Back Matter (PDF)
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Atypical Landslides in the Nilosyrtis Region of Mars Anthony Guimpier, Susan Conway, Nicolas Mangold
Atypical landslides in the Nilosyrtis region of Mars Anthony Guimpier, Susan Conway, Nicolas Mangold To cite this version: Anthony Guimpier, Susan Conway, Nicolas Mangold. Atypical landslides in the Nilosyrtis region of Mars. 14th Europlanet Science Congress, Oct 2020, held online, Unknown Region. 10.5194/epsc2020- 746. hal-03091587 HAL Id: hal-03091587 https://hal.archives-ouvertes.fr/hal-03091587 Submitted on 7 Jan 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. EPSC Abstracts Vol. 14, EPSC2020-746, 2020, updated on 07 Jan 2021 https://doi.org/10.5194/epsc2020-746 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. Atypical landslides in the Nilosyrtis region of Mars Anthony Guimpier, Susan Conway, and Nicolas Mangold Laboratoire de Planétologie et Géodynamique CNRS UMR6112, University of Nantes, France ([email protected]) Introduction:This study focuses on four unusual landslides located inside a 25 km diameter impact crater located in Nilosyrtis Mensae (Fig.1). Our initial study revealed that one of these landslides bears close similarity to a mudslide on Earth [1]. We performed a detailed morphological analysis and a comparison with terrestrial analogues to better understand their formation mechanism. -
MODELED CATASTROPHIC OUTFLOW at ARAM CHAOS CHANNEL, MARS. DA Howard, Earth & Planetary Sciences, University of Tennessee
40th Lunar and Planetary Science Conference (2009) 2179.pdf MODELED CATASTROPHIC OUTFLOW AT ARAM CHAOS CHANNEL, MARS. D. A. Howard, Earth & Planetary Sciences, University of Tennessee, 306 Earth & Planetary Sciences Bldg., 1412 Circle Drive, Knoxville, TN 37996, [email protected]. Introduction: The Aram Chaos channel located at tional algorithms relied on in this study were devel- 2.8°N, 18.5°W, is approximately 100 km long, ranges oped by Komar [1] and I have adapted them for use from 8 to 14 km wide, and has a maximum depth of with the Hydrologic Engineering Center’s River Anal- 2000 m (Figure 1). The confined innermost approx- ysis System (HEC-RAS) based on solution of the con- imately 67 km reach selected for this study includes tinuity and momentum equations [2]. HEC-RAS ad- the area of the channel where the trimline is evident justed for Mars’ gravitational acceleration was only for the stream head at the time of initial catastrophic applied to Mars channels once previously by Burr [3] flow and the outflow height at the channel’s mouth. at Athabasca Vallis and therefore provides the oppor- tunity to further develop the method here. The HEC- RAS model used for both Earth and Mars are identical except that the Mars version was adjusted for the gra- vitational acceleration and the specific weight of water differences between the two planets. Using the HEC- Ares Valles GeoRAS ArcGIS geospatial tool to generate the chan- nel geometry for input to the HEC-RAS flow model, Aram Chaos the hypothesized output potentially quantifies the hy- draulics of the channels more accurately than previous orders-of-magnitude estimates reported in the litera- ture. -
The Eastern Outlet of Valles Marineris: a Window Into the Ancient Geologic and Hydrologic Evolution of Mars
First Landing Site/Exploration Zone Workshop for Human Missions to the Surface of Mars (2015) 1054.pdf The Eastern Outlet of Valles Marineris: A Window into the Ancient Geologic and Hydrologic Evolution of Mars Stephen M. Clifford, David A. Kring, and Allan H. Treiman, Lunar and Planetary Institute/USRA, 3600 Bay Area Bvld., Houston, TX 77058 Over its 3,500 km length, Valles Marineris exhibits enormous range of geologic and environmental diversity. At its western end, the canyon is dominated by the tectonic complex of Noctis Labyrinthus while, in the east, it grades into an extensive region of chaos - where scoured channels and streamlined islands provide evidence of catastrophic floods that spilled into the northern plains [1-4]. In the central portion of the system, debris derived from the massive interior layered deposits of Candor, Ophir and Hebes Chasmas spills into the central trough have been identified as