Book contents
- Frontmatter
- Contents
- Preface
- 1 Perspective on heliophysics
- 2 Introduction to space storms and radiation
- 3 In-situ detection of energetic particles
- 4 Radiative signatures of energetic particles
- 5 Observations of solar and stellar eruptions, flares, and jets
- 6 Models of coronal mass ejections and flares
- 7 Shocks in heliophysics
- 8 Particle acceleration in shocks
- 9 Energetic particle transport
- 10 Energy conversion in planetary magnetospheres
- 11 Energization of trapped particles
- 12 Flares, coronal mass ejections, and atmospheric responses
- 13 Energetic particles and manned spaceflight
- 14 Energetic particles and technology
- Appendix I Authors and editors
- List of illustrations
- List of tables
- References
- Index
- Plate section
8 - Particle acceleration in shocks
Published online by Cambridge University Press: 05 April 2013
- Frontmatter
- Contents
- Preface
- 1 Perspective on heliophysics
- 2 Introduction to space storms and radiation
- 3 In-situ detection of energetic particles
- 4 Radiative signatures of energetic particles
- 5 Observations of solar and stellar eruptions, flares, and jets
- 6 Models of coronal mass ejections and flares
- 7 Shocks in heliophysics
- 8 Particle acceleration in shocks
- 9 Energetic particle transport
- 10 Energy conversion in planetary magnetospheres
- 11 Energization of trapped particles
- 12 Flares, coronal mass ejections, and atmospheric responses
- 13 Energetic particles and manned spaceflight
- 14 Energetic particles and technology
- Appendix I Authors and editors
- List of illustrations
- List of tables
- References
- Index
- Plate section
Summary
In this chapter, we review the basic principles and characteristics of shock acceleration. After a brief description of the pertinent kinetic scales at shocks and a discussion of heating versus acceleration, we outline the different mechanisms that contribute to accelerating charged particles at shocks. The main emphasis throughout this chapter is on ions, and more importantly, on protons. Acceleration of other ion species or electrons is mentioned in passing and when contrasting interesting differences. Also, we restrict the discussion to the collisionless and non-relativistic shocks that occur in the heliosphere. Finally, we describe particle acceleration at interplanetary shocks and at the Earth's bow shock in greater detail, and discuss the differences between these two. Throughout the chapter, fundamental, underlying principles, historic results, and current research interests are brought together as much as possible.
Introduction
More than half a century ago, energetic particle events detected at Earth with energies into the GeV range were for the first time unambiguously associated with activity in the solar corona. While this link was established based on concomitant solar flare observations, in the 1970s and early 1980s evidence accumulated that so-called “gradual” solar energetic particle (SEP) events are actually caused by acceleration at coronal and interplanetary (IP) shocks (Sarris and Van Allen, 1974; Cliver et al., 1982; Mason et al., 1984). The 1970s and early 1980s also saw a rapid development in the theory of charged particle acceleration at shocks, and the realization that virtually all heliospheric shocks carry with them energetic particle populations.
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- Heliophysics: Space Storms and Radiation: Causes and Effects , pp. 209 - 232Publisher: Cambridge University PressPrint publication year: 2010
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