GRAIL-Identified Gravity Anomalies in Oceanus Procellarum: Insight Into 2 Subsurface Impact and Magmatic Structures on the Moon 3 4 Ariel N
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Geologic Structure of Shallow Maria
NASA CR. Photo Data Analysis S-221 NASA Contract NAS 9-13196 GEOLOGIC STRUCTURE OF SHALLOW MARIA Rene' A. De Hon, Principal Investigator John A. Waskom, Co-Investigator (NASA-CR-lq7qoo GEOLOGIC STahJCTUnF OF N76-17001 ISBALOW M1BIA-'(Arkansas Uni.v., mHiticelio.) 96 p BC $5.00' CSCL O3B Unclas G3/91, 09970- University of Arkansas at Monticello Monticello, Arkansas December 1975 Photo Data Analysis S-221 NASA Contract NAS 9-13196 GEOLOGIC STRUCTURE OF SHALLOW MARIA Rene' A. De Hon, Principal Investigator I John A. Waskom, Co-Investigator Un-iversity-of Arkansas-:at-.Monticl o Monticello, Arkansas December 1975 ABSTRACT Isopach maps and structural contour maps of the 0 0 eastern mare basins (30 N to 30 OS; 00 to 100 E) are constructed from measurements of partially buried craters. The data, which are sufficiently scattered to yield gross thickness variations, are restricted to shallow maria with less than 1500-2000 m of mare basalts. The average thickness of b-asalt in the irregular maria is between 200 and 400 m. Multiringed mascon basins are filled to various levels. The Serenitatis and Crisium basins have deeply flooded interiors and extensively flooded shelves. Mare basalts in the Nectaris basin fill only the innermost basin, and mare basalts in the Smythii basin occupy a small portion of the basin floor. Sinus Amoris, Mare Spumans, and Mare Undarum are partially filled troughs concentric to large circular basins. The Tranquillitatis and Fecunditatis are composite depressions containing basalts which flood degraded circular basins and adjacent terrain modified by the formation of nearby cir cular basins. -
EPSC-DPS2011-1845, 2011 EPSC-DPS Joint Meeting 2011 C Author(S) 2011
EPSC Abstracts Vol. 6, EPSC-DPS2011-1845, 2011 EPSC-DPS Joint Meeting 2011 c Author(s) 2011 Analysis of mineralogy of an effusive volcanic lunar dome in Marius Hills, Oceanus Procellarum. A.S. Arya, Guneshwar Thangjam, R.P. Rajasekhar, Ajai Space Applications Centre, Indian Space Research Organization, Ahmedabad-380 015 (India). Email:[email protected] Abstract found on the lunar surface. As a part of initiation of the study of mineralogy of MHC, an effusive dome Domes are analogous to the terrestrial shield located in the south of Rima Galilaei, near the volcanoes and are among the important volcanic contact of Imbrian and Eratosthenian geological units features found on the lunar surface indicative of is taken up for the present study. The morphology, effusive vents of primary volcanism within Mare rheology and the possible dike parameters have regions. Marius Hills Complex (MHC) is one of the already been studied and reported [5]. most important regions on the entire lunar surface, having a complex geological setting and largest distribution of volcanic constructs with an abundant number of volcanic features like domes, cones and rilles. The mineralogical study of an effusive dome located in the south of Rima Galilaei, near the contact of Imbrian and Eratosthenian geological units is done using hyperspectral band parameters and spectral plots so as to understand the compositional variation, the nature of the volcanism and relate it to the rheology of the dome. Fig. 1: Distribution of dome in MHC (Red-the dome under study, Green- from Virtual Moon Atlas, Magenta [6]) and the Study area showing the dome under study on M3 1. -
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. -
Bills Paid by Payee Second Quarter Fiscal Year 20/21
