The frozen, alien landscape of Ganymede contains a little of everything. Shadowy regions of ancient, battered dark terrain are cross-cut by newer patches of ice-rich, grooved bright terrain. Ganymede's diverse surface features bridge the stark divide between its sibling Galilean moons, evoking both Callisto's barren, rocky surface, and Europa's bizarrely cracked and faulted icy landscape.

Ganymede's complexity deepens when you look beyond its surface. Beneath its outer shell of rock and ice lurks a vast ocean that may contain more water than all of Earth's oceans combined. What's more, this planet-sized body (Ganymede is 26% larger than Mercury by volume!) is the only solar-system moon to produce its own, intrinsic magnetic field - which means it hosts a magnetosphere that interacts with the larger Jovian magnetosphere.

Digging Under the Surface
This complicated satellite's properties means that there are many different processes - originating from both its interior and its exterior - that can modify its surface. To better understand what's happening across Ganymede's dramatic landscape, a recent study has now leveraged the high resolution of the Atacama Large Millimeter/submillimeter Array (ALMA) to explore the top layer of this moon's rocky, icy surface.

Scientist Katherine de Kleer (California Institute of Technology) and collaborators observed Ganymede at several different millimeter wavelengths with ALMA and then compared these data to a thermal model, examining the thermal emission of the moon from its surface down to a depth of roughly 50 cm.

From these results, the team built global temperature maps of Ganymede and explored the vertical profile of the moon's near-surface material to identify the physical and chemical processes at play in this region.

Taking Ganymede's Temperature
De Kleer and collaborators found that Ganymede's material becomes rapidly less porous and more densely packed below the surface: its porosity drops from 85% at the surface to just 10% at depth. This measurement tells us how rapidly the moon's material responds to changes in heating (for instance, daytime illumination by the Sun): the more porous surface material loses and gains heat more quickly, whereas the deeper material responds slowly.

From their global temperature maps, the authors identified the regions of Ganymede's surface that deviate from best-fit models - like several bright craters that are substantially colder than predicted. Deviations like this point to variations in the local composition, porosity, and grain properties of the moon's surface material.

De Kleer and collaborators also noted larger-scale deviations in temperature - in particular, excess heat measured at the equator and cooler temperatures than predicted at middle latitudes. These differences suggest that Ganymede's surface is predominantly influenced by external processes, like bombardment by micrometeorites and plasma on its orbit around Jupiter.

More detailed studies of Ganymede are likely in the future, and ALMA observations of Europa and Callisto are currently being analyzed - so we can expect further insight into the surfaces of these complex, icy bodies soon.

"Ganymede's Surface Properties from Millimeter and Infrared Thermal Emission"