99 Years from Discovery : What is our current picture on Cosmic Rays? #6 How cosmic rays travel to Earth? Presented by Nahee Park
|
|
|
- Rhoda Russell
- 6 years ago
- Views:
Transcription
1
2 99 Years from Discovery : What is our current picture on Cosmic Rays? #6 How cosmic rays travel to Earth? Presented by Nahee Park
3 #5 How do Cosmic Rays gain their energy? I. Acceleration mechanism of CR II. Nature-made-accelerator in the universe & measurements
4 #5 How do Cosmic Rays gain their energy? I. Acceleration mechanism of CR -Fermi s acceleration theory : getting energy from encounters with moving magnetic field - Shock acceleration II. Nature-made-accelerator in the universe & measurements - Conditions for accelerate site Magnetic field to contain cosmic rays, Shock wave - Galactic cosmic rays : Supernova Clues from fluxes and gamma-ray sources - Extragalactic cosmic rays : Umm...AGN? Clues from anisotropy
5 #6 How cosmic rays travel to Earth? I. Itinerary of galactic cosmic rays II. Clues in the measurements III.Itinerary of extragalactic cosmic rays
6 Let s start from galactic cosmic rays Galactic Cosmic Rays Up to ~ ev Mostly accepted to be accelerated by Supernova Remnant
7 Let s start from galactic cosmic rays Galactic Cosmic Rays Galactic Cosmic Rays Up to ~ ev Mostly accepted to be accelerated by Supernova Remnant Extragalactic Cosmic Rays
8 Itinerary of Galactic Cosmic Rays source
9 Itinerary of Galactic Cosmic Rays acceleration site in galaxy source
10 Itinerary of Galactic Cosmic Rays acceleration site in galaxy source magnetic field Matter Photon field
11 Itinerary of Galactic Cosmic Rays Tycho 8k ~ 9.8k L.Y. 130k L.Y. SN k L.Y. 27k L.Y. IC443 5k L.Y.
12 Let s think about the scale 1 AU * 1 Astronomical Unit = meter = mile (c.f. length ratio between hair to Sears tower : ~ 10 6 )
13 Let s think about the scale 5.2 AU 1.5 AU ~10 AU ~30 AU ~19 AU 30~49 AU 1 AU * 1 Astronomical Unit = meter = mile (c.f. length ratio between hair to Sears tower : ~ 10 6 )
14 Let s think about the scale 5.2 AU 1.5 AU ~10 AU ~30 AU ~19 AU 30~49 AU 6.8 light hour = LY 1 AU * 1 Astronomical Unit = meter = mile (c.f. length ratio between hair to Sears tower : ~ 10 6 )
15 Let s think about the scale 5.2 AU 1.5 AU ~10 AU ~30 AU ~19 AU 30~49 AU 6.8 light hour = LY 1 AU * 1 Astronomical Unit = meter = mile (c.f. length ratio between hair to Sears tower : ~ 10 6 ) Earth Jupiter Saturn Uranus Neptune Pluto
16 Let s think about the scale 5.2 AU 1.5 AU ~10 AU ~30 AU ~19 AU 30~49 AU 6.8 light hour = LY 1 AU * 1 Astronomical Unit = meter = mile (c.f. length ratio between hair to Sears tower : ~ 10 6 ) Earth Jupiter Saturn Uranus Neptune 200~300 pc 8.5 kpc Pluto 65 kly =20 kpc
17 Propagation Theory Propagation Theory 200~300 pc 8.5 kpc 20 kpc Original amount at source Amount of CR measured at Earth From source to the Earth Convection Re-acceleration Decay : Change into other species Energy Loss : Energy loss ( matter, magnetic field, photon field) Diffusion : Scattering ( mainly magnetic field ) Spallation : Nuclear interaction destroying CR ( matter )
18 Propagation Theory Propagation Theory 200~300 pc 8.5 kpc 20 kpc Original amount at source All possible thing that can happen (Diffusion + re-acceleration + spallation ( +/- ) + decay + energy loss + convection) + = Amount of CR measured at Earth From source to the Earth Convection Re-acceleration Decay : Change into other species Energy Loss : Energy loss ( matter, magnetic field, photon field) Diffusion : Scattering ( mainly magnetic field ) Spallation : Nuclear interaction destroying CR ( matter )
19 Propagation Theory Interactions... Charged particle cosmic rays Coulomb scattering Ionization loss Cherenkov light Our knowledge on interactions Bremsstrahlung Interactions with special conditions Synchrotron radiation (with magnetic field) Transition Radiation (when matter changes) Inverse Compton Scattering (with photon-field) Annihilation (when it meets anti-matter) Our knowledge on the Galaxy Decays (for particular type of particles) Electromagnetic Radiation Photoelectric effect Compton scattering Pair production
20 Clues from the measurements Secondary to Primary ratio Lithium, Beryllium, Boron... Radioactive Clocks Diffused gamma-ray emission Anti-particles Anti-proton, positron Different interaction histories between electron and hadron
