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PDF Files Are Openly Distributed for the Educational Purpose Only. Reuse And/Or Modifications of Figures and Tables in the PDF Files Are Not Allowed
PDF files are openly distributed for the educational purpose only. Reuse and/or modifications of figures and tables in the PDF files are not allowed. 3. Ancient landforms: Understanding the early Mars environment 3.1 Erosional landforms 3.1.1 Outflow channels 3.1.2 Valley networks 3.1.3 Erosional processes on early Mars 3.2 Standing bodies of water 3.2.1 Ocean and shorelines 3.2.2 Crater lakes and deltas 3.2.3 Layered deposits 3.3 Composition of sediments: from geomorphology to geology 3.3.1 MER rover discoveries 3.3.2 Exobiological issues 3.1.1 Outflow channels Length: 100 to 1000 km Width: 1 to 30 km Low gradient (<0.1) Anastomosing patterns, braided systems Teardrop-shaped islands Discharge rate :107 –109 m3 s-1 (Baker, 1981; Komar, 1986) 20 km Mangala valles 500 m Ares Valles Terrestrial floods: high discharge (here due to a storm) The Channeled Scabland analogy (Baker and Milton, 1974) ------- 40 km Columbia Basin (eastern Washington, USA) A glacial dam releases the subglacial lake Discharges of 2 x107 m3 s-1 Geographic distribution: Correlation with volcanic regions Role of geothermal activity Outflow channels (red) and valley networks (yellow) Elysium Mons Tharsis bulge From Carr, 1979 Relationship between chaotic terrains and outflow channels Chryse Planitia Kasei dfg Valles +Viking 1 + Pathfinder Ares Vallis Disruption of the permafrost at the source? Valles Marineris MOLA data Altitude (m) A recent outflow channel: Athabasca Vallis Outflow from fractures Very young: ~10 million years ago (Burr et al, 2002) (Berman and Hartmann, 2003) 6 km Origin of outflow channels 1 -Ground water under pressure confined within the permafrost (M. -
Drainage Network Development in the Keanakāko'i
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 117, E08009, doi:10.1029/2012JE004074, 2012 Drainage network development in the Keanakāko‘i tephra, Kīlauea Volcano, Hawai‘i: Implications for fluvial erosion and valley network formation on early Mars Robert A. Craddock,1 Alan D. Howard,2 Rossman P. Irwin III,1 Stephen Tooth,3 Rebecca M. E. Williams,4 and Pao-Shin Chu5 Received 1 March 2012; revised 11 June 2012; accepted 4 July 2012; published 22 August 2012. [1] A number of studies have attempted to characterize Martian valley and channel networks. To date, however, little attention has been paid to the role of lithology, which could influence the rate of incision, morphology, and hydrology as well as the characteristics of transported materials. Here, we present an analysis of the physical and hydrologic characteristics of drainage networks (gullies and channels) that have incised the Keanakāko‘i tephra, a basaltic pyroclastic deposit that occurs mainly in the summit area of Kīlauea Volcano and in the adjoining Ka‘ū Desert, Hawai‘i. The Keanakāko‘i tephra is up to 10 m meters thick and largely devoid of vegetation, making it a good analog for the Martian surface. Although the scales are different, the Keanakāko‘i drainage networks suggest that several typical morphologic characteristics of Martian valley networks may be controlled by lithology in combination with ephemeral flood characteristics. Many gully headwalls and knickpoints within the drainage networks are amphitheater shaped, which results from strong-over-weak stratigraphy. Beds of fine ash, commonly bearing accretionary lapilli (pisolites), are more resistant to erosion than the interbedded, coarser weakly consolidated and friable tephra layers. -
Volcanism on Mars
