Polar wind is an important source of plasma in the magnetosphere at Earth, and it has been shown to be a contributor to the magnetospheric population at Saturn and Jupiter. We are developing a semi-kinetic, non-classical polar wind model for rapidly rotating systems to characterise the material escaping the upper atmosphere and the physical processes that dominate the escape, including evaluating with the auroral current systems. We present early results from the model and compare to in situ data at Jupiter and Saturn.
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