DOCSLIB.ORG

Lunar and Planetary Science XXXII (2001) Sess19.Pdf

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Lunar and Planetary Science XXXII (2001) Sess19.Pdf Lunar and Planetary Science XXXII (2001) sess19.pdf Tuesday, March 13, 2001 POSTER SESSION I 7:00–9:30 p.m. UHCL Mars Channels, Lakes, and Oceans Berman D. C. Hartmann W. K. Burr D. M. Marte Vallis and the Cerberus Plains: Evidence of Young Water Flow on Mars [#1732] We examine the relationship between apparent fluvial channels and lava flows among the young lavas of the Elysium plains and Cerberus plains. A sequence of lava flows and water release appears to have occurred extending into recent geologic time. Moller S. C. Poulter K. E. Grosfils E. B. Sakimoto S. E. H. Mendelson C. V. Bleacher J. E. Morphology of the Marte Valles Channel System, Mars [#1382] The Marte Valles channel system near Orcus Patera, Mars is reassessed with MOLA topography. We find evidence of ponding, increasing cross-sectional area downstream suggesting multiple sources, and possible intertwined volcanism and water flow. Nelson D. M. Farmer J. D. Greeley R. Hydrologic History of South Elysium Basin-North Terra Cimmeria Area, Mars [#2069] Geologic mapping of the Terra Cimmeria outflow channels suggests a prolonged hydrologic history, sustained by tectonic and volcanic interactions with the ground water-crysophere system. Kereszturi Á. Analysis of the Meanders of Some Runoff Channels on Mars [#1177] Morphometrical and morphological analysis of runoff channels on Mars. Results: possible connection between the meanders’ parameters and the channel width, which may be the base of a future method for paleodischarge estimations. Rosenshein E. B. Greeley R. Arrowsmith J. R. Application of Terrestrial Geomorphic Threshold Theory to the Analysis of Small Channels on Mars [#1921] New terrestrial work on the geomorphic thresholds for channel initiation use the drainage area above a channel head vs. the slope at the channel head to delineate surface process types. This method has been used to characterize martian landscapes. Craddock R. A. Franz G. A. Cook A. C. Howard A. D. High Resolution Morphometric Studies of Martian Valley Networks in the Iapygia Region [#1833] We present detailed information on valley network morphometry in the Iapygia region based on high resolution digital elevation models produced by combining MOLA data with Viking stereophotogrammetric data. Leone G. Wilson L. Orofino V. Fonti S. Gorgonum Chaos: Are the Seepage-Runoff Features Really Recent? [#1649] We discuss the alleged runoff features in Gorgonum Chaos, Mars, which have been suggested as recent features. We conclude that they are more likely of Amazonian age. Harrison K. P. Grimm R. E. Martian Hydrothermal Systems: Relationship Between Magnetic Anomalies and Valley Networks [#1441] Hydrothermal circulation may explain the spatial correlation between concentrated magnetic anomalies and valley networks. Numerical models show that hydrothermal discharge spans a comparable range as the inferred discharge from valley networks. Lunar and Planetary Science XXXII (2001) sess19.pdf Grant J. A. Valley Evolution in Margaritifer Sinus, Mars [#1226] Valley morphometry suggests formation via localized ground-water discharge enabled by surface-fed recharge. Precipitation was largely relegated to subsurface entry by high surface-infiltration capacities. Discharge occurred at exposed aquitards. Bourke M. C. Zimbelman J. R. Finnegan D. Banerdt B. The Modification of Mars Fluvial Surfaces [#2109] The identification of fluvial deposits on Mars is impaired by modifying geological processes. An analysis of surface patterns of superimposed dunes and channels in paleoflood environments in Washington State and Australia can yield information on buried surfaces. Irwin R. P. III Howard A. D. Cratering and Fluvial Erosion in Noachian Terra Cimmeria, Mars [#1377] The