Injection times of near-relativistic solar protons and electrons

Details Injection times of near-relativistic solar protons and electrons Injection times of near-relativistic solar protons and electrons

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsh41a..05h&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH41A-05

Physics

7514 Energetic Particles (2114), 7519 Flares, 2114 Energetic Particles (7514)

Scientific paper

During nine years of operation, nearly an entire solar cycle, the ACE/EPAM instrument has measured well over 600 near-relativistic electron events. Approximately 40% of these electron events are impulsive with beam-like anisotropies and are predominantly from flares on the western hemisphere (or over the west limb). We have argued that they are released onto open coronal field lines, and propagate nearly scatter-free out to 1 AU. We have also identified 16 > 100 MeV proton events from the SOHO/ERNIE instrument associated with our ACE/EPAM electron beam events whose onsets are sufficiently clean that they may be directly compared with those of the near-relativistic electron events. In most events the protons are injected within ~ ± 10 min of the electrons. However, both protons and electrons are almost always injected after the start-time of the associated electromagnetic emissions (whatever their type): chromospheric H-alpha, synchrotron emission (15400 and 8800 MHz), metric and decametric type-III fast-drift bursts, type-II slow-drift events, and type-IV noise storms. We also compare the delays in the proton and electron injections with CME velocity and position angle. We conclude that there is an intimate relationship between the injection mechanism(s) for near-relativisitic protons and electrons.

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