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Largescale Structure and Turbulence Transport in the Inner Solar Wind: Comparison of Parker Solar Probe s First Five Orbits with a Global 3D Reynoldsaveraged MHD Model
Author  Chhiber, Rohit; Usmanov, Arcadi; Matthaeus, William; Goldstein, Melvyn; 
Keywords  Parker Data Used; 830; 1534; 824; 1483; 1477; Physics  Space Physics; Astrophysics  Solar and Stellar Astrophysics; Physics  Plasma Physics 
Abstract  Simulation results from a global magnetohydrodynamic model of the solar corona and solar wind are compared with Parker Solar Probe (PSP) observations during its first five orbits. The fully three dimensional model is based on Reynoldsaveraged meanflow equations coupled with turbulencetransport equations. The model includes the effects of electron heat conduction, Coulomb collisions, turbulent Reynolds stresses, and heating of protons and electrons via a turbulent cascade. Turbulencetransport equations for average turbulence energy, cross helicity, and correlation length are solved concurrently with the meanflow equations. Boundary conditions at the coronal base are specified using solar synoptic magnetograms. Plasma, magnetic field, and turbulence parameters are calculated along the PSP trajectory. Data from the first five orbits are aggregated to obtain trends as a function of heliocentric distance. Comparison of simulation results with PSP data shows good agreement, especially for mean flow parameters. Synthetic distributions of magnetic fluctuations are generated, constrained by the local rms turbulence amplitude given by the model. Properties of this computed turbulence are compared with PSP observations. 
Year of Publication  2021 
Journal  \apj 
Volume  923 
Number of Pages  89 
Section  
Date Published  dec 
ISBN  
URL  
DOI  10.3847/15384357/ac1ac7 