Magnetic Topology of Impulsive and Gradual Solar Energetic Particle Events

By D. Reames. 2002

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In Astronomy and Astrophysics

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Two components in major solar particle events (2003, background): “[4] Another argument against a flare particle component in major particle events is the belief that all flare particles produced at the time of a major CME are trapped on closed field lines and cannot escape to the interplanetary medium [Reames, 2002].”
The Two Sources of Solar Energetic Particles (2012, background): “…and Mason 2006; Nitta et al. 2006), where reconnection between open and closed field lines takes place (e.g. Shibata, et al. 1992; Heyvaerts, Priest, Rust 1977; Shimojo and Shibata 2000; Aschwanden (2002); Reames 2002), accelerating electrons and ions that have direct acc ss to open field lines.”
Coronal Shocks and Solar Energetic Proton Events (2004, background): “In our opinion (see Reames 2002), this is the most likely way in which flare particles can make a significant contribution to large SEP events.”
A Model for Spectral and Compositional Variability at High Energies in Large, Gradual Solar Particle Events (2006, background): “The flare ions in the seed population either could be remnants from previous activity (Mason et al. 1999; Tylka et al. 2001) or come from the associated flare (Reames 2002; Li & Zank 2005) if open field lines connect the flare site to the shock front.”
Shock Geometry, Seed Populations, and the Origin of Variable Elemental Composition at High Energies in Large Gradual Solar Particle Events (2005, background): “These flare suprathermals could be remnants from earlier flare activity (Mason et al. 1999a; Tylka et al. 2001) or come from the associated flare, if open field lines connect the flare site to the shock front (Reames 2002).”
Solar flares, coronal mass ejections and solar energetic particle event characteristics (2016, background): “Nevertheless, both the impulsive and gradual SEP events are defined by the magnetic configurations of their parent solar events with the underlying fundamental difference being the acceleration mechanisms: impulsive SEP events stem from resonant stochastic acceleration or magnetic reconnection (Asch”
Coronal Holes, Jets, and the Origin of 3He-rich Particle Events (2006, background): “As argued by Reames (2002), although reconnection among closed loops might likewise lead to acceleration and fractionation, the resulting energetic particles would remain trapped and precipitate toward the photosphere.”
Modeling Shock-accelerated Solar Energetic Particles Coupled to Interplanetary Alfvén Waves (2003, unknown): “In the numerical model of Zank, Rice, & Wu (2000) assuming Bohm diffusion, SEPs are accelerated to greater than 1 GeV early in the event at an evolving CME-driven shock starting out at 20 R (Rice & Zank 2000).”
SOLAR RELEASE TIMES OF ENERGETIC PARTICLES IN GROUND-LEVEL EVENTS (2009, background): “GLEs appear to be extreme examples of large “gradual” SEP events in which ions are accelerated by shock waves driven out from the Sun by coronal mass ejections (CMEs) (see reviews Reames 1990, 1995, 1999, 2002; Kahler 1992, 1994, 2001; Gosling 1993; Lee 1997, 2005; Tylka 2001; Tylka et al. 2005).”
Coupled Hydromagnetic Wave Excitation and Ion Acceleration at an Evolving Coronal/Interplanetary Shock (2005, background): “Reames (2002) has also argued that ions accelerated at the reconnection site behind the CME do not have easy access to open field lines.”