21 At GeV range Secondary to Primary Ratio Due to interaction between cosmic rays and matter in the galaxy, there should be some result (secondary particles) traveling to Earth If acceleration happens before traveling Longer journey Will have more interaction fluxes of secondary Energy
22 At GeV range Secondary to Primary Ratio Due to interaction between cosmic rays and matter in the galaxy, there should be some result (secondary particles) traveling to Earth If acceleration happens before traveling Longer journey Will have more interaction fluxes of secondary Energy
23 Secondary to Primary Ratio Simon et al., 1990 result from CRN- Chicago egg
24 Secondary to Primary Ratio Simon et al., 1990 result from CRN- Chicago egg
25 Secondary to Primary Ratio Simon et al., 1990 result from CRN- Chicago egg
26 Radioactive Clock Unstable nuclei Known stories about 10 Be 10 Be-> 10 B : half-life of 1.36 x 10 6 years Probability to create 10 Be from interaction 10 Be Other unstable nuclei 26 Al : 7.4 x 10 5 years 36 Cl : 3.1 x 10 5 years 59 Ni : 8.0 x 10 4 years 54 Mn : 303 days
27 Diffuse Gamma-ray Interaction between cosmic rays with matter in the galaxy will create gamma-ray Matter Distribution of gamma-ray should match with distribution of matter in the galaxy Fluxes of gamma-ray and our understanding of galaxy and interactions should agree
28 Diffuse Gamma-ray electron Proton Nuclear interaction π 0 decay gamma-ray Bremsstrahlung gamma-ray Matter Interaction between cosmic rays with matter in the galaxy will create gamma-ray Distribution of gamma-ray should match with distribution of matter in the galaxy Fluxes of gamma-ray and our understanding of galaxy and interactions should agree
29 Diffused gamma-ray (2) 8.5 kpc 200~300 pc 20 kpc dust sky map visible light sky map
30 Diffused gamma-ray (2) dust sky map visible light sky map
31 Diffused gamma-ray (2) dust sky map visible gamma light ray sky sky map
32 Diffused gamma-ray (3) Result from fermi gamma-ray telescope
33 Anti-particle Positron Anti-proton Light nucleus Nuclear Interaction High energy proton Decay γ π 0 γ νμ (νμ ) π + (π - ) neutron Light nucleus neutron μ + (μ - )
34 Different histories between e - & nuclei Proton and heavier nuclei Source site of CR Electron creation and acceleration propagation solar modulation Source site of CR creation and acceleration propagation solar modulation
35 Different histories between e - & nuclei Proton and heavier nuclei Source site of CR diffusion spallation loss by decay or interaction Electron creation and acceleration propagation solar modulation Source site of CR creation and acceleration propagation solar modulation
36 Different histories between e - & nuclei Proton and heavier nuclei Source site of CR diffusion spallation loss by decay or interaction Electron creation and acceleration propagation solar modulation Source site of CR diffusion secondary production loss by interaction creation and acceleration propagation solar modulation
37 Extragalactic cosmic rays Extragalactic Cosmic Rays Bending radius of charged particle in this energy region (10 20 ev) is ~ size of galaxy Probably extragalactic Somewhere ~ ev to higher (10 20 ev?) Acceleration by? Bottom-up scenario Top-bottom scenario Propagation Greisen-Zatsepin-Kuzmin cutoff (GZK cutoff, 1966) ev cosmic rays cannot travel further than ~ 13 Mpc due to interactions with cosmic microwave background (CMB)
38 Extragalactic cosmic rays Extragalactic Cosmic Rays Galactic Cosmic Rays Extragalactic Cosmic Rays Bending radius of charged particle in this energy region (10 20 ev) is ~ size of galaxy Probably extragalactic Somewhere ~ ev to higher (10 20 ev?) Acceleration by? Bottom-up scenario Top-bottom scenario Propagation Greisen-Zatsepin-Kuzmin cutoff (GZK cutoff, 1966) ev cosmic rays cannot travel further than ~ 13 Mpc due to interactions with cosmic microwave background (CMB)
39 Next Lecture What is the origin of Cosmic Rays? Is it really similar to solar system abundances? Coming from Interstellar medium? Coming from Supernova? (Galactic cosmic rays) Extragalactic cosmic rays : what is the origin of these?
40 Questions in the Lecture What is the speed of cosmic rays?
> News < AMS-02 will be launched onboard the Shuttle Endeavour On May 2nd 2:33 P.M. from NASA Kennedy space center!
