Propagation of Solar Energetic Particles Associated with Impulsive Solar Flares in Turbulent Interplanetary Magnetic Fields

Details Propagation of Solar Energetic Particles Associated with Impulsive Solar Flares in Turbulent Interplanetary Magnetic Fields Propagation of Solar Energetic Particles Associated with Impulsive Solar Flares in Turbulent Interplanetary Magnetic Fields

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh43a1640g&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH43A-1640

Physics

2114 Energetic Particles (7514), 7514 Energetic Particles (2114), 7807 Charged Particle Motion And Acceleration, 7859 Transport Processes, 7863 Turbulence (4490)

Scientific paper

We discuss the physics of the propagation of an impulsive release of charged particles in a turbulent magnetic field. Test-particle numerical simulations are used to study the propagation of solar energetic particles (SEPs) in interplanetary magnetic turbulence created by the random transverse motions of magnetic footpoints embedded in the solar atmosphere (Giacalone et al. 2006). The turbulence model includes a Kolmogorov-like magnetic field power spectrum containing a broad range of scales from those that lead to large-scale field-line random walk to small scales leading to resonant pitch-angle scattering of energetic particles. We relate our numerical simulations to spacecraft observations and show that a number of features of SEP events observed by ACE and Wind can be reproduced in these simulations. For instance, we find that,the path lengths traveled by particles are different from that expected for a simple Parker spiral; and thus. The resulting velocity dispersion is energy dependent. We also find flux dropouts associated with steep localized gradients. Moreover, since particles sample different field lines which have different path length, their arriving times are non-uniform.

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