Evidence for a Suprathermal Seed Population of Heavy Ions Accelerated by Interplanetary Shocks near 1 AU

By M. Desai, G. Mason, Joseph R. Dwyer, J. Mazur, R. Gold, S. Krimigis, Charles W. Smith, R. Skoug. 2003

183 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

A Global Picture of CMEs in the Inner Heliosphere (2004, background): “Flare particles (Mason et al., 1999) or SEPs from preceding CMEs (Kahler, 2001) may form seed particles for CME-driven shocks near the 25 Sun as well as at 1 AU (Desai et al., 2003).”
Shock Geometry, Seed Populations, and the Origin of Variable Elemental Composition at High Energies in Large Gradual Solar Particle Events (2005, methodology): “Because quasi-perpendicular shocks tend to 16 For each of the IPS events, Desai et al. (2003) identified a preceding ‘‘upstream’’ time interval whose characteristics they believe to be representative of the shock’s seed population.”
The Interaction of Successive Coronal Mass Ejections: A Review (2016, background): “There are typically significant differences between SEPs accelerated through these two mechanisms, including the duration, elemental abundances, spectra, etc. (Mason, Mazur, and Dwyer, 1999; Desai et al., 2003; Desai et al., 2006; Tylka et al., 2005).”
Coupled Hydromagnetic Wave Excitation and Ion Acceleration at an Evolving Coronal/Interplanetary Shock (2005, background): “These may include the solar wind core distribution and its suprathermal tail (Gloeckler et al. 2000), remnant gradual SEP event ions (Desai et al. 2003), remnant impulsive SEP event ions including specifically 3He (Mason et al. 1999; Desai et al. 2001), interstellar pickup ions (Kucharek et al.…”
SOLAR RELEASE TIMES OF ENERGETIC PARTICLES IN GROUND-LEVEL EVENTS (2009, background): “In some large SEP events, however, intermediate abundances may result when remnant suprathermal ions from impulsive events contribute to the seed population accelerated by CME-driven shock waves (Mason et al. 1999; Tylka et al. 2001, 2005; Desai et al. 2003; Tylka & Lee 2006).”
The Two Sources of Solar Energetic Particles (2012, background): “Desai et al. (2003) showed that lowenergy ion abundances near the shock peak were much more closely rr ated with ambient abundances upstream of the shock than with the abundance of the corresponding elements in the solar wind, as expected from our discussion of the seed population in Section 2.”
Colloquium: Statistical mechanics of money, wealth, and income (2009, background): “Coexistence of the exponential and power-law distributions is also known in plasma physics and astrophysics, where they are called the “thermal” and “superthermal” parts (Collier, 2004; Desai et al., 2003; Hasegawa et al., 1985).”
Heavy-Ion Elemental Abundances in Large Solar Energetic Particle Events and Their Implications for the Seed Population (2006, methodology): “…material from prior SEP events has subsequently been explored in a number of studies of odd compositional and spectral behavior in IP shock events (e.g., Desai et al. 2001, 2003, 2004; Channok et al. 2005) and in LSEP events (Tylka et al. 2001, 2005; Kocharov & Torsti 2003; Li & Zank 2005).”
Stochastic Acceleration by Turbulence (2012, background): “…component (which is below the observable energy range of 0.1 to 10 MeV/nucleon) and a higher energy nonthermal component with high 3He 18In fact there is evidence that energetic (> 0.1 MeV/nucleon) ions are “present upstream of all interplan- etary shocks” (Desai et al. 2003). enrichment.”
Particle acceleration at perpendicular shock waves: Model and observations (2005, background): “However, Desai et al. [2004] find that the distinction between these groups is less sharp when many events are considered.”