The role of the interplanetary shock surface fluctuations in shaping energetic storm particle events

Details The role of the interplanetary shock surface fluctuations in shaping energetic storm particle events The role of the interplanetary shock surface fluctuations in shaping energetic storm particle events

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh23c..04l&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH23C-04

Physics

2114 Energetic Particles (7514), 2139 Interplanetary Shocks

Scientific paper

Solar cycle 23 has provided us with a large variety of shocks and associated energetic particle storm (ESP) events. Statistical analysis of shocks and ESP events detected by ACE has shown a tendency for observing more quasi-perpendicular shocks; whereas the most common types of event are those that do not display any >47 keV ion intensity increase [Lario et al., 2005a; Proc. SW11, ESA SP-592, pp. 81-86]. Faster and stronger shocks have greater effects on the particle intensities at their passage by 1 AU, but the shock parameters do not determine unequivocally the characteristics of the ESP events. A few of these events show characteristics similar to those predicted by the theory of diffusive shock acceleration, although detailed analysis reveals significant inconsistencies between observations and theory [Lario et al., 2005b; Proc. 4th IGPP Conf., AIP-781, pp. 180-184]. A common type of event has irregular structure, showing multiple intensity bursts before and/or after the shock passage. We present both the observations of one of these events and the results of a test-particle, full-orbit-integration simulation of ion shock-acceleration in a corrugated shock surface [Decker, 1990; JGR 95, pp. 11993-12003]. Although meso-scale fluctuations of the shock surface or in magnetic field direction, or both, can produce similar features in shock-accelerated particle distributions, we invoke the rippled shock model in this case because the measured pre-shock field is relatively steady. These simulations allow us to reproduce not only the evolution of the ion intensities but also the observed ion anisotropies and energy spectra. Fluctuations of both the solar wind plasma where the shock travels and of the shock surface may determine the main features of those ESP events with irregular variations of intensities and angular distributions. This presentation constitutes a progress report on NASA LWS TR{&}T grant NAG5-13487.

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