Testing Turbulence Transport Models using Solar Wind Data

Details Testing Turbulence Transport Models using Solar Wind Data Testing Turbulence Transport Models using Solar Wind Data

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh42b..08j&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH42B-08

Physics

Plasma Physics

[7863] Space Plasma Physics / Turbulence

Scientific paper

There are fundamental questions about the Sun and its influence on our local space environment that require a detailed understanding of turbulence throughout the heliosphere, many of which are addressed by the Zank et al (2011) turbulence model, e.g. the transport of turbulence in the solar wind, and the coronal heating issue. In order to test and refine this theory, a comparison with data is vital, with the most easily accessible data set being that which describes the transport of turbulent fluctuations in the solar wind. In this work, we use plasma and magnetic field data from Voyager 2, Pioneer 1 and 2, Helios 1 and 2 and Ulysses in order to fully explore the turbulent fluctuations of the solar wind from 0.3-95 AU, both in and out of the ecliptic plane. We present a a library of reduced data products, including the total energy in turbulent fluctuations, the energy difference between kinetic and magnetic turbulent fluctuations, the energy contained in cross-helicity, the variance in magnetic field, and the Alfven ratio. These can all be compared against predictions from any turbulence model, e.g. Zank et al (2011), in order to fully understand the transport of turbulence throughout the heliosphere.

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