  Ridge-and-trough terrain is a common landform on outer Solar System icy
satellites. Examples include Ganymede's grooved terrain, Europa's gray bands,
Miranda's coronae, and several terrains on Enceladus. The conditions associated
with the formation of each of these terrains are similar: heat flows of order
tens to a hundred milliwatts per meter squared, and deformation rates of order
$10^{-16}$ to $10^{-12}$ s$^{-1}$. Our prior work shows that the conditions
associated with the formation of these terrains on Ganymede and the south pole
of Enceladus are consistent with vigorous solid-state ice convection in a shell
with a weak surface. We show that sluggish lid convection, an intermediate
regime between the isoviscous and stagnant lid regimes, can create the heat
flow and deformation rates appropriate for ridge and trough formation on a
number of satellites, regardless of the ice shell thickness. For convection to
deform their surfaces, the ice shells must have yield stresses similar in
magnitude to the daily tidal stresses. Tidal and convective stresses deform the
surface, and the spatial pattern of tidal cracking controls the locations of
ridge-and-trough terrain.
