  SDO/HMI observations reveal a class of solar flares with substantial energy
and momentum impacts in the photosphere, concurrent with white-light emission
and helioseismic responses, known as sunquakes. Previous radiative hydrodynamic
modeling has demonstrated the challenges of explaining sunquakes in the
framework of the standard flare model of `electron beam' heating. One of the
possibilities to explain the sunquakes and other signatures of the photospheric
impact is to consider additional heating mechanisms involved in solar flares,
for example, via flare-accelerated protons. In this work, we analyze a set of
single-loop Fokker-Planck and radiative hydrodynamics RADYN+FP simulations
where the atmosphere is heated by non-thermal power-law-distributed proton
beams which can penetrate deeper than the electron beams into the low
atmospheric layers. Using the output of the RADYN models, we calculate
synthetic Fe I 6173 A line Stokes profiles and from those the line-of-sight
(LOS) observables of the SDO/HMI instrument, as well as the 3D helioseismic
response and compare them with the corresponding observational characteristics.
These initial results show that the models with proton beam heating can produce
the enhancement of the HMI continuum observable and explain qualitatively
generation of sunquakes. The continuum observable enhancement is evident in all
models but is more prominent in ones with $E_{c}\geq$500 keV. In contrast, the
models with $E_{c}\leq$100 keV provide a stronger sunquake-like helioseismic
impact according to the 3D acoustic modeling, suggesting that low-energy (deka-
and hecto-keV) protons have an important role in the generation of sunquakes.
