Statistics
Scientific paper
Dec 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh21b0155b&link_type=abstract
American Geophysical Union, Fall Meeting 2003, abstract #SH21B-0155
Statistics
2149 Mhd Waves And Turbulence, 2159 Plasma Waves And Turbulence, 7863 Turbulence
Scientific paper
Solar wind turbulence at 1 AU exhibits, on the one hand, a frequent high degree of Alfvenicity (or, cross helicity) and on the other hand, indications of a strong magnetohydrodynamic (MHD) cascade. The former is associated with a high degree of correlation of velocity and magnetic field -- in the limiting case they would be aligned -- while the latter requires nonzero values of v x b so that the cascade is suppressed when the fluctuation fields are aligned. Here we examine the statistics of the induced MHD-scale electric field at 1AU, to demonstrate how the degree of Alfvenicity is consistent with the observed induced electric field. The statistics support the view (Roberts et al, JGR, 92, 12023, 1987) that there remains at 1 AU some preference for an Alfvenicity associated with outward traveling fluctuations. However there is a dominance of non-Alfvenic turbulence that is sufficient to account for the observed distribution of induced electric field. A generic result is obtained that explains the sin(v,b) distribution, which is observed to peak at values corresponding to 90 degrees, even when some Alfvenic fluctuations ("0 degrees" or "180 degrees") are present. This helps to understand how Alfvenic fluctuations and turbulence can coexist in the solar wind.
Breech Ben
Matthaeus William
Milano Leo
Smith Christopher
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