Superevents - Their origin and propagation through the heliosphere from 0.3 to 35 AU

Details Superevents - Their origin and propagation through the heliosphere from 0.3 to 35 AU Superevents - Their origin and propagation through the heliosphere from 0.3 to 35 AU

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...387l..97d&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 387, March 10, 1992, p. L97-L100. Research supported by BMFT.

Other

10

Heliosphere, Interplanetary Medium, Particle Flux Density, Solar Activity, Solar Corpuscular Radiation, Solar Flares, Galactic Cosmic Rays, Solar Rotation, Solar Wind, Stellar Mass Ejection

Scientific paper

Interplanetary particle fluxes between 1974 and 1986 are analyzed and compared with Kiel neutron monitor data to determine whether other less obvious 'superevents' may exist than the five events previously identified by Mueller-Mellin et al. (1986). The solar activity associated with the most prominent superevents is examined, and it is found that these events originate in extended (0.5-2 mo) episodes of coronal mass ejection (CME) activity from single active regions or narrow ranges of active latitudes. Analysis of the variation of the particle peak intensity as a function of time, ecliptic longitude, and radial distance suggests that superevents result when systems of CMEs, with their associated shocks and particle events, create an outward propagating shell encompassing the sun. The relatively weak negative radial intensity gradients of the superevents indicate that local acceleration and trapping, as well as flare-accelerated particles, are key factors in their formation.

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