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Solar flares are 3D phenomenon but modelling a flare in 3D, including many ofthe important processes in the chromosphere, is a computational challenge.Accurately modelling the chromosphere is important, even if the transitionregion and corona are the areas of interest, due to the flow of energy, mass,and radiation through the interconnected layers. We present a solar flarearcade model, that aims to bridge the gap between 1D and 3D modelling. Ourapproach is limited to the synthesis of optically thin emission. Using observedactive region loop structures in a 3D domain we graft simulated 1D flareatmospheres onto each loop, synthesise the emission and then project thatemission onto to the 2D observational plane. Emission from SDO/AIA, GOES/XRS,and IRIS/SG Fe XXI 1354.1A was forward modelled. We analyse the temperatures,durations, mass flows, and line widths associated with the flare, findingqualitative agreement but certain quantitative differences. Compared toobservations, the Doppler shifts are of similar magnitude but decay tooquickly. They are not as ordered, containing a larger amount of scattercompared to observations. The duration of gradual phase emission from GOES andAIA emission is also too short. Fe XXI lines are broadened, but notsufficiently. These findings suggest that additional physics is required in ourmodel. The arcade model that we show here as a proof-of-concept can be extendedto investigate other lines and global aspects of solar flares, providing ameans to better test the coronal response to models of flare energy injection.

Solar Flare Arcade Modelling: Bridging the gap from 1D to 3D Simulations of Optically Thin Radiation