> News < Anti-matter, dark matter measurement By measuring the cosmic rays (Mainly electron, positron, proton, anti-proton and light nuclei) AMS-02 will be launched onboard the Shuttle Endeavour On May
Topic 7. Relevance to the course
Topic 7 Cosmic Rays Relevance to the course Need to go back to the elemental abundance curve Isotopes of certain low A elements such as Li, Be and B have larger abundances on Earth than you would expect
Cosmic Ray Astronomy. Qingling Ni
Cosmic Ray Astronomy Qingling Ni What is Cosmic Ray? Mainly charged particles: protons (hydrogen nuclei)+helium nuclei+heavier nuclei What s the origin of them? What happened during their propagation?
Low-Energy Cosmic Rays
Low-Energy Cosmic Rays Cosmic rays, broadly defined, are charged particles from outside the solar system. These can be electrons, protons, or ions; the latter two dominate the number observed. They are
Propagation in the Galaxy 2: electrons, positrons, antiprotons
Propagation in the Galaxy 2: electrons, positrons, antiprotons As we mentioned in the previous lecture the results of the propagation in the Galaxy depend on the particle interaction cross section. If
Ultrahigh Energy Cosmic Rays propagation II
Ultrahigh Energy Cosmic Rays propagation II The March 6th lecture discussed the energy loss processes of protons, nuclei and gamma rays in interactions with the microwave background. Today I will give
The Physics of Cosmic Rays
The Physics of Cosmic Rays QuarkNet summer workshop July 23-27, 2012 1 Recent History Most natural phenomena can be explained by a small number of simple rules. You can determine what these rules are by
Supernova Remnants and Cosmic. Rays
Stars: Their Life and Afterlife Supernova Remnants and Cosmic 68 th Rays Brian Humensky Series, Compton Lecture #5 November 8, 2008 th Series, Compton Lecture #5 Outline Evolution of Supernova Remnants
Dr. John Kelley Radboud Universiteit, Nijmegen
arly impressive. An ultrahighoton triggers a cascade of particles mulation of the Auger array. The Many Mysteries of Cosmic Rays Dr. John Kelley Radboud Universiteit, Nijmegen Questions What are cosmic
Lecture 9 - Applications of 4 vectors, and some examples
Lecture 9 - Applications of 4 vectors, and some examples E. Daw April 4, 211 1 Review of invariants and 4 vectors Last time we learned the formulae for the total energy and the momentum of a particle in
Interstellar gamma rays. New insights from Fermi. Andy Strong. on behalf of Fermi-LAT collaboration. COSPAR Scientific Assembly, Bremen, July 2010
Interstellar gamma rays New insights from Fermi Andy Strong on behalf of Fermi-LAT collaboration COSPAR Scientific Assembly, Bremen, July 2010 Session E110: ' The next generation of ground-based Cerenkov
Investigation on mass composition of UHE cosmic rays using CRPropa 2.0
Investigation on mass composition of UHE cosmic rays using CRPropa. G Rastegarzade B Parvizi,, Physics Department, Semnan University, Semnan, P.O. Box 596-599, Iran Email: G_ rastegar@alum.sharif.edu Abstract
Ultra-High-Energy Cosmic Rays: A Tale of Two Observatories
Ultra-High-Energy Cosmic Rays: A Tale of Two Observatories RuoYu Shang Nicholas Sherer Fei Sun Bryce Thurston Measurement of the Depth of Maximumof Extensive Air Showers above 10 18 ev,"phys. Rev. Letters104(2010)
Extensive Air Showers and Particle Physics Todor Stanev Bartol Research Institute Dept Physics and Astronomy University of Delaware
Extensive Air Showers and Particle Physics Todor Stanev Bartol Research Institute Dept Physics and Astronomy University of Delaware Extensive air showers are the cascades that develop in the atmosphere
Ultra High Energy Cosmic Rays: Observations and Analysis
Ultra High Energy Cosmic Rays: Observations and Analysis NOT A NEW PROBLEM, STILL UNSOLVED John Linsley (PRL 10 (1963) 146) reports on the detection in Vulcano Ranch of an air shower of energy above 1020
Where do they originate? How do they gain their enourmous energies? What happens to them in transit from sources to us?
What do cosmic rays tell us about : Where do they originate? How do they gain their enourmous energies? What happens to them in transit from sources to us? Energies of cosmic ray particles: 1 watt of power
Neutrino Oscillations and Astroparticle Physics (5) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) Pisa, 10 May 2002
Neutrino Oscillations and Astroparticle Physics (5) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) Pisa, 10 May 2002 n High Energy Astronomy Multi-Messanger Astronomy Cosmic Rays
The High-Energy Interstellar Medium
The High-Energy Interstellar Medium Andy Strong MPE Garching on behalf of Fermi-LAT collaboration Cosmic Ray Interactions: Bridging High and Low Energy Astrophysics Lorentz Centre Workshop March 14-18
Cosmic Rays. M. Swartz. Tuesday, August 2, 2011
Cosmic Rays M. Swartz 1 History Cosmic rays were discovered in 1912 by Victor Hess: he discovered that a charged electroscope discharged more rapidly as he flew higher in a balloon hypothesized they were
Spectra of Cosmic Rays
Spectra of Cosmic Rays Flux of relativistic charged particles [nearly exactly isotropic] Particle density Power-Law Energy spectra Exponent (p, Nuclei) : Why power laws? (constraint on the dynamics of
Ultra High Energy Cosmic Rays I
Ultra High Energy Cosmic Rays I John Linsley (PRL 10 (1963) 146) reports on the detection in Vulcano Ranch of an air shower of energy above 1020 ev. Problem: the microwave background radiation is discovered
The Physics of Ultrahigh Energy Cosmic Rays. Example Poster Presentation Physics 5110 Spring 2009 Reminder: Posters are due Wed April 29 in class.
