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During Parker Solar Probe's first orbit, the solar wind plasma has beenobserved in situ closer than ever before, the perihelion on November 6th 2018revealing a flow that is constantly permeated by large amplitude Alfv\'enicfluctuations. These include radial magnetic field reversals, or switchbacks,that seem to be a persistent feature of the young solar wind. The measurementsalso reveal a very strong, unexpected, azimuthal velocity component. In thiswork, we numerically model the solar corona during this first encounter,solving the MHD equations and accounting for Alfv\'en wave transport anddissipation. We find that the large scale plasma parameters are wellreproduced, allowing the computation of the solar wind sources at Probe withconfidence. We try to understand the dynamical nature of the solar wind toexplain both the amplitude of the observed radial magnetic field and of theazimuthal velocities.

The role of Alfv\'en wave dynamics on the large scale properties of the solar wind: comparing an MHD simulation with PSP E1 data