Pervasive aqueous paleoflow features in the Aeolis/Zephyria Plana region, Mars

dc.contributor.authorBurr, Devon M.
dc.contributor.authorEnga, Marie-Therese
dc.contributor.authorWilliams, Rebecca M. E.
dc.contributor.authorZimbelman, James R.
dc.contributor.authorHoward, Alan D.
dc.contributor.authorBrennand, Tracy A.
dc.date.accessioned2009-03-02T18:05:33Z
dc.date.available2009-03-02T18:05:33Z
dc.date.issued2009
dc.description.abstractA survey of THEMIS visible wavelength images in the Aeolis/Zephyria Plana region over the two western lobes of the equatorial Medusae Fossae Formation (MFF) shows ~150 sinuous ridges having a variety of morphologies and contexts. To systematize investigation, we use a classification scheme including both individual ridge and ridge network types, as well as associations with impact craters and fan-shaped features. The morphology of the ridges, their location downslope from higher topography (e.g., crater rims and scarps), and their association with fan-shaped forms indicate that most sinuous ridges formed through overland aqueous flow. Analysis of observations by individual ridge type leads to interpretation of most of these sinuous ridges as inverted fluvial channels or floodplains and a few as possible eskers, with the origin of the remaining ridges under continuing investigation. About 15% of the sinuous ridges are associated with impact craters, but data analysis does not support a genetic relationship between the craters and the sinuous ridges. Instead, analysis of one sinuous ridge network associated with a crater indicates that the water source for the network was atmospheric in origin, namely, precipitation runoff. The broad areal distribution of these ~150 ridges and the network morphologies, in particular the branched and subparallel types, suggest that an atmospheric water source is generally applicable to the population of sinuous ridges as a whole. This concentration of sinuous ridges is the largest single population of such landforms on Mars and among the youngest. These ridges are situated at a paleoscarp between Cerberus Palus and the Aeolis highlands, suggesting that the precipitation that formed them was orographic in origin. The ages of the equatorial MFF units in which this population of sinuous ridges is found imply that this orographic rain and/or snow fell during some period from the late Hesperian through the middle Amazonian.
dc.format.extent6528655 bytes
dc.format.extent52–76
dc.format.mimetypeapplication/pdf
dc.identifier0019-1035
dc.identifier.citationBurr, Devon M., Enga, Marie-Therese, Williams, Rebecca M. E., Zimbelman, James R., Howard, Alan D., and Brennand, Tracy A. 2009. "<a href="https://repository.si.edu/handle/10088/7049">Pervasive aqueous paleoflow features in the Aeolis/Zephyria Plana region, Mars</a>." <em>Icarus</em>, 200, (1) 52–76. <a href="https://doi.org/10.1016/j.icarus.2008.10.014">https://doi.org/10.1016/j.icarus.2008.10.014</a>.
dc.identifier.issn0019-1035
dc.identifier.urihttp://hdl.handle.net/10088/7049
dc.language.isoen_US
dc.relation.ispartofIcarus 200 (1)
dc.titlePervasive aqueous paleoflow features in the Aeolis/Zephyria Plana region, Mars
dc.typearticle
sro.description.unitNASM
sro.description.unitNASM-CEPS
sro.identifier.doi10.1016/j.icarus.2008.10.014
sro.identifier.itemID77515
sro.identifier.refworksID31645
sro.identifier.urlhttps://repository.si.edu/handle/10088/7049

Files