Outstanding 1977 Ames Achievements
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Planetary Geologic Mappers Annual Meeting
Program Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Planetary Geologic Mappers Annual Meeting June 12–14, 2018 • Knoxville, Tennessee Institutional Support Lunar and Planetary Institute Universities Space Research Association Convener Devon Burr Earth and Planetary Sciences Department, University of Tennessee Knoxville Science Organizing Committee David Williams, Chair Arizona State University Devon Burr Earth and Planetary Sciences Department, University of Tennessee Knoxville Robert Jacobsen Earth and Planetary Sciences Department, University of Tennessee Knoxville Bradley Thomson Earth and Planetary Sciences Department, University of Tennessee Knoxville Abstracts for this meeting are available via the meeting website at https://www.hou.usra.edu/meetings/pgm2018/ Abstracts can be cited as Author A. B. and Author C. D. (2018) Title of abstract. In Planetary Geologic Mappers Annual Meeting, Abstract #XXXX. LPI Contribution No. 2066, Lunar and Planetary Institute, Houston. Guide to Sessions Tuesday, June 12, 2018 9:00 a.m. Strong Hall Meeting Room Introduction and Mercury and Venus Maps 1:00 p.m. Strong Hall Meeting Room Mars Maps 5:30 p.m. Strong Hall Poster Area Poster Session: 2018 Planetary Geologic Mappers Meeting Wednesday, June 13, 2018 8:30 a.m. Strong Hall Meeting Room GIS and Planetary Mapping Techniques and Lunar Maps 1:15 p.m. Strong Hall Meeting Room Asteroid, Dwarf Planet, and Outer Planet Satellite Maps Thursday, June 14, 2018 8:30 a.m. Strong Hall Optional Field Trip to Appalachian Mountains Program Tuesday, June 12, 2018 INTRODUCTION AND MERCURY AND VENUS MAPS 9:00 a.m. Strong Hall Meeting Room Chairs: David Williams Devon Burr 9:00 a.m. -
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. -
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 -
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The Tennessee Meteorite Impact Sites and Changing Perspectives on Impact Cratering
UNIVERSITY OF SOUTHERN QUEENSLAND THE TENNESSEE METEORITE IMPACT SITES AND CHANGING PERSPECTIVES ON IMPACT CRATERING A dissertation submitted by Janaruth Harling Ford B.A. Cum Laude (Vanderbilt University), M. Astron. (University of Western Sydney) For the award of Doctor of Philosophy 2015 ABSTRACT Terrestrial impact structures offer astronomers and geologists opportunities to study the impact cratering process. Tennessee has four structures of interest. Information gained over the last century and a half concerning these sites is scattered throughout astronomical, geological and other specialized scientific journals, books, and literature, some of which are elusive. Gathering and compiling this widely- spread information into one historical document benefits the scientific community in general. The Wells Creek Structure is a proven impact site, and has been referred to as the ‘syntype’ cryptoexplosion structure for the United State. It was the first impact structure in the United States in which shatter cones were identified and was probably the subject of the first detailed geological report on a cryptoexplosive structure in the United States. The Wells Creek Structure displays bilateral symmetry, and three smaller ‘craters’ lie to the north of the main Wells Creek structure along its axis of symmetry. The question remains as to whether or not these structures have a common origin with the Wells Creek structure. The Flynn Creek Structure, another proven impact site, was first mentioned as a site of disturbance in Safford’s 1869 report on the geology of Tennessee. It has been noted as the terrestrial feature that bears the closest resemblance to a typical lunar crater, even though it is the probable result of a shallow marine impact. -
James Hutton's Reputation Among Geologists in the Late Eighteenth and Nineteenth Centuries
