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dc.contributor.authorSutton, Sarah S.
dc.contributor.authorHamilton, Christopher W.
dc.contributor.authorCataldo, Vincenzo
dc.contributor.authorWilliams, David A.
dc.contributor.authorBleacher, Jacob E.
dc.date.accessioned2022-01-13T19:42:41Z
dc.date.available2022-01-13T19:42:41Z
dc.date.issued2022-03
dc.identifier.citationSutton, S. S., Hamilton, C. W., Cataldo, V., Williams, D. A., & Bleacher, J. E. (2022). Sinuous channels east of Olympus Mons, Mars: Implications for volcanic, hydrological, and tectonic processes. Icarus.en_US
dc.identifier.issn0019-1035
dc.identifier.doi10.1016/j.icarus.2021.114798
dc.identifier.urihttp://hdl.handle.net/10150/662888
dc.description.abstractThe Late Amazonian volcanic plains east of Olympus Mons contain numerous channels and fossae. Channel formation hypotheses have included volcanic processes, flowing water, or a combination of both. To evaluate these hypotheses, we conducted detailed geomorphological and facies mapping at two sites containing channels and fossae representative of features in the region. Based on our mapping and morphological analyses using high resolution topography and images from HiRISE and CTX data, we classified channels into three types, and fossae into two types. Channel Type 1 and Type 2 are consistent with the morphology of lava channels, however, we found no evidence of channel formation due to thermo-mechanical erosion. Additionally, we calculated the potential for lava to achieve turbulent flow within our two study sites and found it unlikely. Channel Type 3 is consistent with fluvial bedrock erosion, likely sourced from erupted groundwater that entrained regolith into lahar-like flows. Fossae are classified as linear (Type L) or arcuate and branched (Type A). Type L fossae are interpreted to be surface fractures associated with dike emplacement, whereas Type A fossae are interpreted to be surface fractures due to sill emplacement, which may have melted buried ice deposits and generated meltwater floods. Type 1 and Type 2 channels are associated with Type L fossae and fissure-fed effusive eruptions of lava. In contrast, Type 3 channels are co-located with Type A fossae, and are likely due to outbursts of groundwater possibly related to sill emplacement. We attribute the formation and distribution of channels and fossae throughout the plains east of Olympus Mons to be a consequence of the region's evolving states of stress, which are predominantly influenced by the loading of Olympus Mons. © 2021 Elsevier Inc.en_US
dc.description.sponsorshipNational Science Foundationen_US
dc.language.isoenen_US
dc.publisherElsevier BVen_US
dc.rights© 2021 Elsevier Inc. All rights reserved.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/en_US
dc.subjectGeological processesen_US
dc.subjectMars, interioren_US
dc.subjectMars, surfaceen_US
dc.subjectTectonicsen_US
dc.subjectVolcanismen_US
dc.titleSinuous channels east of Olympus Mons, Mars: Implications for volcanic, hydrological, and tectonic processesen_US
dc.typeArticleen_US
dc.contributor.departmentLunar and Planetary Laboratory, University of Arizonaen_US
dc.identifier.journalIcarusen_US
dc.description.note24 month embargo; available online: 24 November 2021en_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal accepted manuscripten_US
dc.identifier.piiS0019103521004450
dc.source.journaltitleIcarus
dc.source.volume374
dc.source.beginpage114798


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