Apollo 17 Lunar Photography
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Smithsonian Institution Archives (SIA)
SMITHSONIAN OPPORTUNITIES FOR RESEARCH AND STUDY 2020 Office of Fellowships and Internships Smithsonian Institution Washington, DC The Smithsonian Opportunities for Research and Study Guide Can be Found Online at http://www.smithsonianofi.com/sors-introduction/ Version 2.0 (Updated January 2020) Copyright © 2020 by Smithsonian Institution Table of Contents Table of Contents .................................................................................................................................................................................................. 1 How to Use This Book .......................................................................................................................................................................................... 1 Anacostia Community Museum (ACM) ........................................................................................................................................................ 2 Archives of American Art (AAA) ....................................................................................................................................................................... 4 Asian Pacific American Center (APAC) .......................................................................................................................................................... 6 Center for Folklife and Cultural Heritage (CFCH) ...................................................................................................................................... 7 Cooper-Hewitt, -
Geologic Structure of Shallow Maria
NASA CR. Photo Data Analysis S-221 NASA Contract NAS 9-13196 GEOLOGIC STRUCTURE OF SHALLOW MARIA Rene' A. De Hon, Principal Investigator John A. Waskom, Co-Investigator (NASA-CR-lq7qoo GEOLOGIC STahJCTUnF OF N76-17001 ISBALOW M1BIA-'(Arkansas Uni.v., mHiticelio.) 96 p BC $5.00' CSCL O3B Unclas G3/91, 09970- University of Arkansas at Monticello Monticello, Arkansas December 1975 Photo Data Analysis S-221 NASA Contract NAS 9-13196 GEOLOGIC STRUCTURE OF SHALLOW MARIA Rene' A. De Hon, Principal Investigator I John A. Waskom, Co-Investigator Un-iversity-of Arkansas-:at-.Monticl o Monticello, Arkansas December 1975 ABSTRACT Isopach maps and structural contour maps of the 0 0 eastern mare basins (30 N to 30 OS; 00 to 100 E) are constructed from measurements of partially buried craters. The data, which are sufficiently scattered to yield gross thickness variations, are restricted to shallow maria with less than 1500-2000 m of mare basalts. The average thickness of b-asalt in the irregular maria is between 200 and 400 m. Multiringed mascon basins are filled to various levels. The Serenitatis and Crisium basins have deeply flooded interiors and extensively flooded shelves. Mare basalts in the Nectaris basin fill only the innermost basin, and mare basalts in the Smythii basin occupy a small portion of the basin floor. Sinus Amoris, Mare Spumans, and Mare Undarum are partially filled troughs concentric to large circular basins. The Tranquillitatis and Fecunditatis are composite depressions containing basalts which flood degraded circular basins and adjacent terrain modified by the formation of nearby cir cular basins. -
Radar Remote Sensing of Pyroclastic Deposits in the Southern Mare Serenitatis and Mare Vaporum Regions of the Moon Lynn M
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 114, E11004, doi:10.1029/2009JE003406, 2009 Click Here for Full Article Radar remote sensing of pyroclastic deposits in the southern Mare Serenitatis and Mare Vaporum regions of the Moon Lynn M. Carter,1 Bruce A. Campbell,1 B. Ray Hawke,2 Donald B. Campbell,3 and Michael C. Nolan4 Received 21 April 2009; revised 12 July 2009; accepted 3 August 2009; published 5 November 2009. [1] We use polarimetric radar observations to study the distribution, depth, and embedded rock abundance of nearside lunar pyroclastic deposits. Radar images were obtained for Mare Vaporum and the southern half of Mare Serenitatis; the imaged areas contain the large Rima Bode, Mare Vaporum, Sulpicius Gallus, and Taurus-Littrow pyroclastic deposits. Potential pyroclastic deposits at Rima