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Terrestrial gullies and debris-flow tracks on Svalbard as planetary analogs for Mars

By
D. Reiss
D. Reiss
1 Institut für Planetologie, Westfälische Wilhelms-Universität, Wilhelm-Klemm-Strasse 10, 48149 Münster, Germany
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E. Hauber
E. Hauber
2 Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Rutherfordstrasse 2, 12489 Berlin, Germany
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H. Hiesinger
H. Hiesinger
1 Institut für Planetologie, Westfälische Wilhelms-Universität, Wilhelm-Klemm-Strasse 10, 48149 Münster, Germany
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R. Jaumann
R. Jaumann
2 Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Rutherfordstrasse 2, 12489 Berlin, Germany
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F. Trauthan
F. Trauthan
2 Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Rutherfordstrasse 2, 12489 Berlin, Germany
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F. Preusker
F. Preusker
2 Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Rutherfordstrasse 2, 12489 Berlin, Germany
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M. Zanetti
M. Zanetti
1 Institut für Planetologie, Westfälische Wilhelms-Universität, Wilhelm-Klemm-Strasse 10, 48149 Münster, Germany
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M. Ulrich
M. Ulrich
3 Alfred Wegener Institute for Polar and Marine Research, Research Unit Potsdam, Telegrafenberg A43, 14473 Potsdam, Germany
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A. Johnsson
A. Johnsson
4 Department of Earth Sciences, University of Gothenburg, Box 460, SE-405 30 Göteborg, Sweden
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L. Johansson
L. Johansson
4 Department of Earth Sciences, University of Gothenburg, Box 460, SE-405 30 Göteborg, Sweden
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M. Olvmo
M. Olvmo
4 Department of Earth Sciences, University of Gothenburg, Box 460, SE-405 30 Göteborg, Sweden
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E. Carlsson
E. Carlsson
5 Swedish Institute of Space Physics, Box 812, SE-981 28 Kiruna, Sweden
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H.A.B. Johansson
H.A.B. Johansson
6 AlbaNova University Center, Stockholm University, S-10691 Stockholm, Sweden
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S. McDaniel
S. McDaniel
7 Reactive Surfaces, Ltd., 300 West Avenue, Austin, Texas 78701, USA
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Published:
December 01, 2011

We compared the morphology of gully sedimentary fans on Svalbard as possible analogs to gullies on Mars in order to constrain whether fluvial and/or debris-flow processes are predominantly responsible for the formation of Martian gullies. Our analysis is based on high-resolution imagery (High Resolution Stereo Camera [HRSC-AX], ~20 cm/pixel) acquired through a flight campaign in summer 2008 and ground truth during two expeditions in the summers of 2008 and 2009 in Svalbard, compared to high-resolution satellite imagery (High Resolution Imaging Science Experiment [HiRISE], ~25 cm/pixel) from Mars. On Svalbard, fluvial and debris-flow processes are evident in the formation of gullies, but the morphological characteristics clearly show that the transport and sedimentation of eroded material are predominated by debris flows. Most investigated gullies on Mars lack clear evidence for debris-flow processes. The Martian gully fan morphology is more consistent with the deposition of small overlapping fans by multiple fluvial flow events. Clear evidence for debris flows on Mars was only found in one new location, in addition to a few previously published examples. The occurrence of debris-flow processes in the formation of Martian gullies seems to be rare and locally limited. If predominantly fluvial processes caused the formation of gullies on Mars, then large amounts of water would have been required for their formation because of the relatively low sediment supply in stream and/or hyperconcentrated flows. Repeated seasonal or episodic snow deposition and melting during periods of higher obliquity in the recent past on Mars can best explain the formation of the gullies.

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Figures & Tables

Contents

GSA Special Papers

Analogs for Planetary Exploration

W. Brent Garry
W. Brent Garry
Planetary Science Institute, Tucson, Arizona, USA
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Jacob E. Bleacher
Jacob E. Bleacher
NASA Goddard Space Flight Center, Planetary Geodynamics Lab, Greenbelt, Maryland, USA
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Geological Society of America
Volume
483
ISBN print:
9780813724836
Publication date:
December 01, 2011

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