Geologic Context and Potential EVA Targets at the Lunar South Pole
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The Cold Traps Near South Pole of the Moon
THE COLD TRAPS NEAR SOUTH POLE OF THE MOON. Berezhnoy A.A., Kozlova E.A., Shevchenko V.V. Sternberg State Astronomical Institute, Moscow University, Russia, Moscow, Universitetski pr., 13, 199992. [email protected] According to the data from “Lunar Let us note that NH3 content in the lunar Prospector” [1] the areas of high hydrogen regolith is relatively low, because the main N- content in the lunar south pole region coincide containing compound is molecular nitrogen here with the areas of such craters as Faustini (87.2º [5]. The stability of SO2 subsurface ice requires S, 75.8º E), Cabeus (85.2º S, 323º E) and other the diurnal surface temperature of less than 65 crates. We have allocated a number of craters K. However, volatile species may be which can be considered as "cold traps " in the chemisorbed by the dust particles at the surface. south pole region of the Moon (Figure 1). Some In this case we can expect the existence of from these craters has properties similar to those chemisorbed water, CO2, and SO2 at the content of the echo coming from icy satellites of Jupiter less than 0.1 wt%. and from the southern polar cap of Mars. Polar rovers or penetrators with mass We estimate the total permanently spectrometers can detect these species. For shadowed area in the lunar northern polar region solving the question of the origin of lunar polar at 28 260,2 km2. The total permanently volatiles we must determine isotopic shadowed area in the region of the south pole of composition of these species. -
Craters in Shadow
Section 3: Craters in Shadow Kepler Copernicus Eratosthenes Seen it Clavius Seen it Section 3: Craters in Shadow Visibility: A pair of binoculars is the minimum requirement to see these features. When: Look for them when the terminator’s close by, typically a day before last quarter. Not all craters are best seen when the Sun is high in the lunar sky - in fact most aren’t! If craters aren’t par- ticularly bright or dark, they tend to disappear into the background when the Moon’s phase is close to full. These craters are best seen when the ‘terminator’ is nearby, or when the Sun is low in the lunar sky as seen from the crater. This causes oblique lighting to fall on the crater and create exaggerated shadows. Ultimately, this makes the crater look more dramatic and easier to see. We’ll use this effect for the next section on lunar mountains, but before we do, there are a couple of craters that we’d like to bring to your attention. Actually, the Moon is covered with a whole host of wonderful craters that look amazing when the lighting is oblique. During the summer and into the early autumn, it’s the later phases of the Moon are best positioned in the sky - the phases following full Moon. Unfortunately, this means viewing in the early hours but don’t worry as we’ve kept things simple. We just want to give you a taste of what a shadowed crater looks like for this marathon, so the going here is really pretty easy! First, locate the two craters Kepler and Copernicus which were marathon targets pointed out in Section 2. -
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. -
Planning a Mission to the Lunar South Pole
Lunar Reconnaissance Orbiter: (Diviner) Audience Planning a Mission to Grades 9-10 the Lunar South Pole Time Recommended 1-2 hours AAAS STANDARDS Learning Objectives: • 12A/H1: Exhibit traits such as curiosity, honesty, open- • Learn about recent discoveries in lunar science. ness, and skepticism when making investigations, and value those traits in others. • Deduce information from various sources of scientific data. • 12E/H4: Insist that the key assumptions and reasoning in • Use critical thinking to compare and evaluate different datasets. any argument—whether one’s own or that of others—be • Participate in team-based decision-making. made explicit; analyze the arguments for flawed assump- • Use logical arguments and supporting information to justify decisions. tions, flawed reasoning, or both; and be critical of the claims if any flaws in the argument are found. • 4A/H3: Increasingly sophisticated technology is used Preparation: to learn about the universe. Visual, radio, and X-ray See teacher procedure for any details. telescopes collect information from across the entire spectrum of electromagnetic waves; computers handle Background Information: data and complicated computations to interpret them; space probes send back data and materials from The Moon’s surface thermal environment is among the most extreme of any remote parts of the solar system; and accelerators give planetary body in the solar system. With no atmosphere to store heat or filter subatomic particles energies that simulate conditions in the Sun’s radiation, midday temperatures on the Moon’s surface can reach the stars and in the early history of the universe before 127°C (hotter than boiling water) whereas at night they can fall as low as stars formed. -