possible lucustrine sediments that may have been laid down in long-standing ice-covered lakes [3-6]. The potential survival and growth of Martian organisms in such an environment, or in the aquifers whose disruption gave birth to the chaotic terrain at the east end of the canyon, raises the possibility that fossil indicators of life may be present in the local sediment and rock. In other areas, 6 km-deep exposures of Hesperian and Noachian-age canyon wall stratigraphy have collapsed in massive landslides that extend many tens of kilometers across the canyon floor. Ejecta from interior craters, aeolian sediments, and possible volcanics (which appear to have emanated from structurally controlled vents along the base of the scarps), further contribute to the canyon's geologic complexity [2,3]. -
North Polar Region of Mars: Advances in Stratigraphy, Structure, and Erosional Modification
Icarus 196 (2008) 318–358 www.elsevier.com/locate/icarus North polar region of Mars: Advances in stratigraphy, structure, and erosional modification Kenneth L. Tanaka a,∗, J. Alexis P. Rodriguez b, James A. Skinner Jr. a,MaryC.Bourkeb, Corey M. Fortezzo a,c, Kenneth E. Herkenhoff a, Eric J. Kolb d, Chris H. Okubo e a US Geological Survey, Flagstaff, AZ 86001, USA b Planetary Science Institute, Tucson, AZ 85719, USA c Northern Arizona University, Flagstaff, AZ 86011, USA d Google, Inc., Mountain View, CA 94043, USA e Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA Received 5 June 2007; revised 24 January 2008 Available online 29 February 2008 Abstract We have remapped the geology of the north polar plateau on Mars, Planum Boreum, and the surrounding plains of Vastitas Borealis using altimetry and image data along with thematic maps resulting from observations made by the Mars Global Surveyor, Mars Odyssey, Mars Express, and Mars Reconnaissance Orbiter spacecraft. New and revised geographic and geologic terminologies assist with effectively discussing the various features of this region. We identify 7 geologic units making up Planum Boreum and at least 3 for the circumpolar plains, which collectively span the entire Amazonian Period. The Planum Boreum units resolve at least 6 distinct depositional and 5 erosional episodes. The first major stage of activity includes the Early Amazonian (∼3 to 1 Ga) deposition (and subsequent erosion) of the thick (locally exceeding 1000 m) and evenly- layered Rupes Tenuis unit (ABrt), which ultimately formed approximately half of the base of Planum Boreum. As previously suggested, this unit may be sourced by materials derived from the nearby Scandia region, and we interpret that it may correlate with the deposits that regionally underlie pedestal craters in the surrounding lowland plains. -
LAYERED SULFATE-BEARING TERRAINS on MARS: INSIGHTS from GALE CRATER and MERIDIANI PLANUM. K.E. Powell1,2, R.E. Arvidson3, and C.S
Ninth International Conference on Mars 2019 (LPI Contrib. No. 2089) 6316.pdf LAYERED SULFATE-BEARING TERRAINS ON MARS: INSIGHTS FROM GALE CRATER AND MERIDIANI PLANUM. K.E. Powell1,2, R.E. Arvidson3, and C.S. Edwards1, 1Department of Physics & Astrono- my, Northern Arizona University, 2School of Earth & Space Exploration, Arizona State University, 3Department of Earth & Planetary Sciences, Washington University in St. Louis. Introduction: Sulfate species have been detected ronment, with episodes of diagenesis and weathering in late Noachian and Hesperian terrains on Mars lying to form a crystalline hematite lag deposit [4, 5]. The stratigraphically above clay minerals, which has been lag deposit masks the CRISM spectral signature of interpreted as documenting a shift from wetter to more sulfate in most locations. Sulfate minerals including arid environments on the surface. Sulfate detections kieserite and gypsum have been detected in impact are associated with layered deposits in numerous loca- crater walls and windswept regions [6]. The Oppor- tions including Gale Crater, Meridiani Planum, Vallis tunity rover explored southern Meridiani Planum Marineris, and Terra Sirenum, and Aram Chaos [1]. through a campaign of crater-hopping, using craters as These sulfates and clays been identified using their a natural drill to expose strata [6]. The deepest expo- diagnostic absorption features in visible and near- sures explored by Opportunity directly are ~10 meters infrared reflectance (VNIR) data acquired from Mars thick at Victoria Crater. Opportunity results indicate orbit. Additionally, two rover missions have explored that the top layers of Burns formation contain up to sites with massive sulfate deposits. The first, the MER 40% sulfate and included Mg, Ca, and Fe species. -
