The structure of the interplanetary magnetic field as revealed by solar flare particles

Details The structure of the interplanetary magnetic field as revealed by solar flare particles The structure of the interplanetary magnetic field as revealed by solar flare particles

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh11b..07m&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH11B-07

Statistics

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

Scientific paper

The arrival profiles of particles from solar flares provide a picture of the structure of the interplanetary magnetic field. Because the particle arrival at 1 AU and composition are such that we can identify individual injections from the Sun, the particles are useful tracers of their propagation paths and of the relationships between adjacent flux tubes at 1 AU. We will briefly review the observations of 20 keV/n to 2 MeV/n ions from impulsive flares at 1 AU where simultaneous variations in particle intensity across all energies indicate that neighboring flux tubes at 1 AU were separated at the Sun. We have previously reported on of steep (less than 2 minutes) cross-field particle gradients observed with the ACE spacecraft in a few events. The time scale of these features is relevant to the classical scattering of the particles off field lines, and at the meeting we will revisit this scattering with statistics of the gradients measured in many events. Also, we will report new observations of the particle anisotropies inside of individual flux tubes using measurements from the Wind spacecraft.

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