- Conference date: 17–22 June 2012
- Location: Big Island, Hawaii
Single-spacecraft techniques for the determination of multi-dimensional correlation functions in the solar wind were pioneered by . Their production of the so-called “Maltese Cross” result shows that magnetic fluctuations near the correlation scale at 1 AU are divided into two components: quasi-parallel and quasi-perpendicular wave vectors. A later ref nement by  revealed that the two components were largely separated according to wind speed with the slow wind possessing largely perpendicular wave vectors and the fast wind possessing largely parallel wave vectors. We extend those analyses using four different techniques and compare the results of those techniques. As a demonstration of the techniques, we analyze the geometry of magnetic fluctuations at scales comparable to the correlation length. We then examine the underlying geometry for magnetic, velocity, density and temperature fluctuations. We limit the analysis to fast wind observations and show that the underlying geometry for density and temperature fluctuations is a good match to that of magnetic and velocity fluctuations.
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