For a theoretical model to accurately represent the physical evolution of the solar atmosphere, the model must, minimally, be consistent with observations of the modelled system. Accordingly, a starting point for modeling such systems is to directly incorporate information obtained from solar observations, both to determine the model’s initial state and to evolve the model forward in time over a given period. Progress has already been made on (i) extracting static magnetic field models for initial conditions ­­­ from potential­field to Non­Linear, Force­Free Field models ­­­ from observations, and (ii) deriving time­dependent boundary velocity and/or electric field components at the photosphere to evolve dynamic models forward in time. Employing such information, combined from various solar observations, in Magneto­ Hydro­Dynamic (MHD) models will, however, require further exploration and development before such models are capable of producing results that can be compared with corresponding observations. In this project, we attack open problems in the process of running such “observation­driven” simulations. In particular, we shall investigate the development of small­scale magnetic structures, such as Bright Points. Our goal is to go from observations, through MHD modeling, to forward modelling, with the aim of eventually providing synthetic observations that can be directly compared with the original observations. To do this, we shall critically evaluate each step in this
chain, to find an optimal approach to performing the each task, allowing for the most accurate overall solution possible.