Modelling 3D magnetic networks in a realistic solar atmosphere

The magnetic network extending from the photosphere (solar radius \simeq R_\odot) to lower corona (R_\odot + 10 Mm) plays an important role in the heating mechanisms of the solar atmosphere. Here we further develop the models with realistic open magnetic flux tubes of Gent et al. (2013, 2014) in order to model more complicated configurations. Closed magnetic loops, and combinations of closed and open magnetic flux tubes are modelled. These are embedded within a realistic stratified atmosphere, subject to solar gravity and including the Interface Region. Constructing a magnetic field comprising self-similar magnetic flux tubes, an analytic solution for the kinetic pressure and plasma density is derived following Gent et al. (2014). Combining flux tubes of opposite polarity it is possible to create a steady background magnetic field configuration modelling realistic solar atmosphere. The result can be applied to SOHO/MDI and SDO/HMI and other magnetograms from the solar surface, upon which realistic photospheric motions can be simulated to explore the mechanism of energy transport. We demonstrate this powerful and versatile method with an application to Helioseismic and Magnetic Imager data