Unveiling the Face of Selene S.R
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Composition of the Deposits of the Lunar Orientale Basin P.D. Spudis1 and D.J.P
45th Lunar and Planetary Science Conference (2014) 1469.pdf Composition of the Deposits of the Lunar Orientale Basin P.D. Spudis1 and D.J.P. Martin2 1. Lunar and Plane- tary Institute, Houston TX 77058 [email protected] 2. School of Earth, Atmospheric and Environmental Sci- ences, University of Manchester, Oxford Road, Manchester, United Kingdom, M13 9PL Introduction. Orientale is the youngest and best- must constitute some fraction of the subsurface materi- preserved multi-ring impact basin on the Moon and has als of the inner basin as their presence is evident as a long been studied for clues to the processes and histo- mixing component in the ejecta of Maunder crater, the ries of older, more degraded features [1-4]. We have largest post-basin impact crater within Orientale. recently completed a new geological map derived from These basalts probably make up feeder dikes and vent LRO image and topographic data that show the distri- deposits associated with the emplacement of Mare bution and relations of the geological units of the basin Orientale. The other significant departure from the [5]. Using this new map as template, we can isolate feldspathic highlands composition comes in the form individual basin units and study their composition to of numerous basin ring massifs that appear to be com- the exclusion of adjacent and overlying units [6]. Us- posed of pure anorthosite [9, 10]. Anorthosite massifs ing this approach, we have studied the impact melt are most abundant in the Inner Rook ring, suggesting sheet of the Orientale basin and concluded that it has the presence of a regionally contiguous sub-layer of not been differentiated [6] as had been proposed [7]. -
Similarity Laws of Lunar and Terrestrial Volcanic Flows*
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) SIMILARITY LAWS OF LUNAR AND TERRESTRIAL VOLCANIC FLOWS* S. I. Pai and Y. Hsu Institute for Physical Science and Technology and Aerospace Engineering Department, University of Maryland, College Park Maryland 20742, and ^g15Z021.^,, ^.^,121319 7 ^t , John A. O'Keefe Goddard Space Flight Center, Greenbelt, Maryland 204T° JUN 1977 LP '' RECEIVED ^n NASA STI FACILITY INPUT BRANCH \c. STRACT Alt! ; \Z 1Z A mathematical model for the volcanic flow in planets is proposed.^^ This mathematical model, which is one-dimensional, steady duct flow of a mixture of a gas and small solid particles ( rock), has been analyzed. We v+ 0 apply this model to the lunar and the terrestrial volcanic flows under geo- +oN m U co metrically and dynamically similar conditions. -
INTERAGENCY REPORT: ASTROGEOLOGY 7 ADVANCED SYSTEMS TRAVERSE RESEARCH PROJECT REPORT by G
INTERAGENCY REPORT: ASTROGEOLOGY 7 ADVANCED SYSTEMS TRAVERSE RESEARCH PROJECT REPORT By G. E. Ulrich With a Section on Problems for Geologic Investigations of the Orientale Region of the Moon By R. S. Saunders July 1968 CONTENTS Page Abs tract . ............. 1 Introduct ion . •• # • ••• ••• .' • 2 Physiographic subdivision of the lunar surface 3 Site selection and preliminary traverse research. 8 Lunar topographic data •••••••.•.•••••• 17 Objectives and evaluation of traverse concepts • 20 Recommendations for continued traverse research .••• 26 Problems for geologic investigations of the Orientale region of the Moon, by R. S. Saunders 30 Introduct ion •.•• •••. 30 Physiography 30 Pre-Orbiter observations and i~terpretations 35 Geologic interpretations based on Orbiter photography ••••••••• 38 Conelusions •••• .•••. 54 References 56 ILLUSTRATIONS Figure 1. Map and index to photographs of Orientale basin region ••••.