The Physics of Ultrahigh Energy Cosmic Rays Example Poster Presentation Physics 5110 Spring 2009 Reminder: Posters are due Wed April 29 in class. 1 Introduction to Cosmic Rays References: http://www.phy.bris.ac.uk/groups/particle/pus/affo
Dark matter annihilations and decays after the AMS-02 positron measurements
Dark matter annihilations and decays after the AMS-02 positron measurements Anna S. Lamperstorfer Technische Universität München SISSA - International School for Advanced Studies of Trieste Workshop The
IceCube. francis halzen. why would you want to build a a kilometer scale neutrino detector? IceCube: a cubic kilometer detector
IceCube francis halzen why would you want to build a a kilometer scale neutrino detector? IceCube: a cubic kilometer detector the discovery (and confirmation) of cosmic neutrinos from discovery to astronomy
Seeing the moon shadow in CRs
Seeing the moon shadow in CRs and using the Earth field as a spectrometer Tibet III Amenomori et al. arxiv:0810.3757 see also ARGO-YBJ results Bartoli et. al, arxiv:1107.4887 Milargo: 100% coverage r owe
Cosmic rays in the local interstellar medium
Cosmic rays in the local interstellar medium Igor V. Moskalenko Igor V. Moskalenko/NASA-GSFC 1 LMC (Magellanic Cloud Emission Nuclear Data-2004/09/28, Line Survey: Smith, Points) Santa Fe R - H G - [S
Secondary particles generated in propagation neutrinos gamma rays
th INT, Seattle, 20 Feb 2008 Ultra High Energy Extragalactic Cosmic Rays: Propagation Todor Stanev Bartol Research Institute Dept Physics and Astronomy University of Delaware Energy loss processes protons
Fermi-LAT data analysis of young Supernova Remnants for Cosmic-ray acceleration studies
Università degli Studi di Bari Aldo Moro Dipartimento Interateneo di Fisica M. Merlin Dottorato di ricerca in Fisica XXX ciclo Settore scientifico disciplinare FIS/01 Fermi-LAT data analysis of young Supernova
The Large Area Telescope on-board of the Fermi Gamma-Ray Space Telescope Mission
The Large Area Telescope on-board of the Fermi Gamma-Ray Space Telescope Mission 1 Outline Mainly from 2009 ApJ 697 1071 The Pair Conversion Telescope The Large Area Telescope Charged Background and Events
Mass Composition Study at the Pierre Auger Observatory
OBSERVATORY Mass Composition Study at the Pierre Auger Observatory Laura Collica for the Auger Milano Group 4.04.2013, Astrosiesta INAF Milano 1 Outline The physics: The UHECR spectrum Extensive Air Showers
Lecture 14 Cosmic Rays
Lecture 14 Cosmic Rays 1. Introduction and history 2. Locally observed properties 3. Interactions 4. Demodulation and ionization rate 5. Midplane interstellar pressure General Reference MS Longair, High
PHY320 Class Test Topic 1 Elemental Abundances All questions are worth 1 mark unless otherwise stated
Topic 1 Elemental Abundances 1. What is the origin of the Earth s atmosphere? 2. Name the 2 distinct topographical regions on the Moon. 3. In the model of chemical affinities which class of elements forms
Cosmic Rays: A Way to Introduce Modern Physics Concepts. Steve Schnetzer
Cosmic Rays: A Way to Introduce Modern Physics Concepts Steve Schnetzer Rutgers CR Workshop May 19, 2007 Concepts Astrophysics Particle Physics Radiation Relativity (time dilation) Solar Physics Particle
Absorption and production of high energy particles in the infrared background
Roma I, 16 March 2007 Absorption and production of high energy particles in the infrared background Todor Stanev Bartol Research Institute University of Delaware Newark, DE19716 We discuss the role of
The Fermi Gamma-ray Space Telescope
Abstract The Fermi Gamma-ray Space Telescope Tova Yoast-Hull May 2011 The primary instrument on the Fermi Gamma-ray Space Telescope is the Large Area Telescope (LAT) which detects gamma-rays in the energy
Cosmic Rays. Discovered in 1912 by Viktor Hess using electroscopes to measure ionization at altitudes via balloon
Cosmic Rays Discovered in 1912 by Viktor Hess using electroscopes to measure ionization at altitudes via balloon Nobel Prize in 1936 Origin of high energy cosmic rays is still not completely understood
BIG BANG SUMMARY NOTES
