DOCSLIB.ORG

Fundamentals of Selenography

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Fundamentals of Selenography Appendix A Fundamentals of selenography This appendix details some quint-essentials of selenography, and serves as a basic reference for lunar surface features and a first-order map of the lunar geology (se­ lenology). Figures A.l and A.2 schematically show, in a simple cylindrical projec­ tion, the characteristic features of the Moon and relate the names to selenograph­ icallocation. A more detailed description of the quintessential maria, basins and craters, including their location, approximate size and geophysical characteristics is given in near-stenographical form in the extended tables. Most of the tabulated information is extracted and/ or derived from Spudis [1996]. Lunar maria Name and Location Description Mare Crisium Mascon mare near the east limb; low to very low (10-25° N, 50-70° E) titanium basalts, extruded around 3.4 Gyr ago Mare Fecunditatis Complex, shallow mare made up of low-, (5° N - 20° 5, 40-60° E) moderate-, and high-titanium basalts, extruded about 3.4 Gyr ago Mare Humorum Mascon mare on the southwestern near-side of (18-30° 5,31-48° W) the Moon, filled with moderately high-titanium basalts, 3.2-3.5 Gyr old Mare Imbrium Mascon mare on the near-side, deeply filled with (15-50° N, 40° W-5° E) low- and high-titanium basalts; age: from 3.3 to less than 2 Gyr old 232 Fundamentals of selenography Mare N ectaris Mascon mare on the central near-side; low­ (10-20° 5,30-40° E) titanium basalts covering very high titanium basalts; age: 3.8-3.5 Gyr Mare Nubium Complex, shallow mare; low- and high-titanium (10-30° 5,5-25° W) lava flows; age: 3.3-3.0 Gyr Mare Serenitatis Mascon mare; very high titanium lavas around (15-40° N, 5-20° E) the margins and centre of very low titanium lava; age: 3.8-3.3 Gyr Mare Smythii Mascon mare, very shallow; moderate-titanium (5° N-5° 5,80-95° E) lava; possibly extremely young (1-1.5 Gyr) Mare Tranquillitatis Complex, shallow, irregular mare; site of the first (0-20° N, 15-45° E) lunar landing; old (3.8 Gyr), with very high tita­ nium lavas Oceanus Procell arum Complex, shallow, irregular mare; largest on the (10° 5-60° N, 10-80° W) Moon; many compositions, with ages including the youngest lavas on the Moon (less than 1 Gyr old) Sinus Medii Small patch of mare near the exact centre of the (3° 5-5° N, 5° W-5° E) lunar near-side; site of the Surveyor 6 landing (1967) Lunar craters Name and Location Description Albategnius Large crater in the central highlands, sketched (11.2° 5,4.1 ° E; 136 km) by Galileo in 1610 Alphonsus Old crater with three dark, volcanic cinder cones (13.4° 5,2.8° W; 119 km) on its floor Archimedes Crater flooded by mare basalt, demonstrating (29.7° N, 4.0° W; 83 km) time span between Imbrium basin and its mare fill Aristarchus Very fresh crater excavating highland debris (23.7° N,47.4° W; 40 km) from beneath mare basalt cover Compton Small central-peak-plus-ring basin near lunar (56.0° N, 105.0° E; 160 km) north pole Cone Small, fresh crater excavating Fra Mauro brec­ (3S 5, 17S W; 370 m) cias that were sampled on the Apollo 14 mission, 1971 Copernicus Relatively young impact crater south of Mare (9.7° N, 20.0° W; 93 km) Imbrium; defines Copernican stratigraphic sys­ tem A Fundamentals of selenography 233 Descartes Old crater in central highlands, near the landing (11.7° S, 15.7° E; 48 krn) site of Apollo 16, 1972 Eratosthenes Unrayed crater near Mare Imbrium; defines Er­ (14S N, 11.3° W; 58 krn) atosthenian stratigraphic system Flamsteed P Old crater flooded by some of the youngest (1 (3.0° S, 44.0° W; 112 km) Gyr) lavas on the Moon; site