Hyginus crater, the Tacquet Formation, and a dome in Mare Vaporum are also included. Data were acquired at S band (12.6 cm wavelength) using Arecibo Observatory and the Green Bank Telescope in a bistatic configuration. The S band images have resolutions between 20 and 100 m/pixel. The pyroclastic deposits appear dark to the radar and have low circular polarization ratios at S band wavelengths because they are smooth, easily penetrable by radar waves, and generally contain few embedded blocks. Changes in circular polarization ratio (CPR) across some of the pyroclastic deposits show areas with increased rock abundance as well as deposits that are shallower. Radar backscatter and CPR maps are used to identify fine-grained mantling deposits in cases where optical and near-infrared data are ambiguous about the presence of pyroclastics. -
Tracing Subduction Zone Processes with Magnesium Isotopes
Tracing subduction zone processes with magnesium isotopes Yan Hu A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy University of Washington 2018 Reading Committee: Fang-Zhen Teng, Chair Bruce K. Nelson Ronald S. Sletten Program Authorized to Offer Degree: Earth and Space Sciences © Copyright 2018 Yan Hu University of Washington Abstract Tracing subduction zone processes with magnesium isotopes Yan Hu Chair of the Supervisory Committee: Professor Fang-Zhen Teng Department of Earth and Space Sciences Subduction and recycling of oceanic plates change the chemical composition of mantle and affect its physical properties, thereby modulating Earth’s dynamics. Stable Mg isotopes (δ26Mg) can trace this recycling process as crustal materials are highly fractionated compared to the average mantle composition. This dissertation focuses on Mg isotope fractionation during subduction-related processes and the consequent mantle heterogeneity. The dissertation first compares inconsistent δ26Mg values of San Carlos peridotitic olivines that are published by several laboratories. We analyzed mineral grains from two San Carlos peridotites with disparate lithologies and determined that all mineral phases have indistinguishable δ26Mg values to within 0.07‰. With analytical precision and accuracy being confirmed, the significance of anomalous δ26Mg values can be understood in the context of mantle heterogeneity. The next paper investigates the Mg isotopic heterogeneity in mantle pyroxenites that have formed by multi-stage interactions between peridotites and melts with diverse origins. Pyroxenites formed by reaction with melts derived from subducted oceanic crust and carbonate sediments are shown to have variable δ26Mg values (−1.51‰ to −0.10‰). In contrast, pyroxenites that are formed by reaction with silicate melts from deep mantle has δ26Mg values similar to common mantle peridotites. -
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, -
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. -
Cratering Flow Fields
Proc. Lunar Planet. Sci. Conj. !Ith (1980), p. 2347-2378. Printed in the United States of America 1980LPSC...11.2347C Cratering flow fields: Implications for the excavation and transient expansion stages of crater formation Steven Kent Croft Lunar and Planetary Institute, 3303 NASA Road I, Houston, Texas 77058 Abstract-A Maxwell Z-model cratering flow field originating at non-zero depths-of-burst has been used to calculate theoretical depths and volumes of excavation, hinge radii, ejection angles, and transient structural rim uplifts for comparison with experimental and field data from impact and explosion craters. The model flow fields match the observed data well for values of Z between 2.5 and 3.0 for both explosion and impact craters, and effective depths-of-burst near one projectile di- ameter for impacts. The model flow field is therefore inferred to be a reasonable first-order quantitative approximation for several important crater structures, and to embody the important qualitative fea- tures of impact and explosion cratering flows. Formation of a hinge about which the coherent ejecta flap rotates at the rim of the transient crater divides material in the flow field into ejected and down- ward and outward-driven portions. Ejected material originates from an excavation cavity which has a geometry distinct from the transient crater. The excavation cavity and transient crater have the same diameter, D1c, but the depth of the excavation cavity is -0. I D1c, or about one-third of the transient crater depth, and, in the case of simple bowl-shaped craters, about one-half the depth of the final apparent crater. -