BIG BANG SUMMARY NOTES BIG BANG THEORY Studies of red-shifts of distant galaxies show that the universe is expanding. This and other observations has led to the Big Bang Theory The Big Bang Theory claims
Cosmic Accelerators. 2. Pulsars, Black Holes and Shock Waves. Roger Blandford KIPAC Stanford
Cosmic Accelerators 2. Pulsars, Black Holes and Shock Waves Roger Blandford KIPAC Stanford Particle Acceleration Unipolar Induction Stochastic Acceleration V ~ Ω Φ I ~ V / Z 0 Z 0 ~100Ω P ~ V I ~ V 2 /Z
Cosmogenic neutrinos II
Cosmogenic neutrinos II Dependence of fluxes on the cosmic ray injection spectra and the cosmological evolution of the cosmic ray sources Expectations from the cosmic ray spectrum measured by the Auger
Ultra High Energy Cosmic Rays. and
2011 BCVSPIN Advanced Study Institute in Particle Physics and Cosmology, Huê, Vietnam, 25-30 July 2011 Ultra High Energy Cosmic Rays and The Pierre Auger Observatory Paolo Privitera 1 Cosmic Rays are always
The positron and antiproton fluxes in Cosmic Rays
The positron and antiproton fluxes in Cosmic Rays Paolo Lipari INFN Roma Sapienza Seminario Roma 28th february 2017 Preprint: astro-ph/1608.02018 Author: Paolo Lipari Interpretation of the cosmic ray positron
Astronomy 1504 Section 10 Final Exam Version 1 May 6, 1999
Astronomy 1504 Section 10 Final Exam Version 1 May 6, 1999 Reminder: When I write these questions, I believe that there is one one correct answer. The questions consist of all parts a e. Read the entire
RECENT RESULTS FROM THE PIERRE AUGER OBSERVATORY
RECENT RESULTS FROM THE PIERRE AUGER OBSERVATORY (Neutrino 2008, Christchurch, NZ) Esteban Roulet (Bariloche) the Auger Collaboration: 17 countries, ~100 Institutions, ~400 scientists Argentina, Australia,
The Gamma-ray Albedo of the Moon
[albedo] the proportion of the incident light that is reflected by a surface The Gamma-ray Albedo of the Moon Igor V. Moskalenko & Troy A. Porter Astrophys. J. 670, 1467-1472 (2007) Masaki Mori ICRR CANGAROO
STUDY OF EXTENSIVE AIR SHOWERS IN THE EARTH S ATMOSPHERE
STUDY OF EXTENSIVE AIR SHOWERS IN THE EARTH S ATMOSPHERE I. BACIOIU * Institute of Space Science, P.O. Box MG-23, RO-077125 Bucharest-Magurele, Romania, E-mail: iuliana.bacioiu@spacescience.ro Abstract.
Particle Acceleration in the Universe
Particle Acceleration in the Universe Hiroyasu Tajima Stanford Linear Accelerator Center Kavli Institute for Particle Astrophysics and Cosmology on behalf of SLAC GLAST team June 7, 2006 SLAC DOE HEP Program
PH104 Lab 1 Light and Matter Pre-lab
Name: Lab Time: PH04 Lab Light and Matter Pre-lab. Goals Since this is the first lab, we don t want to try to do things that are too complex. We would like to get used to the lab room and some of the steps
a cosmic- ray propagation and gamma-ray code
GALPROP: a cosmic- ray propagation and gamma-ray code A. Strong, MPE Garching Tools for SUSY, Annecy, June 28 2006 The basis: cosmic-ray production & propagation in the Galaxy intergalactic space HALO
Cosmic Rays, Photons and Neutrinos
Cosmic Rays, Photons and Neutrinos Michael Kachelrieß NTNU, Trondheim [] Introduction Outline Plan of the lectures: Cosmic rays Galactic cosmic rays Basic observations Acceleration Supernova remnants Problems
Nonthermal Emission in Starburst Galaxies
Nonthermal Emission in Starburst Galaxies! Yoel Rephaeli!!! Tel Aviv University & UC San Diego Cosmic Ray Origin! San Vito, March 20, 2014 General Background * Stellar-related nonthermal phenomena * Particle
Ultrahigh Energy Cosmic Rays propagation I
Ultrahigh Energy Cosmic Rays propagation I Microwave background Energy loss processes for protons: - photoproduction interactions - pair production interactions - adiabatic loss due to the expansion of
Gamma rays from supernova remnants in clumpy environments.! Stefano Gabici APC, Paris
Gamma rays from supernova remnants in clumpy environments!! Stefano Gabici APC, Paris Overview of the talk Galactic cosmic rays Gamma rays from supernova remnants Hadronic or leptonic? The role of gas
At the conclusion of this lesson the trainee will be able to: a) Write a typical equation for the production of each type of radiation.
