Back Matter (PDF)
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Characteristics of the Bergschrund of an Avalanche-Cone Glacier in the Canadian Rocky Mountains
JOlIl"lla/ o/G/aci%gl'. VoL 29. No. 10 1. 1983 CHARACTERISTICS OF THE BERGSCHRUND OF AN AVALANCHE-CONE GLACIER IN THE CANADIAN ROCKY MOUNTAINS By G ERALD OSBORN (Department of Geology and Geophysics, Uni versity o f Calgary, Calgary, Alberta T2N I N4, Canada) ABSTRACT. Fi eld study of th e bergschrund of a small avalanche-cone glacier at the base of Mt Chephren, in Banff Nati onal Park , has been ca rried out as part of a general ex pl oratory study of glacier-head crevasses in th e Canadi an Roc ki es. The bergsc hrun d consists of a wide. shall ow. partl y bedrock-fl oored gap, und erneath whi ch ex tends a nearl y vertical Ralldklu!I, and a small , offset, subsidi ary crevasse (or crevasses). The fo ll owin g observations rega rdin g the behavior of th e bergsc hruncl and ice adjacent to it are of parti cul ar interest: ( I) topograph y of the subglaeial bedrock is a control on the location of the main bergschrund and subsidi a ry crevasses. (2) th e main bergschrund and subsid ia ry crevasse(s) are conn ected by subglacial gaps betwee n bedrock and ice; th e gaps are part of th e "bergschrund system" , (3) snow/ ice immedi ately down-glacier of the bergschrund system moves nea rl y verticall y dow nwa rd in response to rotational fl ow of the glacier. a ll owin g the bergschrund components to keep the same location and size fro m year to year, (4) an inde pend ent accumul ati on, fl ow. -
MARS an Overview of the 1985–2006 Mars Orbiter Camera Science
MARS MARS INFORMATICS The International Journal of Mars Science and Exploration Open Access Journals Science An overview of the 1985–2006 Mars Orbiter Camera science investigation Michael C. Malin1, Kenneth S. Edgett1, Bruce A. Cantor1, Michael A. Caplinger1, G. Edward Danielson2, Elsa H. Jensen1, Michael A. Ravine1, Jennifer L. Sandoval1, and Kimberley D. Supulver1 1Malin Space Science Systems, P.O. Box 910148, San Diego, CA, 92191-0148, USA; 2Deceased, 10 December 2005 Citation: Mars 5, 1-60, 2010; doi:10.1555/mars.2010.0001 History: Submitted: August 5, 2009; Reviewed: October 18, 2009; Accepted: November 15, 2009; Published: January 6, 2010 Editor: Jeffrey B. Plescia, Applied Physics Laboratory, Johns Hopkins University Reviewers: Jeffrey B. Plescia, Applied Physics Laboratory, Johns Hopkins University; R. Aileen Yingst, University of Wisconsin Green Bay Open Access: Copyright 2010 Malin Space Science Systems. This is an open-access paper distributed under the terms of a Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Abstract Background: NASA selected the Mars Orbiter Camera (MOC) investigation in 1986 for the Mars Observer mission. The MOC consisted of three elements which shared a common package: a narrow angle camera designed to obtain images with a spatial resolution as high as 1.4 m per pixel from orbit, and two wide angle cameras (one with a red filter, the other blue) for daily global imaging to observe meteorological events, geodesy, and provide context for the narrow angle images. Following the loss of Mars Observer in August 1993, a second MOC was built from flight spare hardware and launched aboard Mars Global Surveyor (MGS) in November 1996. -
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]. -
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. -
DATING the RESURFACING EVENTS of the HARMAKHIS VALLIS SOURCE REGIONS, MARS: PRELIMINARY RESULTS. S. Kukkonen and V.-P
44th Lunar and Planetary Science Conference (2013) 2140.pdf DATING THE RESURFACING EVENTS OF THE HARMAKHIS VALLIS SOURCE REGIONS, MARS: PRELIMINARY RESULTS. S. Kukkonen and V.-P. Kostama, Astronomy, Department of Physics, P.O. Box 3000, FI-90014 University of Oulu, Finland ([email protected]). Introduction: Harmakhis Vallis is one of the four [e.g., 15–17]. Usually they have been excluded from major outflow channel systems that cut the eastern Hel- the crater counts because of the uncertainty of their las rim region of Mars (Fig. 1). It is ~800 km long and origin (primary vs. secondary crater). However, small located ~450 km south of Hadriaca Patera starting craters accumulate to the surface more quickly than close to the end of another valley, Reull Vallis. Due to larger ones, and thus the high spatial resolution is nec- the close position to the volcanic features, the channels essary in dating younger surfaces or small units where are suggested to have been formed by the mobilization there are only few large craters. In the case of Harma- and release of subsurface volatiles by volcanic heat [1– khis Vallis, the region has experienced significant re- 5]. Because Harmakhis Vallis cuts the surrounding cent modification and degradation, and thus, we can massifs of the cratered terrains, it is clearly one of the assume that the small crater population mostly post- youngest features in the region [6, 7]. dates the secondary craters forming larger impacts lo- cated in the older regions. Therefore, only the obvious clusters of secondary craters were excluded from the counts. -
