Modeling Shock-accelerated Solar Energetic Particles Coupled to Interplanetary Alfvén Waves

By C. Ng, D. Reames, A. Tylka. 2003

168 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/43f373c5f47131a6250563c043054fcecaadb6fa

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

A Model for Spectral and Compositional Variability at High Energies in Large, Gradual Solar Particle Events (2006, background): “For reasons of both practical application and proper treatment of nonlinear wave growth (Ng et al. 2003; Lee 2005a), a comprehensive SEP model must also deal in absolute intensities; these calculations do not do that.”
THE LONGITUDINAL PROPERTIES OF A SOLAR ENERGETIC PARTICLE EVENT INVESTIGATED USING MODERN SOLAR IMAGING (2011, unknown): “The simulation is based on the Ng et al. (2003) focused transport SEP model.”
Coupled Hydromagnetic Wave Excitation and Ion Acceleration at an Evolving Coronal/Interplanetary Shock (2005, methodology): “Ng et al. (1999, 2003) used a similar approach but included wave excitation by the ad hoc source protons as they escape from the shock location toward Earth orbit.”
Proton, helium, and electron spectra during the large solar particle events of October-November 2003 (2005, background): “It is interesting that the region of positive slope in their wave spectra at 0.1– 0.15 AU [Ng et al., 2003, Figure 5] corresponds to proton rigidities from 100 to 300 MV ( 5 to 50 MeV), the same region where the breaks in the proton spectra are located (see Figure 5).”
Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation (2016, background): “What roles do self-excited Alfvén waves play during intense SEP events and how do they affect the streaming limits (Reames and Ng 1998; Ng et al. 2003)?”
The Two Sources of Solar Energetic Particles (2012, methodology): “This will cause considerable scattering of the SEPs that follow (Ng, Reames, and Tylka 2003) and intensities may even reach the streaming limit (see Section 5.2).”
SOLAR RELEASE TIMES OF ENERGETIC PARTICLES IN GROUND-LEVEL EVENTS (2009, background): “Pitch-angle scattering slows the rise in intensity and delays the apparent onset, a process that has been modeled for large SEP events (Sáiz et al. 2005; see also Ng et al. 2003).”
Shock Geometry, Seed Populations, and the Origin of Variable Elemental Composition at High Energies in Large Gradual Solar Particle Events (2005, background): “…are shocks driven by fast coronal mass ejections (CMEs), are productive opportunities for refining our understanding of shock acceleration (Reames 1999; Lee 2000, 2005; Zank et al. 2000; Rice et al. 2003; Cliver et al. 2004) and particle transport (Ng et al. 1999, 2003; Li et al. 2003).”
PROPAGATION OF SOLAR ENERGETIC PARTICLES IN THREE-DIMENSIONAL INTERPLANETARY MAGNETIC FIELDS (2009, methodology): “…describe the SEP intensity observed near Earth by using the focused transport equation (Roelof 1969; Kallenrode 1993; Bieber et al. 1994; Droge 1994; Ruffolo 1995; Kallenrode & Wibberenz 1997; Ng & Reames 1994; Ng et al. 1999, 2003; Zank et al. 2000; Rice et al. 2003; Li et al. 2003; Lee 2005).”