Authors: B. J. Lynch (SSL/UCB), N. M. Viall (GSFC/NASA), A. K. Higginson (GSFC/NASA), L. Zhao (CLaSP/UM), S. T. Lepri (CLaSP/UM), X. Sun (IfA/UH)

Connecting the solar wind observed throughout the heliosphere to its origins in the solar corona is one of the central aims of heliophysics and a fundamental science objective of the PSP and SolO missions. The slow solar wind exhibits significant variability on relatively short timescales, from minutes to days. It has been argued that this variability in the magnetic field, bulk plasma, and heavy ion composition properties of the slow wind are the result of magnetic reconnection processes in the extended solar corona. We present a detailed analysis of the solar wind from 2003 April 15 to May 13, corresponding to Carrington Rotation 2002. We identify regions of enhanced variability and ionic composition signatures and demonstrate their relationship to the Separatrix–Web (S-Web) structures describing the corona’s large-scale magnetic topology. Specifically, there are four pseudostreamer wind intervals and two heliospheric current sheet/plasma sheet crossings (and an ICME) which all exhibit enhanced alpha-to-proton ratios and elevated ionic charge states of carbon, oxygen, and iron. We apply the recently developed magnetic helicity–partial variance of increments (Hm–PVI) procedure to identify coherent magnetic structures and quantify properties of the turbulence and intermittency during each of these intervals. We discuss our results in the context of upcoming PSP and SolO joint observational campaigns.