none 10.1144/SP356.4 Geological Society of London Geological Society of London 1881 49840281 65091 2024072310092700393 10.1144 2024-07-23T18:54:00Z 2011-08-22T15:04:22Z 9 Geological Society, London, Special Publications SP 0305-8719 2041-4927 08 22 2011 01 2011 356 1 S. Van Gasselt Institute of Geological Sciences, Planetology and Remote Sensing, Freie Universitaet Berlin, Malteserstrasse 74-100, D-12249 Berlin, Germany E. Hauber Institute of Planetary Research, Department of Planetary Geology, German Aerospace Centre (DLR), Rutherfordstrasse 2, D-12489 Berlin, Germany A.-P. Rossi International Space Science Institute (ISSI), Hallerstrasse 6, CH-3012 Bern, Switzerland Jacobs University Bremen, Campus Ring 1, D-28759 Bremen, Germany A. Dumke Institute of Geological Sciences, Planetology and Remote Sensing, Freie Universitaet Berlin, Malteserstrasse 74-100, D-12249 Berlin, Germany R. Orosei Institute of Physics of Interplanetary Space (IFSI), 00133 Rome, Italy G. Neukum Institute of Geological Sciences, Planetology and Remote Sensing, Freie Universitaet Berlin, Malteserstrasse 74-100, D-12249 Berlin, Germany Abstract A systematic survey was undertaken and an investigation carried out into the geomorphological characteristics of lobate debris aprons in the Tempe Terra region of Mars. Based on the most recent high-resolution (sub 15 m per pixel) imagery and on new topography data, this study endeavoured to raise and discuss questions regarding their formation (emplacement) and modification (deformation sequence), as well as the role of a mantling deposit found at mid-latitude locations on Mars. Furthermore, a model for the formation of debris aprons in the Tempe Terra–Mareotis Fossae settings is proposed. Image survey, in combination with basic morphometric observations within a geomorphological context, provided additional insights into the source, emplacement and modification of hillslope debris material. Our results imply that lobate debris aprons are not mainly relicts of remnant degradation but are substantially composed of mantling material probably deposited episodically in the course of planetary obliquity changes and over a long timespan, as derived erosion rates suggest. 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