BILLS PAID BY PAYEE SECOND QUARTER FISCAL YEAR 20/21 A complete detailed record is available at the Elko County Comptroller's Office. Office Hours: Monday-Friday 8:00A.M. until 5:00P.M. 540 Court St. Suite 101 Elko, NV 89801 Office Phone (775)753-7073*Disclaimer-The original and any duplicate or copy of each receipt, bill,check,warrant,voucher or other similar document that supports a transaction, the amount of which is shown in the total of this report, along with the name of the person whom such allowance is made and the purpose of the allowance, is a public record that is available for inspection and copying by any person pursuant to the provisions of chapter 239 of NRS. VENDOR CHECK ARGO COMPANY, INC 821.98 A ARNOLD BECK CONSTRUCTION 1,599.40 AT&T 3,697.06 5TH GEAR POWER SPORTS 41.74 AT&T MOBILITY 42.24 A PLUS URGENT CARE 766 AUTO GRAPHICS 400 A PLUS URGENT CARE ELKO 846.33 B A-1 RADIATOR REPAIR INC. 1,079.00 BARBARA J HOFHEINS 121.9 ACKERMAN MATTHEW 1388.93 BARBARA JO MAPLE 762.5 ADVANCE AUTO CARE 629.89 BARRY RENTAL 86.03 ADVANCED RADIOLOGY 1195.5 BEI CAPELI 5,000.00 AIRGAS 541.3 BERTOLINI VALVES INC 1,859.12 AIRPORT SHELL 9 BETTY HICKS 177.56 ALCOHOL MONITORING SYSTEMS INC 791 BLAINE ROBINSON & NIKIERA CAST 1,132.00 ALERTUS TECHNOLOGIES LLC 4,950.00 BLOHM JEWELERS INC 5,000.00 ALICIA GUAMAN 58 BLUE 360 MEDIA LLC 70.75 ALLIED UNIVERAL SECURITY SERVI 37,229.50 BOARD OF REGENTS 14300.04 ALLUSIVE IMAGES 5,000.00 BOB BARKER COMPANY 4418.55 ALYSSA K DANN 120 BONANZA PRODUCE 320.23 AMANDA JEAN GIRMAUDO 160 BOSS TANKS 5,024.00 AMBER DAWN -
Mare Domes in Mare Tranquillitatis: Identification, Distribution, Characteristics, and Implications for Their Origin and the Oldest Lunar Volcanism
51st Lunar and Planetary Science Conference (2020) 1798.pdf MARE DOMES IN MARE TRANQUILLITATIS: IDENTIFICATION, DISTRIBUTION, CHARACTERISTICS, AND IMPLICATIONS FOR THEIR ORIGIN AND THE OLDEST LUNAR VOLCANISM. L. Qiao1, J. W. Head2, L. Wilson3 and Z. Ling1, 1Inst. Space Sci., Shandong Univ., Weihai, Shan- dong, 264209, China ([email protected]), 2Dep. Earth, Env. & Planet. Sci., Brown Univ., Providence, RI, 02912, USA, 3Lancaster Env. Centre, Lancaster Univ., Lancaster LA1 4YQ, UK. Introduction: Volcanism is one of the major geo- General Characteristics and Identification Crite- logical process on the Moon, directly reflecting the ria of Mare Domes. A preliminary survey of previous- composition and thermal state of lunar interior and its ly-catalogued mare domes [1-4] reveals some of their evolution, and serves as an important window into the fundamental characteristics. A typical well-developed geological and thermal evolution of the Moon. Mare mare dome is characterized by a domical raised struc- domes, small (<~30 km diameter) and generally circu- ture with a generally convex-shape and low-slope (<5°) lar structures with convex-upward shapes [1], are profile and a (quasi-)circular or elliptical outline. Some among the most common volcanic landforms on the domes have summit pit craters, while many lack them, Moon. Over 300 mare domes have been previously possibly being filled up by the last eruptions. The de- identified, using mainly telescope and orbital photo- velopment of the circular mound shape of mare domes graphs [e.g., 1-4]. -
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. -
Special Catalogue Milestones of Lunar Mapping and Photography Four Centuries of Selenography on the Occasion of the 50Th Anniversary of Apollo 11 Moon Landing
