Spatially dependent turbulence and particle diffusion in an interplanetary magnetic flux rope

Details Spatially dependent turbulence and particle diffusion in an interplanetary magnetic flux rope Spatially dependent turbulence and particle diffusion in an interplanetary magnetic flux rope

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh33b1837k&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH33B-1837

Physics

Plasma Physics

[2111] Interplanetary Physics / Ejecta, Driver Gases, And Magnetic Clouds, [2114] Interplanetary Physics / Energetic Particles, [7807] Space Plasma Physics / Charged Particle Motion And Acceleration, [7863] Space Plasma Physics / Turbulence

Scientific paper

Magnetic Clouds (MCs) released by solar storms can strongly affect the transport of energetic charged particles in space. MCs have a rope-like magnetic field structure called an Interplanetary Magnetic Flux Rope (IMFR). We have previously developed an analytic magnetic-field model of IMFRs for studying the trapping and escape of solar energetic particles and Galactic cosmic rays due to drift orbits. In this research work, we develop assumptions for the spatial dependence of turbulence parameters for use with that model. We explore the particles’ perpendicular mean free path and diffusion coefficients calculated from the nonlinear guiding center (NLGC) theory, and also compare with the results from the field line random walk (FLRW) theory. We found that in a homogeneous and weak turbulence environment such as that inside the magnetic cloud, the particles’ perpendicular mean free path and perpendicular diffusion coefficient from both theories can be similar. We expect the perpendicular mean free path at the center of the IMFR is short, and longer along the flux rope radius. Moreover the mean free path should be very long in the loop leg regions, and then shorter at the flux rope’s apex. This work is partially supported by the Thailand Research Fund and NASA grant NNX07AH73G.

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