Description
Low-latitude coronal holes can produce fast solar wind characterized by rapid fluctuations rather than a steady flow. Despite significant advances in solar physics, the precise mechanisms behind the formation of this fast solar wind remain elusive. In this study, we analyze multiple sources of such wind. By linking in-situ measurements from the Solar Orbiter's instruments to their potential source regions through ballistic backmapping and potential-field source-surface modeling, we gain new insights. Coronal spectroscopic data from Hinode’s Extreme Ultraviolet Imaging Spectrometer reveal a complex interplay of upflow and downflow regions within these coronal holes, highlighting their intricate nature. These regions exhibit a mix of open and multi-scale closed magnetic fields, whose interchange reconnections are consistent with the observed up- and downflows, as well as the strahl directions and freeze-in temperatures found in in-situ data. Additionally, the SPICE spectrometer on board Solar Orbiter allows us to study other layers of the solar corona. We emphasize the role of magnetic reconnection in generating the observed upflows, downflows, and intermediate wind streams. The interaction between open and closed magnetic fields in coronal holes and active regions is crucial in this process. Observing the behavior of sulfur with SPICE may provide clues to pinpoint where interchange reconnection is occurring.
