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Motivated by prior remote observations of a transition from striated solar coronal structures to more isotropic ``flocculated fluctuations, we propose that the dynamics of the inner solar wind just outside the Alfven critical zone, and in the vicinity of the first $beta=1$ surface, is powered by the relative velocities of adjacent coronal magnetic flux tubes. We suggest that large amplitude flow contrasts are magnetically constrained at lower altitude but shear-driven dynamics are triggered as such constraints are released above the Alfven critical zone, as suggested by global magnetohydrodynamic (MHD) simulations that include self-consistent turbulence transport. We argue that this dynamical evolution accounts for features observed by {it Parker Solar Probe} ({it PSP}) near initial perihelia, including magnetic ``switchbacks, and large transverse velocities that are partially corotational and saturate near the local Alfven speed. Large-scale magnetic increments are more longitudinal than latitudinal, a state unlikely to originate in or below the lower corona. We attribute this to preferentially longitudinal velocity shear from varying degrees of corotation. Supporting evidence includes comparison with a high Mach number three-dimensional compressible MHD simulation of nonlinear shear-driven turbulence, reproducing several observed diagnostics, including characteristic distributions of fluctuations that are qualitatively similar to {it PSP} observations near the first perihelion. The concurrence of evidence from remote sensing observations, {it in situ} measurements, and both global and local simulations supports the idea that the dynamics just above the Alfven critical zone boost low-frequency plasma turbulence to the level routinely observed throughout the explored solar system.
Measurements and simulations of inertial compressive turbulence in the solar wind are characterized by anti-correlated magnetic fluctuations parallel to the mean field and density structures. This signature has been interpreted as observational evide
We perform a statistical assessment of solar wind stability at 1 AU against ion sources of free energy using Nyquists instability criterion. In contrast to typically employed threshold models which consider a single free-energy source, this method in
The solar wind is a magnetized plasma and as such exhibits collective plasma behavior associated with its characteristic spatial and temporal scales. The characteristic length scales include the size of the heliosphere, the collisional mean free path
Aims: We present the first measurements of the solar-wind angular-momentum (AM) flux recorded by the Solar Orbiter spacecraft. Our aim is the validation of these measurements to support future studies of the Suns AM loss. Methods: We combine 60-minut
We present a statistical analysis for the characteristics and radial evolution of linear magnetic holes (LMHs) in the solar wind from 0.166 to 0.82 AU using Parker Solar Probe observations of the first two orbits. It is found that the LMHs mainly hav