Lunar 1000 Challenge List
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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]. -
University Microfilms International T U T T L E , V Ir G in Ia G R a C E
INFORMATION TO USERS This was produced from a copy of a document sent to us for microfilming. While the most advanced technological means to photograph and reproduce this document have been used, the quality is heavily dependent upon the quality of the material subm itted. The following explanation of techniques is provided to help you understand markings or notations which may appear on this reproduction. 1. The sign or “target” for pages apparently lacking from the document photographed is “Missing Page(s)”. If it was possible to obtain the missing page(s) or section, they are spliced into the film along with adjacent pages. This may have necessitated cutting through an image and duplicating adjacent pages to assure you of complete continuity. 2. When an image on the film is obliterated with a round black mark it is an indication that the film inspector noticed either blurred copy because of movement during exposure, or duplicate copy. Unless we meant to delete copyrighted materials that should not have been filmed, you will find a good image of the page in the adjacent frame. 3. When a map, drawing or chart, etc., is part of the material being photo graphed the photographer has followed a definite method in “sectioning” the material. It is customary to begin filming at the upper left hand corner of a large sheet and to continue from left to right in equal sections with small overlaps. If necessary, sectioning is continued again-beginning below the first row and continuing on until complete. 4. For any illustrations that cannot be reproduced satisfactorily by xerography, photographic prints can be purchased at additional cost and tipped into your xerographic copy. -
University of Cincinnati
UNIVERSITY OF CINCINNATI Date:__7/30/07_________________ I, __ MUNISH GUPTA_____________________________________, hereby submit this work as part of the requirements for the degree of: DOCTORATE OF PHILOSOPHY (Ph.D) in: MATERIALS SCIENCE AND ENGINEERING It is entitled: LOW-PRESSURE AND ATMOSPHERIC PRESSURE PLASMA POLYMERIZED SILICA-LIKE FILMS AS PRIMERS FOR ADHESIVE BONDING OF ALUMINUM This work and its defense approved by: Chair: __Dr. F. JAMES BOERIO ___ ______ __Dr. GREGORY BEAUCAGE __ ___ __ __Dr. RODNEY ROSEMAN _____ ___ __Dr. JUDE IROH _ _____________ _______________________________ LOW-PRESSURE AND ATMOSPHERIC PRESSURE PLASMA POLYMERIZED SILICA-LIKE FILMS AS PRIMERS FOR ADHESIVE BONDING OF ALUMINUM A dissertation submitted to the Division of Research and Advanced Studies of the University of Cincinnati in partial fulfillment of the requirements for the degree of DOCTORATE OF PHILOSOPHY (Ph.D) in the Department of Chemical and Material Engineering of the College of Engineering 2007 by Munish Gupta M.S., University of Cincinnati, 2005 B.E., Punjab Technical University, India, 2000 Committee Chair: Dr. F. James Boerio i ABSTRACT Plasma processes, including plasma etching and plasma polymerization, were investigated for the pretreatment of aluminum prior to structural adhesive bonding. Since native oxides of aluminum are unstable in the presence of moisture at elevated temperature, surface engineering processes must usually be applied to aluminum prior to adhesive bonding to produce oxides that are stable. Plasma processes are attractive for surface engineering since they take place in the gas phase and do not produce effluents that are difficult to dispose off. Reactive species that are generated in plasmas have relatively short lifetimes and form inert products. -
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, -
Testing Hypotheses for the Origin of Steep Slope of Lunar Size-Frequency Distribution for Small Craters
CORE Metadata, citation and similar papers at core.ac.uk Provided by Springer - Publisher Connector Earth Planets Space, 55, 39–51, 2003 Testing hypotheses for the origin of steep slope of lunar size-frequency distribution for small craters Noriyuki Namiki1 and Chikatoshi Honda2 1Department of Earth and Planetary Sciences, Kyushu University, Hakozaki 6-10-1, Higashi-ku, Fukuoka 812-8581, Japan 2The Institute of Space and Astronautical Science, Yoshinodai 3-1-1, Sagamihara 229-8510, Japan (Received June 13, 2001; Revised June 24, 2002; Accepted January 6, 2003) The crater size-frequency distribution of lunar maria is characterized by the change in slope of the population between 0.3 and 4 km in crater diameter. The origin of the steep segment in the distribution is not well understood. Nonetheless, craters smaller