Solar Energetic Particles A Modern Primer on Understanding Sources, Acceleration and Propagation
This open access book serves as a concise primer introducing the non-specialist reader to the physics of solar energetic particles (SEP).It systematically reviews the evidence for the two main mechanisms which lead to the so-called impulsive and gradual SEP events.
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| Format: | eBook |
| Language: | English |
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Netherlands
Springer Nature
2021
Springer International Publishing AG The author |
| Edition: | 2 |
| Series: | Lecture Notes in Physics |
| Subjects: | |
| ISBN: | 9783030664022, 3030664023, 9783030664015, 3030664015 |
| Online Access: | Get full text |
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| Abstract | This open access book serves as a concise primer introducing the non-specialist reader to the physics of solar energetic particles (SEP).It systematically reviews the evidence for the two main mechanisms which lead to the so-called impulsive and gradual SEP events. |
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| AbstractList | This open access book serves as a concise primer introducing the non-specialist reader to the physics of solar energetic particles (SEP). It systematically reviews the evidence for the two main mechanisms which lead to the so-called impulsive and gradual SEP events. This second edition contains two completely new chapters discussing element abundances and shock waves, reflecting new theoretical, modeling, and observational results. Existing chapters have been substantially expanded or updated with additions placed in a broader context.More specifically, the author discusses the timing of the onsets of SEPs, their longitude distributions, their high-energy spectral shapes, their correlations with other solar phenomena, as well as the all-important elemental and isotopic abundances. The book relates impulsive SEP events to magnetic reconnection in solar flares and jets. The concept of shock acceleration by scattering on self-amplified Alfvén waves is introduced, as is the evidence of reacceleration of impulsive-SEP material in the seed population accessed by the shocks in gradual events. The text then develops processes of transport of ions out to an observer. Finally, a technique to determine the source plasma temperature in both impulsive and gradual events is demonstrated.The author also mentions the role of SEP events as a radiation hazard in space and briefly discusses the nature of the main particle telescope designs that have contributed to most of the SEP measurements. This open access book serves as a concise primer introducing the non-specialist reader to the physics of solar energetic particles (SEP).It systematically reviews the evidence for the two main mechanisms which lead to the so-called impulsive and gradual SEP events. |
| Author | Reames, Donald V |
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| Edition | 2 2nd Edition 2021 |
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| Snippet | This open access book serves as a concise primer introducing the non-specialist reader to the physics of solar energetic particles (SEP).It systematically... This open access book serves as a concise primer introducing the non-specialist reader to the physics of solar energetic particles (SEP). It systematically... |
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| SubjectTerms | Astronomy & allied sciences |
| Subtitle | A Modern Primer on Understanding Sources, Acceleration and Propagation |