disruption of catchments by impact craters, divide breaching, valley morphology, and the source of water are discussed for part of the Terra Cimmeria, Mars. Large, integrated catchments are identified that pre-date degraded Noachian craters. Cabrol N. A. Grin E. A. Wynn-Williams D. D. Prolonged Ponding Episode in C-Newton Crater in Recent Geological Times on Mars [#1255] We present the morphological evidence that supports the existence of a lake in a recent past in C-Newton crater. We assess the astrobiological potential of this environment. Carter B. L. Frey H. Sakimoto S. E. H. Roark J. Constraints on Gusev Basin Infill from the Mars Orbiter Laser Altimeter (MOLA) Topography [#2042] MOLA topography provides volume estimates for Gusev crater based on higher resolution. Revisiting work previously done by Grin and Cabrol (1997), we find a substantial increase in original sedimentation estimates. Rakonczai J. Hargitai H. Bérczi Sz. Comparisons of the Ancient Meandering Riverbeds in the Chryse Region, Mars, and on the Tisza Flooded Basin in the Carpathian Basin, Earth [#1507] Hydrogeomorphologic comparisons of meandering martian riverbeds, Chryse Region, and recent/ancient riverbeds of Tisza, Carpathian Basin imply: (1) presence of flowing water; (2) by left-over valleys a longer history of flowings on Mars. Mason D. Caddy B. Melchior R. Annexstad J. The Beaches of Lake Agassiz, an Analog for Martian Shorelines [#1397] Similarities between glacial Lake Agassiz shorelines and martian analogs are noted. Reasons for differences are suggested. Matsui T. Takamiya I. Imamura F. Tajika E. Tsunami Generation and Propagation in Possible Ancient Ocean on Mars [#1716] We study generation and propagation of impact-induced tsunami on Mars by using numerical models. We find that maximum tsunami height is more than 60 m at some coastal regions, which suggests we may find some evidence of tsunami on Mars..
Load more

Recommended publications
  • Seasonality and Surface Properties of Slope Streaks
    51st Lunar and Planetary Science Conference (2020) 2556.pdf SEASONALITY AND SURFACE PROPERTIES OF SLOPE STREAKS. K. M. Primm, R. H. Hoover, H. H. Kaplan, and D. E. Stillman, Dept. of Space Studies, Southwest Research Institute, 1050 Walnut St. #300, Boulder, CO 80302, USA ([email protected]). Background: Slope streaks are large (up to 200 m Methods: We used images from the High wide, up to a few km long), relatively low-albedo Resolution Imagining Science Experiment (HiRISE) to streaks that occur in the dustiest locations on Mars [1]. study the fading rate of slope streaks, Context Camera They are one of the few currently active and (CTX) to create Digital Terrain Models (DTMs) to widespread geologic processes on the surface of Mars. study the slope angles, and lastly the Compact Many slope streaks have persisted for >15 Mars years Reconnaissance Imaging Spectrometer (CRISM) to and others have been observed to form, but many evaluate the mineralogy of slope streaks and the fewer have been seen to completely fade/disappear surrounding terrain. (e.g., [2]). This inconsistency leads us to believe Results: Preliminary observations show that hypothesize that slope streaks might have different within one area (within a few kms), there are slope formation and fading mechanisms depending on their streaks that completely fade within 1 Mars Year and environment. some that form within that same time frame (Fig. 1). There have been several studies of slope streaks The green circles in Fig. 1B shows the newly formed that examine a combination of parameters: slope angles [1,3], mineralogy [4-6], environmental factors, slope streaks and the red circle show the areas where and seasonality [2,7,8] but none have combined all the slope streaks have completely disappeared.
    [Show full text]
  • Martian Crater Morphology
    ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter.
