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During solar flares a tremendous amount of magnetic energy is released andtransported through the Sun's atmosphere and out into the heliosphere. Despiteover a century of study, many unresolved questions surrounding solar flares arestill present. Among those are how does the solar plasma respond to flareenergy deposition, and what are the important physical processes that transportthat energy from the release site in the corona through the transition regionand chromosphere? Attacking these questions requires the concert of advancednumerical simulations and high spatial-, temporal-, and spectral- resolutionobservations. While flares are 3D phenomenon, simulating the NLTE flaringchromosphere in 3D and performing parameter studies of 3D models is largelyoutwith our current computational capabilities. We instead rely onstate-of-the-art 1D field-aligned simulations to study the physical processesthat govern flares. Over the last decade, data from the Interface RegionImaging Spectrograph (IRIS) have provided the crucial observations with whichwe can critically interrogate the predictions of those flare loop models. Herein Paper 2 of a two-part review of IRIS and flare loop models, I discuss howforward modelling flares can help us understand the observations from IRIS, andhow IRIS can reveal where our models do well and where we are likely missingimportant processes, focussing in particular on the plasma properties, energytransport mechanisms, and future directions of flare modelling.

Interrogating Solar Flare Loop Models with IRIS Observations 2: Plasma Properties, Energy Transport, and Future Directions