Table of Contents: Particles and astrophysics

Particles and astrophysics a multi-messenger approach /

This book is an introduction to "multi-messenger" astrophysics. It covers the many different aspects connecting particle physics with astrophysics and cosmology and introduces astrophysics using numerous experimental findings recently obtained through the study of high-energy particles. Ta...

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Main Author:	Spurio, Maurizio,
Other Authors:	SpringerLink (Online service)
Format:	eBook
Language:	English
Published:	Switzerland : Springer, [2015]
Physical Description:	1 online resource (498 pages) : illustrations.
Series:	Astronomy and astrophysics library.
Subjects:	Astrophysics. Particles (Nuclear physics) Physics. Mathematical physics.

Table of Contents:

Machine generated contents note:
1.
Overview of Astroparticle Physics
1.1.
Introduction
1.1.1.
Astrophysics and Astroparticle Physics
1.1.2.
Discoveries and Experiments Not Covered in This Book
1.2.
Cosmic Rays
1.3.
Gamma-Rays of GeV and TeV Energies
1.4.
Neutrino Astrophysics
1.5.
Dark Universe
1.6.
Laboratories and Detectors for Astroparticle Physics
1.6.1.
Space Experiments
1.6.2.
Experiments in the Atmosphere
1.6.3.
Ground-Based Experiments
1.7.
Underground Laboratories for Rare Events
References
2.
Cosmic Rays and Our Galaxy
2.1.
Discovery of Cosmic Rays
2.2.
Cosmic Rays and the Early Days of Particle Physics
2.3.
Discovery of the Positron and Particle Detectors
2.3.1.
Motion in a Magnetic Field and the Particle Rigidity
2.3.2.
Identification of the Positron
2.4.
Toy Telescope for Primary Cosmic Rays
2.5.
Differential and Integral Flux
2.6.
Energy Spectrum of Primary Cosmic Rays
2.7.
Physical Properties of the Galaxy
2.7.1.
Galactic Magnetic Field
2.7.2.
Interstellar Matter Distribution
2.8.
Low-Energy Cosmic Rays from the Sun
2.9.
Effect of the Geomagnetic Field
2.10.
Number and Energy Density of the Cosmic Rays
2.11.
Energy Considerations on Cosmic Ray Sources
References
3.
Direct Cosmic Rays Detection: Protons, Nuclei, Electrons and Antimatter
3.1.
Generalities on Direct Measurements
3.2.
Calorimetric Technique
3.2.1.
Hadronic Interaction Length and Mean Free Path
3.2.2.
Electromagnetic Radiation Length
3.2.3.
Hadronic Interaction Length and Mean Free Path in the Atmosphere
3.3.
Balloon Experiments
3.4.
Satellite Experiments
3.4.1.
IMP Experiments
3.4.2.
PAMELA Experiment
3.5.
AMS-02 Experiment on the International Space Station
3.6.
Abundances of Elements in the Solar System and in CRs
3.6.1.
Cosmic Abundances of Elements
3.7.
Energy Spectrum of CR Protons and Nuclei
3.8.
Antimatter in Our Galaxy
3.9.
Electrons and Positrons
3.9.1.
Positron Component
3.9.2.
Considerations on the e+, e- Components
References
4.
Indirect Cosmic Rays Detection: Particle Showers in the Atmosphere
4.1.
Introduction and Historical Information
4.2.
Structure of the Atmosphere
4.3.
Electromagnetic (EM) Cascade
4.3.1.
Heitler's Model of EM Showers
4.3.2.
Analytic Solutions
4.4.
Showers Initiated by Protons and Nuclei
4.4.1.
Muon Component in a Proton-Initiated Cascade
4.4.2.
EM Component in a Proton-Initiated Cascade
4.4.3.
Depth of the Shower Maximum for a Proton Shower
4.4.4.
Showers Induced by Nuclei: The Superposition Model
4.5.
Monte Carlo Simulations of Showers
4.6.
Detectors of Extensive Air Showers at the Energy of the Knee
4.6.1.
Toy Example of an EAS Array
4.6.2.
Some EAS Experiments
4.6.3.
Cherenkov Light Produced by EAS Showers
4.7.
Time Profile of Cascades
4.8.
Arrival Direction of CRs as Measured with EAS Arrays
4.9.
CR Flux Measured with EAS Arrays
4.10.
Mass Composition of CRs Around the Knee
4.10.1.
Ne Versus N? Method
4.10.2.
Depth of the Shower Maximum
References
5.
Diffusion of Cosmic Rays in the Galaxy
5.1.
Overabundance of Li, Be, and B in CRs
5.1.1.
Production of Li, Be, and B During Propagation
