Solar Particle Radiation Storms Forecasting and Analysis : : The HESPERIA HORIZON 2020 Project and Beyond.

• Superior document: Astrophysics and Space Science Library ; v.444
• Author: Malandraki, Olga E.
• TeilnehmendeR: Crosby, Norma B.
• Place / Publishing House: Cham : : Springer International Publishing AG,, 2018.; ©2018.
• Year of Publication: 2018
• Edition: 1st ed.
• Language: English
• Series: Astrophysics and Space Science Library
• Physical Description: 1 online resource (210 pages)

Table of Contents

• Intro
• Preface
• Acknowledgements
• Contents
• List of Abbreviations
• 1 Solar Energetic Particles and Space Weather: Science and Applications
• 1.1 Science
• 1.1.1 Historical Perspective of Solar Energetic Particle (SEP) Events
• 1.1.2 Large Gradual SEP Events
• 1.1.3 Ground Level Enhancement (GLE) Events
• 1.1.4 Multi-Spacecraft Observations of SEP Events
• 1.1.5 Particle Acceleration
• 1.1.6 Key Open Questions and Future Missions
• 1.2 Applications
• 1.2.1 Why Study SEP Events?
• 1.2.2 SEP Effects on Technology
• 1.2.3 SEPs and Human Health Effects
• 1.2.4 Mitigating the Effects of SEPs
• 1.2.4.1 Hazard Assessment
• 1.2.4.2 Mitigation Procedures
• References
• 2 Eruptive Activity Related to Solar Energetic Particle Events
• 2.1 Introduction
• 2.2 The Scene
• 2.3 Solar Flares: Energy Release and Radiative Signatures of Charged Particle Acceleration
• 2.3.1 Emission Processes
• 2.3.1.1 Bremsstrahlung
• 2.3.1.2 Gyrosynchrotron Radiation
• 2.3.1.3 Plasma Emission from Electron Beams
• 2.3.1.4 Gamma-Rays from Accelerated Protons and Ions
• 2.3.2 Where Are Electrons Accelerated in Solar Flares?
• 2.3.3 A Qualitative View of Acceleration Processes
• 2.4 What Is a Coronal Mass Ejection?
• 2.4.1 CME Magnetic Structure and Eruption
• 2.4.2 Shock Waves and Particle Acceleration at CMEs
• 2.5 Summary and Conclusion
• References
• 3 Particle Acceleration Mechanisms
• 3.1 Introduction
• 3.2 Acceleration Mechanisms
• 3.2.1 Large-Scale Electric Field Acceleration
• 3.2.2 Resonant Wave Acceleration
• 3.2.3 Shock Acceleration
• 3.2.4 Compressional Acceleration and Collapsing Magnetic Traps
• 3.2.5 Stochastic Acceleration
• 3.3 Concluding Remarks
• References
• 4 Charged Particle Transport in the Interplanetary Medium
• 4.1 Introduction
• 4.1.1 Energetic Particles in the Solar System.
• 4.1.2 The Interplanetary Magnetic Field
• 4.1.3 Motion of Charged Particles. First Adiabatic Invariant
• 4.2 Particle Transport
• 4.2.1 Particle Transport Equations
• 4.2.2 Focused Transport
• 4.2.3 Diffusive Transport
• 4.3 Application: Description of Solar Energetic Particle Events
• 4.3.1 Numerical Techniques
• 4.3.2 Observations
• 4.3.3 Inferring Transport Conditions
• 4.4 Concluding Remarks
• References
• 5 Cosmic Ray Particle Transport in the Earth's Magnetosphere
• 5.1 Introduction
• 5.2 Motion of Charged Particles in a Magnetic Field: Lorentz Force
• 5.3 Earth's Magnetic Field
• 5.3.1 The Magnetic Field of the Earth as a Dipole Field
• 5.3.2 Magnetic Field Model Due to Internal Sources: IGRF
• 5.3.3 Contributions to the Earth's Magnetic Field by Magnetospheric Electric Currents
• 5.3.4 Magnetic Field Models of the External Sources
• 5.4 Computation of the Propagation of Cosmic Ray Particles in the Earth's Magnetosphere
