Two-Temperature, Wave-Turbulence-Driven MHD Simulations of the Solar Corona and the Solar Wind

The MAS/CORHEL three-dimensional MHD model of the solar corona and solar wind has been applied to a wide variety of problems in solar and heliospheric physics. The output of the model can be used to simulate observed phenomena, such as EUV, X-ray, and white-light images, as well as in situ plasma measurements, including ion charge states, and it currently incorporates a wave-turbulence-driven model to heat and accelerate the plasma. Recently, we used MAS to predict the structure of the solar corona and in situ measurements that were later observed by Parker Solar Probe. As new PSP perihelion passes occur, and results from Solar Orbiter become available, there is an urgent need for higher accuracy in physical models. Most of our prior experiments employ a single temperature approach to model coronal and solar wind plasmas. However, a multi-temperature approach may be necessary to reproduce plasma properties (e.g. non-equilibrium ionization) with great enough fidelity to meaningfully compare with available measurements. In this presentation we describe MHD simulations using a two-temperature formulation (ions and electrons) and a non-negligible fraction of alpha particles. We have further refined our MHD model by introducing thermal conduction (both collisional and collisionless) for the evolution of the ion temperatures. We describe the consequences and lessons learned by including these subtly important considerations and will explore their role in the upcoming predictions.