Computer Science
Scientific paper
Aug 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icrc....4..342a&link_type=abstract
In NASA. Goddard Space Flight Center 19th Intern. Cosmic Ray Conf., Vol. 4 p 342-345 (SEE N85-34729 23-92)
Computer Science
Interplanetary Magnetic Fields, Propagation, Scattering, Solar Cosmic Rays, Solar Protons, Distribution (Property), International Sun Earth Explorer 3, Magnetic Field Configurations, Solar Flares, Solar Flux Density, Solar Wind
Scientific paper
Bartley (1966) and McCracken and Ness (1966) identified bundles of interplanetary magnetic field (IMF) lines that differed in direction from the interplanetary field lines in which they were imbedded. These bundles, called filaments differed in direction by as much as several tens of degrees from the surrounding field. The filaments werre first noticed due to the large and sudden change in flow direction of highly anisotropic solar flare protons in the energy range 1 to 13 MeV. Passage of the filaments over the spacecraft required a few hours, implying a diameter for the filaments of approximately 3 x 10 to the 6th power km at a distance of 1 AU from the Sun. In 1968, Jakipii and Parker used Leighton's hypothesis of random walk of magnetic field lines associated with granules and supergranules (1964) to develop a picture of an interplanetary medium composed of a tangle of field lines frozen into the solar wind, but whose feet were carried about by the random motions at the solar surface. Jakipii and Parker noted that using a correlation length of 15,000 km - about the radius of a supergranule - the magnetic structure would be 3 x 10 to the 6th power km in size of the filaments as determined by Bartley and McCracken and Ness. These workers did not find changes in the solar particle intensity, anisotropy ratio or energy spectrum as the spacecraft entered the filament.
Anderson Katharine A.
Dougherty W. M.
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