fields exert to plasma dynamics [cf., e.g. @2015ApJ...809..104A; @2015ApJ...813..133R].

The flaring chromospheres resulting from the models can then be compared with proper observational diagnostics to gauge their realism; most often, this is accomplished by using radiative transport codes such as RH [@2001ApJ...557..389U] to synthesize relevant chromospheric lines (including the resonance lines of Mg [ii]{} h&k, Ca [ii]{} H&K, or H$\alpha$) in snapshots of the simulations’ output, to provide a direct comparison with observables. Some of the relevant mechanisms influencing the formation of these strong, optically thick chromospheric spectral lines in flaring conditions remain an active subject of study, including e.g. the effects of partial frequency redistribution for the Mg [ii]{} resonance lines [@2019ApJ...883...57K], or the role of enhanced densities on the broadening of the Hydrogen Balmer lines [@2017ApJ...837..125K]. Still, this method offers the best diagnostic possibilities, especially when the temporal evolution is factored in the comparison, as the dynamics of the flaring plasma are extremely sensitive to the details of heating and energy transport .

Comparisons of this kind have been attempted many times in the past using strong optical lines , and continued to date with data at much higher spatial resolution and spectral coverage [@2015ApJ...798..107K; @2015ApJ...813..125K; @2016ApJ...827...38R; @2017ApJ...847...48H; 