Second Lunar and Planetary Science Conference
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Lunar Impact Crater Identification and Age Estimation with Chang’E
ARTICLE https://doi.org/10.1038/s41467-020-20215-y OPEN Lunar impact crater identification and age estimation with Chang’E data by deep and transfer learning ✉ Chen Yang 1,2 , Haishi Zhao 3, Lorenzo Bruzzone4, Jon Atli Benediktsson 5, Yanchun Liang3, Bin Liu 2, ✉ ✉ Xingguo Zeng 2, Renchu Guan 3 , Chunlai Li 2 & Ziyuan Ouyang1,2 1234567890():,; Impact craters, which can be considered the lunar equivalent of fossils, are the most dominant lunar surface features and record the history of the Solar System. We address the problem of automatic crater detection and age estimation. From initially small numbers of recognized craters and dated craters, i.e., 7895 and 1411, respectively, we progressively identify new craters and estimate their ages with Chang’E data and stratigraphic information by transfer learning using deep neural networks. This results in the identification of 109,956 new craters, which is more than a dozen times greater than the initial number of recognized craters. The formation systems of 18,996 newly detected craters larger than 8 km are esti- mated. Here, a new lunar crater database for the mid- and low-latitude regions of the Moon is derived and distributed to the planetary community together with the related data analysis. 1 College of Earth Sciences, Jilin University, 130061 Changchun, China. 2 Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, 100101 Beijing, China. 3 Key Laboratory of Symbol Computation and Knowledge Engineering of Ministry of Education, College of Computer Science and Technology, Jilin University, 130012 Changchun, China. 4 Department of Information Engineering and Computer ✉ Science, University of Trento, I-38122 Trento, Italy. -
Evolution of Lunar Mantle Properties During Magma Ocean Crystallization and Mantle Overturn
EPSC Abstracts Vol. 13, EPSC-DPS2019-1703-1, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Evolution of Lunar Mantle Properties during Magma Ocean Crystallization and Mantle Overturn Sabrina Schwinger (1) and Doris Breuer (1) (1) German Aerospace Center (DLR) Berlin, Germany ([email protected]) Abstract 2.2 Mantle Mixing and Overturn We apply petrological models to investigate the As a consequence of the higher compatibility of evolution of lunar mantle mineralogy, considering lighter Mg compared to denser Fe in the LMO lunar magma ocean (LMO) crystallization and cumulate minerals, the density of the cumulate overturn of cumulate reservoirs. The results are used increases with progressing LMO solidification. This to test the consistency of different LMO results in a gravitationally unstable cumulate compositions and mantle overturn scenarios with the stratification that facilitates convective overturn. The physical properties of the bulk Moon. changes in pressure and temperature a cumulate layer experiences during overturn as well as mixing and chemical equilibration of different layers can affect 1. Introduction the mineralogy and physical properties of the lunar The mineralogy of the lunar mantle has been shaped mantle. To investigate these changes, we calculated by a sequence of several processes since the equilibrium mineral parageneses of different formation of the Moon, including lunar magma ocean cumulate layers using Perple_X [7]. For simplicity crystallization, cumulate overturn and partial -
South Pole-Aitken Basin: Crater Size-Frequency Distribution Measurements
