HR: 0800h
AN: SM11A-1165    [Abstracts]
TI: Multifractal analysis of magnetic field fluctuations inferred Cluster and solar wind measurements: Evidence for intermittent turbulence in the plasma sheet and solar wind.
AU: Schwarzl, H
EM: schwarzl@igpp.ucla.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Los Angeles, Los Angeles, CA 90095-1567 United States
AU: * Weygand, J M
EM: jweygand@igpp.ucla.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Los Angeles, Los Angeles, CA 90095-1567 United States
AU: Kivelson, M G
EM: mkivelson@igpp.ucla.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Los Angeles, Los Angeles, CA 90095-1567 United States
AU: Khurana, K K
EM: kkhurana@igpp.ucla.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Los Angeles, Los Angeles, CA 90095-1567 United States
AU: McPherron, R L
EM: rmcpherron@igpp.ucla.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Los Angeles, Los Angeles, CA 90095-1567 United States
AU: Kistler, L
EM: kistler@atlas.sr.unh.edu
AF: Department of Physics, University of New Hampshire, Durham, NH 03824 United States
AU: Balogh, A
EM: a.balogh@imperial.ac.uk
AF: The Blackett Laboratory, The Blackett Imperial College Prince Consort Rd., London, SW7 2BZ United Kingdom
AU: Thompson, S
EM: sthompson@igpp.ucla.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Los Angeles, Los Angeles, CA 90095-1567 United States
AB: Solar wind magnetometer and plasma data and magnetometer data acquired by Cluster in the magnetospheric plasma sheet are employed to construct probability distribution functions (PDFs) of velocity fluctuations and magnetic field fluctuations over various temporal and spatial scales. This technique, often used in analysis of laboratory plasmas, is used to look for intermittent plasma turbulence. We examined the distribution of the magnetic field and plasma fluctuations for a single spacecraft, and between pairs of highly correlated spacecraft time series data in both the plasma sheet and the solar wind (fast and slow speed streams). We demonstrate that the plasma sheet fluctuations are multi-fractal and do not rescale to a single master curve. The plasma and magnetic field PDFs are fit with the Castaing et al. [1990] energy cascade model. This model is able to capture the non-Gaussian behavior at small temporal and spatial separations in the wings of the distribution and non-self similar scaling behavior over a range of temporal and spatial separations. The model results provide an experimental test for the Castaing et al. model and allow for a quantitative comparison between different systems and events.
UR: http://www.igpp.ucla.edu/jweygand
DE: 7863 Turbulence
DE: 2164 Solar wind plasma
DE: 2744 Magnetotail
DE: 2764 Plasma sheet
SC: SPA-Magnetospheric Physics [SM]
MN: 2004 AGU Fall Meeting