than a few km in diameter are widely used to estimate the crater retention age for areas so small that the number of larger craters is statistically insufficient. Future missions to the moon, which will obtain high resolution images, will provide a new, large data set of small craters. Thus it is important to review current hypotheses for their distributions before future missions are launched. We examine previous and new arguments and data bearing on the admixture of endogenic and secondary craters, horizontal heterogeneity of the substratum, and the size-frequency distribution of the primary production function. The endogenic crater and heterogeneous substratum hypotheses are seen to have little evidence in their favor, and can be eliminated. The primary production hypothesis fails to explain a wide variation of the size-frequency distribution of Apollo panoramic photographs. -
The Archaeology and Heritage of the Sudanese Red Sea Region: Importance, Findings, and Challenges
The Archaeology and Heritage of the Sudanese Red Sea Region: Importance, Findings, and Challenges AHMED ADAM Head Department of Archaeology - University of Khartoum Director of the Red Sea Project for Archaeological Research Abstract This paper seeks to shed a high light on the archaeological sites discovered in the area of Suakin, Arkaweet, and Sinkat as a part of the project of the department of Archaeology ß university of Khartoum, so, the archaeological sites discovered in this region belong to different periods such as Pre-Historic, Medieval, Islamic, and others are unknown, which means that the region used to link the Red Sea Cultures with those on the central Sudan and Egypt far north and Eretria in the east. Through this study I am also seeking to evaluate the field work (Archaeological and Ethnographic) conducted in the area of Arkaweet and Sinkat town, and Suakin port, then to put a plan for the managing and protecting the archaeologi- cal sites and ethnographic materials. Therefore I will follow or apply a number of approaches in this study such as description, survey analysis of the sites and its contents as well a comparison will be made between the results of the present study with the results of the previous studies in the field of archeology and ethnography conducted on other sites in the Sudanese Red Sea Region. The historical sources will also be compared with the study findings. Keywords Red Sea, Archaeology, Heritage, Sudan, Survey, Suakin 188 1. INTRODUCTION The Red Sea lies in an ideal geographical location between eastern and west- ern seas in general, and between the Mediterranean Sea and the Indian Ocean in particular. -
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. -
Compositional and Mineralogical Characteristics of Archimedes Crater Region Using Chandrayaan – 1 M3 Data
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1040.pdf COMPOSITIONAL AND MINERALOGICAL CHARACTERISTICS OF ARCHIMEDES CRATER REGION USING CHANDRAYAAN – 1 M3 DATA. P. R. Kumaresan1 and J. Saravanavel2, 1Research Scholar, 2Assistant Professor, Department of Remote Sensing, Bharathidasan University, Tiruchirappalli-23, Tamil Nadu, India, email: [email protected], [email protected] Introduction: The Earth’s natural satellite the tometry corrected reflectance data captured during the moon is nearest celestial body appears brightest object OP1B optical period. in our night sky. Moon surfaces are composed of dark and light areas. The dark areas are called Maria which is made up of basaltic terrain and light areas are high- lands mostly made up of Anorthositic rocks. The moon surface is littered with craters, which are formed when meteors hit its surface. To understand the evolution, geological process of the moon it is important to study the surface composition and minerals present in crustal surface. In this regard, in our study, we have attempted to map the minerals and surface composition of Archi- medes crater region. Study area: Archimedes crater is a large impact crater located on the eastern edges of the Mare Imbri- um of near side moon (29.7° N, 4.0° W). The diameter of the crater is 83 km with smooth floor flooded (1) with mare basalt and lack of a central peak. The rim (2) has a significant outer rampart brightened with ejecta (3) and the some portion of a terraced inner wall. Ar- chimedes Crater is named for the Greek mathematician Archimedes, who made many mathematical discoveries in the 200 B.C [1, 2]. -
The Agatharchides Plateau (60 X 45Km) Is Classified As an Intrusive Lunar Mega Plateau, Similar to the Gardner Mega Plateau
