Interplanetary Anisotropic Fluctuation Spectra: Testing Weakly Compressible Mhd Theory With Ace Data

Details Interplanetary Anisotropic Fluctuation Spectra: Testing Weakly Compressible Mhd Theory With Ace Data Interplanetary Anisotropic Fluctuation Spectra: Testing Weakly Compressible Mhd Theory With Ace Data

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.1601b&link_type=abstract

American Astronomical Society, SPD meeting #37, #16.01; Bulletin of the American Astronomical Society, Vol. 38, p.244

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The Weakly Compressible Model (WCM) of turbulence is a reduced system of equations, derived rigorously from the fully compressible MHD equations, that can describe fluctuation spectra in the interplanetary plasma when the plasma beta is of the order unity or less. The model includes in its framework the effect of background inhomogeneities, and has been used suuccessfully in the past to account for density fluctuations in the solar wind. Here we propose to test the predictions of this model with ACE data on anisotropic magnetic fluctuation spectra. For a model of local pressure-driven turbulence, using the principle of scale invarinace, we calculate explicitly the scaling of magnetic field fluctutations with plasma beta and other background plasma parameters. The principle of scale invariance is simple but powerful, and can be stated as follows: if the system of equations are invariant under a scale transformation, then fluctuations calculated from them must exhibit the same invariance. Using this principle, we are able to calculate fluctuation scaling explicitly from the WCM model and compare them with recent ACE observations. These studies have significant implications for determining whether the weakly compressive fluctuations observed in the interplanetary medium are generated from in situ dynamics or have a dominantly solar origin.

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