Physics
Scientific paper
May 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh52b..08b&link_type=abstract
American Geophysical Union, Spring Meeting 2002, abstract #SH52B-08
Physics
2162 Solar Cycle Variations (7536), 2164 Solar Wind Plasma
Scientific paper
This paper provides a multi-scale, statistical description of the speed profile observed near 60 AU from mid-1999 to mid-2000, based on data from Voyager 2. Distribution functions of the running speed differences on scales from 1 day to 256 days provide a relatively complete description of the large-scale speed fluctuations. On a scale of one day the distributions of positive and negative speed differences are approximately exponential; they are similar to the speed distributions observed for intermittent turbulence. On scales greater than 26 days (the solar rotation period) the distribution function of the speed differences is approximately Gaussian. On a scale of the order of 10 days, on which one sees 'jump-ramp' structures in the speed profile, the distribution function of the speed differences is cubic on a semi-log scale. The standard deviation increases with increasing scale, while the skewness and kurtosis are relatively large at small scales and decrease to their Gaussian values at the large scales. The distribution functions of speed differences versus scale at 60 AU were also derived from a speed profile predicted by the spherically symmetric, time-dependent, deterministic MHD model of Chi Wang, using ACE observations at 1 AU to determine the inner boundary conditions. Although the projected speed profile is not the same as the observed speed profile, because ACE and Voyager are not radially aligned throughout the 1-year interval, the statistical properties of the observed and projected speed profiles are essentially the same.
Burlaga Leonard Francis
Richardson John D.
Wang Chenjie
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