Special Catalogue Milestones of Lunar Mapping and Photography Four Centuries of Selenography On the occasion of the 50th anniversary of Apollo 11 moon landing Please note: A specific item in this catalogue may be sold or is on hold if the provided link to our online inventory (by clicking on the blue-highlighted author name) doesn't work! Milestones of Science Books phone +49 (0) 177 – 2 41 0006 www.milestone-books.de [email protected] Member of ILAB and VDA Catalogue 07-2019 Copyright © 2019 Milestones of Science Books. All rights reserved Page 2 of 71 Authors in Chronological Order Author Year No. Author Year No. BIRT, William 1869 7 SCHEINER, Christoph 1614 72 PROCTOR, Richard 1873 66 WILKINS, John 1640 87 NASMYTH, James 1874 58, 59, 60, 61 SCHYRLEUS DE RHEITA, Anton 1645 77 NEISON, Edmund 1876 62, 63 HEVELIUS, Johannes 1647 29 LOHRMANN, Wilhelm 1878 42, 43, 44 RICCIOLI, Giambattista 1651 67 SCHMIDT, Johann 1878 75 GALILEI, Galileo 1653 22 WEINEK, Ladislaus 1885 84 KIRCHER, Athanasius 1660 31 PRINZ, Wilhelm 1894 65 CHERUBIN D'ORLEANS, Capuchin 1671 8 ELGER, Thomas Gwyn 1895 15 EIMMART, Georg Christoph 1696 14 FAUTH, Philipp 1895 17 KEILL, John 1718 30 KRIEGER, Johann 1898 33 BIANCHINI, Francesco 1728 6 LOEWY, Maurice 1899 39, 40 DOPPELMAYR, Johann Gabriel 1730 11 FRANZ, Julius Heinrich 1901 21 MAUPERTUIS, Pierre Louis 1741 50 PICKERING, William 1904 64 WOLFF, Christian von 1747 88 FAUTH, Philipp 1907 18 CLAIRAUT, Alexis-Claude 1765 9 GOODACRE, Walter 1910 23 MAYER, Johann Tobias 1770 51 KRIEGER, Johann 1912 34 SAVOY, Gaspare 1770 71 LE MORVAN, Charles 1914 37 EULER, Leonhard 1772 16 WEGENER, Alfred 1921 83 MAYER, Johann Tobias 1775 52 GOODACRE, Walter 1931 24 SCHRÖTER, Johann Hieronymus 1791 76 FAUTH, Philipp 1932 19 GRUITHUISEN, Franz von Paula 1825 25 WILKINS, Hugh Percy 1937 86 LOHRMANN, Wilhelm Gotthelf 1824 41 USSR ACADEMY 1959 1 BEER, Wilhelm 1834 4 ARTHUR, David 1960 3 BEER, Wilhelm 1837 5 HACKMAN, Robert 1960 27 MÄDLER, Johann Heinrich 1837 49 KUIPER Gerard P. -
A Zircon U-Pb Study of the Evolution of Lunar KREEP
A zircon U-Pb study of the evolution of lunar KREEP By A.A. Nemchin, R.T. Pidgeon, M.J. Whitehouse, J.P. Vaughan and C. Meyer Abstract SIMS U-Pb analyses show that zircons from breccias from Apollo 14 and Apollo 17 have essentially identical age distributions in the range 4350 to 4200 Ma but, whereas Apollo 14 zircons additionally show ages from 4200 to 3900 Ma, the Apollo 17 samples have no zircons with ages <4200 Ma. The zircon results also show an uneven distribution with distinct peaks of magmatic activity. In explaining these observations we propose that periodic episodes of KREEP magmatism were generated from a primary reservoir of KREEP magma, which contracted over time towards the centre of Procellarum KREEP terrane. Introduction One of the most enigmatic features of the geology of the Moon is the presence of high concentrations of large ion lithophile elements in clasts from breccias from non mare regions. This material, referred to as KREEP (1) from its high levels of K, REE and P, also contains relatively high concentrations of other incompatible elements including Th, U and Zr. Fragments of rocks with KREEP trace element signatures have been identified in samples from all Apollo landing sites (2). The presence of phosphate minerals, such as apatite and merrillite (3); zirconium minerals, such as zircon (4), zirconolite (5) and badelleyite (6), and rare earth minerals such as yttrobetafite (7), are direct expressions of the presence of KREEP. Dickinson and Hess (8) concluded that about 9000 ppm of Zr in basaltic melt is required to saturate it with zircon at about 1100oC (the saturation concentration increases exponentially with increasing temperature). -
A Guideline for a Sustainable Lunar Base Design for Constructed in Lunar Lava Tubes and Their Vertical Skylights