of the Surveyor 1 landing in 1966 FraMauro Old crater covered by ejecta from the Imbrium (6.0° S, 17.0° W; 95 krn) impact basin; near the landing site of Apollo 14, 1971 Herigonius Small crater north of Mare Humorum, near some (13.3° S, 34.0° W; 15 krn) of the most spectacular sinuous rilles in the maria Hortensius Small crater, near which occur many small lunar (6.50° N, 28.0° W; 15 krn) shield volcanoes Kopff Unusual crater, long thought to be volcanic, in (17.4° S, 89.6° W; 42 krn) Orientale basin; may have been created by an impact into a semi-molten melt sheet Lamont Ridge ring system in Mare Tranquillitatis, (5.0° N, 23.2° E; 175 krn) formed over a two-ring basin Letronne Crater largely flooded by mare basalt in Oceanus (10.6° S, 42.4° W; 120 km) Procellarum Lichtenberg Rayed crater that is partly covered by a very (31.8° N, 67.7° W; 20 km) young mare lava flow, possibly less than 1 Gyr old Linne Very fresh, bright crater in Mare Serenitatis, re­ (27.7° N, 11.8° E; 2 km) ported before the space age to appear and disap­ pear Ritter Forms together with Sabine an unusual twin (2.0° N, 19.2° E; 29 krn) impact crater in Mare Tranquillitatis, similar in morphology to Kopff Sabine See Ritter (1.4° N, 20.1° E; 30 km) Shorty Small impact crater at the Apollo 17 landing site, (20.0° N, 31.0° E; 110 m) 1972; excavated dark mantle ash from beneath a layer of highland debris Sulpicius Gallus Crater near a large exposure of dark mantle de­ (19.6° N; 11.6° E; 12 krn) posits. Theophilus Large crater on the edge of Mare Nectaris. (11.4° S, 26.4° E; 100 krn) Tsiolkovsky Spectacular, mare-filled crater on the lunar far­ (20.4° S, 129.1 ° E; 180 km) side. 234 Fundamentals of selenography Tycho Fresh, prominent rayed crater on the near-side of (43.3° 5, 11.2° W; 85 km) the Moon; rays extend across entire hemisphere; central peak exposes deep-seated rocks Van de Graaff Double crater on the far-side; site of a major geo­ (27.0° 5, 172.0° E; 234km) chemical anomaly caused by its location just in­ side the rim of 50uth Pole Aitken basin Lunar basins Name and Location Description Crisium basin Nectarian-age multiring basin; ejecta possibly (17S N, 58S E; 740 km) sampled by the Luna 20 mission Humorum basin Nectarian-age basin south of Procellarum (24° 5, 39S W, 820 km) Imbrium basin Major large basin on the Moon; defines base of (33° N, 17° W, 1,150 km) Imbrian 5ystem; formed 3.84 Gyr ago; its ejecta was the sampling objective of the Apollo 14 and 15 missions Nectaris basin Defines base of Nectarian 5ystem; possibly sam­ (16° 5,34° E; 860 km) pled on the Apollo 16 mission in 1972; age: 3.92 Gyr Orientale basin Youngest large, multiring basin on the Moon, (20° 5, 95° W; 930km) formed sometime after 3.84 billion years ago; its interior and exterior deposits were used as a guide to interpret older, degraded basins Procellarum basin Alleged impact basin, supposedly the largest on (26° N, 15° W; 3,200 km) the Moon; Clementine laser altimetry data do not support its existence 5chrbdinger Type example of a two-ring basin, near the south (75.6° 5, 133.7° E; 320 km) pole of the Moon; formed after Imbrium basin but before Orientale basin 5erenitatis basin Nectarian-age multiring basin, sampled and ex­ (27° N, 19° E; 900 km) plored by Apollo 17 mission in 1972; age: 3.87 Gyr 50uth Pole Aitken basin Largest, deepest (over 12 km) impact crater (56° 5, 180° E; 2,500 km) known in the solar system; oldest basin on the Moon; absolute age unknown (4.3 Gyr??) A Fundamentals of selenography 235 Other surface features Name and Location Description Apennine Bench Refers to a relatively elevated region near (25-28° N, 0-10° W) Archimedes and just inside the rim