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Solar flares are transient yet dramatic events in the atmosphere of the Sun,during which a vast amount of magnetic energy is liberated. This energy issubsequently transported through the solar atmosphere or into the heliosphere,and together with coronal mass ejections flares comprise a fundamentalcomponent of space weather. Thus, understanding the physical processes at playin flares is vital. That understanding often requires the use of forwardmodelling in order to predict the hydrodynamic and radiative response of thesolar atmosphere. Those predictions must then be critiqued by observations toshow us where our models are missing ingredients. While flares are of course 3Dphenomenon, simulating the flaring atmosphere including an accuratechromosphere with the required spatial scales in 3D is largely beyond currentcomputational capabilities, and certainly performing parameter studies ofenergy transport mechanisms is not yet tractable in 3D. Therefore,field-aligned 1D loop models that can resolve the relevant scales have acrucial role to play in advancing our knowledge of flares. In recent years,driven in part by the spectacular observations from the Interface RegionImaging Spectrograph (IRIS), flare loop models have revealed many interestingfeatures of flares. For this review I highlight some important results thatillustrate the utility of attacking the problem of solar flares with acombination of high quality observations, and state-of-the-art flare loopmodels, demonstrating: (1) how models help to interpret flare observations fromIRIS, (2) how those observations show us where we are missing physics from ourmodels, and (3) how the ever increasing quality of solar observations drivesmodel improvements. Here in Paper 1 of this two part review I provide anoverview of modern flare loop models, and of electron-beam driven mass flowsduring solar flares.

Interrogating Solar Flare Loop Models with IRIS Observations 1: Overview of the Models, and Mass flows