Apollo 17 Index: 70 Mm, 35 Mm, and 16 Mm Photographs
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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. -
January 2019 Cardanus & Krafft
A PUBLICATION OF THE LUNAR SECTION OF THE A.L.P.O. EDITED BY: Wayne Bailey [email protected] 17 Autumn Lane, Sewell, NJ 08080 RECENT BACK ISSUES: http://moon.scopesandscapes.com/tlo_back.html FEATURE OF THE MONTH – JANUARY 2019 CARDANUS & KRAFFT Sketch and text by Robert H. Hays, Jr. - Worth, Illinois, USA September 24, 2018 04:40-05:04 UT, 15 cm refl, 170x, seeing 7/10, transparence 6/6. I drew these craters and vicinity on the night of Sept. 23/24, 2018. The moon was about 22 hours before full. This area is in far western Oceanus Procellarum, and was favorably placed for observation that night. Cardanus is the southern one of this pair and is of moderate depth. Krafft to the north is practically identical in size, and is perhaps slightly deeper. Neither crater has a central peak. Several small craters are near and within Krafft. The crater just outside the southeast rim of Krafft is Krafft E, and Krafft C is nearby within Krafft. The small pit to the west is Krafft K, and Krafft D is between Krafft and Cardanus. Krafft C, D and E are similar sized, but K is smaller than these. A triangular-shaped swelling protrudes from the north side of Krafft. The tiny pit, even smaller than Krafft K, east of Cardanus is Cardanus E. There is a dusky area along the southwest side of Cardanus. Two short dark strips in this area may be part of the broken ring Cardanus R as shown on the. Lunar Quadrant map. -
General Disclaimer One Or More of the Following Statements May Affect
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) ^i e I !emote sousing sad eeolegio Studies of the llaistary Crusts Bernard Ray Hawke Prince-1 Investigator a EL r Z^ .99 University of Hawaii Hawaii Institute of Geophysics Planetary Geosciences Division Honolulu, Hawaii 96822 ^y 1i i W. December 1983 (NASA —CR-173215) REMOTE SENSING AND N84-17092 GEOLOGIC STUDIES OF THE PLANETARY CRUSTS Final Report ( Hawaii Inst. of Geophysics) 14 p HC A02/MF 101 CSCL 03B Unclas G3/91 11715 Gy -2- ©R1GNAL OF POOR QUALITY Table of Contents Page I. Remote Sensing and Geologic Studies cf Volcanic Deposits . • . 3 A. Spectral reflectance studies of dark-haloed craters. • . 3 B. Remote s^:sing studies of regions which were sites of ancient volcanisa . 3 C. [REEP basalt deposits in the Imbrium Region. -
Imagining Outer Space Also by Alexander C
Imagining Outer Space Also by Alexander C. T. Geppert FLEETING CITIES Imperial Expositions in Fin-de-Siècle Europe Co-Edited EUROPEAN EGO-HISTORIES Historiography and the Self, 1970–2000 ORTE DES OKKULTEN ESPOSIZIONI IN EUROPA TRA OTTO E NOVECENTO Spazi, organizzazione, rappresentazioni ORTSGESPRÄCHE Raum und Kommunikation im 19. und 20. Jahrhundert NEW DANGEROUS LIAISONS Discourses on Europe and Love in the Twentieth Century WUNDER Poetik und Politik des Staunens im 20. Jahrhundert Imagining Outer Space European Astroculture in the Twentieth Century Edited by Alexander C. T. Geppert Emmy Noether Research Group Director Freie Universität Berlin Editorial matter, selection and introduction © Alexander C. T. Geppert 2012 Chapter 6 (by Michael J. Neufeld) © the Smithsonian Institution 2012 All remaining chapters © their respective authors 2012 All rights reserved. No reproduction, copy or transmission of this publication may be made without written permission. No portion of this publication may be reproduced, copied or transmitted save with written permission or in accordance with the provisions of the Copyright, Designs and Patents Act 1988, or under the terms of any licence permitting limited copying issued by the Copyright Licensing Agency, Saffron House, 6–10 Kirby Street, London EC1N 8TS. Any person who does any unauthorized act in relation to this publication may be liable to criminal prosecution and civil claims for damages. The authors have asserted their rights to be identified as the authors of this work in accordance with the Copyright, Designs and Patents Act 1988. First published 2012 by PALGRAVE MACMILLAN Palgrave Macmillan in the UK is an imprint of Macmillan Publishers Limited, registered in England, company number 785998, of Houndmills, Basingstoke, Hampshire RG21 6XS. -
