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Geoscience and a Lunar Base
" t N_iSA Conference Pubhcatmn 3070 " i J Geoscience and a Lunar Base A Comprehensive Plan for Lunar Explora, tion unclas HI/VI 02907_4 at ,unar | !' / | .... ._-.;} / [ | -- --_,,,_-_ |,, |, • • |,_nrrr|l , .l -- - -- - ....... = F _: .......... s_ dd]T_- ! JL --_ - - _ '- "_r: °-__.......... / _r NASA Conference Publication 3070 Geoscience and a Lunar Base A Comprehensive Plan for Lunar Exploration Edited by G. Jeffrey Taylor Institute of Meteoritics University of New Mexico Albuquerque, New Mexico Paul D. Spudis U.S. Geological Survey Branch of Astrogeology Flagstaff, Arizona Proceedings of a workshop sponsored by the National Aeronautics and Space Administration, Washington, D.C., and held at the Lunar and Planetary Institute Houston, Texas August 25-26, 1988 IW_A National Aeronautics and Space Administration Office of Management Scientific and Technical Information Division 1990 PREFACE This report was produced at the request of Dr. Michael B. Duke, Director of the Solar System Exploration Division of the NASA Johnson Space Center. At a meeting of the Lunar and Planetary Sample Team (LAPST), Dr. Duke (at the time also Science Director of the Office of Exploration, NASA Headquarters) suggested that future lunar geoscience activities had not been planned systematically and that geoscience goals for the lunar base program were not articulated well. LAPST is a panel that advises NASA on lunar sample allocations and also serves as an advocate for lunar science within the planetary science community. LAPST took it upon itself to organize some formal geoscience planning for a lunar base by creating a document that outlines the types of missions and activities that are needed to understand the Moon and its geologic history. -
Qiao Et Al., Sosigenes Pit Crater Age 1/51
Qiao et al., Sosigenes pit crater age 1 2 The role of substrate characteristics in producing anomalously young crater 3 retention ages in volcanic deposits on the Moon: Morphology, topography, 4 sub-resolution roughness and mode of emplacement of the Sosigenes Lunar 5 Irregular Mare Patch (IMP) 6 7 Le QIAO1,2,*, James W. HEAD2, Long XIAO1, Lionel WILSON3, and Josef D. 8 DUFEK4 9 1Planetary Science Institute, School of Earth Sciences, China University of 10 Geosciences, Wuhan 430074, China. 11 2Department of Earth, Environmental and Planetary Sciences, Brown University, 12 Providence, RI 02912, USA. 13 3Lancaster Environment Centre, Lancaster University, Lancaster LA1 4YQ, UK. 14 4School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, 15 Georgia 30332, USA. 16 *Corresponding author E-mail: [email protected] 17 18 19 20 Key words: Lunar/Moon, Sosigenes, irregular mare patches, mare volcanism, 21 magmatic foam, lava lake, dike emplacement 22 23 24 25 1/51 Qiao et al., Sosigenes pit crater age 26 Abstract: Lunar Irregular Mare Patches (IMPs) are comprised of dozens of small, 27 distinctive and enigmatic lunar mare features. Characterized by their irregular shapes, 28 well-preserved state of relief, apparent optical immaturity and few superposed impact 29 craters, IMPs are interpreted to have been formed or modified geologically very 30 recently (<~100 Ma; Braden et al. 2014). However, their apparent relatively recent 31 formation/modification dates and emplacement mechanisms are debated. We focus in 32 detail on one of the major IMPs, Sosigenes, located in western Mare Tranquillitatis, 33 and dated by Braden et al. -
Glossary Glossary
Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts. -
Planetary Surfaces
