You Should Know

The interaction of radiation with matter

Particle Interactions in Detectors

Lecture 2 & 3. Particles going through matter. Collider Detectors. PDG chapter 27 Kleinknecht chapters: PDG chapter 28 Kleinknecht chapters:

PHY492: Nuclear & Particle Physics. Lecture 25. Particle Detectors

Ionization Energy Loss of Charged Projectiles in Matter. Steve Ahlen Boston University

ATOMIC WORLD P.1. ejected photoelectrons. current amplifier. photomultiplier tube (PMT)

Propagation in the Galaxy 2: electrons, positrons, antiprotons

The Development of Particle Physics. Dr. Vitaly Kudryavtsev E45, Tel.:

Physics Modern Physics Professor Jodi Cooley. Welcome back. to PHY Arthur Compton

Gaseous Detectors. Bernhard Ketzer University of Bonn

Particle Detectors : an introduction. Erik Adli/Are Strandlie, University of Oslo, August 2017, v2.3

_ int (x) = e ψ (x) γμ ψ(x) Aμ(x)

Introduction to particle physics Lecture 3: Quantum Mechanics

Lecture 3. lecture slides are at:

The Bohr Model of Hydrogen

cgrahamphysics.com Particles that mediate force Book pg Exchange particles

- ~200 times heavier than the e GeV µ travels on average. - does not interact strongly. - does emit bremsstrahlung in

Fermi Summer School Jordan Goodman - University of Maryland AIR SHOWERS. Fermi Summer School - J. Goodman 2017

Particle Physics Homework Assignment 4

AST 105 Intro Astronomy The Solar System. MIDTERM II: Tuesday, April 5 [covering Lectures 10 through 16]

The LHC Experiments. TASI Lecture 2 John Conway

Extensive Air Showers and Particle Physics Todor Stanev Bartol Research Institute Dept Physics and Astronomy University of Delaware

CHAPTER 3 Prelude to Quantum Theory. Observation of X Rays. Thomson s Cathode-Ray Experiment. Röntgen s X-Ray Tube

Higher -o-o-o- Past Paper questions o-o-o- 3.4 Spectra

Detectors in Nuclear Physics (40 hours)

Ultrahigh Energy Cosmic Rays propagation II

Calorimetry in particle physics experiments

Detectors for High Energy Physics

Investigating post-lhc hadronic interaction models and their predictions of cosmic ray shower observables

Numerical study of the electron lateral distribution in atmospheric showers of high energy cosmic rays

Particle Astrophysics

Calorimetry in particle physics experiments. Unit n.2 The physics of calorimetry

Chapter 2 Radiation-Matter Interactions

Particle accelerators. Dr. Alessandro Cianchi

Short Course on High Energy Astrophysics. Exploring the Nonthermal Universe with High Energy Gamma Rays

Tracker material study with the energy flow through the CMS electromagnetic calorimeter. Riccardo Paramatti, Ambra Provenza

Signal Characteristics from Electromagnetic Cascades in Ice

Photons: Interactions

Reconstruction in Collider Experiments (Part IV)

Chapter NP-4. Nuclear Physics. Particle Behavior/ Gamma Interactions TABLE OF CONTENTS INTRODUCTION OBJECTIVES 1.0 IONIZATION

Quantum Mechanics: Blackbody Radiation, Photoelectric Effect, Wave-Particle Duality

Improving H.E.S.S. cosmic-ray background rejection by means of a new Gamma-Ray Air Shower Parametrisation (GRASP)

Compact Muon Solenoid Surapat Ek-In École Polytechnique Fédérale de Lausanne

Detection methods in particle physics

Shower development and Cherenkov light propagation

Rb, which had been compressed to a density of 1013

Week 2: Chap. 2 Interaction of Radiation

Interaction of Ionizing Radiation with Matter

Physics of Radiotherapy. Lecture II: Interaction of Ionizing Radiation With Matter

David Gascón. Daniel Peralta. Universitat de Barcelona, ECM department. E Diagonal 647 (Barcelona) IFAE, Universitat Aut onoma de Barcelona

Last Lecture 1) Silicon tracking detectors 2) Reconstructing track momenta

Zhong-Bo Kang Los Alamos National Laboratory

Chapter Four (Interaction of Radiation with Matter)

Highlights from the 9 th Pisa Meeting on Advanced Detectors Calorimetry Session

A. Lindner 1. University of Hamburg, II. Inst. für Exp. Physik, Luruper Chaussee 149, D Hamburg, Germany

The Physics of Cosmic Rays

The PRIMEX Experiment: A Fundamental Test of the Chiral Anomaly Prediction in QCD. Erik Minges April 23 rd, 2010

Non-thermal emission from pulsars experimental status and prospects

BETHE - SALPETER EQUATION THE ORIGINS Edwin E. Salpeter October 2008

Name: Date: 2. The temperature of the Sun's photosphere is A) close to 1 million K. B) about 10,000 K. C) 5800 K. D) 4300 K.

MDI and detector modeling

Course Evaluation, Department of Theoretical Physics - FYS230 Theoretical Particle Physics, Fall 2006

Radiative Processes in Flares I: Bremsstrahlung

A Short Course on Geant4 Simulation Toolkit. Introduction.

