Solar Electron Bursts at Energies Below 1.35 keV

Details Solar Electron Bursts at Energies Below 1.35 keV Solar Electron Bursts at Energies Below 1.35 keV

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh62b08g&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH62B-08

Other

2118 Energetic Particles, Solar, 2164 Solar Wind Plasma, 7514 Energetic Particles (2114), 7534 Radio Emissions

Scientific paper

Numerous solar electron bursts, characterized by persistent outward streaming from the Sun along the heliospheric magnetic field and exhibiting both velocity and angular dispersion, with the most energetic and field-aligned electrons arriving first, have been observed at energies below 1.35 keV by the solar wind plasma experiment (SWEPAM) on ACE. Burst durations range from ~1 to ~18 hours. Most bursts observed by SWEPAM extend down to ~0.5 keV and some extend to < 0.2 keV; a substantial subset do not contain > 30 keV electrons. Virtually all bursts are observed simultaneously with prolonged type III radio emission at frequencies slightly above the local plasma frequency; however, at energies < 1.35 keV the bursts begin well after the onset of, and typically persist longer than, the locally generated radio emission. Once fully formed, beam angular widths tend to remain roughly constant, but do vary considerably from event to event. Beam FWHMs vary from ~40 to ~100 deg nearly independent of energy below 1.35 keV, and are typically a factor of 2-3 broader than the angular widths of the immediately preceding solar wind electron flux at these same energies. A population of backscattered electrons is commonly observed in conjunction with the broader bursts. These bursts, although significant events, account for only a small fraction of the total variation in electron flux from the Sun at energies between ~0.2 and 1.35 keV. We infer that: (1) the acceleration producing these bursts occurs high in the solar atmosphere and typically persists for many hours; (2) scattering by self-generated waves may be considerable as the electron beams propagate out from the Sun; and (3) other processes are primarily responsible for the substantial variations in electron flux normally observed at energies below 1.35 keV.

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