Case Fil Copy
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Copyrighted Material
Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED -
Land Resource Regions and Major Land Resource Areas in New York
R L NS Land Resource Regions and Major Land Resource Areas in New York State Land Resource Regions and Major Land Resource Areas of the United States, the Caribbean, and the Pacific Basin MLRA Explorer Custom Report L - Lake State Fruit, Truck Crop, and Dairy Region 101 - Ontario-Erie Plain and Finger Lakes Region M - Central Feed Grains and Livestock Region 111E - Indiana and Ohio Till Plain, Eastern Part 111B - Indiana and Ohio Till Plain, Northeastern Part R - Northeastern Forage and Forest Region 144B - New England and Eastern New York Upland, Northern Part 144A - New England and Eastern New York Upland, Southern Part 143 - Northeastern Mountains 142 - St. Lawrence-Champlain Plain 141 - Tughill Plateau 140 - Glaciated Allegheny Plateau and Catskill Mountains 139 - Lake Erie Glaciated Plateau Major Land Resource Regions Custom Report Page 1 Data Source: USDA Agriculture Handbook 296 (2006) 03/26/08 http://soils.usda.gov/MLRAExplorer L - Lake State Fruit, Truck Crop, and Dairy Region Figure L-1: Location of Land Resource Region L LRR Overview This region (shown in fig. L-1) is in Michigan (59 percent), New York (22 percent), Ohio (10 percent), Indiana (8 percent), and Illinois (1 percent). A very small part is in Pennsylvania. The region makes up 45,715 square miles (118,460 square kilometers). Typically, the land surface is a nearly level to gently sloping glaciated plain (fig. L-2). The average annual precipitation is typically 30 to 41 inches (760 to 1,040 millimeters), but it is 61 inches (1,550 millimeters) in the part of the region east of Lake Erie. -
Ice Ic” Werner F
Extent and relevance of stacking disorder in “ice Ic” Werner F. Kuhsa,1, Christian Sippela,b, Andrzej Falentya, and Thomas C. Hansenb aGeoZentrumGöttingen Abteilung Kristallographie (GZG Abt. Kristallographie), Universität Göttingen, 37077 Göttingen, Germany; and bInstitut Laue-Langevin, 38000 Grenoble, France Edited by Russell J. Hemley, Carnegie Institution of Washington, Washington, DC, and approved November 15, 2012 (received for review June 16, 2012) “ ” “ ” A solid water phase commonly known as cubic ice or ice Ic is perfectly cubic ice Ic, as manifested in the diffraction pattern, in frequently encountered in various transitions between the solid, terms of stacking faults. Other authors took up the idea and liquid, and gaseous phases of the water substance. It may form, attempted to quantify the stacking disorder (7, 8). The most e.g., by water freezing or vapor deposition in the Earth’s atmo- general approach to stacking disorder so far has been proposed by sphere or in extraterrestrial environments, and plays a central role Hansen et al. (9, 10), who defined hexagonal (H) and cubic in various cryopreservation techniques; its formation is observed stacking (K) and considered interactions beyond next-nearest over a wide temperature range from about 120 K up to the melt- H-orK sequences. We shall discuss which interaction range ing point of ice. There was multiple and compelling evidence in the needs to be considered for a proper description of the various past that this phase is not truly cubic but composed of disordered forms of “ice Ic” encountered. cubic and hexagonal stacking sequences. The complexity of the König identified what he called cubic ice 70 y ago (11) by stacking disorder, however, appears to have been largely over- condensing water vapor to a cold support in the electron mi- looked in most of the literature. -
MID-LATITUDE MARTIAN ICE AS a TARGET for HUMAN EXPLORATION, ASTROBIOLOGY, and IN-SITU RESOURCE UTILIZATION. D. Viola1 ([email protected]), A
First Landing Site/Exploration Zone Workshop for Human Missions to the Surface of Mars (2015) 1011.pdf MID-LATITUDE MARTIAN ICE AS A TARGET FOR HUMAN EXPLORATION, ASTROBIOLOGY, AND IN-SITU RESOURCE UTILIZATION. D. Viola1 ([email protected]), A. S. McEwen1, and C. M. Dundas2. 