List of Missions Using SPICE (PDF)
1/7/20 Data Restorations Selected Past Users Current/Pending Users Examples of Possible Future Users Apollo 15, 16 [L] Magellan [L] Cassini Orbiter NASA Discovery Program Mariner 2 [L] Clementine (NRL) Mars Odyssey NASA New Frontiers Program Mariner 9 [L] Mars 96 (RSA) Mars Exploration Rover Lunar IceCube (Moorehead State) Mariner 10 [L] Mars Pathfinder Mars Reconnaissance Orbiter LunaH-Map (Arizona State) Viking Orbiters [L] NEAR Mars Science Laboratory Luna-Glob (RSA) Viking Landers [L] Deep Space 1 Juno Aditya-L1 (ISRO) Pioneer 10/11/12 [L] Galileo MAVEN Examples of Users not Requesting NAIF Help Haley armada [L] Genesis SMAP (Earth Science) GOLD (LASP, UCF) (Earth Science) [L] Phobos 2 [L] (RSA) Deep Impact OSIRIS REx Hera (ESA) Ulysses [L] Huygens Probe (ESA) [L] InSight ExoMars RSP (ESA, RSA) Voyagers [L] Stardust/NExT Mars 2020 Emmirates Mars Mission (UAE via LASP) Lunar Orbiter [L] Mars Global Surveyor Europa Clipper Hayabusa-2 (JAXA) Helios 1,2 [L] Phoenix NISAR (NASA and ISRO) Proba-3 (ESA) EPOXI Psyche Parker Solar Probe GRAIL Lucy EUMETSAT GEO satellites [L] DAWN Lunar Reconnaissance Orbiter MOM (ISRO) Messenger Mars Express (ESA) Chandrayan-2 (ISRO) Phobos Sample Return (RSA) ExoMars 2016 (ESA, RSA) Solar Orbiter (ESA) Venus Express (ESA) Akatsuki (JAXA) STEREO [L] Rosetta (ESA) Korean Pathfinder Lunar Orbiter (KARI) Spitzer Space Telescope [L] [L] = limited use Chandrayaan-1 (ISRO) New Horizons Kepler [L] [S] = special services Hayabusa (JAXA) JUICE (ESA) Hubble Space Telescope [S][L] Kaguya (JAXA) Bepicolombo (ESA, JAXA) James Webb Space Telescope [S][L] LADEE Altius (Belgian earth science satellite) ISO [S] (ESA) Armadillo (CubeSat, by UT at Austin) Last updated: 1/7/20 Smart-1 (ESA) Deep Space Network Spectrum-RG (RSA) NAIF has or had project-supplied funding to support mission operations, consultation for flight team members, and SPICE data archive preparation. -
10Great Features for Moon Watchers
Sinus Aestuum is a lava pond hemming the Imbrium debris. Mare Orientale is another of the Moon’s large impact basins, Beginning observing On its eastern edge, dark volcanic material erupted explosively and possibly the youngest. Lunar scientists think it formed 170 along a rille. Although this region at first appears featureless, million years after Mare Imbrium. And although “Mare Orien- observe it at several different lunar phases and you’ll see the tale” translates to “Eastern Sea,” in 1961, the International dark area grow more apparent as the Sun climbs higher. Astronomical Union changed the way astronomers denote great features for Occupying a region below and a bit left of the Moon’s dead lunar directions. The result is that Mare Orientale now sits on center, Mare Nubium lies far from many lunar showpiece sites. the Moon’s western limb. From Earth we never see most of it. Look for it as the dark region above magnificent Tycho Crater. When you observe the Cauchy Domes, you’ll be looking at Yet this small region, where lava plains meet highlands, con- shield volcanoes that erupted from lunar vents. The lava cooled Moon watchers tains a variety of interesting geologic features — impact craters, slowly, so it had a chance to spread and form gentle slopes. 10Our natural satellite offers plenty of targets you can spot through any size telescope. lava-flooded plains, tectonic faulting, and debris from distant In a geologic sense, our Moon is now quiet. The only events by Michael E. Bakich impacts — that are great for telescopic exploring. -
Boguslawsky Crater, Moon: Studying the Luna-Glob Landing Site