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. -
Annual Report, Fiscal Year 1965
1965 TECHNICAL HIGHLIGHTS OF THE NATIONAL BUREAU OF STANDARDS Annual Report for: INSTITUTE FOR BASIC STANDARDS INSTITUTE FOR MATERIALS RESEARCH INSTITUTE FOR APPLIED TECHNOLOGY CENTRAL RADIO PROPAGATION LABORATORY n UNITED STATES DEPARTMENT OF COMMERCE John T. Connor, Secretary J. Herbert Hollomon, Assistant Secretary for Science and Technology NATIONAL BUREAU OF STANDARDS A. V. Astin, Director 1965 Technical Highlights of the National Bureau of Standards Annual Report, Fiscal Year 1965 May 1966 Miscellaneous Publication 279 For sale by the Superintendent of Documents, U.S. Government Printing Office Washington, D. C, 20402 — Price 65 cents Library of Congress Catalog Card Number: 6-23979 CONTENTS THE DIRECTOR'S STATEMENT _ 1 NBS—An Evolving Institution 1 Management Progress 3 NBS As a Scientific Laboratory 5 INSTITUTE FOR BASIC STANDARDS 11 Physical Quantities, Constants, and Calibration Services 12 International Base L nits 13 Length. Mass. Frequency and Time. Temperature. Luminous Intensity. Electric Current. Mechanical Quantities 19 Force. Pressure. Vacuum. Electrical Quantities—DC 24 Resistance Ratios. Voltage. Current Ratio Standards. New Compensated Current Comparator. Absolute Electrical Meas- urements. AC-DC Transfer Standards. Voltage Ratio Detector for Millivolt Signals. Electrical Quantities—Radio 25 Low-Frequency Calibration. High-Frequency Electrical Stand- ards. High-Frequency Impedance Standards. High-Frequency Calibrations. Microwave Standards. Microwave Calibrations. Photometric and Radiometric Quantities 30 Ionizing Radiations 32 Engineering Measurement and Standards 36 Phyical Properties 39 National Standard Reference Data System 40 Nuclear Data. Atomic and Molecular Data. Solid State Data. Thermodynamics and Transport Data. Chemical Kinetics. Col- loid and Surface Properties. Information Services. Measurement 48 Nuclear Properties. Atomic and Molecular Properties. Solid State Properties. -
Annual Report 2017
Koninklijke Sterrenwacht van België Observatoire royal de Belgique Royal Observatory of Belgium Jaarverslag 2017 Rapport Annuel 2017 Annual Report 2017 Cover illustration: Above: One billion star map of our galaxy created with the optical telescope of the satellite Gaia (Credit: ESA/Gaia/DPAC). Below: Three armillary spheres designed by Jérôme de Lalande in 1775. Left: the spherical sphere; in the centre: the geocentric model of our solar system (with the Earth in the centre); right: the heliocentric model of our solar system (with the Sun in the centre). Royal Observatory of Belgium - Annual Report 2017 2 De activiteiten beschreven in dit verslag werden ondersteund door Les activités décrites dans ce rapport ont été soutenues par The activities described in this report were supported by De POD Wetenschapsbeleid De Nationale Loterij Le SPP Politique Scientifique La Loterie Nationale The Belgian Science Policy The National Lottery Het Europees Ruimtevaartagentschap De Europese Gemeenschap L’Agence Spatiale Européenne La Communauté Européenne The European Space Agency The European Community Het Fonds voor Wetenschappelijk Onderzoek – Le Fonds de la Recherche Scientifique Vlaanderen Royal Observatory of Belgium - Annual Report 2017 3 Table of contents Preface .................................................................................................................................................... 6 Reference Systems and Planetology ...................................................................................................... -
Pro.Ffress D &Dentsdc Raddo