•••••• 4 2. Crater-size frequency distributions of Orientale basin terrain units •••••• 11 3. Orientale basin region showing pre- liminary traverse evaluation areas ••••• 14 4. Effect of photographic exposure on shadow measurements 15 5. Alternate traverse areas for short and intermediate duration missions. North eastern sector of central Orientale basin ................... 24 6. Preliminary photogeologic map of the Orientale basin region. .•• .. .. 32 iii Page Figure 7. Sketch map of Mare Orientale region prepared from Earth-based telescopic photography • 36 8-21. Orbiter IV photographs of Orientale basin region showing-- . 8. Part of wr{nk1e ridge . 41 9. Slump scarps around steptoe and collapse depression . 44 10. Slump scarps along margin of central mare basin outlining collapse depression • • . • 44 11. Possible caldera 45 12. Northeast quadrant of inner ring showing central basin material and mare units 45 13. -
Little Learners' Activity Guide
LUNAR RECONNAISSANCE ORBITER CAMERA Little Learners’ Activity Guide Learn about the Moon with puzzles, coloring, and fun facts! Mare Imbrium Mare Serenitatis Mare Tranquillitatis Oceanus Procellarum Mare Humorum Tycho Crater Visit us online at lroc.sese.asu.edu Online resources Additional information and content, including supplemental learning activities, can be accessed at the following online locations: 1. Little Learners’ Activity Guide: lroc.sese.asu.edu/littlelearners 2. LROC website: lroc.sese.asu.edu 3. Resources for teachers: lroc.sese.asu.edu/teach 4. Learn about the Moon’s history: lroc.sese.asu.edu/learn 5. LROC Lunar Quickmap 3D: quickmap.lroc.asu.edu Copyright 2018, Lunar Reconnaissance Orbiter Camera i Lunar Reconnaissance Orbiter Camera Fun Facts for Beginners • The Moon is 363,301 kilometers (225,745 miles) from the Earth. • The surface area of the Moon is almost as large as the continent of Africa. • It takes 27 days for the Moon to orbit around the Earth. • The farside is the side of the Moon we cannot see from Earth. • South Pole Aitken is the largest impact basin on the lunar farside. • Impact basins are formed as the result of impacts from asteroids or comets and are larger than craters. • Regolith is a layer of loose dust, dirt, soil, and broken rock deposits that cover solid rock. • The two main types of rock that make up the Moon’s crust are anorthosite and basalt. • A person weighing 120 lbs on Earth weighs 20 lbs on the Moon because gravity on the Moon is 1/6 as strong as on Earth. -
Characterization of Previously Unidentified Lunar Pyroclastic Deposits Using Lunar Reconnaissance Orbiter Camera Data J
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 117, E00H25, doi:10.1029/2011JE003893, 2012 Characterization of previously unidentified lunar pyroclastic deposits using Lunar Reconnaissance Orbiter Camera data J. Olaf Gustafson,1 J. F. Bell III,2,3 L. R. Gaddis,4 B. R. Hawke,5 and T. A. Giguere5,6 Received 1 July 2011; revised 31 March 2012; accepted 14 April 2012; published 8 June 2012. [1] We used a Lunar Reconnaissance Orbiter Camera (LROC) global monochrome Wide-angle Camera (WAC) mosaic to conduct a survey of the Moon to search for previously unidentified pyroclastic deposits. Promising locations were examined in detail using LROC multispectral WAC mosaics, high-resolution LROC Narrow Angle Camera (NAC) images, and Clementine multispectral (ultraviolet-visible or UVVIS) data. Out of 47 potential deposits chosen for closer examination, 12 were selected as probable newly identified pyroclastic deposits. Potential pyroclastic deposits were generally found in settings similar to previously identified deposits, including areas within or near mare deposits adjacent to highlands, within floor-fractured craters, and along fissures in mare deposits. However, a significant new finding is the discovery of localized pyroclastic deposits within floor-fractured craters Anderson E and F on the lunar farside, isolated from other known similar deposits. Our search confirms that most major regional and localized low-albedo pyroclastic deposits have been identified on the Moon down to 100 m/pix resolution, and that additional newly identified deposits are likely to be either isolated small deposits or additional portions of discontinuous, patchy deposits. Citation: Gustafson, J. O., J. F. Bell III, L. R. Gaddis, B. -
