Schedule by Session

The solar community is moving toward time-dependent simulations of the coronal magnetic field, which we would like to drive from magnetogram observations at the inner, photospheric boundary. Despite recent observational advances, we still face significant challenges. A major limitation is the lack of 360-degree coverage of the solar surface, but more subtle problems arise when one tries to determine the photospheric electric field needed to drive simulations. In this talk, I will present recent progress on addressing these issues, and will suggest what data products we would ideally like from observers. The basic ideas are equally relevant to the modelling of stellar coronae other than the Sun.