Extended Self Similarity in Solar Wind Turbulence

Details Extended Self Similarity in Solar Wind Turbulence Extended Self Similarity in Solar Wind Turbulence

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsm33e..05r&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SM33E-05

Mathematics

Probability

2149 Mhd Waves And Turbulence (2752, 6050, 7836), 2159 Plasma Waves And Turbulence, 3265 Stochastic Processes (3235, 4468, 4475, 7857), 6050 Plasma And Mhd Instabilities (2149, 2752, 7836), 7836 Mhd Waves And Instabilities (2149, 2752, 6050)

Scientific paper

The solar wind provides a natural laboratory for observations of MHD turbulence over extended temporal scales. A hallmark of turbulence is scaling- and scaling in the Probability Density Functions (PDF) of fluctuations in certain solar wind in- situ bulk plasma parameters has been established from WIND and ACE observations on `short' timescales up to a few hours. On longer timescales there is a crossover in scaling to uncorrelated behaviour. The intermittency of the system is expressed in these parameters through the non-Gaussian nature of the fluctuations PDF up to this timescale. Here we apply a generic approach to turbulence- that of Extended Self Similarity (ESS)- to the analysis of solar wind observations. We find that ESS can extend the range of scaling and for some parameters reveals two distinct scaling regions for the `short' and long timescales, whereas for others, a single scaling encompasses the behaviour over the full range of timescales. That certain parameters, and conditions, can be distinguished via ESS may provide physical insight into the turbulent solar wind.

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