Other
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh43c..02h&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SH43C-02
Other
2114 Energetic Particles (7514), 2139 Interplanetary Shocks, 7514 Energetic Particles (2114), 7519 Flares
Scientific paper
During over ten years of operation, nearly an entire solar cycle, the ACE/EPAM instrument has measured well over 700 near-relativistic electron events. Approximately 30% 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 impulsive beam-like 100 MeV proton events from the SOHO/ERNE 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. This additional data set allows us to compare electrons and protons in the same velocity range (0.4c to 0.7c). 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 have been able to fit the entire rise-to-maximum phase of both protons and electrons with the same 3-parameter function of time (although the electron and proton parameters differ somewhat from each other in any particular event). We conclude that the injection mechanism(s) for near-relativistic protons and electrons are clearly related, although the exact time dependences are not identical.
Haggerty Dennis K.
Roelof Edmond C.
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