Modeling Viscoelastic Crater Relaxation In Ice With Applications To Titan

Details Modeling Viscoelastic Crater Relaxation In Ice With Applications To Titan Modeling Viscoelastic Crater Relaxation In Ice With Applications To Titan

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.5611b&link_type=abstract

American Astronomical Society, DPS meeting #38, #56.11; Bulletin of the American Astronomical Society, Vol. 38, p.587

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Scientific paper

Cassini VIMS, ISS and RADAR have collectively examined over half of the surface of Saturn's moon Titan, and to date only a handful of craters have been identified. Many other Saturnian satellites display evidence of heavy cratering, with Rhea and Mimas as prime examples. While the presence of a thick atmosphere can explain the lack of small craters on Titan, close to two hundred craters per billion years with diameters larger than a few kilometers (Korycansky and Zahnle, P&SS 53) are predicted from crater populations on both the Galilean satellites and Triton (Zahnle, Icarus 163).
We use a viscoelastic rheological model to study the plausibility of viscous relaxation as a mechanism to explain the apparent lack of craters on the surface of Titan. Using TEKTON, a finite element code specifically designed for geophysical application, we model craters similar to those found on other icy satellites in the outer Solar System. We will determine whether viscous relaxation of craters in pure ice I can explain Titan's uncratered surface. We will also model other surface materials with different rheologies and lower viscosity that could further reduce relaxation times for craters on Titan.

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