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Evidence for ice flow prior to trough formation in the martian north polar layered deposits |
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| Authors: | Dale P Winebrenner Michelle R Koutnik Asmin V Pathare Bruce C Murray Jonathan L Bamber |
| Institution: | a Applied Physics Laboratory, Box 355640, University of Washington, Seattle, WA 98195, USA b Department of Earth and Space Sciences, Box 351310, University of Washington, Seattle, WA 98195, USA c Planetary Science Institute, 1700 E. Ft. Lowell, Suite 106, Tucson, AZ 85719, USA d Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA e Lunar and Planetary Laboratory, The University of Arizona, Tucson, AZ 85721, USA f Bristol Glaciology Centre, University of Bristol, Bristol BS8 1SS, UK |
| Abstract: | The relative importance of surface mass fluxes and ice flow in shaping the north polar layered deposits (NPLD), now or in the past, remains a fundamental and open question. Motivated by observation of an apparent ice divide on Gemina Lingula (also known as Titania Lobe), we propose a two-stage evolution leading to the present-day topography on that lobe of the NPLD. Ice flow approximately balances surface mass fluxes in the first stage, but in the second stage ice flow has minimal influence and topography is modified predominantly by the formation of troughs. We focus here on evidence for the first stage, by testing the fit of topography between troughs to an ice-flow model. We find that independent model fits on distinct flow paths closely match inter-trough topography, uniformly over a broad region on Gemina Lingula, with mutually consistent and physically reasonable fitting parameters. However, our model requires ice to occupy and flow in spaces where troughs currently incise the ice. We therefore infer that the troughs (and the distribution of mass balance that caused them) post-date deposition of the inter-trough material and its modification by flow. Because trough formation has apparently altered inter-trough topography very little, we infer that trough formation must have been rapid in comparison to the (still unknown) time-scale of flow since troughs began to form. We view the evidence for past flow as strong, but we do not think that topographic evidence alone can be conclusive. Observations of englacial stratigraphy using orbital sounding radars will yield conclusive tests of our inferred mechanism for the formation of inter-trough topography. |
| Keywords: | Mars polar caps Geophysics Ices |
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