RADIOACTIVITY - SPONTANEOUS NUCLEAR PROCESSES OBJECTIVES At the conclusion of this lesson the trainee will be able to: 1. For~, p and 7 decays a) Write a typical equation for the production of each type
VHE emission from radio galaxies
VHE emission from radio galaxies Martin Hardcastle The future of gamma-ray astronomy and the CTA Leicester, October 2010 Outline Recap: radio galaxy physics Inverse-Compton emission Locations of high-energy
Questions 1pc = 3 ly = km
Cosmic Rays Historical hints Primary Cosmic Rays: - Cosmic Ray Energy Spectrum - Composition - Origin and Propagation - The knee region and the ankle Secondary CRs: -shower development - interactions Detection:
Neutrino Astronomy. Ph 135 Scott Wilbur
Neutrino Astronomy Ph 135 Scott Wilbur Why do Astronomy with Neutrinos? Stars, active galactic nuclei, etc. are opaque to photons High energy photons are absorbed by the CMB beyond ~100 Mpc 10 20 ev protons,
Frontiers: Ultra High Energy Cosmic Rays
Frontiers: Ultra High Energy Cosmic Rays We now focus on cosmic rays with almost unimaginable energies: 10 19 ev and beyond. The very highest energy cosmic rays have energies in excess of 50 Joules(!),
New results from the AMS experiment on the International Space Station. Henning Gast RWTH Aachen
New results from the AMS experiment on the International Space Station Henning Gast RWTH Aachen 1 Questions to AMS-02: Are there galaxies made of anti-matter in the Universe? What is the nature of Dark
ISAPP Gran Sasso June 28-July 9, Observations of Cosmic Rays
ISAPP 2004 Gran Sasso June 28-July 9, 2003 Observations of Cosmic Rays Tiina Suomijärvi Institut de Physique Nucléaire Université Paris XI-Orsay, IN2P3/CNRS France Why to Study Cosmic Rays? Cosmic rays
In the Beginning. After about three minutes the temperature had cooled even further, so that neutrons were able to combine with 1 H to form 2 H;
In the Beginning Obviously, before we can have any geochemistry we need some elements to react with one another. The most commonly held scientific view for the origin of the universe is the "Big Bang"
An Auger Observatory View of Centaurus A
An Auger Observatory View of Centaurus A Roger Clay, University of Adelaide based on work particularly done with: Bruce Dawson, Adelaide Jose Bellido, Adelaide Ben Whelan, Adelaide and the Auger Collaboration
A New View of the High-Energy γ-ray Sky with the Fermi Telescope
A New View of the High-Energy γ-ray Sky with the Fermi Telescope Aurelien Bouvier KIPAC/SLAC, Stanford University On behalf of the Fermi collaboration SNOWPAC, 2010 The Fermi observatory Launch: June 11
Upper Limit of the Spectrum of Cosmic Rays
Upper Limit of the Spectrum of Cosmic Rays David Fraebel, Cristian Gaidau, Allycia Gariepy, Rita Garrido Menacho Friday 22.11.2013 G.T. Zatsepin and V.A. Kuzmin 1966, JETP Let. 4, p.78 Outline Motivation
PERSPECTIVES of HIGH ENERGY NEUTRINO ASTRONOMY. Paolo Lipari Vulcano 27 may 2006
PERSPECTIVES of HIGH ENERGY NEUTRINO ASTRONOMY Paolo Lipari Vulcano 27 may 2006 High Energy Neutrino Astrophysics will CERTAINLY become an essential field in a New Multi-Messenger Astrophysics What is
Ultra-High Energy Cosmic Rays and the GeV-TeV Diffuse Gamma-Ray Flux
The 4th International Workshop on The Highest Energy Cosmic Rays and Their Sources INR, Moscow May 20-22, 2008 Ultra-High Energy Cosmic Rays and the GeV-TeV Diffuse Gamma-Ray Flux Oleg Kalashev* (INR RAS)
Particle Physics Beyond Laboratory Energies
Particle Physics Beyond Laboratory Energies Francis Halzen Wisconsin IceCube Particle Astrophysics Center Nature s accelerators have delivered the highest energy protons, photons and neutrinos closing
Nucleosíntesis primordial
Tema 5 Nucleosíntesis primordial Asignatura de Física Nuclear Curso académico 2009/2010 Universidad de Santiago de Compostela Big Bang cosmology 1.1 The Universe today The present state of the Universe
Major Option C1 Astrophysics. C1 Astrophysics
C1 Astrophysics Course co-ordinator: Julien Devriendt jeg@astro.ox.ac.uk C1 offers a total of ~40 lectures on five themes covering a broad range of topics in contemporary astrophysics. Each theme takes
Cosmic Rays - R. A. Mewaldt - California Institute of Technology
Cosmic Rays - R. A. Mewaldt - California Institute of Technology Cosmic rays are high energy charged particles, originating in outer space, that travel at nearly the speed of light and strike the Earth
Formation of the Universe & What is in Space? The Big Bang Theory and components of the Universe
Formation of the Universe & What is in Space? The Big Bang Theory and components of the Universe The Big Bang Theory The Big Bang Theory The Big Bang Theory is the most widely accepted scientific explanation
Multi-Messenger Astonomy with Cen A?
