  Io, the most volcanically active body in the solar system, loses heat through
eruptions of hot lava. Heat is supplied by tidal heating and is thought to be
transferred through the mantle by magmatic segregation, a mode of transport
that sets it apart from convecting terrestrial planets. We present a model that
couples magmatic transport of tidal heat to the volcanic system in the crust,
in order to determine the controls on crustal thickness, magmatic intrusions,
and eruption rates. We demonstrate that magmatic intrusions are a key component
of Io's crustal heat balance; around 80% of the magma delivered to the base of
the crust must be emplaced and frozen as plutons to match rough estimates of
crustal thickness. As magma ascends from a partially molten mantle into the
crust, a decompacting boundary layer forms, which can explain inferred
observations of a high-melt-fraction region.
