Solar Wind MHD Turbulence in Coronal Hole and Streamer Belt wind

Solar wind MHD turbulence depends on solar wind type and can be quite different in coronal hole (fast) wind from streamer belt (slow) wind. In this work we identify the origins of solar wind using the O⁷⁺/O⁶⁺ ratio and proton specific entropy etc, and then study the differences of the MHD turbulence properties of these two winds. We first investigate the dependence of the occurrence rate of current sheets on solar wind type. We also examine how the residual energy and cross helicity behave in different periods of solar wind that are characterized by the occurrence rate of current sheets and solar wind type. The results will help us to get a better understanding of solar wind turbulence as well as the physical mechanisms of the dissipation process associated with current sheets.