SH049-0011
Global MHD Modeling of the Solar Corona and Solar Wind with Turbulent Transport and Heating: Comparisons with Parker Solar Probe Observations

Wednesday, 16 December 2020
Poster
Arcadi V. Usmanov1,2, Rohit Chhiber1,2, William H Matthaeus1, Melvyn L Goldstein3 and Riddhi Bandyopadhyay4, (1)University of Delaware, Department of Physics and Astronomy, Newark, DE, United States, (2)NASA Goddard Space Flight Center, Greenbelt, DE, United States, (3)University of Maryland Baltimore County, Baltimore, MD, United States, (4)Princeton University, Department of Astrophysical Sciences, Princeton, NJ, United States
Abstract:
Simulation results from a global magnetohydrodynamic solar corona and solar wind model are compared with the Parker Solar Probe's (PSP) observations during its first several orbits. The fully three-dimensional model (Usmanov et al., 2018, ApJ, 865, 25) is based on Reynolds-averaged mean-flow equations coupled with turbulence transport equations. The model accounts for the effects of electron heat conduction, Coulomb collisions, Reynolds stresses, and heating of protons and electrons via a turbulent cascade. Turbulence transport equations for turbulence energy, cross helicity, and correlation length are solved concurrently with the mean-flow equations. We specify boundary conditions at the coronal base using solar synoptic magnetograms and calculate plasma, magnetic field, and turbulence parameters along the PSP trajectory. We also accumulate data from all orbits considered, to obtain the trends observed as a function of heliocentric distance. Comparison of simulation results with PSP data show general agreement.
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