EPSC Abstracts Vol. 7 EPSC2012-832 2012 European Planetary Science Congress 2012 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2012 South Pole-Aitken Basin: Crater Size-Frequency Distribution Measurements H. Hiesinger1, C. H. van der Bogert1, J. H. Pasckert1, N. Schmedemann2, M.S. Robinson3, B. Jolliff4, and N. Petro5; 1Institut für Planetologie (IfP), WWU Münster, Wilhelm-Klemm-Straße 10, 48149 Münster, Germany ([email protected]/ +49-251-8339057), 2Institute of Geosciences, Freie Universität Berlin, Germany, 3Arizona State University, Tempe, USA, 4Dept. of Earth and Planet. Sci. Washington Univ., St. Louis, USA, 5Goddard Spaceflight Center, Greenbelt, USA. Introduction morphology and topography derived from the LROC Being the largest basin (>2500 km in diameter) WAC mosaic and LOLA. LOLA topography was and presumably the oldest preserved impact structure also used to identify old and highly degraded impact on the Moon [e.g., 1], the South Pole-Aitken (SPA) structures and to improve our statistics in areas with basin is of particular interest. SPA might have large shadows close to the pole. The CSFDs were penetrated the entire lunar crust and exposed lower plotted with CraterStats [7], applying the lunar crustal or upper mantle material, but despite its deep chronology (CF) of [8] and the production function penetration, it did not reveal KREEP-rich rocks in (PF) of [9]. From this we derived absolute model contrast with the Imbrium basin. In addition, its age ages (AMAs) for craters between ~1.5 km and 300 should shed light on the plausibility of the terminal km in diameter [9]. More details on the technique of cataclysm [e.g., 2]. -
Volcanic History of the Imbrium Basin: a Close-Up View from the Lunar Rover Yutu
Volcanic history of the Imbrium basin: A close-up view from the lunar rover Yutu Jinhai Zhanga, Wei Yanga, Sen Hua, Yangting Lina,1, Guangyou Fangb, Chunlai Lic, Wenxi Pengd, Sanyuan Zhue, Zhiping Hef, Bin Zhoub, Hongyu Ling, Jianfeng Yangh, Enhai Liui, Yuchen Xua, Jianyu Wangf, Zhenxing Yaoa, Yongliao Zouc, Jun Yanc, and Ziyuan Ouyangj aKey Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing 100029, China; bInstitute of Electronics, Chinese Academy of Sciences, Beijing 100190, China; cNational Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; dInstitute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China; eKey Laboratory of Mineralogy and Metallogeny, Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou 510640, China; fKey Laboratory of Space Active Opto-Electronics Technology, Shanghai Institute of Technical Physics, Chinese Academy of Sciences, Shanghai 200083, China; gThe Fifth Laboratory, Beijing Institute of Space Mechanics & Electricity, Beijing 100076, China; hXi’an Institute of Optics and Precision Mechanics, Chinese Academy of Sciences, Xi’an 710119, China; iInstitute of Optics and Electronics, Chinese Academy of Sciences, Chengdu 610209, China; and jInstitute of Geochemistry, Chinese Academy of Science, Guiyang 550002, China Edited by Mark H. Thiemens, University of California, San Diego, La Jolla, CA, and approved March 24, 2015 (received for review February 13, 2015) We report the surface exploration by the lunar rover Yutu that flows in Mare Imbrium was obtained only by remote sensing from landed on the young lava flow in the northeastern part of the orbit. On December 14, 2013, Chang’e-3 successfully landed on the Mare Imbrium, which is the largest basin on the nearside of the young and high-Ti lava flow in the northeastern Mare Imbrium, Moon and is filled with several basalt units estimated to date from about 10 km south from the old low-Ti basalt unit (Fig. -
New Candidate Pits and Caves at High Latitudes on the Near Side of the Moon
52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 2733.pdf NEW CANDIDATE PITS AND CAVES AT HIGH LATITUDES ON THE NEAR SIDE OF THE MOON. 1,2 1,3,4 1 2 Wynnie Avent II and Pascal Lee , S ETI Institute, Mountain View, VA, USA, V irginia Polytechnic Institute 3 4 and State University Blacksburg, VA, USA. M ars Institute, N ASA Ames Research Center. Summary: 35 new candidate pits are identified in Anaxagoras and Philolaus, two high-latitude impact structures on the near side of the Moon. Introduction: Since the discovery in 2009 of the Marius Hills Pit (Haruyama et al. 2009), a.k.a. the “Haruyama Cavern”, over 300 hundred pits have been identified on the Moon (Wagner & Robinson 2014, Robinson & Wagner 2018). Lunar pits are small (10 to 150 m across), steep-walled, negative relief features (topographic depressions), surrounded by funnel-shaped outer slopes and, unlike impact craters, no raised rim. They are interpreted as collapse features resulting from the fall of the roof of shallow (a few Figure 1: Location of studied craters (Polar meters deep) subsurface voids, generally lava cavities. projection). Although pits on the Moon are found in mare basalt, impact melt deposits, and highland terrain of the >300 Methods: Like previous studies searching for pits pits known, all but 16 are in impact melts (Robinson & (Wagner & Robinson 2014, Robinson & Wagner 2018, Wagner 2018). Many pits are likely lava tube skylights, Lee 2018a,b,c), we used imaging data collected by the providing access to underground networks of NASA Lunar Reconnaissance Orbiter (LRO) Narrow tunnel-shaped caves, including possibly complex Angle Camera (NAC). -
Bombardment History of the Moon: What We Think We Know and What We Don’T Know Donald Bogard, ARES-KR, NASA-JSC, Houston, TX 77058 ([email protected])
Planetary Chronology Workshop 2006 6001.pdf Bombardment History of the Moon: What We Think We Know and What We Don’t Know Donald Bogard, ARES-KR, NASA-JSC, Houston, TX 77058 ([email protected]) Summary. The absolute impact history of and 14 soils show a decrease in the number of the moon and inner solar system can in principle beads with age from ~4 Gyr ago to ~0.4 Gyr ago, be derived from the statistics of radiometric ages followed by a significant increase in beads with of shock-heated planetary samples (lunar or age <0.4 Gyr (2). These authors concluded that meteoritic), from the formation ages of specific the projectile flux had decreased over time, impact craters on the moon or Earth; and from followed by a significant flux increase more age-dating samples representing geologic surface recently. However, this data set has also been units on the moon (or Mars) for which crater interpreted to represent variable rates of impact densities have been determined. This impact melt production as a function of regolith maturity history, however, is still poorly defined. (3). In another study, measured ages of 21 small The heavily cratered surface of the moon is a impact melt clasts in four lunar meteorites from testimony to the importance of impact events in the lunar highlands suggested four to six impact the evolution of terrestrial planets and satellites. events over the period ~2.5-4.0 Gyr ago (4). Lunar impacts range in scale from an early Clearly considerable uncertainty exists in the intense flux of large objects that defined the projectile flux over the past ~3.5 Gyr and whether surface geology of the moon, down to recent, this flux has been approximately constant or smaller impacts that continually generate and exhibited appreciable shorter-term variations. -
Exploring the Bombardment History of the Moon
EXPLORING THE BOMBARDMENT HISTORY OF THE MOON Community White Paper to the Planetary Decadal Survey, 2011-2020 September 15, 2009 Primary Author: William F. Bottke Center for Lunar Origin and Evolution (CLOE) NASA Lunar Science Institute at the Southwest Research Institute 1050 Walnut St., Suite 300 Boulder, CO 80302 Tel: (303) 546-6066 [email protected] Co-Authors/Endorsers: Carlton Allen (NASA JSC) Mahesh Anand (Open U., UK) Nadine Barlow (NAU) Donald Bogard (NASA JSC) Gwen Barnes (U. Idaho) Clark Chapman (SwRI) Barbara A. Cohen (NASA MSFC) Ian A. Crawford (Birkbeck College London, UK) Andrew Daga (U. North Dakota) Luke Dones (SwRI) Dean Eppler (NASA JSC) Vera Assis Fernandes (Berkeley Geochronlogy Center and U. Manchester) Bernard H. Foing (SMART-1, ESA RSSD; Dir., Int. Lunar Expl. Work. Group) Lisa R. Gaddis (US Geological Survey) 1 Jim N. Head (Raytheon) Fredrick P. Horz (LZ Technology/ESCG) Brad Jolliff (Washington U., St Louis) Christian Koeberl (U. Vienna, Austria) Michelle Kirchoff (SwRI) David