  We present calculations of the auroral radio powers expected from exoplanets
with magnetospheres driven by an Earth-like magnetospheric interaction with the
solar wind. Specifically, we compute the twin cell-vortical ionospheric flows,
currents, and resulting radio powers resulting from a Dungey cycle process
driven by dayside and nightside magnetic reconnection, as a function of
planetary orbital distance and magnetic field strength. We include saturation
of the magnetospheric convection, as observed at the terrestrial magnetosphere,
and we present power law approximations for the convection potentials, radio
powers and spectral flux densities. We specifically consider a solar-age system
and a young (1 Gyr) system. We show that the radio power increases with
magnetic field strength for magnetospheres with saturated convection potential,
and broadly decreases with increasing orbital distance. We show that the
magnetospheric convection at hot Jupiters will be saturated, and thus unable to
dissipate the full available incident Poynting flux, such that the magnetic
Radiometric Bode's Law (RBL) presents a substantial overestimation of the radio
powers for hot Jupiters. Our radio powers for hot Jupiters are $\sim$5-1300 TW
for hot Jupiters with field strengths of 0.1-10 $B_J$ orbiting a Sun-like star,
while we find that competing effects yield essentially identical powers for hot
Jupiters orbiting a young Sun-like star. However, in particular for planets
with weaker magnetic fields our powers are higher at larger orbital distances
than given by the RBL, and there are many configurations of planet that are
expected to be detectable using SKA.
