  We perform an analysis of the line-of-sight (LOS) observables of the SDO/HMI
for models of the solar atmosphere heated by precipitating high-energy
electrons during solar flares. The radiative hydrodynamic (RADYN) flare models
are obtained from the F-CHROMA database. The Stokes profiles for the Fe 6173 A
line observed by SDO/HMI are calculated using the radiative transfer code
RH1.5D assuming statistical equilibrium for atomic level populations and
imposing uniform background vertical magnetic field of various strength. The
SDO/HMI observing sequence and LOS data processing pipeline algorithm are
applied to derive the observables (continuum intensity, line depth, Doppler
velocity, LOS magnetic field). Our results reveal that the strongest deviations
of the observables from the actual spectroscopic line parameters are found for
the model with a total energy deposited of $E_{total}=1.0\times{}10^{12}$ erg
cm$^{-2}$, injected with power-law spectral index of $\delta=3$ above a
low-energy cutoff of $E_{c}=25$ keV. The magnitudes of the velocity and
magnetic field deviations depend on the imposed magnetic field, and can reach
0.35 km/s for LOS velocities, 90 G for LOS magnetic field, and 3\% for
continuum enhancement for the 1000 G imposed LOS magnetic field setup. For
$E_{total}\geq{}3.0\times{}10^{11}$ erg cm$^{-2}$ models, the velocity and
magnetic field deviations are most strongly correlated with the energy flux
carried by $\sim$50 keV electrons, and the continuum enhancement is correlated
with the synthesized $\sim$55-60 keV hard X-ray photon flux. The relatively low
magnitudes of perturbations of the observables and absence of magnetic field
sign reversals suggest that the considered radiative hydrodynamic beam heating
models augmented with the uniform vertical magnetic field setups cannot explain
strong transient changes found in the SDO/HMI observations.