Kring (LPI) Harold F. (Hal) Levison (SwRI) Simone Marchi (U. Padova, Italy) Charles Meyer (NASA JSC) David A. Minton (U. Arizona) Stephen J. Mojzsis (U. Colorado) Clive Neal (U. Notre Dame) Laurence E. Nyquist (NASA JSC) David Nesvorny (SWRI) Anne Peslier (NASA JSC) Noah Petro (GSFC) Carle Pieters (Brown U.) Jeff Plescia (Johns Hopkins U.) Mark Robinson (Arizona State U.) Greg Schmidt (NASA Lunar Science Institute, NASA Ames) Sen. Harrison H. Schmitt (Apollo 17 Astronaut; U. Wisconsin-Madison) John Spray (U. New Brunswick, Canada) Sarah Stewart-Mukhopadhyay (Harvard U.) Timothy Swindle (U. Arizona) Lawrence Taylor (U. Tennessee-Knoxville) Ross Taylor (Australian National U., Australia) Mark Wieczorek (Institut de Physique du Globe de Paris, France) Nicolle Zellner (Albion College) Maria Zuber (MIT) 2 The Moon is unique. -
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. -
Warren and Taylor-2014-In Tog-The Moon-'Author's Personal Copy'.Pdf
This article was originally published in Treatise on Geochemistry, Second Edition published by Elsevier, and the attached copy is provided by Elsevier for the author's benefit and for the benefit of the author's institution, for non- commercial research and educational use including without limitation use in instruction at your institution, sending it to specific colleagues who you know, and providing a copy to your institution’s administrator. All other uses, reproduction and distribution, including without limitation commercial reprints, selling or licensing copies or access, or posting on open internet sites, your personal or institution’s website or repository, are prohibited. For exceptions, permission may be sought for such use through Elsevier's permissions site at: http://www.elsevier.com/locate/permissionusematerial Warren P.H., and Taylor G.J. (2014) The Moon. In: Holland H.D. and Turekian K.K. (eds.) Treatise on Geochemistry, Second Edition, vol. 2, pp. 213-250. Oxford: Elsevier. © 2014 Elsevier Ltd. All rights reserved. Author's personal copy 2.9 The Moon PH Warren, University of California, Los Angeles, CA, USA GJ Taylor, University of Hawai‘i, Honolulu, HI, USA ã 2014 Elsevier Ltd. All rights reserved. This article is a revision of the previous edition article by P. H. Warren, volume 1, pp. 559–599, © 2003, Elsevier Ltd. 2.9.1 Introduction: The Lunar Context 213 2.9.2 The Lunar Geochemical Database 214 2.9.2.1 Artificially Acquired Samples 214 2.9.2.2 Lunar Meteorites 214 2.9.2.3 Remote-Sensing Data 215 2.9.3 Mare Volcanism -
The Futurist Moment : Avant-Garde, Avant Guerre, and the Language of Rupture
MARJORIE PERLOFF Avant-Garde, Avant Guerre, and the Language of Rupture THE UNIVERSITY OF CHICAGO PRESS CHICAGO AND LONDON FUTURIST Marjorie Perloff is professor of English and comparative literature at Stanford University. She is the author of many articles and books, including The Dance of the Intellect: Studies in the Poetry of the Pound Tradition and The Poetics of Indeterminacy: Rimbaud to Cage. Published with the assistance of the J. Paul Getty Trust Permission to quote from the following sources is gratefully acknowledged: Ezra Pound, Personae. Copyright 1926 by Ezra Pound. Used by permission of New Directions Publishing Corp. Ezra Pound, Collected Early Poems. Copyright 1976 by the Trustees of the Ezra Pound Literary Property Trust. All rights reserved. Used by permission of New Directions Publishing Corp. Ezra Pound, The Cantos of Ezra Pound. Copyright 1934, 1948, 1956 by Ezra Pound. Used by permission of New Directions Publishing Corp. Blaise Cendrars, Selected Writings. Copyright 1962, 1966 by Walter Albert. Used by permission of New Directions Publishing Corp. The University of Chicago Press, Chicago 60637 The University of Chicago Press, Ltd., London © 1986 by The University of Chicago All rights reserved. Published 1986 Printed in the United States of America 95 94 93 92 91 90 89 88 87 86 54321 Library of Congress Cataloging-in-Publication Data Perloff, Marjorie. The futurist moment. Bibliography: p. Includes index. 1. Futurism. 2. Arts, Modern—20th century. I. Title. NX600.F8P46 1986 700'. 94 86-3147 ISBN 0-226-65731-0 For DAVID ANTIN CONTENTS List of Illustrations ix Abbreviations xiii Preface xvii 1. -
