Wet Mars implications of revised scaling calculations for Evros Vallis

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dc.contributor.author Caprarelli, Graziella en_US
dc.contributor.author Wang, Bu en_US
dc.contributor.editor en_US
dc.date.accessioned 2012-10-12T03:32:56Z
dc.date.available 2012-10-12T03:32:56Z
dc.date.issued 2012 en_US
dc.identifier 2011003761 en_US
dc.identifier.citation Caprarelli Graziella and Wang Bu 2012, 'Wet Mars implications of revised scaling calculations for Evros Vallis', Blackwell Publishing Ltd, vol. 59, no. 2 Special Issue, pp. 263-276. en_US
dc.identifier.issn 0812-0099 en_US
dc.identifier.other C1 en_US
dc.identifier.uri http://hdl.handle.net/10453/17983
dc.description.abstract In this paper we report the results of our investigation of Evros Vallis, a martian late Noachian dendritic valley network centered at similar to 12 degrees E, 12 degrees S. The study area is located SSW of Schiaparelli and SE relative to Meridiani Planum. After establishment of the valley system, the region underwent extensive erosion and tectonic activity, which partly obliterated and modified Evros Vallis's original features. We used Mars Global Surveyor Mars Orbiter Laser Altimeter, Mars Odyssey Thermal Emission Imaging System, and Mars Express High Resolution Stereo Camera imagery and altimetry data to carry out observations and morphometric analysis of the system, and applied network scaling parameters to our measurements of valley widths, slopes, lengths and drainage areas. We obtained the following results: (a) Hack's law exponent n-1.02; (b) width-area scaling exponent b-0.21; and (c) slope-area scaling exponent theta=0.23. These values are different from those previously derived from analysis of the eastern extent of the valley system. We found that network scaling is not applicable to the investigation of Evros Vallis, a conclusion that may be relevant also to other martian network valleys. The concave-up 790 km-long profile of the main valley suggests that a classic equilibrium status was reached. Our findings are in agreement with models of a warmer and wetter martian climate at the end of the Noachian. en_US
dc.language en_US
dc.publisher Blackwell Publishing Ltd en_US
dc.relation.isbasedon http://dx.doi.org/10.1080/08120099.2012.622294 en_US
dc.title Wet Mars implications of revised scaling calculations for Evros Vallis en_US
dc.parent Australian Journal of Earth Sciences en_US
dc.journal.volume 59 en_US
dc.journal.number 2 Special Issue en_US
dc.publocation Carlton, Australia en_US
dc.identifier.startpage 263 en_US
dc.identifier.endpage 276 en_US
dc.cauo.name SCI.Environmental Sciences en_US
dc.conference Verified OK en_US
dc.for 040302 en_US
dc.personcode 960836 en_US
dc.personcode 0000076391 en_US
dc.percentage 100 en_US
dc.classification.name Extraterrestrial Geology en_US
dc.classification.type FOR-08 en_US
dc.edition en_US
dc.custom en_US
dc.date.activity en_US
dc.location.activity en_US
dc.description.keywords Mars; MOLA; DEM; valley networks; scaling; climate; MERIDIANI-PLANUM; CHANNEL NETWORKS; DRAINAGE SYSTEMS; MARTIAN VALLEYS; SURFACE RUNOFF; RIVER-BASINS; CRATER-LAKE; HACKS LAW; ORIGIN; PRECIPITATION en_US
dc.staffid en_US


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