Comparing MHD Simulations of the Solar Corona and the Solar Wind with Data

Our global three-dimensional magnetohydrodynamic (MHD) model of the solar corona and the solar wind has been extensively used to model the properties of the magnetic field and of the plasma, from Sun to Earth and beyond. The key observational input to the model is the incorporation of observed photospheric magnetic fields into the boundary conditions. We have studied the geometrical and topological properties of the magnetic field (e.g., the location and evolution of corona holes, the reproduction of streamer structure, the location of the heliospheric current sheet, etc.) and its dynamical reconfiguration (e.g., eruptions and CMEs propagation). Direct comparison with observations have been made in the corona by calculation of emission in several EUV and X-ray bands, both for loops and the global corona. We have also compared the simulated speed, density, temperature, and magnetic field in the solar wind with in situ observations. We will discuss the insights obtained on the strengths and limitations of the models from these comparisons.