The Geology of Aram Chaos. Timothy D
Lunar and Planetary Science XXXIV (2003) 2046.pdf The Geology of Aram Chaos. Timothy D. Glotch1, and Philip R. Christensen1, 1Department of Geological Sciences, Arizona State University, Tempe, AZ 85287-6305 Introduction. The Thermal Emission Spectrometer wavelengths, THEMIS cannot detect the presence of (TES) instrument aboard the Mars Global Surveyor hematite. Three-band, decorrelation-stretched images (MGS) spacecraft located deposits of gray, crystalline can however, provide information about any hematite in Sinus Meridiani, Aram Chaos, and Valles additional mineralogical variability that may be Marineris [1-2]. Since the initial discovery, most present in the area. work has focused on the Sinus Meridiani site, Individual MOLA tracks were used to characterize primarily because of its large size and its probable the regional sloping and tilting occurring within the choice as a landing site for one of NASA’s 2003 crater. In addition to the individual tracks, a 100- Mars Excursion Rover (MER) rovers [3-5]. meter contour map created from the 128 ppd gridded Christensen et al., [1-2] provided five testable data set was overlayed onto a THEMIS daytime hypotheses regarding the formation of crystalline mosaic to understand regional topographic trends. hematite on Mars: 1) low-temperature precipitaion of Results and Discussion. The topmost stratigraphic Fe oxides/hydroxides from standing, oxygenated, Fe- unit in Aram Chaos covers roughly 20% of the rich water, followed by subsequent alteration to gray interior of Aram Chaos. It is unique among the units hematite, 2) low-temperature leaching of iron-bearing in Aram Chaos in that it has a relatively high thermal silicates and other materials leaving a Fe-rich residue inertia (550-700 J/m2Ks1/2), indicating a layer (laterite-style weathering) which is subsequently composed of sand and pebble-sized particles [6], or altered to gray hematite, 3) direct precipitation of alternatively, smaller particles cemented together. -
Mineralogy of the Martian Surface
EA42CH14-Ehlmann ARI 30 April 2014 7:21 Mineralogy of the Martian Surface Bethany L. Ehlmann1,2 and Christopher S. Edwards1 1Division of Geological & Planetary Sciences, California Institute of Technology, Pasadena, California 91125; email: [email protected], [email protected] 2Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109 Annu. Rev. Earth Planet. Sci. 2014. 42:291–315 Keywords First published online as a Review in Advance on Mars, composition, mineralogy, infrared spectroscopy, igneous processes, February 21, 2014 aqueous alteration The Annual Review of Earth and Planetary Sciences is online at earth.annualreviews.org Abstract This article’s doi: The past fifteen years of orbital infrared spectroscopy and in situ exploration 10.1146/annurev-earth-060313-055024 have led to a new understanding of the composition and history of Mars. Copyright c 2014 by Annual Reviews. Globally, Mars has a basaltic upper crust with regionally variable quanti- by California Institute of Technology on 06/09/14. For personal use only. All rights reserved ties of plagioclase, pyroxene, and olivine associated with distinctive terrains. Enrichments in olivine (>20%) are found around the largest basins and Annu. Rev. Earth Planet. Sci. 2014.42:291-315. Downloaded from www.annualreviews.org within late Noachian–early Hesperian lavas. Alkali volcanics are also locally present, pointing to regional differences in igneous processes. Many ma- terials from ancient Mars bear the mineralogic fingerprints of interaction with water. Clay minerals, found in exposures of Noachian crust across the globe, preserve widespread evidence for early weathering, hydrothermal, and diagenetic aqueous environments. Noachian and Hesperian sediments include paleolake deposits with clays, carbonates, sulfates, and chlorides that are more localized in extent. -
