Thermal stability of ice on Ceres with rough topography

The dwarf planet Ceres may have an ice-rich crust, and subsurface ice exposed by impacts or endogenic activity would be subject to sublimation. We model surface and subsurface temperatures on Ceres to assess lifetimes of water ice and other volatiles. Topographic shadowing allows a small but nonnegligible fraction (similar to 0.4%) of Ceres' surface to be perennially below the similar to 110 K criterion for 1 Gyr of stability. These areas are found above 60 degrees latitude. Other molecules (CH3OH, NH3, SO2, and CO2) may be cold trapped in smaller abundances. A model for the transport, gravitational escape, and photoionization of H2O molecules suggests net accumulation in the cold traps. Buried ice is stable within a meter for > 1 Gyr at latitudes higher than similar to 50 degrees. An illuminated polar cap of water ice would be stable within a few degrees of the poles only if it maintained a high albedo (>0.5) at present obliquity. If the obliquity exceeded 5 degrees in the geologically recent past, then a putative polar cap would have been erased. At latitudes 0 degrees-30 degrees, ice is stable under solar illumination only briefly (similar to 10-100 years), unless it has high albedo and thermal inertia, in which case lifetimes of > 10(4) years are possible. Finally, a small hemispheric asymmetry exists due to the timing of Ceres' perihelion passage, which would lead to a detectable enhancement of ice in the northern hemisphere if the orbital elements vary slowly relative to the ice accumulation rate. Our model results are potentially testable during the Dawn science mission.