Physics
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh22a0751k&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #SH22A-0751
Physics
2104 Cosmic Rays, 2134 Interplanetary Magnetic Fields
Scientific paper
We discuss the potential role the meridional component of the large-scale heliospheric magnetic field (HMF) may play in the transport of energetic charged particles. The standard Archimedean spiral lines of the steady, large-scale HMF has no latitudinal component. Hence latitudinal transport of cosmic rays may occur through particle drifts and cross-field diffusion only. Most of the numerical works developed so far were built on and taking advantage of this presumption. The inclusion of additional meridional field components into the transport-equation is straightforward conceptually but is still posing serious challenges for numerical models. Here, we consider examples where organized latitudinal field components are of importance. A 3-dimensional, time dependent numerical code is developed and applied to idealized cases, where the motion of the footpoints of magnetic field lines can be described as a superposition of rotations. We address the Fisk field as the prime target of the present work. Also discussed are the meridional fields that inescapably emerge in connection with the reorganization of the global HMF as the tilt angle of the heliospheric current sheet (HCS) changes. The presence of a small organized latitudinal field is important if cross-field diffusion ({κ perpendicular to }) is small. Our numerical code is custom-designed for this purpose and is optimized for small κ perpendicular to . Results of numerical simulations will be presented.
Jokipii Randy J.
Kota József
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