Authors: Miralles, M. P. (Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA); Cranmer, S. R. (University of Colorado, Boulder, CO)

The origin of the solar wind, and in particular the role of magnetic topology in solar wind acceleration, is still not well understood. Pseudostreamers are ideal targets for studying the relation between magnetic topology and plasma properties. These coronal streamers differ from the more traditional helmet streamers in that they separate open field lines of the same polarity rather than the opposite polarity, and are believed to be sources of slow to intermediate speed solar wind streams. We study these coronal source regions of the solar wind using multi-spacecraft and ground-based observations. We measure and compare the spatiotemporal distribution of physical parameters for different types of structures, and focus on their differences and similarities. Line-of-sight forward modeling (of a range of visible-light and UV emission diagnostics) is used to investigate how the differences in magnetic topology affect the plasma properties of the coronal structures (that may be observed by DKIST) and their wind (that Parker Solar Probe and Solar Orbiter may encounter). This work is supported by NASA grants NNX17AI27G and 80NSSC20K1445 to the Smithsonian Astrophysical Observatory.