Physics – Plasma Physics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm51c1821w&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SM51C-1821
Physics
Plasma Physics
[2134] Interplanetary Physics / Interplanetary Magnetic Fields, [4490] Nonlinear Geophysics / Turbulence, [7863] Space Plasma Physics / Turbulence
Scientific paper
Turbulence in the solar wind has been analyzed both in the time domain and in the spatial domain. Analysis in the time domain uses data from a single spacecraft and makes the assumption that structure in the solar wind is static and is convected at the solar wind velocity, vsw. Autocorrelation of measurements at different times t and t+τ , with τ =l/vsw, provide Ctime}(r{1},r_{1}+l)=C[r_{1}(t),r_{1(t+τ )], taken to represent cross correlations across distances l = τ vsw. Analysis in the spatial domain makes use of 2 spacecraft measurements at fixed time at two different spatial locations, finding Cspatial}[r{1}(t),r_{2(t)] where r2}(t)=r{1(t)+l. Neither of these approaches provides the cross correlation in the frame of greatest theoretical interest, the plasma rest frame or the Eulerian frame. In recent work, Matthaeus et al. [2010] have presented an approach to determining the cross-correlation in the Eulerian frame of reference from 2 spacecraft measurements in the form CE}(r{1},r_{2})=C[r_{1}(t),r_{2(t+τ )]. In this study, we use data from multiple spacecraft to implement analysis of turbulent fluctuations with an interest in comparing the correlation functions CE, Ctime, and Cspatial. Our results are compared with the autocorrelations in Dasso et al. [2005], the cross correlation in Weygand et al. [2009] and the Eulerian correlation in Matthaeus et al. [2010].
Dasso Sergio
Galland Kivelson Margaret
Matthaeus William H.
Smith Walter C.
Weygand James M.
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