The role of Alfvén wave dynamics on the large scale properties of the solar wind: comparing a MHD simulation with PSP E1 data

Victor Réville, Marco Velli, Olga Panasenco, Anna Tenerani, Chen Shi, Samuel T. Badman, Stuart D. Bale, J. C. Kasper, Michael L. Stevens, Kelly E. Korreck, J. W. Bonnell, Anthony W. Case, Thierry Dudok de Wit, Keith Goetz, Peter R. Harvey, Davin E. Larson, Roberto Livi, David M. Malaspina, Robert J. MacDowall, Marc Pulupa, Phyllis L. Whittlesey

Published 2019-12-08Version 1

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