EPSC Abstracts Vol. 9, EPSC2014-699, 2014 European Planetary Science Congress 2014 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2014 Boguslawsky Crater, Moon: Studying the Luna-Glob Landing Site H. Hiesinger (1), M. Ivanov (2), J. W. Head (3), A. T. Basilevsky (2), J. H. Pasckert (1), K. Bauch (1), C. H. van der Bogert (1), A. M. Abdrahimov (2); (1) Institut für Planetologie, Westfälische Wilhelms-Universität, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany ([email protected]), (2) Vernadsky Institute, Moscow, Russia, (3) Brown University, Providence, RI, USA. Abstract rim of Boguslawsky crater and is of Eratosthenian age (Ec) [8]. Boussingault crater, which superposes The main objective of the Russian Luna-Glob Boguslawsly crater in the NE is somewhat younger lander, which will land on the floor of Boguslawsky than Boguslawsky crater, but is still of pre-Nectarian crater (~95 km in diameter, centered at 72.9S, age [8]. 43.26E), is to test landing techniques. However, it will also carry a small scientific payload. Two landing ellipses, 30x15 km each, are under investigation: Ellipse West is at 72.9S, 41.3E, Ellipse East is at 73.3S, 43.9E [1]. 1. Introduction For our study, we used data from the Lunar Reconnaissance Orbiter [Wide and Narrow Angle Camera images (WAC, NAC), Diviner temperature data, MiniRF radar data, laser altimeter data (LOLA)] 3 and Chandraayan (M ). We geologically mapped the crater, investigated its morphology and morphometry, Fig. 1: Geologic map of Boguslawsky crater. Landing ellipses are performed crater size-frequency distribution (CSFD) shown in white. measurements to derive absolute model ages, On the basis of high-resolution LROC images, we calculated temperatures and thermal inertia, derived identified six geologic units within Boguslawsky rock abundances, and counted rocks in selected areas crater, including smooth plains fp, rolling plains rp, of interest. -
Coalescence and Particle Self-Assembly of Inkjet-Printed Colloidal Drops
Coalescence and Particle Self-assembly of Inkjet-printed Colloidal Drops A Thesis Submitted to the Faculty of Drexel University by Xin Yang in partial fulfillment of the requirements for the degree of Doctor of Philosophy December 2014 ii © Copyright 2014 Xin Yang. All Rights Reserved. iii Acknowledgements I would like to thank my advisor Prof. Ying Sun. During the last 3 years, she supports and guides me throughout the course of my Ph.D. research with her profound knowledge and experience. Her dedication and passion for researches greatly encourages me in pursuing my career goals. I greatly appreciate her contribution to my growth during my Ph.D. training. I would like to thank my parents, my girlfriend, my colleagues (Brandon, Charles, Dani, Gang, Dong-Ook, Han, Min, Nate, and Viral) and friends (Abraham, Mahamudur, Kewei, Patrick, Xiang, and Yontae). I greatly appreciate Prof. Nicholas Cernansky, Prof. Bakhtier Farouk, Prof. Adam Fontecchio, Prof. Frank Ji, Prof. Alan Lau, Prof. Christopher Li, Prof. Mathew McCarthy, and Prof. Hongseok (Moses) Noh for their critical assessments and positive suggestions during my candidacy exam, proposal and my defense. I also appreciate the financial supports of National Science Foundation (Grant CAREER-0968927 and CMMI-1200385). iv TABLE OF CONTENTS LIST OF TABLES ............................................................................................................ vii LIST OF FIGURES ......................................................................................................... viii -
The Composition of the Lunar Crust: Radiative Transfer Modeling and Analysis of Lunar Visible and Near-Infrared Spectra
THE COMPOSITION OF THE LUNAR CRUST: RADIATIVE TRANSFER MODELING AND ANALYSIS OF LUNAR VISIBLE AND NEAR-INFRARED SPECTRA A DISSERTATION SUBMITTED TO THE GRADUATE DIVISION OF THE UNIVERSITY OF HAWAI‘I IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN GEOLOGY AND GEOPHYSICS DECEMBER 2009 By Joshua T.S. Cahill Dissertation Committee: Paul G. Lucey, Chairperson G. Jeffrey Taylor Patricia Fryer Jeffrey J. Gillis-Davis Trevor Sorensen Student: Joshua T.S. Cahill Student ID#: 1565-1460 Field: Geology and Geophysics Graduation date: December 2009 Title: The Composition of the Lunar Crust: Radiative Transfer Modeling and Analysis of Lunar Visible and Near-Infrared Spectra We certify that we have read this dissertation and that, in our opinion, it is satisfactory in scope and quality as a dissertation for the degree of Doctor of Philosophy in Geology and Geophysics. Dissertation Committee: Names Signatures Paul G. Lucey, Chairperson ____________________________ G. Jeffrey Taylor ____________________________ Jeffrey J. Gillis-Davis ____________________________ Patricia Fryer ____________________________ Trevor Sorensen ____________________________ ACKNOWLEDGEMENTS I must first express my love and appreciation to my family. Thank you to my wife Karen for providing love, support, and perspective. And to our little girl Maggie who only recently became part of our family and has already provided priceless memories in the form of beautiful smiles, belly laughs, and little bear hugs. The two of you provided me with the most meaningful reasons to push towards the "finish line". I would also like to thank my immediate and extended family. Many of them do not fully understand much about what I do, but support the endeavor acknowledging that if it is something I’m willing to put this much effort into, it must be worthwhile. -