50th International Conference on Environmental Systems ICES-2021-186 12-15 July 2021 A Guideline for a Sustainable Lunar Base Design for Constructed in Lunar Lava Tubes and Their Vertical Skylights Masato Sakurai1, Asuka Shima2, Isao Kawano3, Junichi Haruyama4 Japan Aerospace Exploration Agency (JAXA), Chofu-shi, Tokyo, 182-8522, Japan. and Hiroyuki Miyajima5 International University of Health and Welfare, Narita Campus 1, 4-3, Kōzunomori, Narita, Chiba, 286-8686 Japan The lunar surface is a hostile environment subject to harmful radiation and meteorite impacts. A recently discovered lava tube avoids these risks and, as it undergoes only slight temperature changes, it is a promising location for constructing a lunar base. JAXA engages in research in regenerative ECLSS (Environmental Control Life Support Systems), particularly addressing water and air recycling and treating organic waste. Overcoming these challenges is essential for long-term lunar habitation. This paper presents a guideline for a sustainable lunar base design. Nomenclature ECLSS = Environmental Control Life Support System HTV = H-II Transfer Vehicle ISS = International Space Station JAXA = Japan Aerospace Exploration Agency JSASS = Japan Society for Aeronautical and Space Science MHH = Marius Hills Hole MIH = Mare Ingenii Hole MTH = Mare Tranquillitatis Hole SELENE = Selenological and Engineering Explorer UZUME = Unprecedented Zipangu Underworld of the Moon Exploration (name of the research group for vertical holes) SDGs = Sustainable Development Goals SELENE = Selenological and Engineering Explorer I. Introduction uture space exploration will extend beyond low Earth orbit and dramatically expand in scope. In particular, F industrial activities are planned for the Moon with the development of infrastructure that includes lunar bases. This paper summarizes our study of the construction of a crewed permanent settlement, which will be essential to support long-term habitation, resource utilization, and industrial activities on the Moon. -
Sky and Telescope
SkyandTelescope.com The Lunar 100 By Charles A. Wood Just about every telescope user is familiar with French comet hunter Charles Messier's catalog of fuzzy objects. Messier's 18th-century listing of 109 galaxies, clusters, and nebulae contains some of the largest, brightest, and most visually interesting deep-sky treasures visible from the Northern Hemisphere. Little wonder that observing all the M objects is regarded as a virtual rite of passage for amateur astronomers. But the night sky offers an object that is larger, brighter, and more visually captivating than anything on Messier's list: the Moon. Yet many backyard astronomers never go beyond the astro-tourist stage to acquire the knowledge and understanding necessary to really appreciate what they're looking at, and how magnificent and amazing it truly is. Perhaps this is because after they identify a few of the Moon's most conspicuous features, many amateurs don't know where Many Lunar 100 selections are plainly visible in this image of the full Moon, while others require to look next. a more detailed view, different illumination, or favorable libration. North is up. S&T: Gary The Lunar 100 list is an attempt to provide Moon lovers with Seronik something akin to what deep-sky observers enjoy with the Messier catalog: a selection of telescopic sights to ignite interest and enhance understanding. Presented here is a selection of the Moon's 100 most interesting regions, craters, basins, mountains, rilles, and domes. I challenge observers to find and observe them all and, more important, to consider what each feature tells us about lunar and Earth history. -
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