The solar coronal magnetic field evolves at different time and spatial scales from the quiet Sun to active regions. Space-borne missions such as SDO and Hinode are now providing high spatial and temporal resolutions as well as a broad spectral coverage of the corona to tackle some important coronal physics with an unprecedented accuracy. These new observations provide a direct and systematic view of the coupling between the different scales. Thus this session aims at reviewing the different efforts to understand better the geometry and evolution of the coronal magnetic fields from the quiet Sun, active regions and the global Sun. We invite contributions exploiting SDO and Hinode data, especially emphasising quantitative comparisons between numerical models (field extrapolations, MHD models), and magnetic and spectroscopic observations.