  We investigate the importance of varying the ram pressure to more
realistically mimic the infall of a cluster satellite galaxy when comparing ram
pressure stripping simulations to observations. We examine the gas disk and
tail properties of stripped cluster galaxies in eight "wind-tunnel"
hydrodynamical simulations with either varying or constant ram pressure
strength. In simulations without radiative cooling, applying a varying wind
leads to significantly different density and velocity structure in the tail
than found when applying a constant wind, although the stripping rate, disk
mass, and disk radius remain consistent in both scenarios. In simulations with
radiative cooling, the differences between a constant and varying wind are even
more pronounced. Not only is there a difference in morphology and velocity
structure in the tails, but a varying wind leads to a much lower stripping
rate, even after the varying wind has reached the ram pressure strength of the
constant wind. Also, galaxies in constant and varying wind simulations with the
same gas disk mass do not have in the same gas disk radius. A constant wind
cannot appropriately model the ram pressure stripping of a galaxy entering a
cluster. We conclude that simulations attempting detailed comparisons with
observations must take the variation of the ram pressure profile due to a
galaxy's orbit into consideration.
