Stanev High Energy Cosmic Rays

2. Auflage 2010
ISBN: 978-3-540-85148-6
Verlag: Springer Berlin Heidelberg
Format: PDF
Kopierschutz: 1 - PDF Watermark

E-Book, Englisch, 333 Seiten

Reihe: Astronomy and Planetary Sciences

Offers an accessible text and reference (a cosmic-ray manual) for graduate students entering the field and high-energy astrophysicists will find this an accessible cosmic-ray manual Easy to read for the general astronomer, the first part describes the standard model of cosmic rays based on our understanding of modern particle physics. Presents the acceleration scenario in some detail in supernovae explosions as well as in the passage of cosmic rays through the Galaxy. Compares experimental data in the atmosphere as well as underground are compared with theoretical models

Autoren/Hrsg.

Stanev, Todor

Inhaltsverzeichnis

1;Dedication;5
2;Preface to the second edition;6
3;Preface to the first edition;7
4;Table of Contents;8
5;1 Overview;12
5.1;1.1 Where does the cosmic ray field belong?;12
5.2;1.2 Is progress in the cosmic ray field slow?;18
5.3;1.3 Main topics for future research;20
5.4;1.4 How this book is organized;22
6;Part I The Standard Model of Cosmic Rays;25
6.1;2 Cosmic ray interactions;26
6.1.1;2.1 Components and structure of matter;26
6.1.1.1;2.1.1 Strong, electromagnetic and weak interactions;28
6.1.1.2;2.1.2 Units of energy and interaction strength;28
6.1.2;2.2 Electromagnetic processes in matter;29
6.1.2.1;2.2.1 Coulomb scattering;29
6.1.2.2;2.2.2 Ionization loss;30
6.1.2.3;2.2.3 Cherenkov light;31
6.1.2.4;2.2.4 Compton scattering;32
6.1.2.5;2.2.5 Bremsstrahlung;33
6.1.2.6;2.2.6 Creation of electron–positron pairs;36
6.1.3;2.3 Electromagnetic collisions on magnetic and photon fields;37
6.1.3.1;2.3.1 Synchrotron radiation;37
6.1.3.2;2.3.2 Inverse Compton effect;39
6.1.4;2.4 Inelastic hadronic interactions below 1,000 GeV;40
6.1.4.1;2.4.1 Secondary particles spectra, average multiplicity and inelasticity;43
6.1.4.2;2.4.2 Kinematic variables and invariant cross-section;47
6.1.5;2.5 Nuclear fragmentation;48
6.2;3 The birth of cosmic rays;51
6.2.1;3.1 Stellar energetics. The pp chain;51
6.2.1.1;3.1.1 Solar neutrinos;53
6.2.1.2;3.1.2 Stellar evolution;59
6.2.1.3;3.1.3 Supernova explosions;62
6.2.1.4;3.1.4 Supernova neutrinos;63
6.2.1.5;3.1.5 Supernova remnants;67
6.2.2;3.2 Acceleration of cosmic rays;70
6.2.2.1;3.2.1 Stochastic acceleration of charged particles;70
6.2.2.2;3.2.2 Particle acceleration at astrophysical shocks;73
6.2.2.3;3.2.3 Acceleration with energy loss;78
6.3;4 Cosmic rays in the Galaxy;80
6.3.1;4.1 Interstellar matter and magnetic field;81
6.3.2;4.2 Basic principles of the propagation;85
6.3.2.1;4.2.1 Particle diffusion;86
6.3.3;4.3 Formation of the chemical composition;88
6.3.4;4.4 Diffuse galactic gamma rays;92
6.3.4.1;4.4.1 Relative importance of .-ray production processes;93
6.3.4.2;4.4.2 More exact .-ray yields;94
6.3.4.3;4.4.3 Energy spectrum of .-rays from the central Galaxy;95
6.4;5 Cosmic rays at the top of the atmosphere;98
6.4.1;5.1 Cosmic ray detectors;99
6.4.2;5.2 Solar modulation;103
6.4.3;5.3 Geomagnetic field effects;106
6.4.4;5.4 Cosmic ray spectra and composition;109
6.4.4.1;5.4.1 Energy spectra of different cosmic ray components;114
6.4.4.2;5.4.2 Electron spectrum;123
6.4.4.3;5.4.3 Antiprotons;126