of Imbrium basin; includes light-toned Apennine Mountains Large mountain chain making up the southeast­ (15-30° N, 10° W-50° E) ern rim of the Imbrium basin Cayley plains Light-toned, smooth highland plains, first de­ fined in the central near-side but having moon­ wide distribution; probably a form of impact ejecta from the youngest major basins; may cover ancient mare lavas in some areas Cordillera Mountains Arcuate mountain chain that makes up the rim (10-35° 5,80-90° W) of the Orientale basin Hadley-Apennines Informal name given to the region of the Apollo (26° N,4° W) 15 mission exploration; includes mare, Hadley Rille, and Apennine highlands Hadley Rille See Rima Hadley Marginis swirls Light-toned swirls north of Mare Marginis; ori­ (15° N, 90° E) gin unknown Marius Hills Complex area of small domes, cones, and sinu­ (10-15° N, 50-60° W) ous rilles in Oceanus Procellarum; the dome-like swell may indicate that this region is a large lu­ nar shield volcano Reiner Gamma Bright, swirl-like deposit in Oceanus Procel­ (7° N, 590 W) larum; origin unknown Rima Bode II Cleftlike vent and linear trench outline vent sys­ (13 0 N,4° W) tem for a large, regional blanket of dark volcanic ash Rima Hadley Long sinuous rille starting in the highlands and (25 0 N,3° W) emptying into the maria; probably a lava chan­ nel and/or tube Riimker Hills Complex of cones and domes in Oceanus Procel­ (41 0 N,58° W) larum, similar to Marius Hills but much smaller Taurus-Littrow Informal name given to the region of the Apollo (20 0 N, 31 0 E) 17 mission exploration; includes mare, dark mantle, and the highlands of the Serenitatis basin Tranquillity Base Site, in Mare Tranquillitatis, of man's first land­ W N,23° E) ing on the Moon, Apollo 11, July 20,1969 236 Fundamentals of selenography Figure A.1 The near-side of the Moon.
Load more

Recommended publications
  • 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.
    [Show full text]
  • Regolith Compaction and Its Implications for the Formation Mechanism of Lunar Swirls
    EPSC Abstracts Vol. 13, EPSC-DPS2019-1608-1, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Regolith Compaction and its Implications for the Formation Mechanism of Lunar Swirls Christian Wöhler (1), Megha Bhatt (2), Arne Grumpe (1), Marcel Hess (1), Alexey A. Berezhnoy (3), Vladislav V. Shevchenko (3) and Anil Bhardwaj (2) (1) Image Analysis Group, TU Dortmund University, Otto-Hahn-Str. 4, 44227 Dortmund, Germany, (2) Physical Research Laboratory, Ahmedabad, 380009, India, (3) Sternberg Astronomical Institute, Universitetskij pr., 13, Moscow State University, 119234 Moscow, Russia ([email protected]) Abstract The brightening of the regolith at Reiner Gamma could be a result of reduced space-weathering due to In this study we have examined spectral trends of magnetic shielding [3] and/or due to soil compaction Reiner Gamma (7.5°N, 59°W) using the Moon [5]. According to the model of [9], the spectral Mineralogy Mapper (M3) [1] observations. We variation due to soil compaction is a change in albedo derived maps of solar wind induced OH/H2O and a with negligible effect on spectral slope and compaction index map of the Reiner Gamma swirl. absorption band depths. To quantify soil compaction Our results suggest that the combination of soil at Reiner Gamma, we empirically defined the compaction and magnetic shielding can explain the compaction index c as a positive real number given observed spectral trends. These new findings support by c = M / RSE, where M is the reflectance the hypothesis of swirl formation by interaction modulation at 1.579 µm between a bright on-swirl between a comet and the uppermost regolith layer.