Pro.ffress d_ &dentSdc Raddo FIFTEENTH GENERAL ASSEMBLY OF THE INTERNATIONAL SCIENTIFIC RADIO UNION September 5-15, 1966 Munich, Germany REPORT OF THE U.S.A. NATIONAL COMMITTEE OF THE INTERNATIONAL SCIENTIFIC RADIO UNION Publication 1468 NATIONAL ACADEMY OF SCIENCES NATIONAL RESEARCH COUNCIL Washington, D.C. 1966 Library of Congress Catalog Card No. 55-31605 Available from Printing and Publishing Office National Academy of Sciences 2101 Constitution Avenue Washington, D.C. 20418 Price: $10.00 October28,1966 Dear Dr. Seitz: I ampleasedto transmitherewitha full report to the NationalAcademy of Sciences--NationalResearchCouncil,onthe 15thGeneralAssemblyof URSIwhichwasheldin Munich,September5-15, 1966. TheUnitedStatesNationalCommitteeof URSIhasparticipatedin the affairs of the Unionfor forty-five years. It hashadmuchinfluenceonthe Unionas,.for example,in therecent creationof a Commissiononthe Mag- netosphere.ThisnewCommission,whichis nowvery strong,demonstrates the ability of theUnion,oneof ICSU'sthree oldest,to respondto the changingneedsof its field. AlthoughtheUnitedStatessendsthelargest delegationsof anycountry to the GeneralAssembliesof URSI,theyare neverthelessrelatively small becauseof thestrict mannerin whichURSIcontrolsthe size of its Assem- blies. This is donein order to preventineffectivenessthroughuncontrolled participationbyvery largenumbersof delegates.Accordingly,our delega- tions are carefully selected,andcomprisepeoplequalifiedto prepareand presentour NationalReportto the Assembly.Thepre-Assemblyreport is a report of progressin -
Mighty Eagle: the Development and Flight Testing of an Autonomous Robotic Lander Test Bed
Mighty Eagle: The Development and Flight Testing of an Autonomous Robotic Lander Test Bed Timothy G. McGee, David A. Artis, Timothy J. Cole, Douglas A. Eng, Cheryl L. B. Reed, Michael R. Hannan, D. Greg Chavers, Logan D. Kennedy, Joshua M. Moore, and Cynthia D. Stemple PL and the Marshall Space Flight Center have been work- ing together since 2005 to develop technologies and mission concepts for a new generation of small, versa- tile robotic landers to land on airless bodies, including the moon and asteroids, in our solar system. As part of this larger effort, APL and the Marshall Space Flight Center worked with the Von Braun Center for Science and Innovation to construct a prototype monopropellant-fueled robotic lander that has been given the name Mighty Eagle. This article provides an overview of the lander’s architecture; describes the guidance, navi- gation, and control system that was developed at APL; and summarizes the flight test program of this autonomous vehicle. INTRODUCTION/PROJECT BACKGROUND APL and the Marshall Space Flight Center (MSFC) technology risk-reduction efforts, illustrated in Fig. 1, have been working together since 2005 to develop have been performed to explore technologies to enable technologies and mission concepts for a new genera- low-cost missions. tion of small, autonomous robotic landers to land on As part of this larger effort, MSFC and APL also airless bodies, including the moon and asteroids, in our worked with the Von Braun Center for Science and solar system.1–9 This risk-reduction effort is part of the Innovation (VCSI) and several subcontractors to con- Robotic Lunar Lander Development Project (RLLDP) struct the Mighty Eagle, a prototype monopropellant- that is directed by NASA’s Planetary Science Division, fueled robotic lander. -
Deep Carbon Emissions from Volcanoes Michael R
Reviews in Mineralogy & Geochemistry Vol. 75 pp. 323-354, 2013 11 Copyright © Mineralogical Society of America Deep Carbon Emissions from Volcanoes Michael R. Burton Istituto Nazionale di Geofisica e Vulcanologia Via della Faggiola, 32 56123 Pisa, Italy [email protected] Georgina M. Sawyer Laboratoire Magmas et Volcans, Université Blaise Pascal 5 rue Kessler, 63038 Clermont Ferrand, France and Istituto Nazionale di Geofisica e Vulcanologia Via della Faggiola, 32 56123 Pisa, Italy Domenico Granieri Istituto Nazionale di Geofisica e Vulcanologia Via della Faggiola, 32 56123 Pisa, Italy INTRODUCTION: VOLCANIC CO2 EMISSIONS IN THE GEOLOGICAL CARBON CYCLE Over long periods of time (~Ma), we may consider the oceans, atmosphere and biosphere as a single exospheric reservoir for CO2. The geological carbon cycle describes the inputs to this exosphere from mantle degassing, metamorphism of subducted carbonates and outputs from weathering of aluminosilicate rocks (Walker et al. 1981). A feedback mechanism relates the weathering rate with the amount of CO2 in the atmosphere via the greenhouse effect (e.g., Wang et al. 1976). An