• 5.5 The Concept of Cutoff Rigidities and Asymptotic Directions
• References
• 6 Ground-Based Measurements of Energetic Particles by Neutron Monitors
• 6.1 Introduction
• 6.2 History
• 6.3 Transport of Cosmic Ray Particles in the Earth's Atmosphere
• 6.3.1 Model of the Earth's Atmosphere
• 6.3.2 Particle Cascade in the Atmosphere
• 6.4 Neutron Monitor Detector
• 6.4.1 Components of a Neutron Monitor
• 6.4.2 Neutron Monitor Yield Function
• 6.4.3 Atmospheric Effects
• 6.5 Worldwide Network of Neutron Monitor Stations as a Giant Spectrometer
• 6.6 Neutron Monitor Database: NMDB
• References
• 7 HESPERIA Forecasting Tools: Real-Time and Post-Event
• 7.1 Introduction
• 7.2 Predicting SEP Event Onsets from Historical Microwave Data by Using the UMASEP Scheme
• 7.3 Predicting SEP Energy Spectra from Historical Microwave Data
• 7.4 Predicting 30-50 MeV SEP Events by Using the RELeASE Scheme.
• 7.5 Predicting &gt
• 500 MeV SEP Events by Using the UMASEP Scheme
• 7.6 Concluding Remarks
• References
• 8 X-Ray, Radio and SEP Observations of Relativistic Gamma-Ray Events
• 8.1 Introduction
• 8.2 Theory and Early Observations of Gamma-Ray Emission at Photon Energies &gt
• 60MeV
• 8.2.1 Pion-Decay γ-Ray Emission
• 8.2.2 Long-Duration γ-Ray Events
• 8.3 New Insights of Sustained Emission Events from Fermi Observations
• 8.4 Multiwavelength Observations of Fermi/LAT γ-Ray Events
• 8.4.1 Impulsive and Early Post-impulsive γ-Ray Emission
• 8.4.2 Long-Duration γ-Ray Events
• 8.4.3 Soft X-Ray Bursts and γ-Ray Events
• 8.4.4 Coronal Shock Waves and γ-Ray Events
• 8.5 Solar Energetic Particle Events Associated with Fermi/LAT Gamma-Ray Events
• 8.5.1 SEP Characteristics and Association with Fermi/LAT
• 8.5.2 SEP Spectra
• 8.6 Summary and Discussion
• References
• 9 Modelling of Shock-Accelerated Gamma-Ray Events
• 9.1 Introduction
• 9.2 Model Description
• 9.2.1 Shock and Particle Model
• 9.2.2 Coronal Shock Acceleration Model
• 9.2.3 DownStream Propagation Model
• 9.3 Results
• 9.3.1 2012 May 17 Event
• 9.3.1.1 Modelling of the SEP Event
• 9.3.1.2 Simulations of Proton Acceleration at the Shock
• 9.3.1.3 Modelling of the Proton Transport Back to the Sun
• 9.3.2 2012 January 23 Event
• 9.3.2.1 Modelling of the SEP Event
• 9.3.2.2 Simulation of Proton Acceleration at the Shock
• 9.3.2.3 Modelling of the Proton Transport Back to the Sun
• 9.4 Discussion and Conclusions
• References
• 10 Inversion Methodology of Ground Level Enhancements
• 10.1 Introduction
• 10.2 Space and Ground Based Measurements of GLEs
• 10.2.1 dE/dx-dE/dx-Method
• 10.2.2 dE/dx - C
• 10.2.3 Magnet Spectrometer
• 10.3 Forward Modeling from the Sun to the Observer at Ground.
• 10.3.1 Interplanetary Particle Transport: From the Sun to the Magnetosphere
• 10.3.2 From the Interplanetary Particle Distribution to Neutron Monitor Measurements - Magneto- and Atmospheric Transport of Charged Energetic Particles
• 10.3.3 Combined Greens-Function
• 10.4 Inversion Methodology
• 10.4.1 Inversion of Spacecraft Data to the Sun
• 10.4.2 Inversion of NM Data to the Border of the Earth's Magnetosphere
• 10.4.3 The HESPERIA Approach
• 10.5 Results and Validation
• 10.6 Concluding Remarks
• References
• Index.