The primary loss process for the ionized component of satellite debris in Jupiter's magnetosphere appears to be radial transport, which carries the satellite-derived ions away from the source satellite. Cross L (interchange) diffusion is a likely candidate for the radial transport mechanism. Many consequences are predicted to result from satellite ions that reach regions close to and remote from Jupiter. The ratio of the inward to outward flux of diffusing ions from a given satellite is therefore important as an input to the magnitudes of expected consequences. In the formal analysis of cross L diffusion, the flux ratio depends on poorly know boundary conditions and on a poorly determined diffusion coefficient. We present here an analysis of the sensitivity of the flux ratio to the uncertainties in the mentioned parameters. The main result is that if the diffusion is driven externally, for example by winds in Jupiter's ionosphere, the inward flux exceeds or is of the same order of magnitude as the outward flux. On the other hand, if the diffusion is driven locally by the centrifugal interchange instability, as one interpretation of Voyager plasma data suggests, the outward flux can be one or two orders of magnitude greater than the inward flux. Fits to the Voyager in situ plasma torus data obtained from solutions to the transport equations appropriate to wind driven and centrifugally driven diffusion are compared. In both cases, good fits are obtained. Both require a substantial discontinuity in the diffusion coefficient at Io's orbit, and both require an onset of ion injection a finite time prior to Voyager encounter. The values of the source strength, the duration of injection, and the percentage of inward flux transport, determined thereby differ by a factor of four or less between the two types of diffusion.