Physics
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh44a..06b&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SH44A-06
Physics
2109 Discontinuities (7811), 2149 Mhd Waves And Turbulence (2752, 6050, 7836), 2169 Solar Wind Sources, 7524 Magnetic Fields
Scientific paper
The solar wind at 1 AU is full of discontinuities. These can be seen by sudden large changes in the magnetic- field direction, by sudden changes in the magnetic-field strength, by sudden changes in the plasma properties (density, ion temperature, ionic composition), by sudden large changes in the flow velocity. These discontinuities are interpreted to be the walls of independently moving magnetic flux tubes (plasma tubes) with a spread of orientations about the Parker-spiral direction. This flux-tube texture of the plasma has strong implications for the flow properties of the solar wind: (a) much of the fluctuating flow of the solar wind is owed to relative motions of neighboring flux tubes and (b) often large-scale solar-wind flows break up along these flux tubes. The flux-tube texture also affects the properties of the MHD turbulence in the solar wind: (a) the turbulence is confined to the insides of the flux tubes and (b) any field-line wandering driven by the turbulence is also confined to a flux tube. Using measurements from ACE, the statistical properties of the flux tubes at 1 AU are examined, including their sizes, shapes, and orientations. Mapping the flux tubes back to the rotating sun, they are statistically compared with granule and supergranule structures on the solar surface.
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