October 2006
OCTOBER 2 0 0 6 �������������� http://www.universetoday.com �������������� TAMMY PLOTNER WITH JEFF BARBOUR 283 SUNDAY, OCTOBER 1 In 1897, the world’s largest refractor (40”) debuted at the University of Chica- go’s Yerkes Observatory. Also today in 1958, NASA was established by an act of Congress. More? In 1962, the 300-foot radio telescope of the National Ra- dio Astronomy Observatory (NRAO) went live at Green Bank, West Virginia. It held place as the world’s second largest radio scope until it collapsed in 1988. Tonight let’s visit with an old lunar favorite. Easily seen in binoculars, the hexagonal walled plain of Albategnius ap- pears near the terminator about one-third the way north of the south limb. Look north of Albategnius for even larger and more ancient Hipparchus giving an almost “figure 8” view in binoculars. Between Hipparchus and Albategnius to the east are mid-sized craters Halley and Hind. Note the curious ALBATEGNIUS AND HIPPARCHUS ON THE relationship between impact crater Klein on Albategnius’ southwestern wall and TERMINATOR CREDIT: ROGER WARNER that of crater Horrocks on the northeastern wall of Hipparchus. Now let’s power up and “crater hop”... Just northwest of Hipparchus’ wall are the beginnings of the Sinus Medii area. Look for the deep imprint of Seeliger - named for a Dutch astronomer. Due north of Hipparchus is Rhaeticus, and here’s where things really get interesting. If the terminator has progressed far enough, you might spot tiny Blagg and Bruce to its west, the rough location of the Surveyor 4 and Surveyor 6 landing area. -
Water on the Moon, III. Volatiles & Activity
Water on The Moon, III. Volatiles & Activity Arlin Crotts (Columbia University) For centuries some scientists have argued that there is activity on the Moon (or water, as recounted in Parts I & II), while others have thought the Moon is simply a dead, inactive world. [1] The question comes in several forms: is there a detectable atmosphere? Does the surface of the Moon change? What causes interior seismic activity? From a more modern viewpoint, we now know that as much carbon monoxide as water was excavated during the LCROSS impact, as detailed in Part I, and a comparable amount of other volatiles were found. At one time the Moon outgassed prodigious amounts of water and hydrogen in volcanic fire fountains, but released similar amounts of volatile sulfur (or SO2), and presumably large amounts of carbon dioxide or monoxide, if theory is to be believed. So water on the Moon is associated with other gases. Astronomers have agreed for centuries that there is no firm evidence for “weather” on the Moon visible from Earth, and little evidence of thick atmosphere. [2] How would one detect the Moon’s atmosphere from Earth? An obvious means is atmospheric refraction. As you watch the Sun set, its image is displaced by Earth’s atmospheric refraction at the horizon from the position it would have if there were no atmosphere, by roughly 0.6 degree (a bit more than the Sun’s angular diameter). On the Moon, any atmosphere would cause an analogous effect for a star passing behind the Moon during an occultation (multiplied by two since the light travels both into and out of the lunar atmosphere). -
Landed Science at a Lunar Crustal Magnetic Anomaly
Landed Science at a Lunar Crustal Magnetic Anomaly David T. Blewett, Dana M. Hurley, Brett W. Denevi, Joshua T.S. Cahill, Rachel L. Klima, Jeffrey B. Plescia, Christopher P. Paranicas, Benjamin T. Greenhagen, Lauren Jozwiak, Brian A. Anderson, Haje Korth, George C. Ho, Jorge I. Núñez, Michael I. Zimmerman, Pontus C. Brandt, Sabine Stanley, Joseph H. Westlake, Antonio Diaz-Calderon, R. Ter ik Daly, and Jeffrey R. Johnson Space Science Branch, Johns Hopkins University Applied Physics Lab, USA Lunar Science for Landed Missions Workshop – January, 2018 1 Lunar Magnetic Anomalies • The lunar crust contains magnetized areas, a few tens to several hundred kilometers across, known as "magnetic anomalies". • The crustal fields are