  We investigate roles of Alfvenic waves in the weakly-ionized atmosphere of
hot Jupiters by carrying out non-ideal magnetohydrodynamic (MHD) simulations
with Ohmic diffusion in one-dimensional magnetic flux tubes. Turbulence at the
surface excites Alfven waves and they propagate upward to drive hot (~ 10^4 K)
outflows. The magnetic diffusion plays an important role in the dissipation of
the Alfvenic waves in the weakly ionized atmosphere of hot Jupiters. The
mass-loss rate of the spontaneously driven planetary wind is considerably
reduced, in comparison with that obtained from ideal MHD simulations because
the Alfvenic waves are severely damped at low altitudes in the atmosphere,
whereas the wave heating is still important in the heating of the upper
atmosphere. Dependence on the surface temperature, planetary radius, and
velocity dispersion at the surface is also investigated. We find an inversion
phenomenon of the transmitted wave energy flux; the energy flux carried by
Alfven waves in the upper atmosphere has a nonmonotonic correlation with the
input energy flux from the surface in a certain range of the surface
temperature because the resistivity is determined by the global physical
properties of the atmosphere in a complicated manner. We also point out that
the heating and mass loss are expected only in limited zones if the open
magnetic field is confined in the limited regions.
