Unified model of tectonics and heat transport in a frigid Enceladus
- Departments of *Mechanical Science and Engineering and
- †Geology, University of Illinois at Urbana–Champaign, Urbana, IL 61801
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Contributed by Susan W. Kieffer, June 26, 2007 (received for review May 16, 2007)
Abstract
Recent data from the Cassini spacecraft have revealed that Enceladus, the 500-km-diameter moon of Saturn, has a southern hemisphere with a distinct arrangement of tectonic features, intense heat flux, and geyser-like plumes. How did the tectonic features form? How is the heat transported from depth? To address these questions, we formulate a simple model that couples the mechanics and thermodynamics of Enceladus and gives a unified explanation of the salient tectonic features, the plumes, and the transport of heat from a source at a depth of tens of kilometers to the surface. Our findings imply that tiny, icy moons can develop complex surficial geomorphologies, high heat fluxes, and geyser-like activity even if they do not have hot, liquid, and/or convecting interiors.
Footnotes
- ‡To whom correspondence should be addressed. E-mail: skieffer{at}uiuc.edu
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Author contributions: G.G., P.C., and S.W.K. designed research; G.G., P.C., S.M., and S.W.K. performed research; G.G., P.C., S.M., and S.W.K. analyzed data; and G.G. wrote the paper.
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The authors declare no conflict of interest.
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↵ § Helfenstein, P., Thomas, P. C., Veverka, J., Rathbun, J., Perry, J., Turtle, E., Denk, T., Neukum, G., Roatsch, T., Wagner, R., et al. (2006) Lunar Planet Inst Conf Abstr 37:2182. Available at www.lpi.usra.edu/meetings/Ipsc2006/pdf/2182.pdf.
- Abbreviation:
- TST,
- tiger-stripe terrain.
- © 2007 by The National Academy of Sciences of the USA