appreciable: Strongest anomalies are ~10-20 nT at 30 km altitude, perhaps a few hundred to 1000 nT at the surface. Lunar Prospector magnetometer Btot map (Richmond & Hood 2008 JGR) over LROC WAC 689-nm mosaic 2 Lunar Magnetic Anomalies: Formation Hypotheses • Magnetized basin ejecta: ambient fields amplified by compression as impact-generated plasma converged on the basin antipode (Hood and co-workers) Lunar Prospector magnetometer Btot (Richmond & Hood 2008 JGR) over LROC WAC 689- nm mosaic 3 Lunar Magnetic Anomalies: Formation Hypotheses • Magnetized basin ejecta: ambient fields amplified by compression as impact-generated plasma converged on the basin antipode (Hood and co-workers) • Magnetic field impressed on the surface by plasma interactions when a cometary coma struck the Moon (Schultz) Lunar Prospector magnetometer Btot (Richmond & Hood 2008 JGR) over LROC WAC 689- nm mosaic 4 Lunar Magnetic Anomalies: Formation Hypotheses • Magnetized basin ejecta: ambient fields amplified by compression as impact-generated plasma converged on the basin antipode (Hood and co-workers) • Magnetic field impressed on the surface by plasma interactions when a cometary coma struck the Moon (Schultz) • Magmatic intrusion or impact melt magnetized in an early lunar dynamo field (e.g., Purucker et al. -
South Pole-Aitken Basin
Feasibility Assessment of All Science Concepts within South Pole-Aitken Basin INTRODUCTION While most of the NRC 2007 Science Concepts can be investigated across the Moon, this chapter will focus on specifically how they can be addressed in the South Pole-Aitken Basin (SPA). SPA is potentially the largest impact crater in the Solar System (Stuart-Alexander, 1978), and covers most of the central southern farside (see Fig. 8.1). SPA is both topographically and compositionally distinct from the rest of the Moon, as well as potentially being the oldest identifiable structure on the surface (e.g., Jolliff et al., 2003). Determining the age of SPA was explicitly cited by the National Research Council (2007) as their second priority out of 35 goals. A major finding of our study is that nearly all science goals can be addressed within SPA. As the lunar south pole has many engineering advantages over other locations (e.g., areas with enhanced illumination and little temperature variation, hydrogen deposits), it has been proposed as a site for a future human lunar outpost. If this were to be the case, SPA would be the closest major geologic feature, and thus the primary target for long-distance traverses from the outpost. Clark et al. (2008) described four long traverses from the center of SPA going to Olivine Hill (Pieters et al., 2001), Oppenheimer Basin, Mare Ingenii, and Schrödinger Basin, with a stop at the South Pole. This chapter will identify other potential sites for future exploration across SPA, highlighting sites with both great scientific potential and proximity to the lunar South Pole. -
Apollo 17 Index: 70 Mm, 35 Mm, and 16 Mm Photographs
General Disclaimer One or more of the Following Statements may affect this Document This document has been reproduced from the best copy furnished by the organizational source. It is being released in the interest of making available as much information as possible. This document may contain data, which exceeds the sheet parameters. It was furnished in this condition by the organizational source and is the best copy available. This document may contain tone-on-tone or color graphs, charts and/or pictures, which have been reproduced in black and white. This document is paginated as submitted by the original source. Portions of this document are not fully legible due to the historical nature of some of the material. However, it is the best reproduction available from the original submission. Produced by the NASA Center for Aerospace Information (CASI) Preparation, Scanning, Editing, and Conversion to Adobe Portable Document Format (PDF) by: Ronald A. Wells University of California Berkeley, CA 94720 May 2000 A P O L L O 1 7 I N D E X 7 0 m m, 3 5 m m, A N D 1 6 m m P H O T O G R A P H S M a p p i n g S c i e n c e s B r a n c h N a t i o n a l A e r o n a u t i c s a n d S p a c e A d m i n i s t r a t i o n J o h n s o n S p a c e C e n t e r H o u s t o n, T e x a s APPROVED: Michael C .