title: Unified model of tectonics and heat transport in a frigid Enceladus.
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.
authors: Department of Mechanical Science and Engineering, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USA.
authors: Gustavo
authors: G
authors: Gioia
authors: Pinaki
authors: P
authors: Chakraborty
authors: Stephen
authors: S
authors: Marshak
authors: Susan W
authors: SW
authors: Kieffer
references: Proc Natl Acad Sci U S A. 2004 Sep 14;101(37):13400-7
references: 15289601
references: Science. 2006 Mar 10;311(5766):1389-91
references: 16527962
references: Science. 2006 Mar 10;311(5766):1393-401
references: 16527964
references: Science. 2006 Mar 10;311(5766):1401-5
references: 16527965
references: Nature. 2007 May 17;447(7142):289-91
references: 17507976
references: Science. 2006 Mar 10;311(5766):1422-5
references: 16527971
references: Nature. 2006 Jun 1;441(7093):614-6
references: 16738654
references: Science. 2006 Dec 15;314(5806):1764-6
references: 17170301
references: Science. 2006 Mar 10;311(5766):1419-22
references: 16527970