Observation and Modeling of an Equatorial Coronal hole Observed at the First Parker Solar Probe (PSP) Perihelion

Abstract:

Coronal holes are regions with low density and open magnetic field structures. They are the sources of fast solar wind and the main driver of geomagnetic activity. In this study, we present numerical simulations and observational analysis of an open magnetic flux tube at the center of a coronal hole. We apply our recently developed 3D reduced magnetohydrodynamic (RMHD) turbulence model to a coronal hole observed on November 1, 2018. The coronal hole was first observed on the eastern limb on October 26, 2018, and rotated backside from the western limb on November 7, 2018. We use Coronal Modeling System (CMS) software to construct a potential field (PFSS) of the observed region where the magnetic field measurements are used as input for the RMHD model. The CMS uses the SDO/HMI Line of sight (LOS) magnetograms as the lower boundary condition of the studied region. The global HMI synoptic maps serve as the side boundaries covering the entire Sun. We evaluate the results of our RHMD numerical computations at 20 solar radii. A major objective of our project is to analyze the observations of outflow velocity and density in the solar wind using the Parker Solar Probe (PSP) observations at 35 solar radii and 1 AU using the OMNI database, and Interplanetary Scintillation (IPS) observations.