Chapter 4 PLANETARY SURFACES 4.1 The Absence of Bedrock A striking and obvious observation is that at full Moon, the lunar surface is bright from limb to limb, with only limited darkening toward the edges. Since this effect is not consistent with the intensity of light reflected from a smooth sphere, pre-Apollo observers concluded that the upper surface was porous on a centimeter scale and had the properties of dust. The thickness of the dust layer was a critical question for landing on the surface. The general view was that a layer a few meters thick of rubble and dust from the meteorite bombardment covered the surface. Alternative views called for kilometer thicknesses of fine dust, filling the maria. The unmanned missions, notably Surveyor, resolved questions about the nature and bearing strength of the surface. However, a somewhat surprising feature of the lunar surface was the completeness of the mantle or blanket of debris. Bedrock exposures are extremely rare, the occurrence in the wall of Hadley Rille (Fig. 6.6) being the only one which was observed closely during the Apollo missions. Fragments of rock excavated during meteorite impact are, of course, common, and provided both samples and evidence of co,mpetent rock layers at shallow levels in the mare basins. Freshly exposed surface material (e.g., bright rays from craters such as Tycho) darken with time due mainly to the production of glass during micro- meteorite impacts. Since some magnetic anomalies correlate with unusually bright regions, the solar wind bombardment (which is strongly deflected by the magnetic anomalies) may also be responsible for darkening the surface [I]. -
Evidence for Impact-Generated Deposition
EVIDENCE FOR IMPACT-GENERATED DEPOSITION ON THE LATE EOCENE SHORES OF GEORGIA by ROBERT SCOTT HARRIS (Under the direction of Michael F. Roden) ABSTRACT Modeling demonstrates that the Late Eocene Chesapeake Bay impact would have been capable of depositing ejecta in east-central Georgia with thicknesses exceeding thirty centimeters. A coarse sand layer at the base of the Upper Eocene Dry Branch Formation was examined for shocked minerals. Universal stage measurements demonstrate that planar fabrics in some fine to medium sand-size quartz grains are parallel to planes commonly exploited by planar deformation features (PDF’s) in shocked quartz. Possible PDF’s are observed parallel to {10-13}, {10-11}, {10-12}, {11-22} and {51-61}. Petrographic identification of shocked quartz is supported by line broadening in X-ray diffraction experiments. Other impact ejecta recognized include possible ballen quartz, maskelynite, and reidite-bearing zircon grains. The layer is correlative with an unusual diamictite that contains goethite spherules similar to altered microkrystites. It may represent an impact-generated debris flow. These discoveries suggest that the Chesapeake Bay impact horizon is preserved in Georgia. The horizon also should be the source stratum for Georgia tektites. INDEX WORDS: Chesapeake Bay impact, Upper Eocene, Shocked quartz, Impact shock, Shocked zircon, Impact, Impact ejecta, North American tektites, Tektites, Georgiaites, Georgia Tektites, Planar deformation features, PDF’s, Georgia, Geology, Coastal Plain, Stratigraphy, Impact stratigraphy, Impact spherules, Goethite spherules, Diamictite, Twiggs Clay, Dry Branch Formation, Clinchfield Sand, Irwinton Sand, Reidite, Microkrystite, Cpx Spherules, Impact debris flow EVIDENCE FOR IMPACT-GENERATED DEPOSITION ON THE LATE EOCENE SHORES OF GEORGIA by ROBERT SCOTT HARRIS B. -
DMAAC – February 1973
LUNAR TOPOGRAPHIC ORTHOPHOTOMAP (LTO) AND LUNAR ORTHOPHOTMAP (LO) SERIES (Published by DMATC) Lunar Topographic Orthophotmaps and Lunar Orthophotomaps Scale: 1:250,000 Projection: Transverse Mercator Sheet Size: 25.5”x 26.5” The Lunar Topographic Orthophotmaps and Lunar Orthophotomaps Series are the first comprehensive and continuous mapping to be accomplished from Apollo Mission 15-17 mapping photographs. This series is also the first major effort to apply recent advances in orthophotography to lunar mapping. Presently developed maps of this series were designed to support initial lunar scientific investigations primarily employing results of Apollo Mission 15-17 data. Individual maps of this series cover 4 degrees of lunar latitude and 5 degrees of lunar longitude consisting of 1/16 of the area of a 1:1,000,000 scale Lunar Astronautical Chart (LAC) (Section 4.2.1). Their apha-numeric identification (example – LTO38B1) consists of the designator LTO for topographic orthophoto editions or LO for orthophoto editions followed by the LAC number in which they fall, followed by an A, B, C or D designator defining the pertinent LAC quadrant and a 1, 2, 3, or 4 designator defining the specific sub-quadrant actually covered. The following designation (250) identifies the sheets as being at 1:250,000 scale. The LTO editions display 100-meter contours, 50-meter supplemental contours and spot elevations in a red overprint to the base, which is lithographed in black and white. LO editions are identical except that all relief information is omitted and selenographic graticule is restricted to border ticks, presenting an umencumbered view of lunar features imaged by the photographic base. -
