We report on the physical properties of solar sequential chromospheric brightenings ( SCBs ) observed in conjunction with moderate-sized chromospheric flares with associated CMEs .
To characterize these ephemeral events , we developed automated procedures to identify and track subsections ( kernels ) of solar flares and associated SCBs using high resolution H \alpha images .
Following the algorithmic identification and a statistical analysis , we compare and find the following : SCBs are distinctly different from flare kernels in their temporal characteristics of intensity , Doppler structure , duration , and location properties .
We demonstrate that flare ribbons are themselves made up of subsections exhibiting differing characteristics .
Flare kernels are measured to have a mean propagation speed of 0.2 km s ^ { -1 } and a maximum speed of 2.3 km s ^ { -1 } over a mean distance of 5 \times 10 ^ { 3 } km .
Within the studied population of SCBs , different classes of characteristics are observed with coincident negative , positive , or both negative and positive Doppler shifts of a few km s ^ { -1 } .
The appearance of SCBs precede peak flare intensity by \approx 12 minutes and decay \approx 1 hour later .
They are also found to propagate laterally away from flare center in clusters at 41 km s ^ { -1 } or 89 km s ^ { -1 } .
Given SCBs distinctive nature compared to flares , we suggest a different physical mechanism relating to their origin than the associated flare .
We present a heuristic model of the origin of SCBs .