Antarctic Primer
Antarctic Primer By Nigel Sitwell, Tom Ritchie & Gary Miller By Nigel Sitwell, Tom Ritchie & Gary Miller Designed by: Olivia Young, Aurora Expeditions October 2018 Cover image © I.Tortosa Morgan Suite 12, Level 2 35 Buckingham Street Surry Hills, Sydney NSW 2010, Australia To anyone who goes to the Antarctic, there is a tremendous appeal, an unparalleled combination of grandeur, beauty, vastness, loneliness, and malevolence —all of which sound terribly melodramatic — but which truly convey the actual feeling of Antarctica. Where else in the world are all of these descriptions really true? —Captain T.L.M. Sunter, ‘The Antarctic Century Newsletter ANTARCTIC PRIMER 2018 | 3 CONTENTS I. CONSERVING ANTARCTICA Guidance for Visitors to the Antarctic Antarctica’s Historic Heritage South Georgia Biosecurity II. THE PHYSICAL ENVIRONMENT Antarctica The Southern Ocean The Continent Climate Atmospheric Phenomena The Ozone Hole Climate Change Sea Ice The Antarctic Ice Cap Icebergs A Short Glossary of Ice Terms III. THE BIOLOGICAL ENVIRONMENT Life in Antarctica Adapting to the Cold The Kingdom of Krill IV. THE WILDLIFE Antarctic Squids Antarctic Fishes Antarctic Birds Antarctic Seals Antarctic Whales 4 AURORA EXPEDITIONS | Pioneering expedition travel to the heart of nature. CONTENTS V. EXPLORERS AND SCIENTISTS The Exploration of Antarctica The Antarctic Treaty VI. PLACES YOU MAY VISIT South Shetland Islands Antarctic Peninsula Weddell Sea South Orkney Islands South Georgia The Falkland Islands South Sandwich Islands The Historic Ross Sea Sector Commonwealth Bay VII. FURTHER READING VIII. WILDLIFE CHECKLISTS ANTARCTIC PRIMER 2018 | 5 Adélie penguins in the Antarctic Peninsula I. CONSERVING ANTARCTICA Antarctica is the largest wilderness area on earth, a place that must be preserved in its present, virtually pristine state. -
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. -
Hesiod Theogony.Pdf
Hesiod (8th or 7th c. BC, composed in Greek) The Homeric epics, the Iliad and the Odyssey, are probably slightly earlier than Hesiod’s two surviving poems, the Works and Days and the Theogony. Yet in many ways Hesiod is the more important author for the study of Greek mythology. While Homer treats cer- tain aspects of the saga of the Trojan War, he makes no attempt at treating myth more generally. He often includes short digressions and tantalizes us with hints of a broader tra- dition, but much of this remains obscure. Hesiod, by contrast, sought in his Theogony to give a connected account of the creation of the universe. For the study of myth he is im- portant precisely because his is the oldest surviving attempt to treat systematically the mythical tradition from the first gods down to the great heroes. Also unlike the legendary Homer, Hesiod is for us an historical figure and a real per- sonality. His Works and Days contains a great deal of autobiographical information, in- cluding his birthplace (Ascra in Boiotia), where his father had come from (Cyme in Asia Minor), and the name of his brother (Perses), with whom he had a dispute that was the inspiration for composing the Works and Days. His exact date cannot be determined with precision, but there is general agreement that he lived in the 8th century or perhaps the early 7th century BC. His life, therefore, was approximately contemporaneous with the beginning of alphabetic writing in the Greek world. Although we do not know whether Hesiod himself employed this new invention in composing his poems, we can be certain that it was soon used to record and pass them on. -
3D Geosense Hydrostatic Level Measurement IKAS Evolution