1University of Arizona, Department of Planetary Sciences, 2USGS, Astrogeology Science Center. Introduction: Future human missions to Mars will region of late Noachian highlands terrain, and is com- need to rely on resources available near the Martian prised of a series of grabens and ridges surrounded by surface. Water is of primary importance, and is known later Hesperian/Amazonian lava flows from the Thar- to be abundant on Mars in multiple forms, including sis region [7]. The proposed landing site is within these hydrated minerals [1] and pore-filling and excess ice lava flows (HAv), and provides access to a region of deposits [2]. Of these sources, excess ice (or ice which late Hesperian lowlands in the western region of the exceeds the available regolith pore space) may be the EZ. There is evidence for Amazonian glacial and peri- most promising for in-situ resource utilization (ISRU). glacial activity [e.g., HiRISE images Since Martian excess ice is thought to contain a low PSP_008671_2210 and ESP_017374_2210], and the fraction of dust and other contaminants (~<10% by Gamma Ray Spectrometer water map suggests that volume, [3]) only a modest deposit of excess ice will there is abundant subsurface ice in the uppermost me- be sufficient to support a human presence. ter within this region [10]. Meandering channel-like Subsurface water ice may also be of astrobiological features have been identified in HiRISE images (e.g., interest as a potential current habitat or as a preserva- PSP_003529_2195 in close proximity to apparent ice tion medium for biosignatures. -
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. -
Indiana Glaciers.PM6
How the Ice Age Shaped Indiana Jerry Wilson Published by Wilstar Media, www.wilstar.com Indianapolis, Indiana 1 Previiously published as The Topography of Indiana: Ice Age Legacy, © 1988 by Jerry Wilson. Second Edition Copyright © 2008 by Jerry Wilson ALL RIGHTS RESERVED 2 For Aaron and Shana and In Memory of Donna 3 Introduction During the time that I have been a science teacher I have tried to enlist in my students the desire to understand and the ability to reason. Logical reasoning is the surest way to overcome the unknown. The best aid to reasoning effectively is having the knowledge and an understanding of the things that have previ- ously been determined or discovered by others. Having an understanding of the reasons things are the way they are and how they got that way can help an individual to utilize his or her resources more effectively. I want my students to realize that changes that have taken place on the earth in the past have had an effect on them. Why are some towns in Indiana subject to flooding, whereas others are not? Why are cemeteries built on old beach fronts in Northwest Indiana? Why would it be easier to dig a basement in Valparaiso than in Bloomington? These things are a direct result of the glaciers that advanced southward over Indiana during the last Ice Age. The history of the land upon which we live is fascinating. Why are there large granite boulders nested in some of the fields of northern Indiana since Indiana has no granite bedrock? They are known as glacial erratics, or dropstones, and were formed in Canada or the upper Midwest hundreds of millions of years ago. -
East and Central Farming and Forest Region and Atlantic Basin Diversified Farming Region: 12 Lrrs N and S
East and Central Farming and Forest Region and Atlantic Basin Diversified Farming Region: 12 LRRs N and S Brad D. Lee and John M. Kabrick 12.1 Introduction snowfall occurs annually in the Ozark Highlands, the Springfield Plateau, and the St. Francois Knobs and Basins The central, unglaciated US east of the Great Plains to the MLRAs. In the southern half of the region, snowfall is Atlantic coast corresponds to the area covered by LRR N uncommon. (East and Central Farming and Forest Region) and S (Atlantic Basin Diversified Farming Region). These regions roughly correspond to the Interior Highlands, Interior Plains, 12.2.2 Physiography Appalachian Highlands, and the Northern Coastal Plains. The topography of this region ranges from broad, gently rolling plains to steep mountains. In the northern portion of 12.2 The Interior Highlands this region, much of the Springfield Plateau and the Ozark Highlands is a dissected plateau that includes gently rolling The Interior Highlands occur within the western portion of plains to steeply sloping hills with narrow valleys. Karst LRR N and includes seven MLRAs including the Ozark topography is common and the region has numerous sink- Highlands (116A), the Springfield Plateau (116B), the St. holes, caves, dry stream valleys, and springs. The region also Francois Knobs and Basins (116C), the Boston Mountains includes many scenic spring-fed rivers and streams con- (117), Arkansas Valley and Ridges (118A and 118B), and taining clear, cold water (Fig. 12.2). The elevation ranges the Ouachita Mountains (119). This region comprises from 90 m in the southeastern side of the region and rises to 176,000 km2 in southern Missouri, northern and western over 520 m on the Springfield Plateau in the western portion Arkansas, and eastern Oklahoma (Fig. -
