Interplanetary Proton and Electron Enhancements Associated with Radio-loud and Radio-quiet CME-driven Shocks

Physics – Plasma Physics

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[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7514] Solar Physics, Astrophysics, And Astronomy / Energetic Particles, [7534] Solar Physics, Astrophysics, And Astronomy / Radio Emissions, [7851] Space Plasma Physics / Shock Waves

Scientific paper

We present the results on electron and proton acceleration in association with radio-quiet (RQ) and radio-loud (RL) shocks driven by coronal mass ejections (CMEs) during 1996-2006. The CME-driven shocks are classified into RL or RQ shocks based on the presence or the lack of type II radio bursts in the metric and decameter-hectometric wavelength range. We studied proton flux enhancements at L1 in the 66 keV - 50 MeV energy range observed by the ACE/EPAM and SOHO/ERNE instruments. Electron flux enhancements were studied in the 38-53~keV energy channel of EPAM. In general, the RL shocks are more likely to be associated with an energetic storm particle (ESP) event than RQ shocks. Approximately one third of RQ shocks and slightly over a half of RL shocks produced an ESP event at energies above 1.8 MeV. In overall both RQ and RL electron ESP events are rarer, but they follow a similar pattern to the proton observations, i.e. ESP events are observed in approximately one fifth versus two fifths of shocks, respectively. We also studied correlations of ESP event size with CME and shock properties. As expected, the ESP events associated with the RQ shocks are less intense than those with RL shocks. In addition, particle acceleration in RQ shocks occurs predominately in quasi-perpendicular shocks. There is a modest positive correlation between ESP event size and the CME and shock speed and the Mach number. Again, the correlations are stronger for the RL shocks. It appears that shocks can accelerate particles, although less efficiently, even when they do not produce observable type II radio bursts. The variation between the presence of type IIs and ESP events is probably connected to variations in the coronal conditions of shock formation and to the consequent evolution of the shock as it travels through diverse coronal and interplanetary plasmas.

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