  All stars produce explosive surface events such as flares and coronal mass
ejections. These events are driven by the release of energy stored in coronal
magnetic fields, generated by the stellar dynamo. However, it remains unclear
if the energy deposition in the magnetic fields is driven by direct or
alternating currents. Recently, we presented observational measurements of the
flare intensity distributions for a sample of $\sim10^5$ stars across the main
sequence observed by $\textit{TESS}$, all of which exhibited power-law
distributions similar to those observed in the Sun, albeit with varying slopes.
Here we investigate the mechanisms required to produce such a distribution of
flaring events via direct current energy deposition, in which coronal magnetic
fields braid, reconnect, and produce flares. We adopt a topological model for
this process which produces a power-law distribution of energetic flaring
events. We expand this model to include the Coriolis effect, which we
demonstrate produces a shallower distribution of flare energies in stars that
rotate more rapidly (corresponding to a weaker decline in occurrence rates
toward increasing flare energies). We present tentative evidence for the
predicted rotation-power-law index correlation in the observations. We advocate
for future observations of stellar flares that would improve our measurements
of the power-law exponents, and yield key insights into the underlying dynamo
mechanisms that underpin the self-similar flare intensity distributions.
