The Nature of Magnetohydrodynamic Fluctuations in the Solar Wind as Determined from Four-Point Measurements of Magnetic Field and (Electron) Plasma Velocity on Cluster

Details The Nature of Magnetohydrodynamic Fluctuations in the Solar Wind as Determined from Four-Point Measurements of Magnetic Field and (Electron) Plasma Velocity on Cluster The Nature of Magnetohydrodynamic Fluctuations in the Solar Wind as Determined from Four-Point Measurements of Magnetic Field and (Electron) Plasma Velocity on Cluster

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsm53a1441g&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SM53A-1441

Physics

2149 Mhd Waves And Turbulence (2752, 6050, 7836), 3379 Turbulence (4490)

Scientific paper

One of the goals of the Cluster mission is to use large spacecraft separations (≍ 10,000 km) to examine the three-dimensional structure of magnetohydrodynamic turbulence in the solar wind. Pioneering work using the magnetometer data has been done in recent years. Analyses have included use of k-filtering or wave telescope, and correlation techniques (e.g., see, Glassmeier et al., 2001; Sahraoui et al., 2003; Matthaeus et al., 2005). The plasma properties of these fluctuations have not been examined due primarily to the lack of four-point measurements of the plasma velocity. We have examined the possibility of using velocity moments computed from high-resolution three-dimensional distribution functions obtained during burst mode from the PEACE experiment on all four Cluster spacecraft. Preliminary analysis suggests that for fluctuations with periods below about 10 sec, spectra of Elsässer variables have spectral indices close to the Kolmogorov value of -5/3 seen in fluid turbulence and known to be characteristic of solar wind turbulence when proton velocities are used. The spectra using PEACE data compare well with spectra for the same time intervals computed using proton velocity moments from the CIS experiment on C1. For some intervals, the PEACE spectra show the presence of highly compressible waves in the Earth's foreshock with periods of ≍ 30 sec. We will report on progress using multi-spacecraft techniques (e.g., the wave telescope) to identify the wave modes present at times when the spacecraft are in the solar wind at separations as large as 10,000 km. Glassmeier, K. H. et al. (2001), Cluster as a wave telescope--first results from the fluxgate magnetometer, Ann. Geophys., 19, 1439-1447. Sahraoui, F. et al. (2003), Ulf wave identification in the magnetosheath: K-filtering technique applied to Cluster II data, J. Geophys. Res., 108, 1335. Matthaeus, W. H. et al. (2005), Spatial correlation of solar-wind turbulence from two-point measurements, Phys. Rev. Lett., 95.

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