On the Occurrence of Energetic Storm Particle Events and Type II Radio Bursts in CME-driven Shocks

Details On the Occurrence of Energetic Storm Particle Events and Type II Radio Bursts in CME-driven Shocks On the Occurrence of Energetic Storm Particle Events and Type II Radio Bursts in CME-driven Shocks

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh23b1847m&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH23B-1847

Astronomy and Astrophysics

Astrophysics

[2114] Interplanetary Physics / Energetic Particles, [2139] Interplanetary Physics / Interplanetary Shocks, [7514] Solar Physics, Astrophysics, And Astronomy / Energetic Particles, [7534] Solar Physics, Astrophysics, And Astronomy / Radio Emissions

Scientific paper

We discuss correlations between energetic storm particle (ESP) events and type II radio emission associated with coronal mass ejection-driven shocks detected during 1996-2006. Shocks that could not be associated with any type II radio emission within metric-to-kilometric wavelength range were defined to be radio-quiet (RQ). All other shocks were defined to be radio-loud (RL). ESP events were identified from the 66 keV-50 MeV proton intensities measured by the Electron, Proton and Alpha Monitor (EPAM) instrument on the Advanced Composition Explorer (ACE) spacecraft and the Energetic and Relativistic Nuclei and Electron (ERNE) experiment on the Solar and Heliospheric Observatory (SOHO). Electron ESP events were identified in the 38-53 keV energy channel of EPAM. It is remarkable that a large fraction (32%) of RQ shocks produced a particle flux increase at energies above 1.8 MeV. On the other hand, only 52% of RL shocks produced ESP events. Electron ESP events were observed in 20% of RQ shocks and 39% of RL shocks. We also find that ESP events during RQ shocks are less intense than those associated with RL shocks. Among RQ shocks, those with an ESP event have slightly more eastern source longitudes (median longitude E07), whereas those without have more western longitudes (median longitude W03). This difference probably reflects the asymmetry in the relative size of ESP events between the eastern and western flanks of the shock. Our results indicate that type II emission is important for the occurrence of ESP events. RL shocks produce frequently ESP events, and the associated ESP events are also more intense than those observed during RQ shocks. The variability in the occurrence of ESP events and type II radio bursts is probably due to differences in the shock formation in the low corona and changes in the properties of the shocks as they propagate through interplanetary space, and the escape efficiency of accelerated particles from the shock front.

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