User Guide to 1:250,000 Scale Lunar Maps
CORE https://ntrs.nasa.gov/search.jsp?R=19750010068Metadata, citation 2020-03-22T22:26:24+00:00Z and similar papers at core.ac.uk Provided by NASA Technical Reports Server USER GUIDE TO 1:250,000 SCALE LUNAR MAPS (NASA-CF-136753) USE? GJIDE TO l:i>,, :LC h75- lu1+3 SCALE LUNAR YAPS (Lumoalcs Feseclrch Ltu., Ottewa (Ontario) .) 24 p KC 53.25 CSCL ,33 'JIACA~S G3/31 11111 DANNY C, KINSLER Lunar Science Instltute 3303 NASA Road $1 Houston, TX 77058 Telephone: 7131488-5200 Cable Address: LUtiSI USER GUIDE TO 1: 250,000 SCALE LUNAR MAPS GENERAL In 1972 the NASA Lunar Programs Office initiated the Apollo Photographic Data Analysis Program. The principal point of this program was a detailed scientific analysis of the orbital and surface experiments data derived from Apollo missions 15, 16, and 17. One of the requirements of this program was the production of detailed photo base maps at a useable scale. NASA in conjunction with the Defense Mapping Agency (DMA) commenced a mapping program in early 1973 that would lead to the production of the necessary maps based on the need for certain areas. This paper is designed to present in outline form the neces- sary background informatiox or users to become familiar with the program. MAP FORMAT * The scale chosen for the project was 1:250,000 . The re- search being done required a scale that Principal Investigators (PI'S) using orbital photography could use, but would also serve PI'S doing surface photographic investigations. Each map sheet covers an area four degrees north/south by five degrees east/west. -
Impact Structures and Events – a Nordic Perspective
107 by Henning Dypvik1, Jüri Plado2, Claus Heinberg3, Eckart Håkansson4, Lauri J. Pesonen5, Birger Schmitz6, and Selen Raiskila5 Impact structures and events – a Nordic perspective 1 Department of Geosciences, University of Oslo, P.O. Box 1047, Blindern, NO 0316 Oslo, Norway. E-mail: [email protected] 2 Department of Geology, University of Tartu, Vanemuise 46, 51014 Tartu, Estonia. 3 Department of Environmental, Social and Spatial Change, Roskilde University, P.O. Box 260, DK-4000 Roskilde, Denmark. 4 Department of Geography and Geology, University of Copenhagen, Øster Voldgade 10, DK-1350 Copenhagen, Denmark. 5 Division of Geophysics, University of Helsinki, P.O. Box 64, FIN-00014 Helsinki, Finland. 6 Department of Geology, University of Lund, Sölvegatan 12, SE-22362 Lund, Sweden. Impact cratering is one of the fundamental processes in are the main reason that the Nordic countries are generally well- the formation of the Earth and our planetary system, as mapped. reflected, for example in the surfaces of Mars and the Impact craters came into the focus about 20 years ago and the interest among the Nordic communities has increased during recent Moon. The Earth has been covered by a comparable years. The small Kaalijärv structure of Estonia was the first impact number of impact scars, but due to active geological structure to be confirmed in northern Europe (Table 1; Figures 1 and processes, weathering, sea floor spreading etc, the num- 7). First described in 1794 (Rauch), the meteorite origin of the crater ber of preserved and recognized impact craters on the field (presently 9 craters) was proposed much later in 1919 (Kalju- Earth are limited. -
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. -
Tossup Roentgen, Archimedes, Gauss, Balboa an D~¥As.:.? Da