Author's personal copy Chapter 41 Volcanism on Mars James R. Zimbelman Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC, USA William Brent Garry and Jacob Elvin Bleacher Sciences and Exploration Directorate, Code 600, NASA Goddard Space Flight Center, Greenbelt, MD, USA David A. Crown Planetary Science Institute, Tucson, AZ, USA Chapter Outline 1. Introduction 717 7. Volcanic Plains 724 2. Background 718 8. Medusae Fossae Formation 725 3. Large Central Volcanoes 720 9. Compositional Constraints 726 4. Paterae and Tholi 721 10. Volcanic History of Mars 727 5. Hellas Highland Volcanoes 722 11. Future Studies 728 6. Small Constructs 723 Further Reading 728 GLOSSARY shield volcano A broad volcanic construct consisting of a multitude of individual lava flows. Flank slopes are typically w5, or less AMAZONIAN The youngest geologic time period on Mars identi- than half as steep as the flanks on a typical composite volcano. fied through geologic mapping of superposition relations and the SNC meteorites A group of igneous meteorites that originated on areal density of impact craters. Mars, as indicated by a relatively young age for most of these caldera An irregular collapse feature formed over the evacuated meteorites, but most importantly because gases trapped within magma chamber within a volcano, which includes the potential glassy parts of the meteorite are identical to the atmosphere of for a significant role for explosive volcanism. Mars. The abbreviation is derived from the names of the three central volcano Edifice created by the emplacement of volcanic meteorites that define major subdivisions identified within the materials from a centralized source vent rather than from along a group: S, Shergotty; N, Nakhla; C, Chassigny. -
Durangoko Azoka & Durango Da Azoka
egitaraua Durangoko azoka & Durango da azoka Durango uriaren hegaletik Mañarierreka bideratzen da Kantauri itsasoaren bila. Erreka-bazterrean, urtero, 1965az geroztik, gizaki-tantekin osatutako Durangoko azoka izeneko ur-putzua sortzen izan da. Baina… nahiz eta urtero ur berria izan putzuak, lau hamarkada luze igaro ondoren tanta, beste tanta batzuekin bilduz, putzu izateari utzi eta erreka izatearen beharra ikusi zuten. Putzua Kulturerreka bihurtzea. Errekaondoko bidezidorrean zehar, abenduko euri zaparradako tangadak bilduz, euskal kulturaren uholdea sortu eta bideratu. Landakotik Larizdorre kalera kokatzen diren azoka, saguganbara, ahotsenea, irudienea, szenatokia eta beste izen batzuetako ur-putzuak lotuz Errekaondoko kultur bidezidorra burutu. Tabirako Uriberri guztira AZOKA zabalduz. Durangoko azoka & Durango da azoka. Aurkibidea 04 Durangoko mapa 06 Landako erakustazoka 08 Artisau Azoka 09 Abenduaren 5ean 13 Abenduaren 6an 17 Abenduaren 7an 21 Abenduaren 8an Erretentxu K. Kurutziaga Kalea Matxinestarta Kalea Ibaizabal Auzunea Pablo Pedro Astarloa Kalea Murueta Torre A. Murueta Torre Komentukalea Kalea Andra Mari Kalea 1 2 3 Antso Estegiz Zumardia Aldapa Azoka Kabi@ Areto Nagusia Arandoño Torre K. Kalebarria K. Azoka K. Goienkalea Kalea Monago K. P Parkinga Hiribidea Montevideo Artisau Azoka Kanpatorrosteta K. Artekalea Kalea Uribarri Kalea Barrenkalea K. Oiz Kalea 4 5 6 7 Lariz Torre K. Saguganbara Plateruena Ahotsenea Irudienea Zeharkalea K. Andra Mari K. Oiz Kalea Oiz Zumalakarregi K. Zumalakarregi K. 8 Szenatokia Arkotxa K. Arkotxa Turismo Ermodo Kalea Bulegoa Bus Geltokia Ezkurdi Plaza Arte eta Historia Museoa Juan Antonio Abasolo K Geltoki Zaharra Argazki Erakusketa “Noctis Labyrinthus” Josemiel Barandiaran K, Tronperri Kalea Galtzareta K. Tren Landako Hiribidea Geltokia Bruno Mauricio Zabala K. Fray Juan de Zumarraga K. 4 2013ko abenduaren 5etik 8ra Erretentxu K. -
Mars-Match-Slides.Pdf
MA RS Clouds A B Clouds A Eastern 2/3 of the U.S. Clouds Clouds on Mars are made of _____ . A. water B. carbon dioxide C. water and carbon dioxide Clouds on Mars are made of _____ . A. water B. carbon dioxide C. water and carbon dioxide Ice cap, Antarctica A B Ice cap, Antarctica Sout A h Nort B h Ice cap, Antarctica The northern ice cap on Mars consists of frozen _____ . A. water B. carbon dioxide C. water and carbon dioxide The northern ice cap on Mars consists of frozen _____ . A. water B. carbon dioxide C. water and carbon dioxide Dust storm A B Dust storm A Sahara dust storm Polar dust storm True or False? Dust storms on Mars can cover the entire planet. True! Dust storms on Mars can cover the entire planet. 2018 Dust Devil A B Dust Devil A Seen from the ground by the Opportunity rover B Dust Devil Seen from above by the Mars Reconnaissance Orbiter Barchan dunes, Mawrth Valles A B Barchan dunes, Mawrth Valles A Sahara Desert Barchan dunes, Mawrth Valles Aorounga impact crater, Chad A B Aorounga impact crater, Chad B Lowell Crater Aorounga impact crater, Chad River Delta, Jezero Crater A B River Delta, Jezero Crater B Horton River Delta, Canada River Delta, Jezero Crater What is the name of the rover that will land in Jezero crater in 2021? A. Perseverance B. Curiosity C. Spirit What is the name of the rover that will land in Jezero crater in 2021? A. Perseverance B. -