    [Show full text]
  • GLOBAL HISTORY of WATER and CLIMATE. M. H. Carr, U.S. Geological Survey, 345 Middlefield Road, Menlo Park CA 94025, USA ([email protected])
    Fifth International Conference on Mars 6030.pdf GLOBAL HISTORY OF WATER AND CLIMATE. M. H. Carr, U.S. Geological Survey, 345 Middlefield Road, Menlo Park CA 94025, USA ([email protected]). Introduction: Despite acquisition of superb new ages.(05803,08205, 51304). In addition, areas that altimetry and imagery by Mars Global Surveyor, most appear densely dissected in Viking images commonly aspects of the water and climate story are likely to have poorly organized drainage patterns when viewed remain controversial. The relative roles of surface at the MOC scale (04304, 08905, 09306). Through- runoff and groundwater seepage in the formation of going valleys and an ordered set of tributaries are dif- valley networks are yet to be resolved as are the cli- ficult to discern. These areas more resemble terrestrial matic conditions required for their formation. Simi- thermokarst terrains than areas where fluvial proc- larly, the fate of the floodwaters involved in formation esses dominate. A few areas do, have more typical of the outflow channels remains unresolved. While the fluvial erosion patterns. At 26S, 84W numerous MOC images provide little supporting evidence for closely spaced tributaries feed larger valleys to form a proposed shorelines around an extensive global ocean dense, well integrated valley system (07705). Such [1], the altimetry suggests the presence of a bench at examples, are however, rare. constant altitude around the lowest parts of the north- Debates about the origin of valley networks have ern plains [2]. Here I describe some of the attributes of focused mainly on (1) the role of fluvial erosion versus the channels and valleys as seen in the early MOC other processes, (2) the relative roles of groundwaer images, summarize the evidence for climate change sapping and surface runoff, and (3) the climatic con- on Mars, and discuss some processes that might have ditions required for valley formation.
    [Show full text]
  • THE CURIOUS SHORELINES of GORGONUM CHAOS. A. D. Howard1 and J
    Sixth International Conference on Mars (2003) 3190.pdf THE CURIOUS SHORELINES OF GORGONUM CHAOS. A. D. Howard1 and J. M. Moore2, 1Department of Environmental Sciences, University of Virginia, Charlottesville, VA 22904 ([email protected]), 2NASA Ames Re- search Center, MS 245-3, Moffett Field, CA 94035 ([email protected]). Introduction: Level, bench-like platforms in the The center of the concave basin is partially occu- interior of the Gorgonum Chaos basin appear to be pied by the knobby “chaos”. These are generally flat- shorelines associated with an ancient lake. These topped mesas that appear at one time to have been a shorelines, however, seem to lack the typical features continuous deposit that has been dissected into isolated of shorelines associated with wave and current trans- mesas along linear trends. We have interpreted such port and erosion, such as crescentic embayments, spits, deposits in this and other basins in the region to be barrier islands, and wave-cut cliffs. Rather, the lake- lake-related deposits, possibly evaporates that have facing platform edges are commonly rounded and cu- been partially dissolved [5]. These deposits were em- mulate in planform, often evenly encircling presumed placed and eroded prior to the features discussed here. islands. We interpret these shorelines to have been Shoreline Features: The center of Gorgonum ba- formed by outward growth in a quiescent environment, sin is relatively free of chaos knobs (Fig. 1) and is a possibly in ice-covered bodies of water and possibly, in relatively level plain at an elevation of about -350 to - part, as chemical precipitates.
