working in the optical range appears also very promising: recently presented results obtained with CRISP, using the He [i]{} ${\rm D}_3$ line to study the chromospheric dynamics in a small C-class flare. The large field of view afforded by the instrument made possible the spatial characterization of condensation motions, that were found in the leading edge of ribbons, as previously reported by . Further, the condensation is found to decay from its maximum value of $\sim$ 60 km s$^{-1}$ down to zero in around 60 seconds, a very similar evolution to what reported in Paper I using the Mg [ii]{} 2791.6Å subordinate line.

An interesting result of is that the interpretation of their spectro-polarimetric He [i]{} data in the flaring footpoints requires the use of two separate chromospheric components (“slabs”), one related to the condensation, and another one pertaining to a deeper layer, where the spectral component appears enhanced with respect to quiet conditions, and modestly blue-shifted. This second component starts being visible about one time step (15 s) after the condensation’s maximum red-shift, and has been interpreted by the authors as due to shock heating (and possible rebound) of the undisturbed chromosphere by the moving condensation. A similar scenario 