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The self-correlation level contours at the 1010 cm scale reveal a 3Disotropic feature in the slow solar wind and a quasi-anisotropic feature in thefast solar wind. However, the 1010 cm scale is approximately near thelowfrequency break (outer scale of turbulence cascade), especially in the fastwind. How the self-correlation level contours behave with dependence on thescales in the inertial range of solar wind turbulence remains unknown. Here wepresent the 3D self-correlation function level contours and their dependence onthe scales in the inertial range for the first time. We use data at 1 au frominstruments on the Wind spacecraft in the period 2005-2018. We show the 3Disotropic self-correlation level contours of the magnetic field in the inertialrange of both slow and fast solar wind turbulence. We also find that theself-correlation level contours of the velocity in the inertial range present2D anisotropy with an elongation in the perpendicular direction and 2D isotropyin the plane perpendicular to the mean magnetic field. These results indicatedifferences between the magnetic field and the velocity, providing new clues tointerpret the solar wind turbulence on the inertial scale.

Dependence of 3D Self-correlation Level Contours on the Scales in the Inertial Range of Solar Wind Turbulence