Structure functions and intermittency of velocity fluctuations in the inner solar wind

Details Structure functions and intermittency of velocity fluctuations in the inner solar wind Structure functions and intermittency of velocity fluctuations in the inner solar wind

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993angeo..11..227m&link_type=abstract

Annales Geophysicae (ISSN 0992-7689), vol. 11, no. 4, p. 227-238.

Physics

82

Flow Velocity, Magnetohydrodynamic Turbulence, Solar Wind, Variations, Power Spectra, Scaling Laws, Solar Magnetic Field, Spectrum Analysis

Scientific paper

In this paper we provide evidence for the intermittent nature of the fluctuations of the flow velocity and Alfven velocity in the inner solar wind between 0.3 and 1.0 AU. We analyze the pth order structure functions in the time domain between 40.5 s and 24 hrs and investigate their scaling properties in the Alfvenic range from fractions of minutes to several hours. Generally, the fast and slow wind regimes have to be discriminated, because the scaling features of the velocity differences with time lag vary systematically with the wind speed. Radial trends are established by comparison of Helios data obtained near 0.3 AU and 1.0 AU. The second-order structure function for p = 2, which is equivalent to the power spectrum, shows essentially an exponent s(p) = alpha-1, as is predicted from self-similar scaling for a spectral index alpha. Yet there appears substantial departure from simple self-similarity, and also from homogeneous intermittency (uniform fractality) at higher-order p's for all types of flows analyzed, which is clearly evident in the normalized dimensionless structure functions.

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