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As was discovered with other wide field, precise imagers, the stablephotometry necessary for the microlensing surveys is well-suited to generalstellar astrophysics, including stellar flares, which are important forunderstanding stellar magnetic activity and even the space weather environmentsof exoplanets. Large stellar flare surveys have never been performed before inthe Roman spectral range, and Roman may reveal new information about flareemission mechanisms (blackbody, recombination continuum, chromospheric emissionlines) and how flare rates change with stellar age and metallicity. Forinstance, the Galactic Bulge stars will be much older than the typical studiedflare stars, and Roman's wide field and exquisite imaging may providesufficient statistics to probe the flare behavior and properties of such an oldstellar population. However, the information yield will likely depend on skylocation, cadence, read-out strategy, and filter choices. Stellar flaretimescales range from seconds to hours, so Roman may only be able to resolvethe longest, most energetic events. However, because a single exposure in theGalactic Bulge Time Domain Survey will consist of several non-destructivereads, short duration events can be modeled from the flux variations within asingle exposure. Here we provide a proof of concept, showing that flaremorphologies can be significantly better constrained if sub-exposure data areanalyzed. As a result, we advocate that such data be made publicly availablefor Roman flare studies, with minimal on-board processing.

Enabling Stellar Flare Science in the Roman Galactic Bulge Survey: Cadence, Filters, and the Read-Out Strategy Matter