6.5;6 Cosmic rays in the atmosphere;128
6.5.1;6.1 Atmospheric structure;129
6.5.2;6.2 Analytic approximations;131
6.5.2.1;6.2.1 Muons from meson decay;133
6.5.3;6.3 Muon fluxes in the atmosphere;135
6.5.3.1;6.3.1 Experimental results on atmospheric muons;136
6.6;7 Cosmic rays underground;144
6.6.1;7.1 High energy muons underground;145
6.6.2;7.2 Atmospheric neutrinos;153
6.6.2.1;7.2.1 Upward-going muons;158
6.6.2.2;7.2.2 Flux calculations;162
6.6.2.3;7.2.3 Experimental data;166
6.6.3;7.3 Neutrino oscillations;169
6.6.3.1;7.3.1 Matter effects;171
6.6.3.2;7.3.2 Oscillation parameters;172
7;Part II Contemporary Challenges;179
7.1;8 Cosmic ray showers;180
7.1.1;8.1 Electromagnetic cascades;181
7.1.1.1;8.1.1 Electromagnetic cascade theory;182
7.1.1.2;8.1.2 Monte Carlo calculations;186
7.1.2;8.2 Hadronic showers;190
7.1.2.1;8.2.1 Air shower detection;197
7.1.2.2;8.2.2 Reconstruction of the shower parameters from the observations;199
7.1.3;8.3 Extension of the hadronic interaction models;210
7.1.3.1;8.3.1 The minijet model;211
7.1.3.2;8.3.2 Monte Carlo realization of QCD models;213
7.1.3.3;8.3.3 Contemporary models used for the analysis of air shower data;216
7.1.4;8.4 Energy spectrum and composition at the knee;219
7.2;9 The end of the cosmic ray spectrum;227
7.2.1;9.1 Cosmic microwave background;228
7.2.2;9.2 UHECR interactions on the microwave background;229
7.2.2.1;9.2.1 Propagation of UHE protons in the Universe;233
7.2.2.2;9.2.2 Propagation of UHE nuclei;237
7.2.3;9.3 Experimental results and implications;239
7.2.3.1;9.3.1 Giant air shower detectors;239
7.2.3.2;9.3.2 Spectrum and composition of UHECR;243
7.2.3.3;9.3.3 Possible astrophysical sources of UHECR;249
7.2.3.4;9.3.4 Exotic models;253
7.2.4;9.4 UHECR astronomy;257
7.2.4.1;9.4.1 Arrival directions of UHECR;258
7.2.4.2;9.4.2 UHECR and the cosmic magnetic fields;262
7.2.5;9.5 Current status of the field;266
7.2.6;9.6 Future detectors;268
7.3;10 High energy neutrino and gamma-ray astronomy;272
7.3.1;10.1 The neutrino cross-section at very high energy;274
7.3.2;10.2 Gamma-ray telescopes;275
7.3.2.1;10.2.1 Satellite gamma-ray telescopes;275
7.3.2.2;10.2.2 Ground-based gamma-ray telescopes;276
7.3.3;10.3 Galactic gamma-ray and neutrino fluxes;279
7.3.3.1;10.3.1 Galactic binary systems – Cygnus X-3 tales;280
7.3.3.2;10.3.2 Supernova remnants;282
7.3.3.3;10.3.3 Observational constraints;283
7.3.4;10.4 Extragalactic sources;287
7.3.4.1;10.4.1 Observations of GeV and TeV gamma-rays from extragalactic sources;288
7.3.4.2;10.4.2 Models of gamma-ray production in AGN;290
7.3.4.3;10.4.3 Models of neutrino production in AGN;294
7.3.4.4;10.4.4 Neutrino production in GRB;296
7.3.4.5;10.4.5 Diffuse extragalactic neutrinos;297
7.3.4.6;10.4.6 Summary of the expected neutrino fluxes;298
7.3.5;10.5 Neutrinos and UHE cosmic rays;301
7.3.5.1;10.5.1 Neutrinos from propagation of ultra high energy cosmic rays;303
7.3.6;10.6 Detection of high energy astrophysical neutrinos;306
7.3.6.1;10.6.1 Detection of neutrino-induced showers;307
7.3.6.2;10.6.2 Neutrino oscillations and neutrino telescopes;310
7.3.6.3;10.6.3 Neutrino telescopes;311
8;A Appendix;317
8.1;A.1 Physical constants;317
8.2;A.2 Astrophysical constants;318
8.3;A.3 Properties of particles discussed in the book;318
9;References;320
10;Index;331