Cosmic ray decreases and shock structure: A multispacecraft study

Details Cosmic ray decreases and shock structure: A multispacecraft study Cosmic ray decreases and shock structure: A multispacecraft study

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994jgr....9921429c&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 99, no. A11, p. 21,429-21,441

Physics

40

Cosmic Rays, Ejecta, Interplanetary Magnetic Fields, Neutrons, Plasma-Particle Interactions, Shock Wave Interaction, Shock Waves, Solar Wind, Field Strength, Helios 1, Helios 2, Imp, Neutron Counters, Plasma Density, Plasma Temperature

Scientific paper

We examine greater than 60-MeV/amu ion data from three spacecraft (IMP 8 and Helios 1 and 2) at the time of a number of short term (less than 20-day duration) cosmic ray decreases (greater than 1 GeV) detected by ground-based neutron monitors in the years 1976 to 1979. The multispacecraft data allow us to investigate the structure of the modulation region and in particular the relative importance, as a function of location, of the shock and shock driver (ejecta) in causing the reduction in particle densities. Although the shocks contributing to cosmic ray decrease often have particle enhancements associated with them in the greater than 60-meV/amu data, this is not the case for three of the events discussed in this paper where a shock-associated decrease is also evident. Whereas the shock can cause an increase or decrease at low (i.e., less than neutron monitor) energies, the reduction of particle densities in the driver, if it is intercepted, is usually evident at all energies. Thus the overall shape of a decrease at greater than 60 MeV/amu depends primarily on whether the ejecta is intercepted. We find that the particle density inside ejecta increases with increasing radical distance from the Sun. In many of the events in this study, entry and exit of ejecta are accompanied by abrupt changes in the decrease and recovery rates which indicate that the effect of the ejecta is local. In contrast, the effect of the shock lasts many days after the shock has passed by and is evident at large angular distances from the longitude of the solar source, i.e., the effect of the shock is nonlocal. Within 1 AU there seems to be no radial dependence of the shock effect. One cosmic ray decrease seen at Earth, which had an unusual profile, can be understood if the median plane of the ejecta was inclined to the ecliptic.

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