The Geological Society of America Memoir 216 Revising the Revisions: James Hutton’s Reputation among Geologists in the Late Eighteenth and Nineteenth Centuries A. M. Celâl Şengör* İTÜ Avrasya Yerbilimleri Enstitüsü ve Maden Fakültesi, Jeoloji Bölümü, Ayazağa 34469 İstanbul, Turkey ABSTRACT A recent fad in the historiography of geology is to consider the Scottish polymath James Hutton’s Theory of the Earth the last of the “theories of the earth” genre of publications that had begun developing in the seventeenth century and to regard it as something behind the times already in the late eighteenth century and which was subsequently remembered only because some later geologists, particularly Hutton’s countryman Sir Archibald Geikie, found it convenient to represent it as a precursor of the prevailing opinions of the day. By contrast, the available documentation, pub- lished and unpublished, shows that Hutton’s theory was considered as something completely new by his contemporaries, very different from anything that preceded it, whether they agreed with him or not, and that it was widely discussed both in his own country and abroad—from St. Petersburg through Europe to New York. By the end of the third decade in the nineteenth century, many very respectable geologists began seeing in him “the father of modern geology” even before Sir Archibald was born (in 1835). Before long, even popular books on geology and general encyclopedias began spreading the same conviction. A review of the geological literature of the late eighteenth and the nineteenth centuries shows that Hutton was not only remembered, but his ideas were in fact considered part of the current science and discussed accord- ingly. -
Morphology and Morphometry of Double Layered Ejecta Craters on Mars
Western University Scholarship@Western Electronic Thesis and Dissertation Repository August 2015 Morphology and Morphometry of Double Layered Ejecta Craters on Mars Ryan Schwegman The University of Western Ontario Supervisor Dr. Gordon Osinski The University of Western Ontario Joint Supervisor Dr. Livio Tornabene The University of Western Ontario Graduate Program in Geology A thesis submitted in partial fulfillment of the equirr ements for the degree in Master of Science © Ryan Schwegman 2015 Follow this and additional works at: https://ir.lib.uwo.ca/etd Part of the Geology Commons Recommended Citation Schwegman, Ryan, "Morphology and Morphometry of Double Layered Ejecta Craters on Mars" (2015). Electronic Thesis and Dissertation Repository. 3074. https://ir.lib.uwo.ca/etd/3074 This Dissertation/Thesis is brought to you for free and open access by Scholarship@Western. It has been accepted for inclusion in Electronic Thesis and Dissertation Repository by an authorized administrator of Scholarship@Western. For more information, please contact [email protected]. MORPHOLOGY AND MORPHOMETRY OF DOUBLE LAYERED EJECTA CRATERS ON MARS (Thesis format: Integrated Article) by Ryan Schwegman Graduate Program in Geology: Planetary Science A thesis submitted in partial fulfillment of the requirements for the degree of Master of Science The School of Graduate and Postdoctoral Studies The University of Western Ontario London, Ontario, Canada © Ryan Schwegman 2015 Abstract Double layered ejecta (DLE) craters display two distinct layers of ejecta that appear to have been emplaced as a mobile, ground-hugging flow. While volatile content within the target, atmosphere, or some combination of the two is generally considered a major variable enhancing the mobility of ejecta, the presence of unconsolidated surface materials may also have some effect. -
Mars Pathfinder Landing Site Workshop Ii: Characteristics of the Ares Vallis Region and Field Trips in the Channeled Scabland, Washington
/, NASA-CR-200508 L / MARS PATHFINDER LANDING SITE WORKSHOP II: CHARACTERISTICS OF THE ARES VALLIS REGION AND FIELD TRIPS IN THE CHANNELED SCABLAND, WASHINGTON LPI Technical Report Number 95-01, Part 1 Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPI/TR--95-01, Part 1 "lp MARS PATHFINDER LANDING SITE WORKSHOP II: CHARACTERISTICS OF THE ARES VALLIS REGION AND FIELD TRIPS IN THE CHANNELED SCABLAND, WASHINGTON Edited by M. P. Golombek, K. S. Edgett, and J. W. Rice Jr. Held at Spokane, Washington September 24-30, 1995 Sponsored by Arizona State University Jet Propulsion Laboratory Lunar and Planetary Institute National Aeronautics and Space Administration Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPI Technical Report Number 95-01, Part 1 LPI/TR--95-01, Part 1 Compiled in 1995 by LUNAR AND PLANETARY INSTITUTE The Institute is operated by the University Space Research Association under Contract No. NASW-4574 with the National Aeronautics and Space Administration. Material in this volume may he copied without restraint for library, abstract service, education, or personal research purposes; however, republication of any paper or portion thereof requires the written permission of the authors as well as the appropriate acknowledgment of this publication. This report may he cited as Golomhek M. P., Edger K. S., and Rice J. W. Jr., eds. ( 1992)Mars Pathfinder Landing Site Workshop 11: Characteristics of the Ares Vallis Region and Field Trips to the Channeled Scabland, Washington. LPI Tech. Rpt. 95-01, Part 1, Lunar and Planetary Institute, Houston. 63 pp. -
Geological Analysis of Martian Rover‐Derived Digital Outcrop Models
Earth and Space Science RESEARCH ARTICLE Geological Analysis of Martian Rover-Derived Digital Outcrop 10.1002/2018EA000374 Models Using the 3-D Visualization Tool, Planetary Special Section: Robotics 3-D Viewer—PRo3D Planetary Mapping: Methods, Tools for Scientific Analysis and Robert Barnes1 , Sanjeev Gupta1 , Christoph Traxler2 , Thomas Ortner2, Arnold Bauer3, Exploration Gerd Hesina2, Gerhard Paar3 , Ben Huber3,4, Kathrin Juhart3, Laura Fritz2, Bernhard Nauschnegg3, 5 5 Key Points: Jan-Peter Muller , and Yu Tao • Processing of images from 1 2 stereo-cameras on Mars rovers Department of Earth Science and Engineering, Imperial College London, London, UK, VRVis Zentrum für Virtual Reality 3 4 produces 3-D Digital Outcrop und Visualisierung Forschungs-GmbH, Vienna, Austria, Joanneum Research, Graz, Austria, Now at ETH Zürich, Zürich, Models (DOMs) which are rendered Switzerland, 5Mullard Space Science Laboratory, University College London, London, UK and analyzed in PRo3D • PRo3D enables efficient, real-time rendering and geological analysis of Abstract Panoramic camera systems on robots exploring the surface of Mars are used to collect images of the DOMs, allowing extraction of large amounts of quantitative data terrain and rock outcrops which they encounter along their traverse. Image mosaics from these cameras • Methodologies for sedimentological are essential in mapping the surface geology and selecting locations for analysis by other instruments on and structural DOM analyses in PRo3D the rover’s payload. 2-D images do not truly portray the depth of field of features within an image, nor are presented at four localities along the MSL and MER traverses their 3-D geometry. This paper describes a new 3-D visualization software tool for geological analysis of Martian rover-derived Digital Outcrop Models created using photogrammetric processing of stereo-images Supporting Information: using the Planetary Robotics Vision Processing tool developed for 3-D vision processing of ExoMars • Supporting Information S1 • Data Set S1 PanCam and Mars 2020 Mastcam-Z data. -
Science Concept 3: Key Planetary
Science Concept 6: The Moon is an Accessible Laboratory for Studying the Impact Process on Planetary Scales Science Concept 6: The Moon is an accessible laboratory for studying the impact process on planetary scales Science Goals: a. Characterize the existence and extent of melt sheet differentiation. b. Determine the structure of multi-ring impact basins. c. Quantify the effects of planetary characteristics (composition, density, impact velocities) on crater formation and morphology. d. Measure the extent of lateral and vertical mixing of local and ejecta material. INTRODUCTION Impact cratering is a fundamental geological process which is ubiquitous throughout the Solar System. Impacts have been linked with the formation of bodies (e.g. the Moon; Hartmann and Davis, 1975), terrestrial mass extinctions (e.g. the Cretaceous-Tertiary boundary extinction; Alvarez et al., 1980), and even proposed as a transfer mechanism for life between planetary bodies (Chyba et al., 1994). However, the importance of impacts and impact cratering has only been realized within the last 50 or so years. Here we briefly introduce the topic of impact cratering. The main crater types and their features are outlined as well as their formation mechanisms. Scaling laws, which attempt to link impacts at a variety of scales, are also introduced. Finally, we note the lack of extraterrestrial crater samples and how Science Concept 6 addresses this. Crater Types There are three distinct crater types: simple craters, complex craters, and multi-ring basins (Fig. 6.1). The type of crater produced in an impact is dependent upon the size, density, and speed of the impactor, as well as the strength and gravitational field of the target. -