Observing the Lunar Libration Zones
Observing the Lunar Libration Zones Alexander Vandenbohede 2005 Many Look, Few Observe (Harold Hill, 1991) Table of Contents Introduction 1 1 Libration and libration zones 3 2 Mare Orientale 14 3 South Pole 18 4 Mare Australe 23 5 Mare Marginis and Mare Smithii 26 6 Mare Humboldtianum 29 7 North Pole 33 8 Oceanus Procellarum 37 Appendix I: Observational Circumstances and Equipment 43 Appendix II: Time Stratigraphical Table of the Moon and the Lunar Geological Map 44 Appendix III: Bibliography 46 Introduction – Why Observe the Libration Zones? You might think that, because the Moon always keeps the same hemisphere turned towards the Earth as a consequence of its captured rotation, we always see the same 50% of the lunar surface. Well, this is not true. Because of the complicated motion of the Moon (see chapter 1) we can see a little bit around the east and west limb and over the north and south poles. The result is that we can observe 59% of the lunar surface. This extra 9% of lunar soil is called the libration zones because the motion, a gentle wobbling of the Moon in the Earth’s sky responsible for this, is called libration. In spite of the remainder of the lunar Earth-faced side, observing and even the basic task of identifying formations in the libration zones is not easy. The formations are foreshortened and seen highly edge-on. Obviously, you will need to know when libration favours which part of the lunar limb and how much you can look around the Moon’s limb. -
4. Lunar Architecture
4. Lunar Architecture 4.1 Summary and Recommendations As defined by the Exploration Systems Architecture Study (ESAS), the lunar architecture is a combination of the lunar “mission mode,” the assignment of functionality to flight elements, and the definition of the activities to be performed on the lunar surface. The trade space for the lunar “mission mode,” or approach to performing the crewed lunar missions, was limited to the cislunar space and Earth-orbital staging locations, the lunar surface activities duration and location, and the lunar abort/return strategies. The lunar mission mode analysis is detailed in Section 4.2, Lunar Mission Mode. Surface activities, including those performed on sortie- and outpost-duration missions, are detailed in Section 4.3, Lunar Surface Activities, along with a discussion of the deployment of the outpost itself. The mission mode analysis was built around a matrix of lunar- and Earth-staging nodes. Lunar-staging locations initially considered included the Earth-Moon L1 libration point, Low Lunar Orbit (LLO), and the lunar surface. Earth-orbital staging locations considered included due-east Low Earth Orbits (LEOs), higher-inclination International Space Station (ISS) orbits, and raised apogee High Earth Orbits (HEOs). Cases that lack staging nodes (i.e., “direct” missions) in space and at Earth were also considered. This study addressed lunar surface duration and location variables (including latitude, longi- tude, and surface stay-time) and made an effort to preserve the option for full global landing site access. Abort strategies were also considered from the lunar vicinity. “Anytime return” from the lunar surface is a desirable option that was analyzed along with options for orbital and surface loiter. -
Nasa Contract Nas 9-14413 Final Report Apollo
