Are Solar Electron Burst Acceleration Sites Highly Localized?

Details Are Solar Electron Burst Acceleration Sites Highly Localized? Are Solar Electron Burst Acceleration Sites Highly Localized?

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh22c..05g&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH22C-05

Physics

2114 Energetic Particles, Heliospheric (7514), 2118 Energetic Particles, Solar, 7514 Energetic Particles (2114), 7534 Radio Emissions

Scientific paper

More than 300 solar electron bursts have been observed at energies below 1.4 keV by the SWEPAM experiment on ACE. All of these bursts are strongly beamed outward along the heliospheric magnetic field. In addition, a backscattered component is also commonly present. A large fraction of these bursts are closely associated with type III radio bursts that extend down in frequency close to the local plasma frequency. Electron burst durations range from about 1 to greater than 30 hrs. Burst beam intensity-time profiles below 1.4 keV usually are relatively smooth and structureless at all energies, although notable exceptions to this rule occur. In contrast, impulsive solar energetic ion events commonly contain significant dispersionless (in energy) temporal structure. That structure has been interpreted as evidence that heliospheric field lines are commonly braided and that the ion acceleration site at the Sun is spatially localized. One possible interpretation of the SWEPAM electron measurements is that the electron burst acceleration sites typically are considerably less spatially localized than are the impulsive ion acceleration sites.

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