The Turbulent Correlation Length in the Distant Solar Wind

Details The Turbulent Correlation Length in the Distant Solar Wind The Turbulent Correlation Length in the Distant Solar Wind

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh51c0286i&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH51C-0286

Physics

7827 Kinetic And Mhd Theory, 7863 Turbulence, 2149 Mhd Waves And Turbulence, 2152 Pickup Ions, 2164 Solar Wind Plasma

Scientific paper

A model of turbulent evolution in the distant solar wind has recently been presented which incorporates the detailed quasilinear generation of fluctuations by interstellar pickup protons to drive the turbulence [Isenberg et al., ApJ, 592, 564, 2003; Isenberg, ApJ, submitted, 2004]. The dissipation of the turbulent fluctuations at the standard Kolmogorov rate has been shown to provide a reasonable agreement with observed heating of the core solar wind protons out to almost 75 AU [Smith et al., ApJ, submitted, 2004]. In this model, the correlation length of the turbulence λ (r) is a fundamental quantity, since it controls the turbulent dissipation rate. Although analysis of observations out to 30 AU indicates that λ steadily increases with r, the model calls for this quantity to decrease beyond about 10 AU due to the turbulent driving by the pickup protons. Here, we investigate modifications to the present model which will bring the correlation length more in line with the observations. These modifications will, in turn, affect the predicted turbulent intensities and solar wind temperatures. We will present and discuss the modified model and compare its results with solar wind observations.

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