    [Show full text]
  • Explosive Lava‐Water Interactions in Elysium Planitia, Mars: Geologic and Thermodynamic Constraints on the Formation of the Tartarus Colles Cone Groups Christopher W
    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115, E09006, doi:10.1029/2009JE003546, 2010 Explosive lava‐water interactions in Elysium Planitia, Mars: Geologic and thermodynamic constraints on the formation of the Tartarus Colles cone groups Christopher W. Hamilton,1 Sarah A. Fagents,1 and Lionel Wilson2 Received 16 November 2009; revised 11 May 2010; accepted 3 June 2010; published 16 September 2010. [1] Volcanic rootless constructs (VRCs) are the products of explosive lava‐water interactions. VRCs are significant because they imply the presence of active lava and an underlying aqueous phase (e.g., groundwater or ice) at the time of their formation. Combined mapping of VRC locations, age‐dating of their host lava surfaces, and thermodynamic modeling of lava‐substrate interactions can therefore constrain where and when water has been present in volcanic regions. This information is valuable for identifying fossil hydrothermal systems and determining relationships between climate, near‐surface water abundance, and the potential development of habitable niches on Mars. We examined the western Tartarus Colles region (25–27°N, 170–171°E) in northeastern Elysium Planitia, Mars, and identified 167 VRC groups with a total area of ∼2000 km2. These VRCs preferentially occur where lava is ∼60 m thick. Crater size‐frequency relationships suggest the VRCs formed during the late to middle Amazonian. Modeling results suggest that at the time of VRC formation, near‐surface substrate was partially desiccated, but that the depth to the midlatitude ice table was ]42 m. This ground ice stability zone is consistent with climate models that predict intermediate obliquity (∼35°) between 75 and 250 Ma, with obliquity excursions descending to ∼25–32°.
    [Show full text]
  • Crater Ice Deposits Near the South Pole of Mars Owen William Westbrook
    Crater Ice Deposits Near the South Pole of Mars by Owen William Westbrook Submitted to the Department of Earth, Atmospheric, and Planetary Sciences in partial fulfillment of the requirements for the degree of Master of Science in Earth and Planetary Sciences at the MASSACHUSETTS INSTITUTE OF TECHNOLOGY June 2009 © Massachusetts Institute of Technology 2009. All rights reserved. A uth or ........................................ Department of Earth, Atmospheric, and Planetary Sciences May 22, 2009 Certified by . Maria T. Zuber E. A. Griswold Professor of Geophysics Thesis Supervisor 6- Accepted by.... ...... ..... ........................................... Daniel Rothman Professor of Geophysics Department of Earth, Atmospheric and Planetary Sciences MASSACHUSETTS INSTWITE OF TECHNOLOGY JUL 2 0 2009 ARCHIES LIBRARIES Crater Ice Deposits Near the South Pole of Mars by Owen William Westbrook Submitted to the Department of Earth, Atmospheric, and Planetary Sciences on May 22, 2009, in partial fulfillment of the requirements for the degree of Master of Science in Earth and Planetary Sciences Abstract Layered deposits atop both Martian poles are thought to preserve a record of past climatic conditions in up to three km of water ice and dust. Just beyond the extent of these south polar layered deposits (SPLD), dozens of impact craters contain large mounds of fill material with distinct similarities to the main layered deposits. Previously identified as outliers of the main SPLD, these deposits could offer clues to the climatic history of the Martian south polar region. We extend previous studies of these features by cataloging all crater deposits found near the south pole and quantifying the physical parameters of both the deposits and their host craters.
    [Show full text]
  • Appendix I Lunar and Martian Nomenclature
    APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei
    [Show full text]
  • In Pdf Format
    lós 1877 Mik 88 ge N 18 e N i h 80° 80° 80° ll T 80° re ly a o ndae ma p k Pl m os U has ia n anum Boreu bal e C h o A al m re u c K e o re S O a B Bo l y m p i a U n d Planum Es co e ria a l H y n d s p e U 60° e 60° 60° r b o r e a e 60° l l o C MARS · Korolev a i PHOTOMAP d n a c S Lomono a sov i T a t n M 1:320 000 000 i t V s a Per V s n a s l i l epe a s l i t i t a s B o r e a R u 1 cm = 320 km lkin t i t a s B o r e a a A a A l v s l i F e c b a P u o ss i North a s North s Fo d V s a a F s i e i c a a t ssa l vi o l eo Fo i p l ko R e e r e a o an u s a p t il b s em Stokes M ic s T M T P l Kunowski U 40° on a a 40° 40° a n T 40° e n i O Va a t i a LY VI 19 ll ic KI 76 es a As N M curi N G– ra ras- s Planum Acidalia Colles ier 2 + te .