Plains Volcanism on Mars Revisited: the Topography and Morphology of Low Shields and Related Landforms
Seventh International Conference on Mars 3287.pdf PLAINS VOLCANISM ON MARS REVISITED: THE TOPOGRAPHY AND MORPHOLOGY OF LOW SHIELDS AND RELATED LANDFORMS. E. Hauber1, 1Institute of Planetary Research, German Aerospace Center (DLR), Rutherfordstr. 2, 12489 Berlin, Germany ([email protected]). Introduction: The morphometry of Martian vol- cent study [1] used MOLA topography to measure the canoes provides critical input to the investigation of morphometric properties of several large Martian vol- their tectonic setting and the rheology of their eruption canoes. However, images of the Viking Orbiter mis- products. It is also an important prerequisite for studies sion showed that there are also numerous small and of comparative planetology, e.g., the comparison be- low shield volcanoes on Mars [2-7]. Almost all of tween terrestrial and planetary surface features. A re- these low shields are located within Tharsis and Ely- sium, the major volcanic provinces on Mars. A com- prehensive description of low shields in Tempe Terra based on Viking Orbiter images is given by [5], who describes shield fields with broad, very low shields, often associated with linear fissure vents, and several steeper edifices (Fig. 1). Many of the low shields have one or more summit craters. The craters are relatively small as compared to the basal diameter, and their form may be circular or elongated along the dominant tectonic trend. Plescia [ref. 5] compared low shields in the Tempe Terra region with terrestrial volcanoes and found that they are similar in many aspects to low shields in the eastern Snake River Plains in Idaho (USA; hereafter referred to as ESRP). -
The Role of Subsurface Volatiles in the Formational History of Noctis Labyrinthus, Mars
51st Lunar and Planetary Science Conference (2020) 1997.pdf THE ROLE OF SUBSURFACE VOLATILES IN THE FORMATIONAL HISTORY OF NOCTIS LABYRINTHUS, MARS. Corbin L. Kling ([email protected])1, Paul K. Byrne1, and Karl W. Wegmann1, 1Depart- ment of Marine, Earth, and Atmospheric Sciences, North Carolina State University, Raleigh, NC, 27695. Introduction: Noctis Labyrinthus on Mars boasts Landforms of Noctis Labyrinthus: The region many interesting geomorphological signatures contains abundant normal faults, pit craters (collapse indicating a complex history (Figure 1). Situated pits with circular to elliptical/elongate shapes), and between the Tharsis Rise and Valles Marineris, Noctis rampart craters (impact craters with morphologies is understudied compared with its more famous indicating volatiles were mobilized in the ejecta) neighboring regions. Noctis Labyrinthus itself contains surrounding the deep troughs (Figure 1). The troughs abundant normal faults, pit craters, and deep troughs. contain many landforms indicating mass wasting The area was first mapped in 1977 on Mariner imagery processes and hint at the presence of ice. Landslides [1], and interpreted as akin to the East African Rift dominate trough slopes, whereas periglacial landforms system with respect to the large amount of faulting and are common along troughs floors. the orientations of those faults. The formational history The occurrence of landslides and periglacial features of Noctis Labyrinthus, however, is still debated, with in the large troughs of Noctis provide useful information explanations for its deep troughs ranging from lava tube regarding the final stages of formation, and potentially collapse [2] to groundwater release through faulting give clues to what process(es) contributed to the initial pathways and psuedokarst [3, 4]. -
Constraints on Overland Fluid Transport Through Martian Valley Networks. M
