Physics – Plasma Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh53a1305p&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #SH53A-1305
Physics
Plasma Physics
[2109] Interplanetary Physics / Discontinuities, [2134] Interplanetary Physics / Interplanetary Magnetic Fields, [7863] Space Plasma Physics / Turbulence
Scientific paper
High resolution magnetic field data from the Ulysses spacecraft have been analyzed in three types of solar wind streams: fast streams coming from coronal holes, slow wind streams of low latitudes origin, and mixed streams present in regions of transition between fast and slow wind. The data sets analyzed are characterized by rapid variations in all the three magnetic field components, as well as by sharp peaks in the variances of the magnetic field fluctuations and in the cross-helicity, suggesting a structured (possibly filamentary) nature of the solar wind at small scales. The typical sizes of such structures have been found to be roughly close to the granules' size on the solar surface, when 10 min average quantities are considered. At smaller scales, below 1 min, the characteristic size of variations becomes smaller and smaller, that would correspond to very fine structures on the solar atmosphere. In the regions of transition those variations are much more dramatic, causing a sudden change in the properties of the wind over very short time intervals. Further, the level of intermittency of the magnetic field fluctuations has been studied in the three types of streams. In the regions of transition it has been found to be higher than in the other types of wind, indeed, the Probability Density Functions (PDFs) of the magnetic field increments exhibit non Gaussian tails for a wider range of temporal scales.
Balogh André
Perri Simona
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