Two components in major solar particle events

By H. Cane, T. V. von Rosenvinge, C. Cohen, R. Mewaldt. 2003

152 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/81ad977def25ee48855a4e18757f1ece168d445e

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In Astronomy and Astrophysics

Citations in the corpus

The Plasma and Suprathermal Ion Composition (PLASTIC) Investigation on the STEREO Observatories (2008, background): “…classified as “gradual” (Möbius et al. 1999; Popecki 2006, and references therein); that enrichments in 3He are also common in interplanetary shock accelerated populations (Desai et al. 2001); and that enrichments in heavy ions are often observed in large events at high energies (Cane et al. 2003).”
Coupled Hydromagnetic Wave Excitation and Ion Acceleration at an Evolving Coronal/Interplanetary Shock (2005, background): “However, it is possible, particularly if the more extended reconnection behind CMEs accelerates ions muchmore efficiently (Litvinenko & Somov 1995).”
THE LONGITUDINAL PROPERTIES OF A SOLAR ENERGETIC PARTICLE EVENT INVESTIGATED USING MODERN SOLAR IMAGING (2011, unknown): “It has also been suggested that enhanced Fe/O at high energies is the signature of ions accelerated in the concomitant flare (Cane et al. 2003), similar to the heavy-ion enhancements seen in impulsive SEP events at lower energies.”
Shock Geometry, Seed Populations, and the Origin of Variable Elemental Composition at High Energies in Large Gradual Solar Particle Events (2005, background): “However, particle instruments onWind andACE did not observe increases in 20MeV nucleon 1 protons and heavy ions until 2200 UT.Wind LEMT, which monitors arrival directions covering nearly the whole sky, confirmed that the particles were flowing outward from the direction of the Sun.”
Proton, helium, and electron spectra during the large solar particle events of October-November 2003 (2005, background): “[55] Of course, it is also possible that some of the observed particles were accelerated at the flare site by other energy sources [see, e.g., Cane et al., 2003] or that some flare-accelerated particles were further accelerated by the shock [Mewaldt et al., 2003; Li and Zank, 2005].”
The Two Sources of Solar Energetic Particles (2012, background): “Early increases in Fe/O (but not in 3He), for example, were erroneously ascribed to the presence of material accelerated in the impulsive flare preceding the shock acceleration, especially in magnetically well-connected events (e.g. Reames 1990a, Cane et al. 2003).”
STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview (2008, unknown): “Events at western longitudes peak early and are initially Fe-rich, the ion composition presumably having been affected by flare-like processes in the hot corona (e.g. Cane et al. 2003).”
Heavy-Ion Elemental Abundances in Large Solar Energetic Particle Events and Their Implications for the Seed Population (2006, background): “However, this sample is too small to allow firmer conclusions about reported associations between eastern hemisphere events and lower Fe/O ratios above 25 MeV nucleon 1 (e.g., see Cane et al. 2003).”
A Model for Spectral and Compositional Variability at High Energies in Large, Gradual Solar Particle Events (2006, background): “The results of the reanalysis agree with our values. enhancements to a direct flare component, unaided by processing through a shock (e.g., Cane et al. 2003).”