The Logan Plateau, a Young Physiographic Region in West Virginia, Kentucky, Virginia, and Tennessee
The Logan Plateau, a Young Physiographic Region in West Virginia, Kentucky, Virginia, and Tennessee U.S. GEOLOGICAL SURVEY BULLETIN 1620 . II • r ,j • • ~1 =1 i1 .. ·~ II .I '1 .ill ~ I ... ... II 'II .fi :. I !~ ...1 . ~ !,~ .,~ 'I ~ J ·-=· ..I ·~ tJ 1;1 .. II "'"l ,,'\. d • .... ·~ I 3: ... • J ·~ •• I -' -\1 - I =,. The Logan Plateau, a Young Physiographic Region in West Virginia, Kentucky, Virginia, and Tennessee By WILLIAM F. OUTERBRIDGE A highly dissected plateau with narrow valleys, steep slopes, narrow crested ridges, and landslides developed on flat-lying Pennsylvanian shales and subgraywacke sandstone during the past 1.5 million years U.S. GEOLOGICAL SURVEY BULLETIN 1620 DEPARTMENT OF THE INTERIOR DONALD PAUL HODEL, Secretary U.S. GEOLOGICAL SURVEY Dallas L. Peck, Director UNITED STATES GOVERNMENT PRINTING OFFICE: 1987 For sale by the Books and Open-File Reports Section, U.S. Geological Survey, Federal Center, Box 25425, Denver, CO 80225 Library of Congress Cataloging-in-Publication Data Outerbridge, William F. The Logan Plateau, a young physiographic region in West Virginia, Kentucky, Virginia, and Tennessee. (U.S. Geological Survey bulletin ; 1620) Bibliography: p. 18. Supt. of Docs. no.: I 19.3:1620 1. Geomorphology-Logan Plateau. I. Title. II. Series. QE75.B9 no. 1620 557.3 s [551.4'34'0975] 84-600132 [GB566.L6] CONTENTS Abstract 1 Introduction 1 Methods of study 3 Geomorphology 4 Stratigraphy 9 Structure 11 Surficial deposits 11 Distribution of residuum 11 Depth of weathering 11 Soils 11 Landslides 11 Derivative maps of the Logan Plateau and surrounding area 12 History of drainage development since late Tertiary time 13 Summary and conclusions 17 References cited 18 PLATES [Plates are in pocket] 1. -
8.5 X 13.5 Doublelines.P65
Cambridge University Press 978-0-521-74128-6 - Exploring the Solar System with Binoculars: A Beginner’s Guide to the Sun, Moon, and Planets Stephen James O’Meara’s Index More information Index Adams, John Couch, 96 Carrington, Richard C., 15 degree of condensation (DC) of, Agesinax, 24 Carroll, Lewis, 60 111–112 Aionwantha (Hiawatha), 45 Ceres, 70, 99–101 estimating the brightness of, Airy, George Biddell, 50, 51, 55 discovery and history as a planet, 111–112 Alcock, George, 116 99–100 In–Out method, 111 Allen, Richard Hinckley, 136 general description of, 99, Modified–Out method, 111–112 Alphonsus VI (King of Portugal), 104 100–101 experience helps in observing, 112 Andersen, Hans Christian, 92 how to find, 101 flaring in brightness, 111 Arago, Francois, 59 Chaikin, Andrew, 54 how to locate and identify, 110 Araki, Genichi, 116 Challis, James, 50 in history, relating to, 103–108 Arend, Silvio, 115 Chambers, George F., 8, 19 King David, 103 Aristotle, 65 Cheshire Cat, 60 Melville’s Moby-Dick, 107–108 Arlt, Rainer, 132 Children of God (cult), 108 Napoleon, 106 Arrehenius, Svente, 78, 79 Chinese Catalogue (Biot’s), 131–132 Shakespeare’s Julius Caesar, 103–104 Arter, T. R., 131 Cicero (Roman emperor), 77 the broadside of the comets of Asteroid Belt, 101 City of God, The, 90 1680 and 1682, 104 brightest objects in, 101–102 Collins, Peter, 116 the death of Julius Caesar, 104 asteroids Cometographia, 103 the Middle Ages, 104 2003 EH1, 131 comets, 103–117 the Old Testament?, 103 3200 Phaeton, 142 1P (Halley), 103, 109, 114–115, the whaling ship -
Shallow Crustal Composition of Mercury As Revealed by Spectral Properties and Geological Units of Two Impact Craters