https://ntrs.nasa.gov/search.jsp?R=19750010480 2020-03-22T22:42:40+00:00Z NASA CONTRACT NAS 9-14413 FINAL REPORT APOLLO EXPERIME]NT S-211 LOW BRIGfHTNESS, ASTRONOMICAL 3 T8 RAP7{ December 31, 1974 i 1 8 5 5 2 7 S-211 N75- (NASA-CR-14166 ) APOLLO EXPERIMENT LOW BRIGHTNESS, ASTRONOMICAL PHOTOGRAPHY Final Report (Institute for ScientifiSC and Spale 0 CInstt teCSCL s inclas E space) 100 p HC $475 G3/35 13355 NASA CR- NASA CONTRACT NAS 9-14413 FINAL REPORT APOLLO EXPERIMENT S-211 LOW BRIGHTNESS, ASTRONOMICAL PHOTOGRAPHY Prepared for Lyndon B. Johnson Space Center NATIONAL AERONAUTICS AND SPACE ADMINISTRATION Houston, Texas 77058 Robert D. Mercer Principal Investigator December 31, 1974 INSTITUTE FOR SCIENTIFIC AND SPACE RESEARCH, INC. 463 Kenwood Avenue Delmar, New York 12054 FOREWORD This is the Final Report to the Lyndon B. Johnson Space Center, National Aeronautics and Space Administration, under Contract NAS 9-14413 for Apollo Experiment S-211, Low-Brightness, Astronomical Photography. This report has been prepared to satisfy two requirements: to document results of the photographic acquisition of data and analysis of low bright- ness, astronomical sources, and to present this information in a format suitable for direct publication by the National Space Science Data Center. Principal Investigator for this work has been Mr. Robert D. Mercer of the Institute for Scientific and Space Research, Inc., Delmar, New York. Co- Investigator has been Mr. Lawrence Dunkelman of the Robert H. Goddard Space Flight Center, Greenbelt, Maryland- The analyses of data on low brightness, astronomical sources are heavily dependent on the technique used in the data collection, in the photometric calibration of the photographic emulsions and in the methods of computer manipulation of this information. -
LPSC YXI 473 O Lunar and Planetary Institute Provided by the NASA
LPSC YXI 473 THE COMPOSITION OF THE CRUST IN THE ORIENTALE REGION OF THE MOON: A PRE-GALILEO VIEW. B. Ray ~awkel,P.D. Spudisz, P.G. ~uceyl,and J.F. ~elll,1 Planetary Geosciences Division, Hawaii Institute of Geophysics, University of Hawaii, Honolulu, HI 96822, 2~.~.~.~.,Flagstaff, AZ 86001. In December, 1990, the Galileo spacecraft will encounter the Moon and provide a wealth of new spectral data and imagery for the western limb region that can be used to address a variety of important lunar issues. In order to prepare for this encounter, we are in the process of collecting new spectral data for the Orientale region. In November, 1989, we obtained a large number of UVNlS spectra (0.4-0.8 pm) for the western limb and this data are currently being reduced and analyzed. Other observing runs are planned in the near future. The Orientale basin has been the subject of extensive geologic and remote sensing studies in recent years and much has been leamede.g-, l1p12 . The purpose of this paper is to review recent remote sensing studies of Orientale and summarize our current understanding of the composition of the crust in this region. The Orientale impact occurred in rugged highlands on the southwestern limb of the Moon and was the last of the major basin-forming events. Valuable insight concerning lateral and vertical changes in the composition of the lunar crust can be provided by studies of material exposed by lunar impact basins. These impacts have excavated material from a variety of depths and deposited this ejecta in a systematic manner. -
LUNAR CRATERS with CRACKED FLOORS by Roger Nelson Weller a Thesis Submitted to the Faculty of the DEPARTMENT of GEOSCIENCES in P
Lunar craters with cracked floors Item Type text; Thesis-Reproduction (electronic) Authors Weller, Roger Nelson, 1944- Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 24/09/2021 00:53:28 Link to Item http://hdl.handle.net/10150/347802 LUNAR CRATERS WITH CRACKED FLOORS by Roger Nelson Weller A Thesis Submitted to the Faculty of the DEPARTMENT OF GEOSCIENCES In Partial Fulfillment of the Requirements For the Degree of MASTER OF SCIENCE In the Graduate, College THE UNIVERSITY OF ARIZONA 19 7 2 STATEMENT BY AUTHOR This thesis has been submitted in partial fulfillment of re quirements for an advanced degree at The University of Arizona and is deposited in the University