Turbulent Cascade Dynamics in the Interplanetary Plasma

Details Turbulent Cascade Dynamics in the Interplanetary Plasma Turbulent Cascade Dynamics in the Interplanetary Plasma

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmng43b..03s&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #NG43B-03

Physics

2134 Interplanetary Magnetic Fields, 2149 Mhd Waves And Turbulence (2752, 6050, 7836), 2159 Plasma Waves And Turbulence, 7513 Coronal Mass Ejections (2101)

Scientific paper

For years it was common to assume that the spectrum of interplanetary fluctuations was a remnant signature of solar photospheric sources imparting a spectrum on propagating Alfven waves as they passed through the acceleration region and into the solar wind. Such a spectrum was merely a remnant of the acceleration region dynamics and assumed to possess no intrinsic evolution apart from wave propagation and weakly nonlinear WKB dynamics. We now know that while there may be elements of truth to the view that the early solar wind possesses a remnant signature of the acceleration region, the eventual evolution of the interplanetary spectrum is the result of interplanetary MHD dynamics that result in a self-generated spectrum of magnetic and velocity field fluctuations. We know this because we can measure directly the rate at which energy cascades through the inertial range spectrum and we can compare this rate to the rate at which the background plasma is heated. We find these rates to be in good agreement. We can also show that the MHD dynamics are acting to move energy toward perpendicular wave vectors as shown in numerous simulations in a manner that is likely to result in a nearly 2D geometry which is also seen in numerous simulations of MHD turbulence.

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