TRANSIENT LUNAR PHENOMENA: REGULARITY and REALITY Arlin P
The Astrophysical Journal, 697:1–15, 2009 May 20 doi:10.1088/0004-637X/697/1/1 C 2009. The American Astronomical Society. All rights reserved. Printed in the U.S.A. TRANSIENT LUNAR PHENOMENA: REGULARITY AND REALITY Arlin P. S. Crotts Department of Astronomy, Columbia University, Columbia Astrophysics Laboratory, 550 West 120th Street, New York, NY 10027, USA Received 2007 June 27; accepted 2009 February 20; published 2009 April 30 ABSTRACT Transient lunar phenomena (TLPs) have been reported for centuries, but their nature is largely unsettled, and even their existence as a coherent phenomenon is controversial. Nonetheless, TLP data show regularities in the observations; a key question is whether this structure is imposed by processes tied to the lunar surface, or by terrestrial atmospheric or human observer effects. I interrogate an extensive catalog of TLPs to gauge how human factors determine the distribution of TLP reports. The sample is grouped according to variables which should produce differing results if determining factors involve humans, and not reflecting phenomena tied to the lunar surface. Features dependent on human factors can then be excluded. Regardless of how the sample is split, the results are similar: ∼50% of reports originate from near Aristarchus, ∼16% from Plato, ∼6% from recent, major impacts (Copernicus, Kepler, Tycho, and Aristarchus), plus several at Grimaldi. Mare Crisium produces a robust signal in some cases (however, Crisium is too large for a “feature” as defined). TLP count consistency for these features indicates that ∼80% of these may be real. Some commonly reported sites disappear from the robust averages, including Alphonsus, Ross D, and Gassendi. -
Rare Earth Elements in Planetary Crusts: Insights from Chemically Evolved Igneous Suites on Earth and the Moon
minerals Article Rare Earth Elements in Planetary Crusts: Insights from Chemically Evolved Igneous Suites on Earth and the Moon Claire L. McLeod 1,* and Barry J. Shaulis 2 1 Department of Geology and Environmental Earth Sciences, 203 Shideler Hall, Miami University, Oxford, OH 45056, USA 2 Department of Geosciences, Trace Element and Radiogenic Isotope Lab (TRaIL), University of Arkansas, Fayetteville, AR 72701, USA; [email protected] * Correspondence: [email protected]; Tel.: +1-513-529-9662 Received: 5 July 2018; Accepted: 8 October 2018; Published: 16 October 2018 Abstract: The abundance of the rare earth elements (REEs) in Earth’s crust has become the intense focus of study in recent years due to the increasing societal demand for REEs, their increasing utilization in modern-day technology, and the geopolitics associated with their global distribution. Within the context of chemically evolved igneous suites, 122 REE deposits have been identified as being associated with intrusive dike, granitic pegmatites, carbonatites, and alkaline igneous rocks, including A-type granites and undersaturated rocks. These REE resource minerals are not unlimited and with a 5–10% growth in global demand for REEs per annum, consideration of other potential REE sources and their geological and chemical associations is warranted. The Earth’s moon is a planetary object that underwent silicate-metal differentiation early during its history. Following ~99% solidification of a primordial lunar magma ocean, residual liquids were enriched in potassium, REE, and phosphorus (KREEP). While this reservoir has not been directly sampled, its chemical signature has been identified in several lunar lithologies and the Procellarum KREEP Terrane (PKT) on the lunar nearside has an estimated volume of KREEP-rich lithologies at depth of 2.2 × 108 km3.