The total fitted intensity of the Fe [ii]{} 2814.45Å line is shown in the inverted color table, red diamonds mark the position and times sampled above, while blue diamonds correspond to the spectra in Figures \[fig:spectraA\_16\] to \[fig:spectraB\_52\].[]{data-label="fig:ltspec"}](absorption_spec_fe2_rev.eps "fig:"){width="9cm"} ![Temporal evolution of Fe [i]{} 2814.1Å and Fe [ii]{} 2813.33 & 2814.45Å spectral profiles (top panel) and Mg [ii]{} 2791.6Å subordinate (middle panel), for flaring pixel y = 119.53. The intensity scale is reversed for clarity. The presence of a separate, rapidly evolving strongly redshifted component is obvious for all lines (horizontal dashed lines mark the rest wavelengths). The red diamonds (all panels) indicate the time of the spectra sampled in Fig. \[fig:spectraA\] and \[fig:spectraB\]. Bottom panel: space-time plot from a subset of 81 pixels along the IRIS slit (see Figure \[fig:irisaia\] or Paper I for context). The total fitted intensity of the Fe [ii]{} 2814.45Å line is shown in the inverted color table, red diamonds mark the position and times sampled above, while blue diamonds correspond to the spectra in Figures \[fig:spectraA\_16\] to \[fig:spectraB\_52\].[]{data-label="fig:ltspec"}](absorption_spec_mg2_rev.eps "fig:"){width="9cm"}

![image](figure5A_2019_rev_32.eps){width="14cm"}

![image](figure5B_32.eps){width="16cm"}

The presence of “satellite” red-wing components is clearly observed in multiple chromospheric lines, as vividly demonstrated in Figure \[fig:ltspec\]. In the figure we 