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. -
Into the Unknown Together the DOD, NASA, and Early Spaceflight
Frontmatter 11/23/05 10:12 AM Page i Into the Unknown Together The DOD, NASA, and Early Spaceflight MARK ERICKSON Lieutenant Colonel, USAF Air University Press Maxwell Air Force Base, Alabama September 2005 Frontmatter 11/23/05 10:12 AM Page ii Air University Library Cataloging Data Erickson, Mark, 1962- Into the unknown together : the DOD, NASA and early spaceflight / Mark Erick- son. p. ; cm. Includes bibliographical references and index. ISBN 1-58566-140-6 1. Manned space flight—Government policy—United States—History. 2. National Aeronautics and Space Administration—History. 3. Astronautics, Military—Govern- ment policy—United States. 4. United States. Air Force—History. 5. United States. Dept. of Defense—History. I. Title. 629.45'009'73––dc22 Disclaimer Opinions, conclusions, and recommendations expressed or implied within are solely those of the editor and do not necessarily represent the views of Air University, the United States Air Force, the Department of Defense, or any other US government agency. Cleared for public re- lease: distribution unlimited. Air University Press 131 West Shumacher Avenue Maxwell AFB AL 36112-6615 http://aupress.maxwell.af.mil ii Frontmatter 11/23/05 10:12 AM Page iii To Becky, Anna, and Jessica You make it all worthwhile. THIS PAGE INTENTIONALLY LEFT BLANK Frontmatter 11/23/05 10:12 AM Page v Contents Chapter Page DISCLAIMER . ii DEDICATION . iii ABOUT THE AUTHOR . ix 1 NECESSARY PRECONDITIONS . 1 Ambling toward Sputnik . 3 NASA’s Predecessor Organization and the DOD . 18 Notes . 24 2 EISENHOWER ACT I: REACTION TO SPUTNIK AND THE BIRTH OF NASA . 31 Eisenhower Attempts to Calm the Nation . -
Constraining the Evolutionary History of the Moon and the Inner Solar System: a Case for New Returned Lunar Samples
Space Sci Rev (2019) 215:54 https://doi.org/10.1007/s11214-019-0622-x Constraining the Evolutionary History of the Moon and the Inner Solar System: A Case for New Returned Lunar Samples Romain Tartèse1 · Mahesh Anand2,3 · Jérôme Gattacceca4 · Katherine H. Joy1 · James I. Mortimer2 · John F. Pernet-Fisher1 · Sara Russell3 · Joshua F. Snape5 · Benjamin P. Weiss6 Received: 23 August 2019 / Accepted: 25 November 2019 / Published online: 2 December 2019 © The Author(s) 2019 Abstract The Moon is the only planetary body other than the Earth for which samples have been collected in situ by humans and robotic missions and returned to Earth. Scien- tific investigations of the first lunar samples returned by the Apollo 11 astronauts 50 years ago transformed the way we think most planetary bodies form and evolve. Identification of anorthositic clasts in Apollo 11 samples led to the formulation of the magma ocean concept, and by extension the idea that the Moon experienced large-scale melting and differentiation. This concept of magma oceans would soon be applied to other terrestrial planets and large asteroidal bodies. Dating of basaltic fragments returned from the Moon also showed that a relatively small planetary body could sustain volcanic activity for more than a billion years after its formation. Finally, studies of the lunar regolith showed that in addition to contain- ing a treasure trove of the Moon’s history, it also provided us with a rich archive of the past 4.5 billion years of evolution of the inner Solar System. Further investigations of samples returned from the Moon over the past five decades led to many additional discoveries, but also raised new and fundamental questions that are difficult to address with currently avail- able samples, such as those related to the age of the Moon, duration of lunar volcanism, the Role of Sample Return in Addressing Major Questions in Planetary Sciences Edited by Mahesh Anand, Sara Russell, Yangting Lin, Meenakshi Wadhwa, Kuljeet Kaur Marhas and Shogo Tachibana B R.