| TableOfContents | 4.10 Open Questions -- References -- 5: Gradual SEP Events -- 5.1 Parallel Transport -- 5.1.1 Diffusive Transport -- 5.1.2 Wave Growth -- 5.1.3 Particle Transport -- 5.1.4 Initial Abundance Ratios -- 5.1.5 The Streaming Limit -- 5.1.6 Electron Transport -- 5.2 Angular Distributions -- 5.3 Models and Shock Acceleration -- 5.4 Shock Acceleration In Situ -- 5.5 Averaging SEP Abundances -- 5.6 Source-Plasma Temperatures -- 5.7 Spatial Distributions and the Reservoir -- 5.7.1 Reservoirs, Loops, and Long-Duration γ Rays -- 5.8 Non-thermal Variations: Impulsive vs. Gradual SEPs -- 5.9 The Abundance of He and the FIP Effect -- 5.10 Open Questions -- References -- 6: High Energies and Radiation Effects -- 6.1 High-Energy Spectra -- 6.2 The Streaming Limit -- 6.3 Radial Dependence -- 6.4 Radiation Hazards and an SEP Storm Shelter -- 6.5 A Mission to Mars -- 6.6 The Upper Atmosphere of Earth -- 6.7 SEPs and Exoplanets -- References -- 7: Measurements of SEPs -- 7.1 Single-Element Detectors -- 7.2 DeltaE Versus E Telescopes -- 7.2.1 An Example: LEMT -- 7.2.2 Isotope Resolution: SIS -- 7.2.3 Angular Distributions -- 7.2.4 Onboard Processing -- 7.3 Time-of-Flight Versus E -- 7.4 NOAA/GOES -- 7.5 High-Energy Measurements -- 7.6 Problems and Errors -- References -- 8: Element Abundances and FIP: SEPs, Corona, and Solar Wind -- 8.1 Element Abundances in the Sun -- 8.2 The Solar Wind -- 8.3 Corotating Interaction Regions: Accelerated Solar Wind -- 8.4 Comparing FIP Patterns of SEPs and the Solar Wind -- 8.5 FIP Theory: The Sources of SEPs and the Solar Wind -- 8.6 A Full-Sun Map of FIP -- 8.7 A Possible SW-SEP Model -- 8.8 FIP-Dependent Variations in He -- 8.9 Open Questions -- References -- 9: Hydrogen Abundances and Shock Waves -- 9.1 Impulsive SEP Events -- 9.2 Gradual SEP Events -- 9.3 Waves Coupling Proton Velocity with A/Q -- 9.4 Compound Seed Particles 9.5 CME Associations of Impulsive and Gradual Events -- 9.6 Four Subtypes of SEP Events -- 9.7 Spatial Distributions -- 9.8 Rigidity-Dependence: Acceleration or Transport? -- 9.9 Correlations Between Spectra and Abundances -- 9.10 Open Questions -- References -- 10: Summary and Conclusions Intro -- Preface -- Acknowledgments -- Contents -- About the Author -- Abbreviations -- 1: Introducing the Sun and SEPs -- 1.1 The Structure of the Sun -- 1.2 The Solar Magnetic Field -- 1.3 Coronal Mass Ejections (CMEs) -- 1.4 Interplanetary Space -- 1.5 Solar Energetic Particles -- 1.5.1 Time Duration -- 1.5.2 Abundances -- 1.5.3 The Solar Cycle -- 1.5.4 Relativistic Kinematics -- 1.6 What Do We ``See´´ at the Sun? -- References -- 2: A Turbulent History -- 2.1 The First SEPs -- 2.2 Solar Radio Bursts and Electrons -- 2.3 The Spatial Distribution -- 2.3.1 Lateral Diffusion and the Birdcage Model -- 2.3.2 Large Scale Shock Acceleration and CMEs -- 2.3.3 The Longitude Distribution -- 2.3.4 Scatter-Free Events -- 2.3.5 Field-Line Random Walk -- 2.4 Shock Theory -- 2.5 Element Abundances -- 2.5.1 First Ionization Potential (FIP) and Powers of A/Q -- 2.5.2 3He-rich Events -- 2.5.3 The Seed Population for Shocks -- 2.6 Ionization States -- 2.7 Disappearing-Filament Events -- 2.8 ``The Solar-Flare Myth´´ -- 2.9 Wave Generation and the Streaming Limit -- 2.10 SEP-CME Correlation -- 2.11 SEPs Actually Cause Flares, Not the Reverse -- References -- 3: Distinguishing the Sources -- 3.1 SEP Onset Times -- 3.2 Realistic Shock-SEP Timing and Correlations -- 3.3 Injection Profiles -- 3.4 High-Energy Spectra and Spectral Knees -- 3.5 Intensity Dropouts and Compact Sources -- 3.6 Abundances -- 3.7 Electrons -- 3.8 Why Not Flares? -- 3.9 SEPs as Probes -- References -- 4: Impulsive SEP Events (and Flares) -- 4.1 Selecting Impulsive Events -- 4.2 Sample Impulsive Events -- 4.3 Energy Dependence -- 4.4 Abundances for Z 26 -- 4.5 Abundances for 34 Z 82 -- 4.6 Power-Law Enhancements in A/Q: Source-Plasma Temperatures -- 4.7 Associations: CMEs, Flares, and Jets -- 4.8 Can We Have It Both Ways? -- 4.9 Nuclear Reactions: Gamma-Ray Lines and Neutrons |
| Title | Solar Energetic Particles |
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