Physics
Scientific paper
Dec 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991soph..136..361j&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 136, Dec. 1991, p. 361-377.
Physics
4
Solar Electrons, Solar Flares, Solar Magnetic Field, Solar Radio Bursts, Type 3 Bursts, Data Bases, International Sun Earth Explorer 3, Magnetic Field Configurations, Solar Longitude
Scientific paper
A variety of proxy methods such as solar flare positions and metric and kilometric type III radio bursts from the sun are used to trace electrons from the sun until they can be observed in situ as electrons at the ISEE-3 spacecraft. Timing within the data sets involved is carefully restricted in order to find a peak in the number of flares associated with in situ electrons near 60 deg west solar longitude. This peak shows that type III bursts can be fairly limited in spatial extent, and that the best connection with the solar surface to the flare is along the Archimedean magnetic field spiral. This spiral determination is used to define an 'average' beam shape for an event. The electron numbers at 2 and 29-45-keV energies combined with this average beam shape are used to approximate the total numbers of electrons and energy per burst for individual events. The total number of electrons and total energy for events are found to vary significantly with flare type; on average, brighter flares are associated with more electrons.
Jackson Bernard V.
Leblanc Yolande
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