Physics
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh21a0277n&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #SH21A-0277
Physics
2149 Mhd Waves And Turbulence (2752, 6050, 7836), 2164 Solar Wind Plasma, 2169 Solar Wind Sources, 3270 Time Series Analysis (1872, 4277, 4475), 4440 Fractals And Multifractals
Scientific paper
Solar wind fluctuations typically are suggestive both of intermittent turbulence (for example, a robust power law region of the power spectrum with ~ -5/3 exponent) and at lower frequencies, of fluctuations of coronal origin (with scaling close to ~ 1/f). The respective roles of the coronal driver, and the evolving turbulence, in generating the observed scaling signature are yet to be unambiguously determined. In order to eliminate the effect of the large scale complex magnetic topology of the corona, which can also show scaling, we examine ULYSSES magnetic field data during intervals when the spacecraft spent many months in the quiet fast solar wind above the Sun's polar coronal holes. We quantify the scaling properties of fluctuations in a statistical sense, on different time-scales τ using generalised structure functions (GSF) to test for a power law scaling ~ τζp. We recover approximate power law scaling for the ~ 1/f range using GSF and test the scaling exponents for secular trend with latitude and radial distance from the sun. At higher frequencies, were we would expect an inertial range of turbulence, the structure functions do not show power law scaling with τ; however power law scaling is recovered under Extended Self Similarity (ESS), that is, in the ratios of structure functions. Thus the inertial range scaling is of the form g(τ)ζp. We show that a single function g(τ) captures all the time periods examined, i.e. no latitudinal or radial dependency was found. This is highly suggestive that the higher frequency range is indeed generated by local phenomenology, that is, evolving turbulence, whereas at lower frequencies (the ~ 1/f range) the relevant phenomenology may be coronal, with implications for our understanding of coronal heating of the solar wind.
Chapman Sandra C.
Dendy R. O.
Nicol R. M.
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