Lunar and Planetary Science XXXI 1189.pdf CONSTRAINTS ON OVERLAND FLUID TRANSPORT THROUGH MARTIAN VALLEY NETWORKS. M. C. Malin and K. S. Edgett, Malin Space Science Systems, Box 910148, San Diego, CA 92191-0148, USA. Introduction: Since their discovery in Mariner 9 networks. images [1,2], Òrunoff channelsÓ [3], or more properly, Flow Integration: Arguably the best example Òmartian valley networksÓ [4,5] have been almost uni- found on Mars of an arborescent network are the War- versally cited as the best evidence that Mars once rego Valles. Earlier Viking data, and now MGS im- maintained an environment capable of supporting the ages, raise serious questions concerning the interpreta- flow of liquid water across its surface. Unlike Òoutflow tion of these valleys as surficial drainage. First, the channels,Ó that appear to indicate brief, catastrophic valleys are not Òthrough-going,Ó but rather consist of releases of fluid from very localized sources, valley transecting, elongate, occasionally isolated depres- networks often display arborescent patterns, sinuosity sions. Second, mass movements appear to have played and occasionally meandering patterns that imply proc- a role in both extending and widening the valleys. esses of overland flow: drainage basin development Third, the valley walls are extremely subdued, reflect- and sustained surficial transport of fluid. As part of the ing either mantling or an origin by collapse. These on-going Mars Global Surveyor (MGS) Mars Orbiter attributes suggest that collapse may have played the Camera (MOC) imaging activities, many observations dominant role in formation of valley networks of valley networks have been planned and executed; the Discussion: Groundwater follows topographic gra- results of some of these observations have been previ- dients nearly as effectively as surface water. -
NOCTIS LANDING: a Proposed Landing Site/Exploration Zone For
NOCTIS LANDING: A Proposed Landing Site/Exploration Zone for Human Missions to the Surface of Mars Pascal Lee1,2,3, Shannen Acedillo1,2, Stephen Braham1, Adrian Brown2, Richard Elphic3, Terry Fong3, Brian Glass3, Christopher Hoftun1, Brage W. Johansen1, Kira Lorber1, David Mittlefehldt4, Yuta Tagaki1,2, Peter Thomas5, Mi- chael West1, Stephen West1, Michael Zolensky4. 1Mars Institute, NASA Research Park, Moffett Field, CA 94035, USA, [email protected]. 2SETI Institute, 3NASA Ames Research Center, 4NASAJohnson Space Center, 5Cornell University. Exploration Zone Name: Noctis Landing Landing Site Coordinates: 6o 29’ 38.33” S, 92o 27’ 12.34” W. The proposed Noctis Landing Landing Site/Exploration Zone (LS/EZ) is shown in Figure 1. Our preliminary study suggests that the proposed site meets all key Science and Resources (incl. Civil Engineering) requirements. The site is of significant interest, as the EZ not only offers a large number and wide range of regions of interest (ROIs) for short-term exploration, it is also located strategically at the crossroads between Tharsis and Valles Marineris, which are key for long-term exploration. Figure 1: Map of the Noctis Landing LS/EZ. The solid red circle marks the distance of 100 km radial range from the Landing Site (LS), defining the primary Exploration Zone (EZ). The dotted red circle marks 200 km radial range from the LS. Areas circled (or ellipsed) in blue are high value science targets located within the primary EZ. Areas outlined in yellow are high-value science targets located outside the EZ, but within 200 km radial range from the LS. White dotted lines represent potential paths for pressurized rover traverses. -
Gypsum, Opal, and Fluvial Channels Within a Trough of Noctis
Planetary and Space Science 87 (2013) 130–145 Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Gypsum, opal, and fluvial channels within a trough of Noctis Labyrinthus, Mars: Implications for aqueous activity during the Late Hesperian to Amazonian Catherine M. Weitz a,n, Janice L. Bishop b, John A. Grant c a Planetary Science Institute, 1700 E. Fort Lowell, Suite 106, Tucson, AZ 85719, United States b SETI Institute, 189 Bernardo Ave., Mountain View, CA 94043, United States c Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, 6th at Independence Ave. SW, Washington, DC 20560, United States article info abstract Article history: We investigate in detail the morphology, mineralogy, and stratigraphy of light-toned deposits within one Received 27 March 