  As was discovered with other wide field, precise imagers, the stable
photometry necessary for the microlensing surveys is well-suited to general
stellar astrophysics, including stellar flares, which are important for
understanding stellar magnetic activity and even the space weather environments
of exoplanets. Large stellar flare surveys have never been performed before in
the Roman spectral range, and Roman may reveal new information about flare
emission mechanisms (blackbody, recombination continuum, chromospheric emission
lines) and how flare rates change with stellar age and metallicity. For
instance, the Galactic Bulge stars will be much older than the typical studied
flare stars, and Roman's wide field and exquisite imaging may provide
sufficient statistics to probe the flare behavior and properties of such an old
stellar population. However, the information yield will likely depend on sky
location, cadence, read-out strategy, and filter choices. Stellar flare
timescales range from seconds to hours, so Roman may only be able to resolve
the longest, most energetic events. However, because a single exposure in the
Galactic Bulge Time Domain Survey will consist of several non-destructive
reads, short duration events can be modeled from the flux variations within a
single exposure. Here we provide a proof of concept, showing that flare
morphologies can be significantly better constrained if sub-exposure data are
analyzed. As a result, we advocate that such data be made publicly available
for Roman flare studies, with minimal on-board processing.
