  Chromospheric flare ribbons observed in H-alpha appear well-organized when
first examined: ribbons impulsively brighten, morphologically evolve, and
exponentially decay back to pre-flare levels. Upon closer inspection of H-alpha
flares, there is often a significant number of compact areas brightening in
concert with the flare eruption but are spatially separated from the evolving
flare ribbon. One class of these brightenings is known as sequential
chromospheric brightenings (SCBs). SCBs are often observed in the intimidate
vicinity of erupting flares and are associated with coronal mass ejections. In
the past decade there have been several previous investigations of SCBs. These
studies have exclusively relied upon H-alphaimages to discover and analyze
these ephemeral brightenings. This work employs the automated detection
algorithm of Kirk et al. (2011) to extract the physical qualities of SCBs in
observations of ground-based H-alpha images and complementary AIA images in
HeII, Civ, and 1700 \AA. The meta-data produced in this tracking process are
then culled using complementary Doppler velocities to isolate three
distinguishable types of SCBs. From a statistical analysis, we find that the
SCBs at the chromospheric H-alpha layer appear earlier, and last longer than
their corresponding signatures measured in AIA. From this multi-layer analysis,
we infer that SCBs are spatially constrained to the mid-chromosphere. We also
derive an energy budget to explain SCBs in which SCBs have a postulated energy
of not more than 0.01% of the total flare energy.
