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Simulation results from a global magnetohydrodynamic model of the solarcorona and solar wind are compared with Parker Solar Probe (PSP) observationsduring its first five orbits. The fully three-dimensional model is based onReynolds-averaged mean-flow equations coupled with turbulence transportequations. The model includes the effects of electron heat conduction, Coulombcollisions, turbulent Reynolds stresses, and heating of protons and electronsvia a turbulent cascade. Turbulence transport equations for average turbulenceenergy, cross helicity, and correlation length are solved concurrently with themean-flow equations. Boundary conditions at the coronal base are specifiedusing solar synoptic magnetograms. Plasma, magnetic field, and turbulenceparameters are calculated along the PSP trajectory. Data from the first fiveorbits are aggregated to obtain trends as a function of heliocentric distance.Comparison of simulation results with PSP data shows good agreement, especiallyfor mean-flow parameters. Synthetic distributions of magnetic fluctuations aregenerated, constrained by the local rms turbulence amplitude given by themodel. Properties of this computed turbulence are compared with PSPobservations.

astrophysical journal/the astrophysical journal

Large-scale Structure and Turbulence Transport in the Inner Solar Wind  -- Comparison of Parker Solar Probe's First Five Orbits with a Global 3D  Reynolds-averaged MHD Model