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Pediment formation and subsequent erosion in Gale crater: Clues to the climate history of Mars

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  • معلومة اضافية
    • Contributors:
      Department of Earth and Planetary Science UC Berkeley (EPS); University of California Berkeley (UC Berkeley); University of California (UC)-University of California (UC); US Geological Survey Flagstaff (USGS); United States Geological Survey Reston (USGS); Carleton College; The University of Tennessee Knoxville; Caltech Division of Geological and Planetary Sciences; California Institute of Technology (CALTECH); University of Chicago; Planetary and Space Science Centre (PASSC); University of New Brunswick (UNB); Department of Earth Science and Engineering Imperial College London; Imperial College London; Department of Geological Sciences Bloomington; Indiana University Bloomington; Indiana University System-Indiana University System; Smithsonian National Air and Space Museum; Smithsonian Institution; Jet Propulsion Laboratory (JPL); NASA-California Institute of Technology (CALTECH); Los Alamos National Laboratory (LANL); Purdue University West Lafayette; Washington University in Saint Louis (WUSTL); Institut de recherche en astrophysique et planétologie (IRAP); Université Toulouse III - Paul Sabatier (UT3); Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP); Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3); Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales Toulouse (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales Toulouse (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS); Laboratoire de Planétologie et Géosciences UMR_C 6112 (LPG); Le Mans Université (UM)-Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST); Nantes Université - pôle Sciences et technologie; Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie; Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ); Planetary Science Institute Tucson (PSI); Institut d'astrophysique spatiale (IAS); Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales Paris (CNES); Johns Hopkins University (JHU); University of California Santa Cruz (UC Santa Cruz); University of California (UC); IT University of Copenhagen (ITU); Cornell Center for Astrophysics and Planetary Science (CCAPS); Cornell University New York; Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE); École normale supérieure de Lyon (ENS de Lyon); Université de Lyon-Université de Lyon-Université Claude Bernard Lyon 1 (UCBL); Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS); The University of New Mexico Albuquerque; New Mexico Consortium (NMC); Malin Space Science Systems (MSSS)
    • بيانات النشر:
      CCSD
      Elsevier
    • الموضوع:
      2025
    • Collection:
      Université Jean Monnet – Saint-Etienne: HAL
    • نبذة مختصرة :
      International audience ; Evidence of paleo-rivers, fans, deltas, lakes, and channel networks across Mars has prompted much debate about what climate conditions would permit the formation of these surface water derived features. Pediments, gently sloping erosional surfaces of low relief developed in bedrock, have also been identified on Mars. On Earth, these erosional landforms, often thought to be created by overland flow and shallow channelized runoff, are typically capped by fluvial sediments, and thus in exceptionally arid regions, pediments are interpreted to record past wet periods. Here we document the Greenheugh pediment in Gale crater, exploiting the observational capability of the Curiosity rover. The absence of a fluvial cap suggests that the pediment was likely cut by wind erosion, not fluvial processes. The pediment was then buried by an aeolian deposit (Stimson sandstone) that mantled the lower footslopes of Aeolis Mons (informally known as Mt. Sharp). This burial terminated active wind erosion, preserving the pediment surface (as an angular unconformity). Groundwater was present prior-to, during, and shortly after Stimson deposition, perhaps contributing to lithification and certainly to early diagenesis. Post lithification, wind erosion first cut canyons in the northern most footslopes (north of Vera Rubin ridge). Unlithified gravels were deposited in these canyons, likely due to runoff from Mt. Sharp. Boulder-rich fluvial and debris flow deposits built a > 70 m thick sequence (Gediz Vallis ridge) on the southern Greenheugh pediment. Continued wind erosion left elevated patches of gravel on the northern footslopes, and exposure age dating shows that erosion essentially ceased before 1 Ga (but possibly much earlier). Erosion to the south led to emergence of Vera Rubin ridge, retreat of the Greenheugh pediment, and the formation of Glen Torridon valley. Hence, this footslope environment of Mt. Sharp records climate-driven periods of wind erosion, aeolian deposition (and groundwater activity), ...
    • الرقم المعرف:
      10.1016/j.icarus.2024.116445
    • الدخول الالكتروني :
      https://hal.science/hal-04924951
      https://hal.science/hal-04924951v1/document
      https://hal.science/hal-04924951v1/file/Bryk2025.pdf
      https://doi.org/10.1016/j.icarus.2024.116445
    • Rights:
      http://creativecommons.org/licenses/by/ ; info:eu-repo/semantics/OpenAccess
    • الرقم المعرف:
      edsbas.4D281517