Planetary and Space Science 119 (2015) 250–263 Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Shallow crustal composition of Mercury as revealed by spectral properties and geological units of two impact craters Piero D’Incecco a,n, Jörn Helbert a, Mario D’Amore a, Alessandro Maturilli a, James W. Head b, Rachel L. Klima c, Noam R. Izenberg c, William E. McClintock d, Harald Hiesinger e, Sabrina Ferrari a a Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, D-12489 Berlin, Germany b Department of Geological Sciences, Brown University, Providence, RI 02912, USA c The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA d Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80303, USA e Westfälische Wilhelms-Universität Münster, Institut für Planetologie, Wilhelm-Klemm Str. 10, D-48149 Münster, Germany article info abstract Article history: We have performed a combined geological and spectral analysis of two impact craters on Mercury: the Received 5 March 2015 15 km diameter Waters crater (106°W; 9°S) and the 62.3 km diameter Kuiper crater (30°W; 11°S). Using Received in revised form the Mercury Dual Imaging System (MDIS) Narrow Angle Camera (NAC) dataset we defined and mapped 9 October 2015 several units for each crater and for an external reference area far from any impact related deposits. For Accepted 12 October 2015 each of these units we extracted all spectra from the MESSENGER Atmosphere and Surface Composition Available online 24 October 2015 Spectrometer (MASCS) Visible-InfraRed Spectrograph (VIRS) applying a first order photometric correc- Keywords: tion. -
Genesis and Geographical Aspects of Glaciers - Vladimir M
HYDROLOGICAL CYCLE – Vol. IV - Genesis and Geographical Aspects of Glaciers - Vladimir M. Kotlyakov GENESIS AND GEOGRAPHICAL ASPECTS OF GLACIERS Vladimir M. Kotlyakov Institute of Geography, Russian Academy of Sciences, Moscow, Russia Keywords: Chionosphere, cryosphere, equilibrium line, firn line, glacial climate, glacier, glacierization, glaciosphere, ice, seasonal snow line, snow line, snow-patch Contents 1. Introduction 2. Properties of natural ice 3. Cryosphere, glaciosphere, chionosphere 4. Snow-patches and glaciers 5. Basic boundary levels of snow and ice 6. Measures of glacierization 7. Occurrence of glaciers 8. Present-day glacierization of the Arctic Glossary Bibliography Biographical Sketch Summary There exist ten crystal variants of ice and one amorphous form in Nature, however only one form ice-1 is distributed on the Earth. Ten other ice variants steadily exist only under a certain combinations of pressure, specific volume and temperature of medium, and those are not typical for our planet. The ice density is less than that of water by 9%, and owing to this water reservoirs are never totally frozen., Thus life is sustained in them during the winter time. As a rule, ice is much cleaner than water, and specific gas-ice compounds called as crystalline hydrates are found in ice. Among the different spheres surrounding our globe there are cryosphere (sphere of the cold), glaciosphere (sphere of snow and ice) and chionosphere (that part of the troposphere where the annual amount of solid precipitation exceeds their losses). The chionosphere envelopes the Earth with a shell 3 to 5 km in thickness. In the present epoch, snow and ice cover 14.2% of the planet’s surface and more than half of the land surface. -
Magnetized Impact Craters
Icarus xxx (2011) xxx–xxx Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Predicted and observed magnetic signatures of martian (de)magnetized impact craters ⇑ Benoit Langlais a, , Erwan Thébault b a CNRS UMR 6112, Université de Nantes, Laboratoire de Planétologie et Géodynamique, 2 Rue de la Houssinière, F-44000 Nantes, France b CNRS UMR 7154, Institut de Physique du Globe de Paris, Équipe de Géomagnétisme, 1 Rue Cuvier, F-75005 Paris, France article info abstract Article history: The current morphology of the martian lithospheric magnetic field results from magnetization and Received 3 May 2010 demagnetization processes, both of which shaped the planet. The largest martian impact craters, Hellas, Revised 6 January 2011 Argyre, Isidis and Utopia, are not associated with intense magnetic fields at spacecraft altitude. This is Accepted 6 January 2011 usually interpreted as locally non- or de-magnetized areas, as large impactors may have reset the mag- Available online xxxx netization of the pre-impact material. We study the effects of impacts on the magnetic field. First, a care- ful analysis is performed to compute the impact demagnetization effects. We assume that the pre-impact Keywords: lithosphere acquired its magnetization while cooling in the presence of a global, centered and mainly Mars, Surface dipolar magnetic field, and that the subsequent demagnetization is restricted to the excavation area cre- Mars, Interior Impact processes ated by large craters, between 50- and 500-km diameter. Depth-to-diameter ratio of the transient craters Magnetic fields is set to 0.1, consistent with observed telluric bodies. Associated magnetic field is computed between 100- and 500-km altitude.