Computer Science
Scientific paper
Sep 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aipc..679..597s&link_type=abstract
SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP Conference Proceedings, Volume 679, pp. 597-6
Computer Science
Particle Emission, Solar Wind, Particle Acceleration, Solar Wind Plasma, Sources Of Solar Wind
Scientific paper
53 impulsive (38-315 keV) near-relativistic solar electron events with beam-like pitch-angle distributions were observed by the ACE/EPAM experiment while the SOHO/LASCO coronographs were observing coronal mass ejections (CME) between 2.5 and 30 Rsolar. Simnett, Roelof and Haggerty [in companion papers to be published in Ap. J., 2002] report a close association among the impulsive electron beams, solar electromagnetic emissions, and western hemisphere CMEs, jets, etc. They find that the electron injections are delayed ~10 minutes after the electromagnetic emissions and ~20 minutes after the CME launches, so that the electron release occurs when the CME has travelled 1-2 Rsolar beyond the CME launch altitude. The median exciter speed of the associated solar type III radio bursts (deduced from WIND/WAVES decametric spectrograms) is 0.08c, implying that the characteristic electron energies in the exciter front are only a few keV. Since no prompt near-relativistic electrons are injected until ~10 minutes after the type III burst, the energy spectrum of the type III associated electrons must be steep at these energies. Therefore the near-relativistic electrons that must be present to produce the microwave and hard X-ray bursts also do not escape promptly with intensities measurable by ACE/EPAM. Inverse correlation between the finite delays of near-relativistic electrons after the CME launch confirms that the electrons are injected when the CMEs are ~1-2 Rsolar above the photosphere. The positive correlation between CME speed and electron intensity (as well as spectral hardness) is consistent with the process of shock acceleration. Therefore we conclude that the simplest explanation of the observational associations is that the electrons are accelerated by CME-driven shocks in the corona at altitudes ~1-2 Rsolar above the photosphere. We see no reason why ions should not also be accelerated concurrently in the corona by this same process, although the final velocity of the ions may be less than that of the electrons.
Roelof Edmond C.
Simnett George M.
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