IKAS evolution Configuration options 3D GeoSense MiniLite with extra counter and NANO L 3D Hydrostatic IKAS evolution level 3D GeoSense, pipe routing data ORION 3 SD L 3D with PHOBOS 3D measurement Special software tools are used to support the processing of the data cap- 3D GeoSense flushing: 3D GeoSense without flushing: tured by the camera. IKAS evolution is capable of capturing the 3D sensor's measurement data Large-scale system: Large-scale system: (xyz coordinates) in a fully automated process. This is done simultaneous- Cameras1): ORION 3 SD (L) 3D, ORION 3 (L) 3D, NANO (L) 3D ORION 3 SD (L) 3D, ORION 3 (L) 3D, NANO (L) 3D ly with the TV inspection. POLARIS 3D POLARIS 3D, ORPHEUS 2 3D2), ORPHEUS 3 3D2) Satellite-based inspection system: LISY 3 or LISY HD ORPHEUS 2 HD 3D2), ARGUS 62) IKAS evolution also allows displaying the measured course of the piping with control camera LISYCam 3, LISYCam 200, 3D funnel Satellite-based inspection system: LISY 3 or LISY HD in real time while conducting a TV survey in a network diagram*. It is pos- with control camera LISYCam 3, LISYCam 200, 3D funnel sible to import maps (such as a house's floor plan) to the software and Flushing nozzle: PHOBOS 3D Camera guide unit DEIMOS 3D to scale it to the required size to display the course of the piping which is Operating system: BS7, BS5, BS 3.5 generated in the process directly on the map. The pipe run is stored with Cable winch: KW 305 / KW 505 with camera cable Operating system: BS7, BS5, BS 3.5 three-dimensional coordinates and precise geographical information (geo- Synchronous winch: LISY synchronous winch (with camera cable KW 305 / KW 505 with camera cable referencing) to allow tracing the exact physical location of the course of instead of push rod) Synchronous winch: LISY synchronous winch with camera cable the pipes from above the ground at any time. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Dikes of Distinct Composition Intruded Into Noachian-Aged Crust Exposed in the Walls of Valles Marineris Jessica Flahaut, John F
Dikes of distinct composition intruded into Noachian-aged crust exposed in the walls of Valles Marineris Jessica Flahaut, John F. Mustard, Cathy Quantin, Harold Clenet, Pascal Allemand, Pierre Thomas To cite this version: Jessica Flahaut, John F. Mustard, Cathy Quantin, Harold Clenet, Pascal Allemand, et al.. Dikes of dis- tinct composition intruded into Noachian-aged crust exposed in the walls of Valles Marineris. Geophys- ical Research Letters, American Geophysical Union, 2011, 38, pp.L15202. 10.1029/2011GL048109. hal-00659784 HAL Id: hal-00659784 https://hal.archives-ouvertes.fr/hal-00659784 Submitted on 19 Jan 2012 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. GEOPHYSICAL RESEARCH LETTERS, VOL. 38, L15202, doi:10.1029/2011GL048109, 2011 Dikes of distinct composition intruded into Noachian‐aged crust exposed in the walls of Valles Marineris Jessica Flahaut,1 John F. Mustard,2 Cathy Quantin,1 Harold Clenet,1 Pascal Allemand,1 and Pierre Thomas1 Received 12 May 2011; revised 27 June 2011; accepted 30 June 2011; published 5 August 2011. [1] Valles Marineris represents the deepest natural incision and HiRISE (High Resolution Imaging Science Experiment) in the Martian upper crust. -
Iani Chaos As a Landing Site for the Mars Science Laboratory. T. D. Glotch1, 1Jet Propulsion Laboratory, Cali- Fornia Institute of Technology
Iani Chaos as a landing site for the Mars Science Laboratory. T. D. Glotch1, 1Jet Propulsion Laboratory, Cali- fornia Institute of Technology. [email protected] Iani Chaos, the source region of Ares Valles, is centered at ~342°E, 2°S. The chaotic terrain is widely- believed to have formed via the removal of subsurface water or ice, resulting in flooding at the surface, and the formation of Ares Vallis. Within Iani Chaos, de- posited stratigraphically above the chaotic terrain, are smooth, low-slope, intermediate-to-light-toned depos- its that are rich in a hydrated mineral that is most likely gypsum [1] as well as hematite[2-3] (Figure 1). Crystalline hematite and sulfates have been de- tected from orbit in numerous locations, including Me- ridiani Planum [4], Aram Chaos [1,5-6], Valles Marin- eris[5], and Aureum and Iani Chaos[2-3]. The MER Opportunity rover landed at Meridiani Planum and has shown that hematite is present as spherules that erode from a light-toned sulfate-rich outcrop. The MER team’s hypothesis of an ancient dune/interdune playa environment at Meridiani Planum[7] has been chal- lenged by both volcanic[8] and impact[9] models. A Figure 1. Map of hematite abundance in Iani Chaos. Hema- rover sent to one of the other locations rich in hematite tite abundance varies from ~5-20%. Based on OMEGA and sulfates will help to resolve the current debate and data[1], the presence of sulfate roughly correlates with that increase understanding of the role of ground and sur- of hematite.