Physics
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsm22b..06b&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #SM22B-06
Physics
2100 Interplanetary Physics, 2134 Interplanetary Magnetic Fields, 2149 Mhd Waves And Turbulence, 2164 Solar Wind Plasma
Scientific paper
The many modes of magnetic field transport in the solar wind include several that will be discussed in this paper: 1) injection of magnetic flux by transient events on the sun, including both CMEs and short-lived coronal holes, and subsequent convection through the solar wind; 2) redistribution in space by stream interactions and shock interactions; 3) latitudinal redistribution of existing open magnetic flux; and 4) transfer to smaller scales by fragmentation processes and to larger scales by merging processes. Each of these transport modes involves non-linear dynamical MHD processes. Significant progress is being made in observing these processes, in describing the complex observations using statistical methods, and in the modeling the processes using analytical and numerical deterministic methods. We shall give a brief overview of this work. Evidence for reconnection in the solar wind continues to be found, but the observations are not definitive and the relative importance of reconnection in the solar wind is still an open topic.
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