Tossup , Roentgen, Archimedes, Gauss, Balboa an_d ~¥as.:.? Da Gama all have one bigger than Einstein's. Rutherford's is inside of..G!avius'. ' ~e three largest are Hertzsprung, Korolev and Apollo. For 10 points );IlUlt are t!1e~ objects, seven of which will be named for the astronauts who ~e..s-p~ttle disaster. / . Lunar Craters (' ,/ J- This Athenjan wa~ an admirer of Socrates ~ndji . him' such works as the Symposium and the Apo!?gy of Socrates. ~ - - st known wever, as an historian, the author of the Hellemca and the AnaEiastS, an a t of a mercenary expedition into Asia Minor. For 10 points, name ntury B.C. author. Xenophon ,. .. .. "The seizure of $3~&;gWo Y Hills," "Savage Lu~y ... 'Teeth Like Baseballs, Eyes Like J llied ire, '" and "A Terrible Experience with Extremely Dangerous Drugs." These e apters from, for 10 points, .what book? Fear and Loathing in Las Vegas (by Hunter S. Thompson) .' Lazlo Toth attacked her with a h~e, screaming "I Jesus Christ". He severed her left arm, smas~er nose-and lsfigured her I eye. That was in 1972, and today she and her ~n~i~ ·- behlnd i ss wall in J) Peter's Basilica the scars barely visible. For 10 y.Qin(s, "Yho are .... y, re ? ' The Pieul . L/ Accept: C~st and the Virgin Mary In 1649She invited Rene Descartes to her court to teach her philosophy. She had her lessons at 5 in the morning; Des.cartes, more used to rising at noon, caught a c . d died. Fo t's: who was this Swedish queen, \ the daughter of Gustavus Christina \, \ \ / Tossup Its biological name Ailuropod I 'l- " --~ . -
A Paleozoic Age for the Tunnunik Impact Structure Camille Lepaulard, Jerome Gattacceca, Nicholas Swanson-Hysell, Yoann Quesnel, François Demory, Gordon Osinski
A Paleozoic age for the Tunnunik impact structure Camille Lepaulard, Jerome Gattacceca, Nicholas Swanson-Hysell, Yoann Quesnel, François Demory, Gordon Osinski To cite this version: Camille Lepaulard, Jerome Gattacceca, Nicholas Swanson-Hysell, Yoann Quesnel, François Demory, et al.. A Paleozoic age for the Tunnunik impact structure. Meteoritics and Planetary Science, Wiley, 2019, 54 (4), pp.740-751. 10.1111/maps.13239. hal-02048190 HAL Id: hal-02048190 https://hal.archives-ouvertes.fr/hal-02048190 Submitted on 26 Apr 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. 1 2 A Paleozoic age for the Tunnunik impact structure 3 4 Camille Lepaulard1, Jérôme Gattacceca1, Nicholas Swanson-Hysell2, Yoann Quesnel1, 5 François Demory1 , Gordon R. Osinski3,4, 6 7 1Aix Marseille Univ, CNRS, IRD, Coll France, INRA, CEREGE, Aix-en-Provence, France 8 2 Department of Earth and Planetary Science, University of California, Berkeley, California 9 94720-4767, USA 10 3 Dept. of Earth Sciences, Centre for Planetary Science and Exploration, University of Western 11 Ontario, -
Carlyle Smith Beals Fonds (R15735) Finding Aid No MSS2580 MIKAN
Date: 15/06/2017 Carlyle Smith Beals fonds (R15735) Page 1 Finding aid no MSS2580 Y:\App\Impromptu\Mikan\Reports\Description_reports\finding_aids_&_subcontainers_simplelist.imr MIKAN Container File/Item Cr. file/item Hierarchy Title, etc Date of/de Extent/Media/Dim/Access cde # Contenant Dos./pièce Dos./item cr. Hiérarchie Titre, etc création Support ou Média / Dim. / Accès 4938572 Series Personnal papers [textual record, graphic material] 1922-1978 4941473 1 1 File Personal papers 1947-1972 Textual records / 90 S&C : Biographical information, genealogical information on the Beals family. Contains also a passeport and a manual with french expressions and vocabulary. 4941474 1 2 File Personal correspondence 1965-1978 Textual records / 90 S&C : Correspondence not related to the professional activities of C.S. Beals. Contains also several postal cards. 4941475 1 3 File Scholarship records, Degrees, Honors and letters of 1922-1977 Textual records / 90 recommendation S&C : Contains a scholarship record of Yale University for 1922, letters from the University of London that certify the reception of two Ph.D. by C.S. Beals in 1926 and 1934. Contains the certification of the registrar's Office of the University of Toronto for the M.A. of 1923. Contains also letters of recommendation from the different schools attented by C.S. Beals. Contains also a letter from the Royal Society of Canada informing C..S. Beals.that he'll be recommended as fellow of the RSC, a letter from The Profesionnal Institute of the Public Service of Canada for the reception of the Institute's Gold Medal (1977), correspondence and documentation concerning the reception of a Honorary Degree from Queen's University in Kingston in 1960 and a certificate of the Royal Society of Canada certifying 45 years of membership.