    [Show full text]
  • 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
    [Show full text]
  • Archons (Commanders) [NOTICE: They Are NOT Anlien Parasites], and Then, in a Mirror Image of the Great Emanations of the Pleroma, Hundreds of Lesser Angels
    A R C H O N S HIDDEN RULERS THROUGH THE AGES A R C H O N S HIDDEN RULERS THROUGH THE AGES WATCH THIS IMPORTANT VIDEO UFOs, Aliens, and the Question of Contact MUST-SEE THE OCCULT REASON FOR PSYCHOPATHY Organic Portals: Aliens and Psychopaths KNOWLEDGE THROUGH GNOSIS Boris Mouravieff - GNOSIS IN THE BEGINNING ...1 The Gnostic core belief was a strong dualism: that the world of matter was deadening and inferior to a remote nonphysical home, to which an interior divine spark in most humans aspired to return after death. This led them to an absorption with the Jewish creation myths in Genesis, which they obsessively reinterpreted to formulate allegorical explanations of how humans ended up trapped in the world of matter. The basic Gnostic story, which varied in details from teacher to teacher, was this: In the beginning there was an unknowable, immaterial, and invisible God, sometimes called the Father of All and sometimes by other names. “He” was neither male nor female, and was composed of an implicitly finite amount of a living nonphysical substance. Surrounding this God was a great empty region called the Pleroma (the fullness). Beyond the Pleroma lay empty space. The God acted to fill the Pleroma through a series of emanations, a squeezing off of small portions of his/its nonphysical energetic divine material. In most accounts there are thirty emanations in fifteen complementary pairs, each getting slightly less of the divine material and therefore being slightly weaker. The emanations are called Aeons (eternities) and are mostly named personifications in Greek of abstract ideas.
    [Show full text]
  • Science Concept 5: Lunar Volcanism Provides a Window Into the Thermal and Compositional Evolution of the Moon
    Science Concept 5: Lunar Volcanism Provides a Window into the Thermal and Compositional Evolution of the Moon Science Concept 5: Lunar volcanism provides a window into the thermal and compositional evolution of the Moon Science Goals: a. Determine the origin and variability of lunar basalts. b. Determine the age of the youngest and oldest mare basalts. c. Determine the compositional range and extent of lunar pyroclastic deposits. d. Determine the flux of lunar volcanism and its evolution through space and time. INTRODUCTION Features of Lunar Volcanism The most prominent volcanic features on the lunar surface are the low albedo mare regions, which cover approximately 17% of the lunar surface (Fig. 5.1). Mare regions are generally considered to be made up of flood basalts, which are the product of highly voluminous basaltic volcanism. On the Moon, such flood basalts typically fill topographically-low impact basins up to 2000 m below the global mean elevation (Wilhelms, 1987). The mare regions are asymmetrically distributed on the lunar surface and cover about 33% of the nearside and only ~3% of the far-side (Wilhelms, 1987). Other volcanic surface features include pyroclastic deposits, domes, and rilles. These features occur on a much smaller scale than the mare flood basalts, but are no less important in understanding lunar volcanism and the internal evolution of the Moon. Table 5.1 outlines different types of volcanic features and their interpreted formational processes. TABLE 5.1 Lunar Volcanic Features Volcanic Feature Interpreted Process
