deposited, either via conduction or accelerated particles; this gives rise to the largest contribution to the flare radiative output [@2011SSRv..159...19F; @2014ApJ...793...70M], and, via chromospheric evaporation, to the necessary mass and energy to fill the flaring loops with plasma at temperatures in excess of 10 MK [@1985ApJ...289..414F].

After a long period of relative neglect, the past decade has seen a renewed interest into the chromospheric response to flares. This has been driven partly by the availability of novel instrumentation, such as the imaging spectro-polarimeters IBIS [@2006SoPh..236..415C] and CRISP [@2008ApJ...689L..69S], as well as the recent [*Interface Region Imaging Spectrograph*]{} [IRIS, @2014SoPh..289.2733D], which has been utilized in numerous flare studies. On the other hand, building on the pioneering work of Fisher and colleagues in the 1980’s [@1985ApJ...289..414F; @Fisher:1986aa; @Fisher:1987aa; @1989ApJ...346.1019F], several groups have developed radiative hydrodynamical (RHD) simulations that aim at understanding the effects of a strong and sudden heating burst affecting the lower solar atmosphere [@2005ApJ...630..573A; @2015ApJ...809..104A; @2015ApJ...808..177R; @2015ApJ...813..133R; @2016IAUS..320..233H]. The complexities of fully accounting for hydrodynamical (including the presence of shocks) and radiative transfer effects in determining the chromosphere’s response to flaring limit the simulations to the 1-D case only; this however is usually well justified by the control that magnetic 