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We investigate the cause of the suppressed Balmer series and the origin ofthe white-light continuum emission in the X1.0 class solar flare on 2014 June11. We use radiative hydrodynamic simulations to model the response of theflaring atmosphere to both electron and proton beams which are energeticallyconstrained using RHESSI and Fermi observations. A comparison of syntheticspectra with the observations allow us to narrow the range of beam fluxes andlow energy cut-off that may be applicable to this event. We conclude that theelectron and proton beams that can reproduce the observed spectral features arethose that have relatively low fluxes and high values for the low energycut-off. While electron beams shift the upper chromosphere and transitionregion to greater geometrical heights, proton beams with a similar flux leavethese areas of the atmosphere relatively undisturbed. It is easier for protonbeams to penetrate to the deeper layers and not deposit their energy in theupper chromosphere where the Balmer lines are formed. The relatively weakparticle beams that are applicable to this flare do not cause a significantshift of the $\tau=1$ surface and the observed excess WL emission is opticallythin.

Reproducing Type II White-Light Solar Flare Observations with Electron and Proton Beam Simulations