    [Show full text]
  • Crater Geometry and Ejecta Thickness of the Martian Impact Crater Tooting
    Meteoritics & Planetary Science 42, Nr 9, 1615–1625 (2007) Abstract available online at http://meteoritics.org Crater geometry and ejecta thickness of the Martian impact crater Tooting Peter J. MOUGINIS-MARK and Harold GARBEIL Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i, Honolulu, Hawai‘i 96822, USA (Received 25 October 2006; revision accepted 04 March 2007) Abstract–We use Mars Orbiter Laser Altimeter (MOLA) topographic data and Thermal Emission Imaging System (THEMIS) visible (VIS) images to study the cavity and the ejecta blanket of a very fresh Martian impact crater ~29 km in diameter, with the provisional International Astronomical Union (IAU) name Tooting crater. This crater is very young, as demonstrated by the large depth/ diameter ratio (0.065), impact melt preserved on the walls and floor, an extensive secondary crater field, and only 13 superposed impact craters (all 54 to 234 meters in diameter) on the ~8120 km2 ejecta blanket. Because the pre-impact terrain was essentially flat, we can measure the volume of the crater cavity and ejecta deposits. Tooting crater has a rim height that has >500 m variation around the rim crest and a very large central peak (1052 m high and >9 km wide). Crater cavity volume (i.e., volume below the pre-impact terrain) is ~380 km3 and the volume of materials above the pre-impact terrain is ~425 km3. The ejecta thickness is often very thin (<20 m) throughout much of the ejecta blanket. There is a pronounced asymmetry in the ejecta blanket, suggestive of an oblique impact, which has resulted in up to ~100 m of additional ejecta thickness being deposited down-range compared to the up-range value at the same radial distance from the rim crest.
    [Show full text]
  • Location #1: Peary/Whipple Crater
    Location, Location, Location A Lunar Investment Strategy Hoyt Davidson Near Earth LLC June 2017 ISU's International Institute of Space Commerce Lunar Economic Action Plan (LEAP) Space and Questions from 1960 Still Relevant Today Economic Development • How can we utilize our dynamic system of competitive private enterprise in space, as on earth, to make newly discovered resources useful to man? • How can private enterprise and private capital make their maximum contribution? Philosophy and Policy The ultimate goal is not to impress others, or merely to explore our planetary system, but to use accessible space for the benefit of humankind. It is a goal that is not confined to a decade or a century. Nor is it confined to a single nearby destination, or to a fleeting dash to plant a flag. The idea is to begin preparing now for a future in which the material trapped in the Sun's vicinity is available for incorporation into our way of life. Dr. John Marburger, Head of the Office of Science and Technology Policy 2006 3 The Investment Premise • Just as on Earth, lunar real estate “value” is driven by location, location, location Rank Location Why Valuable 1 Peary Crater Best 1st industrial base and settlement 2 Sinus Medii Good cargo port & space elevator site 3 Largest skylights / lava tubes Best large scale settlements 4 Tsiolkovskiy crater, dark side Prime radio astronomy site 5 High helium-3 concentrations Potential high value mining 6 Lipsky Crater Space elevator site for Earth-Moon L2 7 Aristillus High Thorium concentrations • Lunar real
    [Show full text]
  • 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.
