Abstract
A spatial structure of the plasma micro-turbulence in the solar wind is studied with the interplanetary scintillation method. The diffraction pattern produced by the scintillation represents the projection of the plasma turbulence structure on the observer's plane. Since the method to analyze the structure of the diffraction pattern is generally sensitive to the quality of data, i. e., signal to noise ratio, four different analysis methods are used to derive trustworthy results.
The diffraction pattern has an anisotropic structure, and the direction of its elongation deviates from the radial flow direction systematically in the heliographic coordinate. In the northern hemisphere the elongation deviates counterclockwise from the radial. This situation is reversed in the southern hemisphere, where there is a clockwise deviation from the radial. These evidences imply that the microturbulence is distributed and elongated along the magnetic field.