2013 trough of Noctis Labyrinthus, centered at À6.81N, 261.11E. CRISM spectra taken from light-toned layered Received in revised form deposits in the northern portion of the trough exhibit absorptions around 1.41, 1.92 and 2.21 μm, 3 July 2013 consistent with mixtures of opal and Al-clays that are exposed beneath younger lava flows and between Accepted 8 August 2013 high-standing mesas of chaotic terrain. In the southern portion of the trough, opal occurs as a patchy Available online 22 August 2013 surficial deposit along the southwestern lower wall. Gypsum appears to be present in the southern Keywords: portion of the trough where spectra show triplet absorptions at 1.44, 1.48, and 1.54 μm, and additional Mars absorptions at 1.20, 1.74, 1.95, 2.22, 2.27, and 2.49 μm. -
PSRD: Timeline of Martian Volcanism
PSRD: Timeline of Martian Volcanism http://www.psrd.hawaii.edu/May11/Mars_volc_timeline.html May 27, 2011 --- High-resolution images allow a larger range of crater sizes to date calderas and the last major periods of volcanic activity on Mars. Written by Linda M. V. Martel Hawai'i Institute of Geophysics and Planetology A recent study of Martian volcanism presents a timeline of the last major eruptions from 20 large volcanoes, based on the relative ages of caldera surfaces determined by crater counting. Stuart Robbins, Gaetano Di Achille, and Brian Hynek (University of Colorado) counted craters on high-resolution images from the the Context Camera (CTX) on Mars Reconnaissance Orbiter to date individual calderas, or terraces within calderas, on the 20 major Martian volcanoes. Based on their timeline and mapping, rates and durations of eruptions and transitions from explosive to effusive activity varied from volcano to volcano. The work confirms previous findings by others that volcanism was continuous throughout Click for full image data Martian geologic history until about one to two hundred million years ago, the final volcanic . events were not synchronous across the planet, and the latest large-scale caldera activity ended about 150 million years ago in the Tharsis province. This timing correlates well with the crystallization ages (~165-170 million years) determined for the youngest basaltic Martian meteorites. Reference: Robbins, S. J., Di Achille, G., and Hynek, B. M. (2011) The Volcanic History of Mars: High-Resolution Crater-Based Studies of the Calderas of 20 Volcanoes, Icarus, v. 211, p. 1179-1203, doi: 10.1016/j.icarus.2010.11.012. -
Valley Formation on Early Mars by Subglacial and Fluvial Erosion
ARTICLES https://doi.org/10.1038/s41561-020-0618-x Valley formation on early Mars by subglacial and fluvial erosion Anna Grau Galofre! !1,2 ✉ , A. Mark Jellinek1 and Gordon R. Osinski! !3,4 The southern highlands of Mars are dissected by hundreds of valley networks, which are evidence that water once sculpted the surface. Characterizing the mechanisms of valley incision may constrain early Mars climate and the search for ancient life. Previous interpretations of the geological record require precipitation and surface water runoff to form the valley networks, in contradiction with climate simulations that predict a cold, icy ancient Mars. Here we present a global comparative study of val- ley network morphometry, using a principal-component-based analysis with physical models of fluvial, groundwater sapping and glacial and subglacial erosion. We found that valley formation involved all these processes, but that subglacial and fluvial erosion are the predominant mechanisms. This is supported by predictions from models of steady-state erosion and geomor- phological comparisons to terrestrial analogues. The inference of subglacial channels among the valley networks supports the presence of ice sheets that covered the southern highlands during the time of valley network emplacement. alley networks are ancient (3.9–3.5 billion years ago (Ga)) angle between tributaries and main stem (γ), (2) streamline fractal 1–4 systems of tributaries with widely varying morphologies dimension (Df), (3) maximum network stream order (Sn), (4) width Vpredominately incised on the southern hemisphere high- of first-order tributaries (λ), (5) length-to-width aspect ratio (R) lands of Mars (Fig. 1).