increase in atmospheric CO2 concentrations induces higher temperatures, leading to higher rates of weathering, which draw down atmospheric CO2 concentrations (Ber- ner 1991). Atmospheric CO2 concentrations are therefore stabilized over long timescales by this feedback mechanism (Zeebe and Caldeira 2008). This process may have played a role (Feulner et al. 2012) in stabilizing temperatures on Earth while solar radiation steadily increased due to stellar evolution (Bahcall et al. 2001). In this context the role of CO2 degassing from the Earth is clearly fundamental to the stability of the climate, and therefore to life on Earth. -
Relative Ages
CONTENTS Page Introduction ...................................................... 123 Stratigraphic nomenclature ........................................ 123 Superpositions ................................................... 125 Mare-crater relations .......................................... 125 Crater-crater relations .......................................... 127 Basin-crater relations .......................................... 127 Mapping conventions .......................................... 127 Crater dating .................................................... 129 General principles ............................................. 129 Size-frequency relations ........................................ 129 Morphology of large craters .................................... 129 Morphology of small craters, by Newell J. Fask .................. 131 D, method .................................................... 133 Summary ........................................................ 133 table 7.1). The first three of these sequences, which are older than INTRODUCTION the visible mare materials, are also dominated internally by the The goals of both terrestrial and lunar stratigraphy are to inte- deposits of basins. The fourth (youngest) sequence consists of mare grate geologic units into a stratigraphic column applicable over the and crater materials. This chapter explains the general methods of whole planet and to calibrate this column with absolute ages. The stratigraphic analysis that are employed in the next six chapters first step in reconstructing -
Open Hanagan Thesis Schreyer.Pdf
THE PENNSYLVANIA STATE UNIVERSITY SCHREYER HONORS COLLEGE DEPARTMENT OF EARTH AND MINERAL SCIENCES CHANGES IN CRATER MORPHOLOGY ASSOCIATED WITH VOLCANIC ACTIVITY AT TELICA VOLCANO, NICARAGUA: INSIGHT INTO SUMMIT CRATER FORMATION AND ERUPTION TRIGGERING CATHERINE E. HANAGAN SPRING 2019 A thesis submitted in partial fulfillment of the requirements for a baccalaureate degree in the Geosciences with honors in the Geosciences Reviewed and approved* by the following: Peter La Femina Associate Professor of Geosciences Thesis Supervisor Maureen Feineman Associate Research Professor and Associate Head for Undergraduate Programs Honors Adviser * Signatures are on file in the Schreyer Honors College. i ABSTRACT Telica is a persistently active basaltic-andesite stratovolcano in the Central American Volcanic Arc of Nicaragua. Poorly predicted sub-decadal, low explosivity (VEI 1-2) phreatic eruptions and background persistent activity with high-rates of seismic unrest and frequent degassing contribute to morphologic change in Telica’s active crater on a small spatiotemporal scale. These changes sustain a morphology similar to those of commonly recognized calderas or pit craters (Roche et al., 2001; Rymer et al., 1998), and have been related to sealing of the hydrothermal system prior to eruption (INETER Buletin Anual, 2013). We use photograph observations and Structure from Motion point cloud construction and comparison (Multiscale Model to Model Cloud Comparison, Lague et al., 2013; Westoby et al., 2012) from 1994 to 2017 to correlate changes in Telica’s crater with sustained summit crater formation and eruptive pre- cursors. Two previously proposed mechanisms for sealing at Telica are: 1) widespread hydrothermal mineralization throughout the magmatic-hydrothermal system (Geirsson et al., 2014; Rodgers et al., 2015; Roman et al., 2016); and/or 2) surficial blocking of the vent by landslides and rock fall (INETER Buletin Anual, 2013).