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In-situ measurements by several spacecraft have revealed that the solar windis frequently perturbed by transient structures (magnetic folds, jets, waves,flux-ropes) that propagate rapidly away from the Sun over large distances.Parker Solar Probe has detected frequent rotations of the magnetic field vectorat small heliocentric distances, accompanied by surprisingly large solar windrotation rates. The physical origin of such magnetic field bends, theconditions for their survival across the interplanetary space, and theirrelation to solar wind rotation are yet to be clearly understood. We tracedmeasured solar wind flows from the spacecraft position down to the surface ofthe Sun to identify their potential source regions and used a global MHD modelof the corona and solar wind to relate them to the rotational state of the lowsolar corona. We identified regions of the solar corona for which solar windspeed and rotational shear are important and long-lived, that can be favourableto the development of magnetic deflections and to their propagation acrossextended heights in the solar wind. We show that coronal rotation is highlystructured and that enhanced flow shear develops near the boundaries betweencoronal holes and streamers, around and above pseudo-streamers, even when suchboundaries are aligned with the direction of solar rotation. A large fractionof the switchbacks identified by PSP map back to these regions, both in termsof instantaneous magnetic field connectivity and of the trajectories of windstreams that reach the spacecraft. These regions of strong shears are likely toleave an imprint on the solar wind over large distances and to increase thetransverse speed variability in the slow solar wind. The simulations andconnectivity analysis suggest they can be a source of the switchbacks andspikes observed by Parker Solar Probe.

Solar wind rotation rate and shear at coronal hole boundaries, possible consequences for magnetic field inversions