Mathematics – Probability
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh51a1595l&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SH51A-1595
Mathematics
Probability
2159 Plasma Waves And Turbulence, 2162 Solar Cycle Variations (7536), 2169 Solar Wind Sources, 3270 Time Series Analysis (1872, 4277, 4475), 4440 Fractals And Multifractals
Scientific paper
The Ulysses spacecraft spent many months at high heliospheric latitudes above the Sun's polar coronal holes, in the quiet fast solar wind with a highly ordered magnetic field. The power spectra of fluctuations in solar wind bulk parameters, such as the magnetic field, show inverse power law behaviour that contains both an inertial range of intermittent turbulence and, at lower frequencies, a scaling range with approximate "1/f" dependence. Here we use statistical analysis methods, such as the generalized structure function (GSF) and extended self-similarity (ESS), to quantify the scaling of the moments of the probability density function of fluctuations in the magnetic field. We present corroborating results from both the South 1994 and the North 1995 polar passes by Ulysses. GSF is sufficient to reveal approximate power law scaling for the "1/f" range, and we test the resultant scaling exponents for secular trends with heliospheric latitude and with radial distance from the sun. At higher frequencies, where we would anticipate an inertial range of turbulence, the scaling properties of the structure functions, as well as being characteristic of intermittent turbulence, also show evidence of an 'envelope' function which we identify. We find that within these regions of quiet fast polar flows, this envelope function does not vary with heliospheric radius or latitude, and in particular is the same for both polar passes. This suggests that while the higher frequency, or inertial range, fluctuations found in the solar wind at high heliospheric latitudes are consistent with locally evolving turbulence, their envelope also reflects some aspects of the evolution of coronal structure and flows into the quiet fast solar wind. RN acknowledges the STFC and UKAEA Culham for financial support and A. Balogh and the ULYSSES team for data provision.
Chapman Sandra C.
Dendy R. O.
Leonardis Ersilia
Nicol R. M.
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