Astroparticle Physics

Detector Simulation. Mihaly Novak CERN PH/SFT

Passage of Charged Particles in matter. Abstract:

Transcription:

ELECTROMAGNETIC SHOWERS Paolo Lipari Lecture 2 Corsika school 26/Nov/2008

Bremsstrahlung Pair Creation

BREMSSTRAHLUNG Fully ionized free nucleus (approximation of infinite mass) High Energy Limit (Full screening)

PAIR PRODUCTION Fully ionized free nucleus (approximation of infinite mass) High Energy Limit (Full screening)

Radiation Length: Meaning: Length where the energy of an electron is reduced to E/e 7/9 of the mean free path of photons

From Particle Data Book

The SPLITTING FUNCTIONS

ELECTROMAGNETIC SHOWERS Pair Production Brems strahlung Radiation Length (Energy independent) Vertices : theoretically understood (and scaling)

AVERAGE LONGITUDINAL EVOLUTION for a PURELY ELECTRO-MAGNETIC SHOWER Two functions of energy and depth

Possible Generalizations: 3-Dimensional treatment. Hadronic Showers: add other components

SYSTEM of INTEGRO-DIFFERENTIAL EQUATIONS that describe the evolution with t of for a given initial condition.

Variation with t of the number of photons with energy E

Variation with t of the number of photons with energy E =

Electrons

Electrons

Electrons

Electrons 2 divergent e -> e contributions. Their combination is finite.

Approximation A

INTRODUCTION of ENERGY LOSS of ELECTRONS for COLLISIONS

INTRODUCTION of ENERGY LOSS of ELECTRONS for COLLISIONS

Bethe-Bloch formula Very Simple Approximation: ENERGY INDEPENDENT LOSS Critical energy

Insert the collision energy loss in the shower equations: General treatment: Energy variation Law

=

=

Approximation A

Approximation B

Bruno Rossi 1933 Eritrea East West effect

Kenneth Greisen NCAR Texas 1971 after discovery of 200 MeV photons from the Crab Nebula

Shower Equations in Approximation A (neglect electron ionization losses) No Parameters with the Dimension of Energy

Solutions to the shower equations. Initial Condition: Photon of energy E0 Electron of energy E0

Let us consider an electron population that is has the spectral shape of an unbroken power law and no photons: Study the Shower evolution using approximation A

Initial condition Electron and Photon population remain a power law of same slope Only the normalizations are a function of the depth t Depth evolution

Coefficients Ke, (t) are linear combinations of two exponential

One controls the (faster) convergence to an s-dependent gamma/e ratio (large and negative) A second exponential describes the (slower ) evolution of the two population with a constant ratio.

S=1 Special spectrum Equal amount of energy per decade of E

S=1 Special spectrum Equal amount of energy per decade of E depth-independent solution

What can we say about: Without explicit calculation? Spectrum E-2 equal power per decade of E Pair Production and Bremsstrahlung redistribute the energy but nothing can change

What can we say about: Spectrum flatter than E-2 power per decade of E grows with E

What can we say about: Spectrum steeper than E-2 power per decade of E decreases with E

Insert functional form of the solution in the shower equation. Obtain simple quadratic equation connecting s

Time derivative Example of one term

Stability Ratio for the Photon/Electron Ratio

t-slope and E-slope are connected Integral Electron Spectrum Evolution Can deduce the AGE (and spectral shape)

Approximate simple analytic expression proposed by Greisen

Include the effects of electron ionization losses de/dt = constant= Approximation B critical energy

s=1 Approximation B elementary solution e

Include the effects of electron ionization losses de/dt = constant= critical energy Elementary Solutions that develop as exponential in depth Limit for small x

Equations for the correction functions

Rossi and Greisen show how the shape of the elementary functions can be obtained as a Power Series

Earlier results

Concept of : Shower AGE Shower Longitudinal Development Often used but (in my view) unsatisfactory definition Shower at maximum: s=1 Shower before maximum s < 1 Shower after maximum s > 1 S=

Age as a function of t/tmax

The Spectral shape of the electron Spectrum is determined (on very good approximation) by the shower Age The Photon Spectral; shape is (in good Approximation) also determined by the shower Age Calculated first by Rossi, Greisen in 1941 The Ratio photon/electron is determined by the shower Age Model Independent Definition of AGE

Go Beyond the Elementary Solutions Exponential Depth Dependent Realistic initial condition Depth Evolution of Monochromatic Photon E0 Monochromatic Electron E0 Age is a function of depth: s(t)

Monochromatic Photon

Monochromatic Photon Critical energy

Write initial condition as a superposition of power law component Inverse Mellin transform

Write initial condition as a superposition of power law component Inverse Mellin transform Depth Evolution

For a given E0, E, t what is the parameter s that dominate? Solution of this equation

For a given E0, E, t what is the parameter s that dominate? Solution of this equation

Monochromatic Photon

Monochromatic Photon. Approximation A,B

Different Energy : Same Age (Shower Maximum)

What About the Universality of Longitudinal Development?

Age and Longitudinal Development

Age and Longitudinal Developmen t S=

Age and Longitudinal Developmen t S= Differential Equation

Differential Equation Boundary Condition Solution : Greisen Profile

For real showers the longitudinal development is not identical to the Greisen Profile and fluctuates from shower to shower Violations of the Universality

For real showers the longitudinal development is not identical to the Greisen Profile and fluctuates from shower to shower Violations of the Universality General Model Independent Definition of Age