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

The Journey Counts: The Importance of Including Orbits when Simulating Ram Pressure Stripping