Coronal magnetic field evolution modulates our space environment via coronal mass ejections, flares, and changes in solar wind conditions. However, routine observations of magnetic field in the optically thin solar corona are not yet well-developed. Hence understanding the coronal magnetic field distribution using data-constrained global magnetohydrodynamic (MHD) models is of paramount importance nowadays. There are several factors which can drive the evolution e.g. flux emergence, photospheric flows, stratification in thermodynamic variables, solar wind conditions. Simulations using MHD models will help us generate the global magnetic field distribution, which can be constrained using total solar eclipse observations. Apart from this, such models have the potential to generate polarization characteristics utilizing the model output, which will help in better interpretation of data from future solar missions like PUNCH. We discuss the magnetic field distribution and polarization characteristics for past solar eclipses based on MHD simulations for global solar corona using a variety of approaches based on data-driven surface flux transport models, potential field source surface models and full MHD models.