Particle acceleration and coronal mass ejection driven shocks: A theoretical model

By Gary Zank, W. Rice, C. Wu. 2000

294 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/060921e6d30cef05359e390af8d2c7a4e3ebf38a

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In Astronomy and Astrophysics

Citations in the corpus

Coronal Mass Ejection Shock and Sheath Structures Relevant to Particle Acceleration (2005, unknown): “Recent time-dependent calculations of shockdriven solar energetic particle (SEP) acceleration have relied on spherically symmetric shock propagation models that do not include CME initiation or interaction of the shock with a structured solar wind (Zank et al. 2000; Li et al. 2003; Lario 1998).”
Coupled Hydromagnetic Wave Excitation and Ion Acceleration at an Evolving Coronal/Interplanetary Shock (2005, methodology): “There exist three other theoretical treatments of SEP acceleration and transport in gradual events: the seminumerical theory of Zank and coworkers (Zank et al. 2000; Rice & Zank 2003; Rice et al. 2003; Li et al. 2003) is described in x 1, while the numerical theory of Ng et al. (1999, 2001, 2003)…”
A Model for Spectral and Compositional Variability at High Energies in Large, Gradual Solar Particle Events (2006, unknown): “7 of Zank et al. 2000).”
The Two Sources of Solar Energetic Particles (2012, background): “The theory of Bell (1978) was adapted to acceleration at interplanetary shock by Lee (1983), providing a basis for studies of acceleration of protons to ~GeV en rgies near the Sun (Zank, Rice, and Wu 2000; Lee 2005; Sandroos and Vainio 2007; Vainio and Laitinen 2007, 2008; Ng and Reames 2008; Battar”
Modeling Shock-accelerated Solar Energetic Particles Coupled to Interplanetary Alfvén Waves (2003, unknown): “…the ion spectra with an exponential factor, in which the e-folding energy per amu constant EeQs/As of s-ions varies inversely with the shock radius (Zank et al. 2000) and is proportional toQs/As (Ellison & Ramaty 1985; Tylka et al. 2000), where Qs is the ionic charge in units of elementary charge…”
Particle acceleration at perpendicular shock waves: Model and observations (2005, methodology): “Also, the wave number k = rL 1, the particle gyroradius, and p0 is a constant momentum scale and B0 is a normalizing magnetic field (taken to be the interplanetary magnetic field at the co-rotation radius [see Zank et al., 2000]).”
The Interaction of Successive Coronal Mass Ejections: A Review (2016, background): “In the past two decades, with remote observations of CMEs and in situ measurements of SEPs, it has become well established that the largest gradual SEP events are associated with fast and wide CMEs (Kahler, 1992; Reames, 1990; Zank, Rice, and Wu, 2000).”
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).”
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).”
A brief review of “solar flare effects” on the ionosphere (2009, methodology): “Details of the models are described by Zank et al. [2000, 2007] , Li et al. [2003, 2005], and Verkhoglyadova et al. [2009].”