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In the near future, Parker Solar Probe will put theories about the dynamicsand nature of the transition between the solar corona and the solar wind tostringent tests. The most popular mechanism aimed to explain the dynamics ofthe nascent solar wind, including its heating and acceleration ismagnetohydrodynamic (MHD) turbulence. Most of the previous models focus onnonlinear cascade induced by interactions of outgoing Alfv\'en waves and theirreflections, ignoring effects that might be related to perpendicularstructuring of the solar coronal plasma, despite overwhelming evidence for it.In this paper, for the first time, we analyse through 3D MHD numericalsimulations the dynamics of the perpendicularly structured solar corona andsolar wind, from the low corona to 15 R_Sun. We find that backgroundstructuring has a strong effect on the evolution of MHD turbulence, on muchfaster time scales than in the perpendicularly homogeneous case. On time scalesshorter than nonlinear times, linear effects related to phase mixing result ina 1/f perpendicular energy spectrum. As the turbulent cascade develops, weobserve a perpendicular (parallel) energy spectrum with the power law index of-3/2 or -5/3 (-2), a steeper perpendicular magnetic field than velocityspectrum, and a strong build-up of negative residual energy. We conclude thatthe turbulence is most probably generated by the self-cascade of the driventransverse kink waves, referred to previously as `uniturbulence', which mightrepresent the dominant nonlinear energy cascade channel in the pristine solarwind.

Three-dimensional simulations of the inhomogeneous Low Solar Wind