    [Show full text]
  • Geologic History of Water on Mars
    GEOLOGIC HISTORY OF WATER ON MARS: REGIONAL EVOLUTION OF AQUEOUS AND GLACIAL PROCESSES IN THE SOUTHERN HIGHLANDS, THROUGH TIME Dissertation zur Erlangung des akademischen Grades eines Doktors der Naturwissenschaften (Dr. rer. nat) vorgelegt als kumulative Arbeit am Fachbereich Geowissenschaften der Freien Universität Berlin von SOLMAZ ADELI Berlin, 2016 Erstgutachter: Prof. Dr. Ralf Jaumann Freie Universität Berlin Institut für Geologische Wissenschaften Arbeitsbereich Planetologie sowie Deutsches Zentrum für Luft- und Raumfahrt Institut für Planetenforschung, Abteilung Planetengeologie Zweitgutachter: Prof. Dr. Michael Schneider Freie Universität Berlin Institut für Geologische Wissenschaften Arbeitsbereich Hydrogeologie Tag der Disputation: 22 July 2016 i To my mother and my grandmother, the two strong women who inspired me the most, to follow my dreams, and to never give up. تقديم به مادر و مادر بزرگم به دو زن قوى كه الهام دهنده ى من بودند تا آرزو هايم را دنبال كنم و هرگز تسليم نشوم ii iii EIDESSTATTLICHE ERKLAERUNG Hiermit versichere ich, die vorliegende Arbeit selbstständig angefertigt und keine anderen als die angeführten Quellen und Hilfsmittel benutzt zu haben. Solmaz Adeli Berlin, 2016 iv v Acknowledgement First of all, I would like to thank my supervisor Prof. Dr. Ralf Jaumann for giving me the opportunity of working at the Deutsches Zentrum für Luft- und Raumfahrt (DLR). I wish to thank him particularly for standing behind me in all the ups and downs. Herr Jaumann, I am so deeply grateful for your support and your trust. Danke schön! This work would have not been achieved without the support of Ernst Hauber, my second supervisor. I have also been most fortunate to be able to work with him, and I have greatly appreciated the countless hours of discussions, all his advice regarding scientific issues, his feedbacks on my manuscripts, and everything.
    [Show full text]
  • Summary of Sexual Abuse Claims in Chapter 11 Cases of Boy Scouts of America
    Summary of Sexual Abuse Claims in Chapter 11 Cases of Boy Scouts of America There are approximately 101,135sexual abuse claims filed. Of those claims, the Tort Claimants’ Committee estimates that there are approximately 83,807 unique claims if the amended and superseded and multiple claims filed on account of the same survivor are removed. The summary of sexual abuse claims below uses the set of 83,807 of claim for purposes of claims summary below.1 The Tort Claimants’ Committee has broken down the sexual abuse claims in various categories for the purpose of disclosing where and when the sexual abuse claims arose and the identity of certain of the parties that are implicated in the alleged sexual abuse. Attached hereto as Exhibit 1 is a chart that shows the sexual abuse claims broken down by the year in which they first arose. Please note that there approximately 10,500 claims did not provide a date for when the sexual abuse occurred. As a result, those claims have not been assigned a year in which the abuse first arose. Attached hereto as Exhibit 2 is a chart that shows the claims broken down by the state or jurisdiction in which they arose. Please note there are approximately 7,186 claims that did not provide a location of abuse. Those claims are reflected by YY or ZZ in the codes used to identify the applicable state or jurisdiction. Those claims have not been assigned a state or other jurisdiction. Attached hereto as Exhibit 3 is a chart that shows the claims broken down by the Local Council implicated in the sexual abuse.
