Physics
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh43b..08k&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SH43B-08
Physics
2114 Energetic Particles (7514), 7514 Energetic Particles (2114), 7807 Charged Particle Motion And Acceleration, 7827 Kinetic And Mhd Theory, 7867 Wave/Particle Interactions (2483, 6984)
Scientific paper
Impulsive, 3He-rich events originate close to the interface between slow solar wind overlying active regions and a faster solar wind coming from small coronal holes, which causes magnetic compressions near and beyond the Earth's orbit to be the interplanetary environment for the solar energetic particle (SEP) transport. We have modeled SEP transport in a simplified corotating solar wind structure to estimate possible effect of the rising wind speed on propagation of particles in impulsive events. Along with traditional modeling of SEP transport in the static magnetic field and the field aligned solar wind flow of the corotating frame of reference, we have formulated and tested a new method that is the first SEP modeling method applicable to a general case of realistic, dynamic and structured solar wind and can be used in the inertial heliocentric frame. Numerical modeling shows that a fast increase of the wind speed by only 200~km~s-1, typically associated with coronal sources of impulsive SEPs, can significantly affect the SEP flux anisotropy at 1~AU and results in a larger value of empirical mean free path than would be estimated based on the standard model of solar wind. The new modeling method can be used for time-dependent MHD structures with solar wind velocity not necessarily parallel to the magnetic field and thus can be applied to modeling of SEPs in interplanetary CMEs.
Kocharov Leon
Pizzo Vic
Zwickl Ron
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