Possible Recessional Moraines in the Nilosyrtis Mensae Region, Mars
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 3085.pdf POSSIBLE RECESSIONAL MORAINES IN THE NILOSYRTIS MENSAE REGION, MARS. A. Johnsson1, 2 3 1 J. Raack , E. Hauber . Department of Earth Sciences, University of Gothenburg, Gothenburg, Sweden ([email protected]), 2Institut für Planetologie, Westfälische Wilhelms-Universität, Münster, Germany. 3Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany. Introduction: Previously, numerous studies re- age is available of the studied landforms. For Earth ported on glacier landforms on Mars such as viscous comparison we used publicly available Google Earth flow features (VVF) [1], glacier-like flows (GLF) [2] images. and lobate debris aprons (LDA) [3] where water-ice is Observations and results: The area is dominated by believed to be present under insulating debris cover fretted terrain, mesas, cliffs and flat floored valleys. [1]. This notion was confirmed by SHARAD meas- The studied north-facing cliff range is ~250 km long urements [4]. In terms of possible glacial erosional and and are a few hundred to a more than a thousand me- depositional landforms most studies have focused on ters in height. The cliff is characterized by deeply in- small-scale moraine-like ridges that are associated to cised valley systems. Here we report observations from gully systems in interior crater environments [e.g., 5], two valleys. large-scale glacier landforms at the equatorial volcanic province [e.g., 6], landforms suggesting basal glacial meltwater processes [7,8] and possible drop-moraines from past CO2 glaciers [9]. In this study we surveyed an area that border areas of known VVF's and GLF's along the dichotomy. -
Glacial and Gully Erosion on Mars: a Terrestrial Perspective Susan Conway, Frances Butcher, Tjalling De Haas, Axel A.J
Glacial and gully erosion on Mars: A terrestrial perspective Susan Conway, Frances Butcher, Tjalling de Haas, Axel A.J. Deijns, Peter Grindrod, Joel Davis To cite this version: Susan Conway, Frances Butcher, Tjalling de Haas, Axel A.J. Deijns, Peter Grindrod, et al.. Glacial and gully erosion on Mars: A terrestrial perspective. Geomorphology, Elsevier, 2018, 318, pp.26-57. 10.1016/j.geomorph.2018.05.019. hal-02269410 HAL Id: hal-02269410 https://hal.archives-ouvertes.fr/hal-02269410 Submitted on 22 Aug 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. *Revised manuscript with no changes marked Click here to view linked References 1 Glacial and gully erosion on Mars: A terrestrial perspective 2 Susan J. Conway1* 3 Frances E. G. Butcher2 4 Tjalling de Haas3,4 5 Axel J. Deijns4 6 Peter M. Grindrod5 7 Joel M. Davis5 8 1. CNRS, UMR 6112 Laboratoire de Planétologie et Géodynamique, Université de Nantes, France 9 2. School of Physical Sciences, Open University, Milton Keynes, MK7 6AA, UK 10 3. Department of Geography, Durham University, South Road, Durham DH1 3LE, UK 11 4. Faculty of Geoscience, Universiteit Utrecht, Heidelberglaan 2, 3584 CS Utrecht, The Netherlands 12 5. -
Space News Update – June 2019
Space News Update – June 2019 By Pat Williams IN THIS EDITION: • Curiosity detects unusually high methane levels. • Scientists find largest meteorite impact in the British Isles. • Space station mould survives high doses of ionizing radiation. • NASA selects missions to study our Sun, its effects on space weather. • Subaru Telescope identifies the outermost edge of our Milky Way system. • Links to other space and astronomy news published in June 2019. Disclaimer - I claim no authorship for the printed material; except where noted (PW). CURIOSITY DETECTS UNUSUALLY HIGH METHANE LEVELS This image was taken by the left Navcam on NASA's Curiosity Mars rover on June 18, 2019, the 2,440th Martian day, or sol, of the mission. It shows part of "Teal Ridge," which the rover has been studying within a region called the "clay-bearing unit." Credits: NASA/JPL-Caltech Curiosity's team conducted a follow-on methane experiment. The results show that the methane levels have sharply decreased, with less than 1 part per billion by volume detected. That's a value close to the background levels Curiosity sees all the time. The finding suggest the previous week's methane detection, the largest amount of the gas Curiosity has ever found, was one of the transient methane plumes that have been observed in the past. While scientists have observed the background levels rise and fall seasonally, they haven't found a pattern in the occurrence of these transient plumes. The methane mystery continues. Curiosity doesn't have instruments that can definitively say whether the source of the methane is biological or geological. -
