  We present radiative hydrodynamic simulations of solar flares generated by
the RADYN and RH codes to study the perturbations induced in photospheric Fe I
lines by electron beam heating. We investigate how variations in the beam
parameters result in discernible differences in the induced photospheric
velocities. Line synthesis revealed a significant chromospheric contribution to
the line profiles resulting in an apparent red asymmetry by as much as 40 m/s
close to the time of maximum beam heating which was not reflective of the
upflow velocities that arose from the radiative hydrodynamic simulations at
those times. The apparent redshift to the overall line profile was produced by
significant chromospheric emission that was blueshifted by as much as 400 m/s
and fills in the blue side of the near stationary photospheric absorption
profile. The velocity information that can be retrieved from photospheric line
profiles during flares must therefore be treated with care to mitigate the
effects of higher parts of the atmosphere providing an erroneous velocity
signal.