Multi-Messenger Astonomy with Cen A? Michael Kachelrieß NTNU, Trondheim [] Outline of the talk 1 Introduction 2 Dawn of charged particle astronomy? Expectations vs. Auger data Effects of cluster fields
Constraints on cosmic-ray origin from gamma-ray observations of supernova remnants
Constraints on cosmic-ray origin from gamma-ray observations of supernova remnants Marianne Lemoine-Goumard (CENBG, Université Bordeaux, CNRS-IN2P3, France) On behalf of the Fermi-LAT and HESS Collaborations
Galactic cosmic rays propagation
Galactic cosmic rays propagation Side view of the Galaxy The Solar system is 8.5 kpc away from the galactic center. One pc is 3.10 18 cm, so we are at a distance of 2.55 10 17 km and the light from it
1939 Baade&Zwicky 1949 Fermi 1977 (Krymski; Axford; Bell; Blandford & Ostriker
46 1939 Baade&Zwicky 1949 Fermi 1977 (Krymski; Axford; Bell; Blandford & Ostriker From Aharonian et al. 2011 From Letessier-Sevon & Stanev 2011 Fermi 2-year sky map Outline 1. 2. 3. 4. knee ankle (b)
3 Radioactivity - Spontaneous Nuclear Processes
3 Radioactivity - Spontaneous Nuclear Processes Becquerel was the first to detect radioactivity. In 1896 he was carrying out experiments with fluorescent salts (which contained uranium) and found that
Emphasis on what happens to emitted particle (if no nuclear reaction and MEDIUM (i.e., atomic effects)
LECTURE 5: INTERACTION OF RADIATION WITH MATTER All radiation is detected through its interaction with matter! INTRODUCTION: What happens when radiation passes through matter? Emphasis on what happens
The Expanding Universe
Cosmology Expanding Universe History of the Universe Cosmic Background Radiation The Cosmological Principle Cosmology and General Relativity Dark Matter and Dark Energy Primitive Cosmology If the universe
Gamma ray and antiparticles (e + and p) as tools to study the propagation of cosmic rays in the Galaxy
Gamma ray and antiparticles (e + and p) as tools to study the propagation of cosmic rays in the Galaxy INFN Sez. La Sapienza, Rome, Italy E-mail: paolo.lipari@roma1.infn.it The spectra of cosmic rays observed
Ryan Stillwell Paper: /10/2014. Neutrino Astronomy. A hidden universe. Prepared by: Ryan Stillwell. Tutor: Patrick Bowman
Neutrino Astronomy A hidden universe Prepared by: Ryan Stillwell Tutor: Patrick Bowman Paper: 124.129 Date: 10 October 2014 i Table of Contents 1. Introduction pg 1 1.1 Background pg 1 2. Findings & Discussion
Cosmic rays and the diffuse gamma-ray emission
Cosmic rays and the diffuse gamma-ray emission Dipartimento di Fisica, Torino University and INFN Sezione di Torino via P. Giuria 1, 10125 Torino, Italy E-mail: donato@to.infn.it The diffuse γ-ray emission
PHY326/426 Dark Matter and the Universe. Dr. Vitaly Kudryavtsev F9b, Tel.:
PHY326/426 Dark Matter and the Universe Dr. Vitaly Kudryavtsev F9b, Tel.: 0114 2224531 v.kudryavtsev@sheffield.ac.uk Indirect searches for dark matter WIMPs Dr. Vitaly Kudryavtsev Dark Matter and the Universe
Cosmic ray electrons from here and there (the Galactic scale)
Cosmic ray electrons from here and there (the Galactic scale) Julien Lavalle Department of Theoretical Physics Torino University and INFN Outline: (i) local electrons (ii) comments on synchrotron [based
FYST17 Lecture 13 The cosmic connection. Thanks to R. Durrer, L. Covi, S. Sakar
FYST17 Lecture 13 The cosmic connection Thanks to R. Durrer, L. Covi, S. Sakar 1 Today s outline High energy cosmic rays GKZ cut-off Detectors in space The PAMELA signal Some words on the expansion of
On the GCR/EGCR transition and UHECR origin
UHECR 2014 13 15 October 2014 / Springdale (Utah; USA) On the GCR/EGCR transition and UHECR origin Etienne Parizot 1, Noémie Globus 2 & Denis Allard 1 1. APC Université Paris Diderot France 2. Tel Aviv
Dark Matter in the Universe
Dark Matter in the Universe NTNU Trondheim [] Experimental anomalies: WMAP haze: synchrotron radiation from the GC Experimental anomalies: WMAP haze: synchrotron radiation from the GC Integral: positron
Lecture 6: The Physics of Light, Part 1. Astronomy 111 Wednesday September 13, 2017