5.2.
Dating of Cosmic Rays with Radioactive Nuclei
5.2.1.
Unstable Secondary-to-Primary Ratios
5.3.
Diffusion-Loss Equation
5.3.1.
Diffusion Equation with Nuclear Spallation
5.3.2.
Numerical Estimate of the Diffusion Coefficient D
5.4.
Leaky box Model and its Evolutions
5.5.
Energy-Dependence of the Escape Time ?esc
5.6.
Energy Spectrum of Cosmic Rays at the Sources
5.7.
Anisotropies due to the Diffusion
5.7.1.
Compton
Getting Effect
5.8.
Electron Energy Spectrum at the Sources
5.8.1.
Synchrotron Radiation
5.8.2.
Measured Energy Spectrum of Electrons
5.8.3.
Average Distance of Accelerators of Electrons
References
6.
Acceleration Mechanisms and Galactic Cosmic Ray Sources
6.1.
Second- and First-Order Fermi Acceleration Mechanisms
6.1.1.
Magnetic Mirrors
6.1.2.
Second-Order Fermi Acceleration Mechanism
6.1.3.
First-Order Fermi Acceleration Mechanism
6.1.4.
Power-Law Energy Spectrum from the Fermi Model
6.2.
Diffusive Shock Acceleration in Strong Shock Waves
6.2.1.
Supernova Explosions and Cosmic Rays Acceleration
6.2.2.
Relevant Quantities in a Supernova Explosion
6.3.
Maximum Energy Attainable in the Supernova Model
6.4.
Spectral Index of the Energy Spectrum
6.4.1.
Escape Probability
6.4.2.
Shock Front in a Mono-Atomic Gas
6.5.
Success and Limits of the Standard Model of Cosmic Ray Acceleration
6.6.
White Dwarfs and Neutron Stars
6.6.1.
White Dwarfs
6.6.2.
Neutron Stars and Pulsars
6.7.
Possible Galactic Sources of Cosmic Rays Above the Knee
6.7.1.
Simple Model Involving Pulsars
6.7.2.
Simple Model Involving Binary Systems
References
7.
Ultra High Energy Cosmic Rays
7.1.
Observational Cosmology and the Universe
7.2.
Large-Scale Structure of the Universe
7.3.
Anisotropy of UHECRs: The Extragalactic Magnetic Fields
7.4.
Quest for Extragalactic Sources of UHECRs
7.5.
Propagation of UHECRs
7.5.1.
Adiabatic Energy Loss
7.5.2.
Propagation in the CMB: The GZK Cut-Off
7.5.3.
e± Pair Production by Protons on the CMB
7.5.4.
Propagation in the Extragalactic Magnetic Field
7.6.
Fluorescence Light and Fluorescence Detectors
7.7.
UHECR Measurements with a Single Technique
7.7.1.
Results from HiRes and AGASA
7.8.
Large Hybrid Observatories of UHECRs
7.9.
Flux of UHECRs
7.10.
Chemical Composition of UHECRs
7.11.
Correlation of UHECRs with Astrophysical Objects
7.12.
Constraints on Top-Down Models
7.13.
Summary and Discussion of the Results
References
8.
Sky Seen in ?-rays
8.1.
Spectral Energy Distribution (SED) and Multiwavelength Observations
8.2.
Astrophysical ?-rays: The Hadronic Model
8.2.1.
Energy Spectrum of ?-rays from ?° Decay
8.3.
Galactic Sources and ?-rays
8.3.1.
Simple Estimate of the ?-ray Flux from a Galactic Source
8.4.
Astrophysical ?-rays: The Leptonic Model
8.4.1.
Synchrotron Radiation from a Power-Law Spectrum
8.4.2.
Synchrotron Self-Absorption
8.4.3.
Inverse Compton Scattering and SSC
8.5.
Compton Gamma Ray Observatory Legacy
8.5.1.
EGRET ?-ray Sky
8.6.
Fermi-LAT and Other Experiments for ?-ray Astronomy
8.6.1.
Fermi-LAT
8.6.2.
AGILE and Swift
8.7.
Diffuse ?-rays in the Galactic Plane
8.7.1.
Estimate of the Diffuse ?-ray Flux
8.8.
Fermi-LAT Catalogs
8.9.
Gamma Ray Bursts
8.9.1.
Classification of GRBs
8.10.
Limits of ?-ray Observations from Space
References
9.
TeV Sky and Multiwavelength Astrophysics
9.1.
Imaging Cherenkov Technique
9.1.1.
Gamma-Ray Versus Charged CR Discrimination
9.1.2.
HESS, VERITAS and MAGIC
9.2.
EAS Arrays for ?-astronomy
9.2.1.
Sensitivity of ?-ray Experiments
9.3.
TeV Astronomy: The Catalog
9.4.
Gamma-Rays from Pulsars
9.5.
CRAB Pulsar and Nebula
9.6.
Problem of the Identification of Galactic CR Sources
9.7.
Extended Supernova Remnants
9.7.1.
SED of Some Peculiar SNRs
9.8.
Summary of the Study of Galactic Accelerators
9.9.
Active Galaxies
9.10.
Extragalactic ?-ray Sky
9.11.
Spectral Energy Distributions of Blazars
9.11.1.
Quasi-Simultaneous.
SEDs of Fermi-LAT Blazars