Cambridge University Press 978-1-107-03629-1 — the Atlas of Mars Kenneth S
Cambridge University Press 978-1-107-03629-1 — The Atlas of Mars Kenneth S. Coles, Kenneth L. Tanaka, Philip R. Christensen Index More Information Index Note: page numbers in italic indicates figures or tables Acheron Fossae 76, 76–77 cuesta 167, 169 Hadriacus Cavi 183 orbit 1 Acidalia Mensa 86, 87 Curiosity 9, 32, 62, 195 Hadriacus Palus 183, 184–185 surface gravity 1, 13 aeolian, See wind; dunes Cyane Catena 82 Hecates Tholus 102, 103 Mars 3 spacecraft 6, 201–202 Aeolis Dorsa 197 Hellas 30, 30, 53 Mars Atmosphere and Volatile Evolution (MAVEN) 9 Aeolis Mons, See Mount Sharp Dao Vallis 227 Hellas Montes 225 Mars Chart 1 Alba Mons 80, 81 datum (zero elevation) 2 Hellas Planitia 220, 220, 226, 227 Mars Exploration Rovers (MER), See Spirit, Opportunity albedo 4, 5,6,10, 56, 139 deformation 220, See also contraction, extension, faults, hematite 61, 130, 173 Mars Express 9 alluvial deposits 62, 195, 197, See also fluvial deposits grabens spherules 61,61 Mars Global Surveyor (MGS) 9 Amazonian Period, history of 50–51, 59 Deimos 62, 246, 246 Henry crater 135, 135 Mars Odyssey (MO) 9 Amenthes Planum 143, 143 deltas 174, 175, 195 Herschel crater 188, 189 Mars Orbiter Mission (MOM) 9 Apollinaris Mons 195, 195 dikes, igneous 82, 105, 155 Hesperia Planum 188–189 Mars Pathfinder 9, 31, 36, 60,60 Aram Chaos 130, 131 domical mound 135, 182, 195 Hesperian Period, history of 50, 188 Mars Reconnaissance Orbiter (MRO) 9 Ares Vallis 129, 130 Dorsa Argentea 239, 240 Huygens crater 183, 185 massif 182, 224 Argyre Planitia 213 dunes 56, 57,69–70, 71, 168, 185, -
Extensive Aqueous Deposits at the Base of the Dichotomy Boundary in Nilosyrtis Mensae, Mars
Extensive aqueous deposits at the base of the dichotomy boundary in Nilosyrtis Mensae, Mars Joshua L. Bandfield1 and Elena S. Amador2 1Space Science Institute 2Earth and Space Sciences, University of Washington, Seattle Manuscript Correspondence: 5 Joshua Bandfield Space Science Institute 4750 Walnut Street, Suite 205 Boulder, CO 80301, USA [email protected] 10 Manuscript Pages: 32 Figures: 13 Keywords: Mars, surface; Infrared observations; Spectroscopy; Mineralogy; Geological processes 1 Abstract Thermal Emission Imaging System (THEMIS) and Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) spectral datasets were used to identify high bulk SiO2 and hydrated 15 compositions throughout the Nilosyrtis Mensae region. Four isolated locations were identified across the region showing short wavelength silicate absorptions within the 8–12 μm spectral region, indicating surfaces dominated by high Si phases. Much more extensive exposures of hydrated compositions are present throughout the region, indicated by a spectral absorption near 1.9 μm in CRISM data. Although limited in spatial coverage, detailed spectral observations indicate that the hydrated materials contain 20 Fe/Mg-smectites and hydrated silica along with minor exposures of Mg-carbonates and an unidentified hydrated phase. The high SiO2 and hydrated materials are present in layered sediments near the base of topographic scarps at the hemispheric dichotomy boundary, typically near or within low albedo sand deposits. The source of the high SiO2 and hydrated materials appears to be from groundwater discharge from Nili Fossae and Syrtis Major to the south, where there is evidence for extensive aqueous alteration 25 of the subsurface. Although discontinuous, the exposures of high SiO2 and hydrated materials span a wide area and are present in a similar geomorphological context to previously identified deposits in western Hellas Basin.