  A three-dimensional, multifluid simulation of a giant planet's magnetospheric
interaction with steady-state stellar wind from a Sun-like star was performed
for four different orbital semi-major axes - 10, 5, 1 and 0.2 AU. We simulate
the effect of the increasing, steady-state stellar wind pressure related to the
planetary orbital semi-major axis on the global magnetospheric dynamics for a
Saturn-like planet, including an Enceladus-like plasma torus. Mass loss
processes are shown to vary with orbital distance, with the centrifugal
interchange instability displayed only in the 10 AU and 5 AU cases which reach
a state of mass loss equilibrium more slowly than the 1 AU or 0.2 AU cases. The
compression of the magnetosphere in the 1 AU and 0.2 AU cases contributes to
the quenching of the interchange process by increasing the ratio of total
plasma thermal energy to corotational energy. The strength of field-aligned
currents (FAC), associated with auroral radio emissions, are shown to increase
in magnitude and latitudinal coverage with a corresponding shift equatorward
from increased dynamic ram pressure experienced in the hotter orbits. Similar
to observed hot Jovian planets, the warm exo-Saturn simulated in the current
work shows enhanced ion density in the magnetosheath and magnetopause regions,
as well as the plasma torus which could contribute to altered transit signals,
suggesting that for planets in warmer ($>$0.1 AU) orbits, planetary magnetic
field strengths and possibly exomoons - via the plasma torus - could be
observable with future missions.
