Constraining the heat flux between Enceladus’ tiger stripes: Numerical modeling of funiscular plains formation

• Published in: Icarus (New York, N.Y. 1962) N.Y. 1962), 2015-11, Vol.260, p.232-245
• Main Authors: Bland, Michael T., McKinnon, William B., Schenk, Paul M.
• Format: Article
• Language: English
• Subjects: Enceladus; Folding; Heat transfer; Lithosphere; Mathematical models; Morphology; Satellites, surfaces; Surface layer; Tectonics; Terrain; Texture; Thermal histories
• ISSN: 0019-1035; 1090-2643
• DOI: 10.1016/j.icarus.2015.07.016

•Enceladus’ funiscular terrain consists of short wavelength, periodic ridges.•We simulate lithospheric shortening to test whether the terrain formed by folding.•A folding origin requires extreme heat flow, conductivity, and surface temperature.•While extreme, these conditions can be met within the south polar terrain. The Cassini spacecraft’s Composite Infrared Spectrometer (CIRS) has observed at least 5GW of thermal emission at Enceladus’ south pole. The vast majority of this emission is localized on the four long, parallel, evenly-spaced fractures dubbed tiger stripes. However, the thermal emission from regions between the tiger stripes has not been determined. These spatially localized regions have a unique morphology consisting of short-wavelength (∼1km) ridges and troughs with topographic amplitudes of ∼100m, and a generally ropy appearance that has led to them being referred to as “funiscular terrain.” Previous analysis pursued the hypothesis that the funiscular terrain formed via thin-skinned folding, analogous to that occurring on a pahoehoe flow top (Barr, A.C., Preuss, L.J. [2010]. Icarus 208, 499–503). Here we use finite element modeling of lithospheric shortening to further explore this hypothesis. Our best-case simulations reproduce funiscular-like morphologies, although our simulated fold wavelengths after 10% shortening are 30% longer than those observed. Reproducing short-wavelength folds requires high effective surface temperatures (∼185K), an ice lithosphere (or high-viscosity layer) with a low thermal conductivity (one-half to one-third that of intact ice or lower), and very high heat fluxes (perhaps as great as 400mWm−2). These conditions are driven by the requirement that the high-viscosity layer remain extremely thin (≲200m). Whereas the required conditions are extreme, they can be met if a layer of fine grained plume material 1–10m thick, or a highly fractured ice layer >50m thick insulates the surface, and the lithosphere is fractured throughout as well. The source of the necessary heat flux (a factor of two greater than previous estimates) is less obvious. We also present evidence for an unusual color/spectral character of the ropy terrain, possibly related to its unique surface texture. Our simulations demonstrate that producing the funiscular ridges via folding remains plausible, but the relatively extreme conditions required to do so leaves their origin open to further investigation. The high heat fluxes required to produce the