The Agatharchides Plateau (60 x 45km) is classified as an intrusive lunar Mega Plateau, similar to the Gardner Mega Plateau. The composition of the rocks is similar to the Gruithuisen domes and the mountain Mons Hansteen. On the eastern edge of the plateau is an extremely narrow - unnamed - rille. Unofficially this structure is named "The Helmet" because its shape is reminiscent of the helmets of the famous Star Wars movies. The Hortensius Domes are a classic small-scale lunar field of 7 lunar effusive shield volcanoes with diameters of 10 to 15 kilometers and small summit calderas. In this region between Kepler in the west and Copernicus in the east are around 2 dozen other domes, e.g. west of Milichius the great Dome Milichius Phi. Heinzel (68 x 19km) has, due to its shape, the nickname "Peanut crater". It is the result of a superposition of 3 impacts over a total length of nearly 70 km. Hesiodus A (14 km) is the largest and most easily observable double concentric crater on the front of the moon. Copernicus measures roughly 100 kilometers in diameter and is the prototype of a very young, complex crater. He has clearly terraced crater walls and the central mountains are divided into two parts. The crater floor is partially smooth and flat (covered with molten ejecta), on the opposite side there is a hilly region. The crater floor is 3.8 kilometers beneath the crater walls which rises less than 1 km above the surrounding landscape. The longest rays of the young ray system can be tracked up to a distance of 800 km. -
THE STUDY of SATURN's RINGS 1 Thesis Presented for the Degree Of
1 THE STUDY OF SATURN'S RINGS 1610-1675, Thesis presented for the Degree of Doctor of Philosophy in the Field of History of Science by Albert Van Haden Department of History of Science and Technology Imperial College of Science and Teohnology University of London May, 1970 2 ABSTRACT Shortly after the publication of his Starry Messenger, Galileo observed the planet Saturn for the first time through a telescope. To his surprise he discovered that the planet does.not exhibit a single disc, as all other planets do, but rather a central disc flanked by two smaller ones. In the following years, Galileo found that Sa- turn sometimes also appears without these lateral discs, and at other times with handle-like appendages istead of round discs. These ap- pearances posed a great problem to scientists, and this problem was not solved until 1656, while the solution was not fully accepted until about 1670. This thesis traces the problem of Saturn, from its initial form- ulation, through the period of gathering information, to the final stage in which theories were proposed, ending with the acceptance of one of these theories: the ring-theory of Christiaan Huygens. Although the improvement of the telescope had great bearing on the problem of Saturn, and is dealt with to some extent, many other factors were in- volved in the solution of the problem. It was as much a perceptual problem as a technical problem of telescopes, and the mental processes that led Huygens to its solution were symptomatic of the state of science in the 1650's and would have been out of place and perhaps impossible before Descartes. -
Glossary of Lunar Terminology
Glossary of Lunar Terminology albedo A measure of the reflectivity of the Moon's gabbro A coarse crystalline rock, often found in the visible surface. The Moon's albedo averages 0.07, which lunar highlands, containing plagioclase and pyroxene. means that its surface reflects, on average, 7% of the Anorthositic gabbros contain 65-78% calcium feldspar. light falling on it. gardening The process by which the Moon's surface is anorthosite A coarse-grained rock, largely composed of mixed with deeper layers, mainly as a result of meteor calcium feldspar, common on the Moon. itic bombardment. basalt A type of fine-grained volcanic rock containing ghost crater (ruined crater) The faint outline that remains the minerals pyroxene and plagioclase (calcium of a lunar crater that has been largely erased by some feldspar). Mare basalts are rich in iron and titanium, later action, usually lava flooding. while highland basalts are high in aluminum. glacis A gently sloping bank; an old term for the outer breccia A rock composed of a matrix oflarger, angular slope of a crater's walls. stony fragments and a finer, binding component. graben A sunken area between faults. caldera A type of volcanic crater formed primarily by a highlands The Moon's lighter-colored regions, which sinking of its floor rather than by the ejection of lava. are higher than their surroundings and thus not central peak A mountainous landform at or near the covered by dark lavas. Most highland features are the center of certain lunar craters, possibly formed by an rims or central peaks of impact sites.