Lecture 6: The Physics of Light, Part 1 Astronomy 111 Wednesday September 13, 2017 Reminders Star party tonight! Homework #3 due Monday Exam #1 Monday, September 25 The nature of light Look, but don t
Gamma-ray Astrophysics
Gamma-ray Astrophysics AGN Pulsar SNR GRB Radio Galaxy The very high energy -ray sky NEPPSR 25 Aug. 2004 Many thanks to Rene Ong at UCLA Guy Blaylock U. of Massachusetts Why gamma rays? Extragalactic Background
The Galactic diffuse gamma ray emission in the energy range 30 TeV 3 PeV
The Galactic diffuse gamma ray emission in the energy range 30 TeV 3 PeV Mount Rainier by Will Christiansen Silvia Vernetto & Paolo Lipari 35th ICRC 12-20 July 2017 - Busan - South Korea Gamma ray astronomy
The AGN Jet Model of the Fermi Bubbles
The AGN Jet Model of the Fermi Bubbles Fulai Guo Shanghai Astronomical Observatory IAU 322 Symposium, Palm Cove, July 18-22, 2016 1 The All-sky Fermi View at E >10 GeV The Fermi bubbles! (NASA image based
Ultra-High Energy Cosmic Rays and Astrophysics. Hang Bae Kim Hanyang University Hangdang Workshop,
Ultra-High Energy Cosmic Rays and Astrophysics Hang Bae Kim Hanyang University Hangdang Workshop, 2012. 08. 22 Ultra High Energy Cosmic Rays Ultra High Energy Cosmic Ray (UHECR)» E 3 E & 10 18 ev Energy
Supernova Remnants as Cosmic Ray Accelerants. By Jamie Overbeek Advised by Prof. J. Finley
Supernova Remnants as Cosmic Ray Accelerants By Jamie Overbeek Advised by Prof. J. Finley Cosmic Rays Discovered by Victor Hess in 1911 during a balloon flight through Austria He used an electroscope to
Special Topics in Nuclear and Particle Physics
Special Topics in Nuclear and Particle Physics Astroparticle Physics Lecture 5 Gamma Rays & x-rays Sept. 22, 2015 Sun Kee Kim Seoul National University Gamma ray astronomy gamma ray synchrotron radition
STATUS OF ULTRA HIGH ENERGY COSMIC RAYS
STATUS OF ULTRA HIGH ENERGY COSMIC RAYS Esteban Roulet (Bariloche) COSMO / CosPA 2010, Tokyo Power law flux stochastic (Fermi) acceleration in shocks cosmic ray flux Small fractional energy gain after
Linear and non-linear evolution of the gyroresonance instability in Cosmic Rays
Linear and non-linear evolution of the gyroresonance instability in Cosmic Rays DESY Summer Student Programme, 2016 Olga Lebiga Taras Shevchenko National University of Kyiv, Ukraine Supervisors Reinaldo
Units and Definition
RADIATION SOURCES Units and Definition Activity (Radioactivity) Definition Activity: Rate of decay (transformation or disintegration) is described by its activity Activity = number of atoms that decay
Cosmic Rays. This showed that the energy of cosmic rays was many times that of any other natural or artificial radiation known at that time.
Cosmic Rays 1. Discovery As long ago as 1900, C. T. R. Wilson and others found that the charge on an electroscope always 'leaked' away in time, and this could never be prevented, no matter how good the
Cosmic Ray Transport (in the Galaxy) Luke Drury. Dublin Institute for Advanced Studies Institiúid Ard-Léinn Bhaile Átha Cliath
Cosmic Ray Transport (in the Galaxy) Luke Drury Dublin Institute for Advanced Studies Institiúid Ard-Léinn Bhaile Átha Cliath 1 A few disclaimers and preliminary remarks! Not my main field of research
Astro2020 Science White Paper Prospects for the detection of synchrotron halos around middle-age pulsars
Astro2020 Science White Paper Prospects for the detection of synchrotron halos around middle-age pulsars Thematic Areas: Planetary Systems Star and Planet Formation Formation and Evolution of Compact Objects
The slides with white background you need to know. The slides with blue background just have some cool information.
The slides with white background you need to know. The slides with blue background just have some cool information. The Big Bang cosmology the study of the origin, properties, processes, and evolution
Dark gas contribution to diffuse gamma-ray emission
Dark gas contribution to diffuse gamma-ray emission Masaki Mori ICRR CANGAROO group internal seminar, November 7, 2005 Adrian Cho S. Hunter, GLAST meeting, Oct.2004 The Galactic Diffuse Gamma-ray Emission...