Simulating Solar Maximum Conditions with the Alfven Wave Solar Atmosphere Model (AWSoM)

Abstract:

The Alfven Wave Solar atmosphere Model (AWSoM) within the Space Weather Modeling Framework (SWMF) is a physics-based solar corona model that solves magnetohydrodynamic (MHD) equations along with Alfven wave turbulence, radiative cooling and heat conduction. The Alfven wave pressure and dissipation account for solar wind acceleration and heating. AWSoM extends from the upper chromosphere up to 1 AU and beyond and includes the description of electron temperature and perpendicular and parallel proton temperature. AWSoM is driven by observations of the photospheric magnetic field, which are applied at the inner boundary. In this study, we use the ADAPT (Air Force Data Assimilative Photospheric Flux Transport) synchronic maps to drive our solar corona model. The ADAPT model uses observations of the solar photospheric magnetic field to produce an ensemble of magnetic field maps using a flux-transport model and data assimilation. We simulate solar maximum conditions using AWSoM and compare the results with SDO/AIA observations in the low corona and observations of solar wind density, speed and magnetic field at 1 AU (OMNI data). The background solar wind derived from our model provides the plasma environment into which Coronal Mass Ejections (CMEs) can be launched. We use the Gibson-Low Flux Rope model to initiate a CME and propagate it into the inner heliosphere. We validate the CME simulation by comparing the results with remote as well as in-situ observations from SOHO, SDO, STEREO, and WIND.