Stratigraphic Architecture of Bedrock Reference Section, Victoria Crater, Meridiani Planum, Mars
STRATIGRAPHIC ARCHITECTURE OF BEDROCK REFERENCE SECTION, VICTORIA CRATER, MERIDIANI PLANUM, MARS LAUREN A. EDGAR, JOHN P. GROTZINGER, AND ALEX G. HAYES Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125 USA e-mail: [email protected] DAVID M. RUBIN US Geological Survey Pacific Science Center, Santa Cruz, California 95060 USA STEVE W. SQUYRES AND JAMES F. BELL Astronomy Department, Cornell University, Ithaca, New York 14853 USA AND KEN E. HERKENHOFF US Geological Survey Astrogeology Science Center, Flagstaff, Arizona 86001 USA ABSTRACT: The Mars Exploration Rover Opportunity has investigated bedrock outcrops exposed in several craters at Meridiani Planum, Mars, in an effort to better understand the role of surface processes in its geologic history. Opportunity has recently completed its observations of Victoria crater, which is 750 m in diameter and exposes cliffs up to ;15 m high. The plains surrounding Victoria crater are ;10 m higher in elevation than those surrounding the previously explored Endurance crater, indicating that the Victoria crater exposes a stratigraphically higher section than does the Endurance crater; however, Victoria strata overlap in elevation with the rocks exposed at the Erebus crater. Victoria crater has a well-developed geomorphic pattern of promontories and embayments that define the crater wall and that reveal thick bedsets (3–7 m) of large-scale cross-bedding, interpreted as fossil eolian dunes. Opportunity was able to drive into the crater at Duck Bay, located on the western margin of Victoria crater. Data from the Microscopic Imager and Panoramic Camera reveal details about the structures, textures, and depositional and diagenetic events that influenced the Victoria bedrock. -
GEOLOGICAL MAPPING and CHRONOLOGICAL BASED CRATER COUNTING ANALYSIS (CSFD) of MARS. Fares M. Howari*1, Manish Sharma1, Yousef Na
51st Lunar and Planetary Science Conference (2020) 1265.pdf GEOLOGICAL MAPPING AND CHRONOLOGICAL BASED CRATER COUNTING ANALYSIS (CSFD) OF MARS. Fares M. Howari*1, Manish Sharma1, Yousef Nazzal1, Fatima AlAydaroos2, and Cijo M Xavier1, 1College of Natural and Health Sciences, Zayed University, P.O. Box 144534, Abu Dhabi, UAE (*[email protected]),2 UAE Space Agency, P.O. Box 7133, Abu Dhabi, UAE. Introduction: Although only half the size of the Earth, tary bodies, One method links radiogenic isotope age Mars has a remarkably rich and complex preserved [4] and another method, rates for formation of impact geological record. The knowledge on Martian Geology craters [5,6]. Crater based age determination of surface has enormously increased in last 40 years. Several mis- features for any kind of planetary body is essential for sions orbiting or roving Mars revolutionized our under- understanding the categorization of geological events in standing of its evolution and geological features, in the past [7]. The chronological based crater counting is several ways like Earth, but extremely different in many a well-established technique for determining relative respects. and absolute model ages of planetary surfaces of Mars, The study area (Latitude 0°N-45°N, Longi- Moon, Mercury [8,9]. tude 60°E-120°E) lies near to the landing site of Viking Relative ages can be derived by measuring the 2 and MSL (Mars Science Laboratory), having a total size-frequency distribution of impact craters that have area of 9,080,730 square kilometers (5642505 square accumulated in a planet’s history through time which Miles) is shown in Fig.1.