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[1] Three-dimensional multifluid simulations of the solar wind interaction with a magnetized Mars are used to determine both the effect of the crustal magnetic field on ionospheric loss rate and the ionospheric loss rate as a function of solar wind conditions. Ionospheric losses on the order of 10 25 O 2 + ions per second are found for quiet solar wind conditions. This is of the same order as that estimated from Phobos 2 measurements. Varying the orientation of Mars' magnetic anomalies relative to the incident solar wind direction leads to only minor variation in the ionospheric loss rates of O 2 + for each set of solar wind conditions studied. Solar wind parameters were varied from nominal solar wind conditions to conditions with high-speed flows, high densities, and large IMF magnitudes. Outflow rates on the order of 10 26 O 2 + ions per second were seen for storm-like conditions. The simulations indicate that ionospheric outflow rates increase by a larger percentage for high solar wind number density when compared to high solar wind speed or strong IMF conditions alone. This is due to the higher solar wind density and temperature of the precipitating ions. The results also indicate a significant influence of pickup on ionospheric loss.

[1] Multifluid modeling of Saturn's magnetosphere produces the first numerical simulation showing the development of hot, tenuous plasma from the plasma sheet interchanging with cold, denser plasma from the inner magnetosphere. Individual injection events are seen regularly by Cassini, but with a single observation it is impossible to determine the global distribution. Multifluid simulations enable us to characterize the growth and development of not merely one injection event but show that it is a global process dependent on both the plasma distribution of ions from Enceladus and forcing by solar wind conditions. Development of the interchange arises in a fashion similar to a Rayleigh-Taylor instability, except that the heavy ions are being driven outward not by gravity but by centrifugal forces. Interplanetary magnetic field (IMF) parallel to the planetary magnetic field reduces centrifugal forcing, whereas antiparallel IMF increases the forcing, by altering the bowl-like shape of the plasma sheet. However, the interchange instability also develops under normally quiet parallel IMF conditions when the mass loading of the Enceladus torus is increased. The total number of interchange events is 1-2 higher for the antiparallel case versus the increased mass case. Interchange develops in the vicinity of 7 R S , and once the fingers of cold plasma reach $12-14 R S (close to the inner edge of the plasma sheet) they spread in the azimuthal direction, because of the fact that the magnetic field is too weak to keep the fingers solidly locked in rotation. The derived energy characteristics of the interchanging plasma are shown to be consistent with Cassini data.