    [Show full text]
  • Psychology of Space Exploration Psychology of About the Book Douglas A
    About the Editor Contemporary Research in Historical Perspective Psychology of Space Exploration Psychology of About the Book Douglas A. Vakoch is a professor in the Department As we stand poised on the verge of a new era of of Clinical Psychology at the California Institute of spaceflight, we must rethink every element, including Integral Studies, as well as the director of Interstellar Space Exploration the human dimension. This book explores some of the Message Composition at the SETI Institute. Dr. Vakoch Contemporary Research in Historical Perspective contributions of psychology to yesterday’s great space is a licensed psychologist in the state of California, and Edited by Douglas A. Vakoch race, today’s orbiter and International Space Station mis- his psychological research, clinical, and teaching interests sions, and tomorrow’s journeys beyond Earth’s orbit. include topics in psychotherapy, ecopsychology, and meth- Early missions into space were typically brief, and crews odologies of psychological research. As a corresponding were small, often drawn from a single nation. As an member of the International Academy of Astronautics, intensely competitive space race has given way to inter- Dr. Vakoch chairs that organization’s Study Groups on national cooperation over the decades, the challenges of Interstellar Message Construction and Active SETI. communicating across cultural boundaries and dealing Through his membership in the International Institute with interpersonal conflicts have become increasingly of Space Law, he examines
    [Show full text]
  • PROJECT PENGUIN Robotic Lunar Crater Resource Prospecting VIRGINIA POLYTECHNIC INSTITUTE & STATE UNIVERSITY Kevin T
    PROJECT PENGUIN Robotic Lunar Crater Resource Prospecting VIRGINIA POLYTECHNIC INSTITUTE & STATE UNIVERSITY Kevin T. Crofton Department of Aerospace & Ocean Engineering TEAM LEAD Allison Quinn STUDENT MEMBERS Ethan LeBoeuf Brian McLemore Peter Bradley Smith Amanda Swanson Michael Valosin III Vidya Vishwanathan FACULTY SUPERVISOR AIAA 2018 Undergraduate Spacecraft Design Dr. Kevin Shinpaugh Competition Submission i AIAA Member Numbers and Signatures Ethan LeBoeuf Brian McLemore Member Number: 918782 Member Number: 908372 Allison Quinn Peter Bradley Smith Member Number: 920552 Member Number: 530342 Amanda Swanson Michael Valosin III Member Number: 920793 Member Number: 908465 Vidya Vishwanathan Dr. Kevin Shinpaugh Member Number: 608701 Member Number: 25807 ii Table of Contents List of Figures ................................................................................................................................................................ v List of Tables ................................................................................................................................................................vi List of Symbols ........................................................................................................................................................... vii I. Team Structure ........................................................................................................................................................... 1 II. Introduction ..............................................................................................................................................................
    [Show full text]
  • 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.
    [Show full text]
  • Surveyor 1 Space- Craft on June 2, 1966 As Seen by the Narrow Angle Camera of the Lunar Re- Connaissance Orbiter Taken on July 17, 2009 (Also See Fig
    i “Project Surveyor, in particular, removed any doubt that it was possible for Americans to land on the Moon and explore its surface.” — Harrison H. Schmitt, Apollo 17 Scientist-Astronaut ii Frontispiece: Landing site of the Surveyor 1 space- craft on June 2, 1966 as seen by the narrow angle camera of the Lunar Re- connaissance Orbiter taken on July 17, 2009 (also see Fig. 13). The white square in the upper photo outlines the area of the enlarged view below. The spacecraft is ca. 3.3 m tall and is casting a 15 m shadow to the East. (NASA/LROC/ ASU/GSFC photos) iii iv Surveyor I: America’s First Moon Landing by William F. Mellberg v © 2014, 2015 William F. Mellberg vi About the author: William Mellberg was a marketing and public relations representative with Fokker Aircraft. He is also an aerospace historian, having published many articles on both the development of airplanes and space vehicles in various magazines. He is the author of Famous Airliners and Moon Missions. He also serves as co-Editor of Harrison H. Schmitt’s website: http://americasuncommonsense.com Acknowledgments: The support and recollections of Frank Mellberg, Harrison Schmitt, Justin Rennilson, Alexander Gurshstein, Paul Spudis, Ronald Wells, Colin Mackellar and Dwight Steven- Boniecki is gratefully acknowledged. vii Surveyor I: America’s First Moon Landing by William F. Mellberg A Journey of 250,000 Miles . December 14, 2013. China’s Chang’e 3 spacecraft successfully touched down on the Moon at 1311 GMT (2111 Beijing Time). The landing site was in Mare Imbrium, the Sea of Rains, about 25 miles (40 km) south of the small crater, Laplace F, and roughly 100 miles (160 km) east of its original target in Sinus Iridum, the Bay of Rainbows.
    [Show full text]