9.11.2.
Simultaneous SED Campaigns and Mrk 421
9.12.
Jets in Astrophysics
9.12.1.
Time Variability in Jets
9.13.
Extragalactic Background Light
References
10.
High-Energy Neutrino Astrophysics
10.1.
CRs, ?-rays and Neutrino Connection
10.1.1.
Neutrino Detection Principle
10.2.
Background in Large Volume Neutrino Detectors
10.3.
Neutrino Detectors and Neutrino Telescopes
10.3.1.
Muon Neutrino Detection
10.3.2.
Showering Events
10.4.
Cosmic Neutrino Flux Estimates
10.4.1.
Reference Neutrino Flux from a Galactic Source
10.4.2.
Extragalactic Diffuse Neutrino Flux
10.4.3.
Neutrinos from GRBs
10.4.4.
Cosmogenic Neutrinos
10.5.
Why km3-Scale Telescopes
10.5.1.
Neutrino Effective Area of Real Detectors
10.5.2.
Number of Optical Sensors in a Neutrino Telescope
10.6.
Water and Ice Properties
10.7.
Operating Neutrino Telescopes
10.7.1.
Telescope in the Antarctic Ice
10.7.2.
Telescope in the Mediterranean Sea
10.8.
Results from Neutrino Telescopes
10.8.1.
Point-Like Sources
10.8.2.
Limits from GRBs and Unresolved Sources
10.9.
First Measurement of Cosmic Neutrinos
References
11.
Atmospheric Muons and Neutrinos
11.1.
Nucleons in the Atmosphere
11.2.
Secondary Mesons in the Atmosphere
11.3.
Muons and Neutrinos from Charged Meson Decays
11.3.1.
Conventional Atmospheric Neutrino Flux
11.3.2.
Prompt Component in the Muon and Neutrino Flux
11.4.
Particle Flux at Sea Level
11.5.
Measurements of Muons at Sea Level
11.6.
Underground Muons
11.6.1.
Depth-Intensity Relation
11.6.2.
Characteristics of Underground/Underwater Muons
11.7.
Atmospheric Neutrinos
11.7.1.
Early Experiments
11.8.
Oscillations of Atmospheric Neutrinos.
Note continued:
11.9.
Measurement of Atmospheric ?? Oscillations in Underground Experiments
11.9.1.
Event Topologies in Super-Kamiokande
11.9.2.
Iron Calorimeter Soudan 2 Experiment
11.9.3.
Upward-Going Muons and MACRO
11.10.
Atmospheric ?? Oscillations and Accelerator Confirmations
11.11.
Atmospheric Neutrino Flux at Higher Energies
References
12.
Connections Between Physics and Astrophysics of Neutrinos
12.1.
Stellar Evolution of Solar Mass Stars
12.2.
Standard Solar Model and Neutrinos
12.3.
Solar Neutrino Detection
12.4.
SNO Measurement of the Total Neutrino Flux
12.5.
Oscillations and Solar Neutrinos
12.6.
Oscillations Among Three Neutrino Families
12.6.1.
Three Flavor Oscillation and KamLAND
12.6.2.
Measurements of ?13
12.7.
Matter Effect and Experimental Results
12.8.
Summary of Experimental Results and Consequences for Neutrino Astrophysics
12.8.1.
Effects of Neutrino Mixing on Cosmic Neutrinos
12.9.
Formation of Heavy Elements in Massive Stars
12.10.
Stellae Novae
12.11.
Core-Collapse Supernovae (Type II)
12.11.1.
GRB Supernovae
12.12.
Neutrino Signal from a Core-Collapse SN
12.12.1.
Supernova Rate and Location
12.12.2.
Neutrino Signal
12.12.3.
Detection of Supernova Neutrinos
12.13.
SN1987A
12.14.
Stellar Nucleosynthesis of Trans-Fe Elements
References
13.
Microcosm and Macrocosm
13.1.
Standard Model of the Microcosm: The Big Bang
13.2.
Standard Model of Particle Physics and Beyond
13.3.
Gravitational Evidence of Dark Matter
13.4.
Dark Matter
13.5.
Supersymmetry
13.5.1.
Minimal Standard Supersymmetric Model
13.5.2.
Cosmological Constraints and WIMP
13.6.
Interactions of WIMPs with Ordinary Matter
13.6.1.
WIMPs Annihilation
13.6.2.
WIMPs Elastic Scattering
13.7.
Direct Detection of Dark Matter: Event Rates
13.8.
WIMPs Direct Detection
13.8.1.
Solid-State Cryogenic Detectors
13.8.2.
Scintillating Crystals
13.8.3.
Noble Liquid Detectors
13.8.4.
Present Experimental Results and the Future
13.9.
Indirect WIMPs Detection
13.9.1.
Neutrinos from WIMP Annihilation in Massive Objects
13.9.2.
Gamma-Rays from WIMPs
13.9.3.
Positron Excess: A WIMP Signature
13.10.
What's Next
References.

Particles and astrophysics a multi-messenger approach /

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