Relativistic Electrons in Ground-Level Enhanced (GLE) Solar Particle Events

Details Relativistic Electrons in Ground-Level Enhanced (GLE) Solar Particle Events Relativistic Electrons in Ground-Level Enhanced (GLE) Solar Particle Events

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh33a1818d&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH33A-1818

Physics

Plasma Physics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7514] Solar Physics, Astrophysics, And Astronomy / Energetic Particles, [7807] Space Plasma Physics / Charged Particle Motion And Acceleration, [7984] Space Weather / Space Radiation Environment

Scientific paper

Ground-level enhanced (GLE) solar particle events are one of the most spectacular manifestations of solar activity, with protons accelerated to multi-GeV energies in minutes. Although GLEs have been observed for more than sixty years, the processes by which the particle acceleration takes place remain controversial. Relativistic electrons provide another means of investigating the nature of the particle accelerator, since some processes that can efficiently accelerate protons and ions are less attractive candidates for electron acceleration. We report on observations of relativistic electrons, at ~0.5 - 5 MeV, during GLEs of 1976-2005, using data from the University of Chicago’s Cosmic Ray Nuclei Experiment (CRNE) on IMP-8, whose electron response has recently been calibrated using GEANT-4 simulations (Novikova et al. 2010). In particular, we examine onset times, temporal structure, fluences, and spectra of electrons in GLEs and compare them with comparable quantities for relativistic protons derived from neutron monitors. We discuss the implications of these comparisons for the nature of the particle acceleration process. We also compare relativistic electrons in GLEs to those in other, non-GLE SEP events with very large proton fluences above 30 MeV. Supported by ONR and by NASA LWS/TRT under DPR NNH09AL11I.

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