Near-ultraviolet continuum modeling of the 1985 April 12 great flare of AD Leo

White-light stellar flares are now reported by the thousands in long-baseline, high-precision, broad-band photometry from missions like Kepler , K2, and TESS. These observations crucial inputs for assessments of biosignatures exoplanetary atmospheres surface ultraviolet radiation dosages habitable-zone planets around low-mass stars. A limitation these assessments, however, is lack near-ultraviolet spectral flares. To motivate further empirical investigation, we use a grid radiative-hydrodynamic simulations with an updated treatment pressure broadening hydrogen lines to predict λ ≈ 1800 − 3300 Å continuum flux during rise peak phases well-studied superflare dM3e star AD Leo. predictions based on semi-empirical superpositions radiative spectra consisting high-flux electron beam simulation large, low-energy cutoff (≳ 85 keV) lower-flux smaller, (≲ 40 keV). The two-component models comprehensively explain Balmer line broadening, optical color temperature, jump strength, far-ultraviolet strength shape rise/peak phase this flare. We spatially resolved analyses solar flare data Interface Region Imaging Spectrograph, combined results previous modeling 2014 March 29 X1 (SOL20140329T17:48), interpret model as representing spatial superposition bright kernels fainter ribbons over larger area.