    [Show full text]
  • Water-Related Processes and Associated Landforms in Eastern Atlantis and Northern Gorgonum Basins, Mars R
    Geophysical Research Abstracts, Vol. 8, 01160, 2006 SRef-ID: 1607-7962/gra/EGU06-A-01160 © European Geosciences Union 2006 Water-related processes and associated landforms in Eastern Atlantis and Northern Gorgonum Basins, Mars R. D. Capitan (1,2) 1. Department of Geography, University of Western Ontario, London, Canada N6A 5C2, [email protected] , fax. 1-519-661 3750 2. Department of Geography and Geology, “Al. I. Cuza” University, Iasi, Romania, Blvd. Carol I, nr. 11 Martian water-related landforms developed in Atlantis and Gorgonum areas are re- lated to volcanic processes in the Tharsis area via long radial fracture zones. This is the only mechanism which could bring into the Martian system sufficient amounts of water and energy to create water-related processes at the surface. The uplift of the Tharsis area formed deep crustal fractures in the Martian megaregolith such as those located inside Gorgonum and Atlantis Chaos (e.g. Sirenum Fossae) [1]. We describe here the mechanism which made possible the formation of three distinct water-related landforms, by different processes, and relate them to the regional context of north- ern Gorgonum basin. Tectonic movements played an important role in defining the base-level for different fluvial basins, and the general dynamics of aqueous reservoirs inside the regolith. At the first site, water accumulated beneath the Magelhaens crater rim has been released catastrophically inside the crater, forming a fan-delta in a pre- existing crater lake. Later, due to tectonic movements, the outer rim collapsed toward the Atlantis Chaos, enabling the formation of fault-related stream channels. In north- ern Gorgonum Chaos the formation of outflow channels in the southern MEM-Vy crater first formed alluvial fans and a delta inside an unnamed pair of craters located at 169.94˚W, 34.35˚S, and then filled and partially eroded them, as a second outflow channel broke the neighbour’s crater rim.
    [Show full text]
  • RECONSTRUCTING the BURIED FLOOR of ATHABASCA VALLES: INCREASED CHANNEL DEPTH ESTIMATES from RADAR STUDIES. G. A. Morgan1, B. A. Campbell1, L, Carter2, J
    Lunar and Planetary Science XLVIII (2017) 2563.pdf RECONSTRUCTING THE BURIED FLOOR OF ATHABASCA VALLES: INCREASED CHANNEL DEPTH ESTIMATES FROM RADAR STUDIES. G. A. Morgan1, B. A. Campbell1, L, Carter2, J. Holt3, J. Plaut4 and A. Jasper5, 1Center for Earth and Planetary Studies, Smithsonian Institution, MRC 315, PO Box 37012, Wash- ington DC 20013, [email protected]. 2University of Arizona, 3University of Texas. 4Jet Propulsion Laboratory 5. Pennsylvania State University. Introduction: The ability of the SHARAD sounder and debouch ~280 km to the southwest within the Cer- to delineate subsurface structural features has proved berus Palus basin (Fig. 1). Though several smaller dis- pertinent in revealing the morphologic properties of tributary channels also feed off the main channel to- buried Amazonian outflow channels [1]. Morgan et al wards the southeast. Athabasca Valles contains many of [1] investigation of the >1000 km long Marte Vallis the morphological assemblages suggestive of the action outflow channel demonstrated that SHARAD data of liquid water - such as tear drop shaped islands - that could be used to reconstruct complex channel features are present within the larger, Hesperian outflow chan- that have been embayed by lava flows. The study also nels surrounding Chryse Planitia. Consequently, the provided refined depth estimates of the channel floors. predominant interpretation is that Athabasca Valles was Marte Vallis is not the only Amazonian aged outflow formed through fluvial erosion [2,4-5]. The abrupt channel on Mars. The Elysium Planitia region contains opening of the channels directly to the south of Cerber- multiple channel systems, including the >300 km long us Fossae argues the floods were sourced from a Athabasca Valles system, which represents the young- groundwater reservoir and released to the surface as a est outflow channel on Mars [2-3].
    [Show full text]