Uninterrupted Tracking of Solar Wind Outflows Along Radial and Non-Radial Paths

Understanding the source of the variability in the slow solar wind is a key part of Space Weather research because it can lead to an understanding of the physical processes that drive solar activity, heat the corona and accelerate the solar wind. Achieving this requires establishing connections between the low corona, through the upper corona, and into the solar wind. Our work provides the capabilities to study features in the solar wind and subsequently study the evolution between EUV/WL and in situ of the plasma flows that give rise to them. Here, we discuss differences and similarities between the properties of outflows identified propagating along radial and non-radial paths (e.g. occurrence rate, formation height and velocities). Some of these structures match previously identified solar wind periodic density structures in coronagraph observations. These results have important implications for the understanding of solar wind formation (height at which the structures form, unprecedentedly enabled by the uninterrupted field of view) and heating (velocity profiles provide information on the acceleration of these plasma parcels) thus supporting the interpretation and the understanding of the evolution of solar wind plasma as well as the distribution of the coronal plasma density.