Library to be made available to borrowers under rules of the Library. Brief quotations from this thesis are allowable without special permission, provided that accurate acknowledgment of source is made. Requests for permission for extended quotation from or reproduction of this manuscript in whole or in part may be granted by the head of the major department or the Dean of the Graduate College when in his judg ment the proposed use of the material is in the interests of scholarship. In all other instances, however, permission must be obtained from the author. APPROVAL BY THESIS DIRECTOR This thesis has been approved on the date shown below: SPENCER R. -
Thedatabook.Pdf
THE DATA BOOK OF ASTRONOMY Also available from Institute of Physics Publishing The Wandering Astronomer Patrick Moore The Photographic Atlas of the Stars H. J. P. Arnold, Paul Doherty and Patrick Moore THE DATA BOOK OF ASTRONOMY P ATRICK M OORE I NSTITUTE O F P HYSICS P UBLISHING B RISTOL A ND P HILADELPHIA c IOP Publishing Ltd 2000 All rights reserved. No part of this publication may be reproduced, stored in a retrieval system or transmitted in any form or by any means, electronic, mechanical, photocopying, recording or otherwise, without the prior permission of the publisher. Multiple copying is permitted in accordance with the terms of licences issued by the Copyright Licensing Agency under the terms of its agreement with the Committee of Vice-Chancellors and Principals. British Library Cataloguing-in-Publication Data A catalogue record for this book is available from the British Library. ISBN 0 7503 0620 3 Library of Congress Cataloging-in-Publication Data are available Publisher: Nicki Dennis Production Editor: Simon Laurenson Production Control: Sarah Plenty Cover Design: Kevin Lowry Marketing Executive: Colin Fenton Published by Institute of Physics Publishing, wholly owned by The Institute of Physics, London Institute of Physics Publishing, Dirac House, Temple Back, Bristol BS1 6BE, UK US Office: Institute of Physics Publishing, The Public Ledger Building, Suite 1035, 150 South Independence Mall West, Philadelphia, PA 19106, USA Printed in the UK by Bookcraft, Midsomer Norton, Somerset CONTENTS FOREWORD vii 1 THE SOLAR SYSTEM 1 -
National Aeronautics and Space Administration) 111 P HC AO,6/MF A01 Unclas CSCL 03B G3/91 49797
https://ntrs.nasa.gov/search.jsp?R=19780004017 2020-03-22T06:42:54+00:00Z NASA TECHNICAL MEMORANDUM NASA TM-75035 THE LUNAR NOMENCLATURE: THE REVERSE SIDE OF THE MOON (1961-1973) (NASA-TM-75035) THE LUNAR NOMENCLATURE: N78-11960 THE REVERSE SIDE OF TEE MOON (1961-1973) (National Aeronautics and Space Administration) 111 p HC AO,6/MF A01 Unclas CSCL 03B G3/91 49797 K. Shingareva, G. Burba Translation of "Lunnaya Nomenklatura; Obratnaya storona luny 1961-1973", Academy of Sciences USSR, Institute of Space Research, Moscow, "Nauka" Press, 1977, pp. 1-56 NATIONAL AERONAUTICS AND SPACE ADMINISTRATION M19-rz" WASHINGTON, D. C. 20546 AUGUST 1977 A % STANDARD TITLE PAGE -A R.,ott No0... r 2. Government Accession No. 31 Recipient's Caafog No. NASA TIM-75O35 4.-"irl. and Subtitie 5. Repo;t Dote THE LUNAR NOMENCLATURE: THE REVERSE SIDE OF THE August 1977 MOON (1961-1973) 6. Performing Organization Code 7. Author(s) 8. Performing Organizotion Report No. K,.Shingareva, G'. .Burba o 10. Coit Un t No. 9. Perlform:ng Organization Nome and Address ]I. Contract or Grant .SCITRAN NASw-92791 No. Box 5456 13. T yp of Report end Period Coered Santa Barbara, CA 93108 Translation 12. Sponsoring Agiicy Noms ond Address' Natidnal Aeronautics and Space Administration 34. Sponsoring Agency Code Washington,'.D.C. 20546 15. Supplamortary No9 Translation of "Lunnaya Nomenklatura; Obratnaya storona luny 1961-1973"; Academy of Sciences USSR, Institute of Space Research, Moscow, "Nauka" Press, 1977, pp. Pp- 1-56 16. Abstroct The history of naming the details' of the relief on.the near and reverse sides 6f .