Physics
Scientific paper
Jun 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sowi.conf...84z&link_type=abstract
Calabria Univ., International Solar Wind 8 Conference, p. 84
Physics
Solar Wind, Magnetic Field Configurations, Plasma Waves, Shock Waves, Electron Plasma, Three Dimensional Models, Plasma Turbulence, Shock Fronts, Fine Structure, Boundaries, Mean Square Values, Random Walk
Scientific paper
The upstream boundary of electron foreshocks is defined as the path of the fastest electrons reflected by collisionless shocks and moving along the magnetic field in the solar wind. Considerable levels of magnetic fluctuations are found in these regions of the solar wind, and their effect is to create both a broadening and a fine structure of the electron foreshock boundary. The magnetic structure is studied by means of a 3-D numerical simulation of a turbulent magnetic field. Enhanced, anomalous diffusion is found, (Delta x2) varies as salpha, where alpha is greater than 1 for typical values of the parameters (here, Delta x2 is the mean square width of the tangent magnetic surface and s is the field line length). This corresponds to a Levy flight regime for the magnetic field line random walk, and allows very efficient electron propagation perpendicular to the magnetic field. Implications on the observations of planetary foreshocks and of the termination shock foreshock are considered.
Veltri Pierluigi
Zimbardo Gaetano
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