Geologic Structure of Shallow Maria
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Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED -
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. -
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. -
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 -
Planetary Science : a Lunar Perspective
APPENDICES APPENDIX I Reference Abbreviations AJS: American Journal of Science Ancient Sun: The Ancient Sun: Fossil Record in the Earth, Moon and Meteorites (Eds. R. 0.Pepin, et al.), Pergamon Press (1980) Geochim. Cosmochim. Acta Suppl. 13 Ap. J.: Astrophysical Journal Apollo 15: The Apollo 1.5 Lunar Samples, Lunar Science Insti- tute, Houston, Texas (1972) Apollo 16 Workshop: Workshop on Apollo 16, LPI Technical Report 81- 01, Lunar and Planetary Institute, Houston (1981) Basaltic Volcanism: Basaltic Volcanism on the Terrestrial Planets, Per- gamon Press (1981) Bull. GSA: Bulletin of the Geological Society of America EOS: EOS, Transactions of the American Geophysical Union EPSL: Earth and Planetary Science Letters GCA: Geochimica et Cosmochimica Acta GRL: Geophysical Research Letters Impact Cratering: Impact and Explosion Cratering (Eds. D. J. Roddy, et al.), 1301 pp., Pergamon Press (1977) JGR: Journal of Geophysical Research LS 111: Lunar Science III (Lunar Science Institute) see extended abstract of Lunar Science Conferences Appendix I1 LS IV: Lunar Science IV (Lunar Science Institute) LS V: Lunar Science V (Lunar Science Institute) LS VI: Lunar Science VI (Lunar Science Institute) LS VII: Lunar Science VII (Lunar Science Institute) LS VIII: Lunar Science VIII (Lunar Science Institute LPS IX: Lunar and Planetary Science IX (Lunar and Plane- tary Institute LPS X: Lunar and Planetary Science X (Lunar and Plane- tary Institute) LPS XI: Lunar and Planetary Science XI (Lunar and Plane- tary Institute) LPS XII: Lunar and Planetary Science XII (Lunar and Planetary Institute) 444 Appendix I Lunar Highlands Crust: Proceedings of the Conference in the Lunar High- lands Crust, 505 pp., Pergamon Press (1980) Geo- chim. -
DMAAC – February 1973
LUNAR TOPOGRAPHIC ORTHOPHOTOMAP (LTO) AND LUNAR ORTHOPHOTMAP (LO) SERIES (Published by DMATC) Lunar Topographic Orthophotmaps and Lunar Orthophotomaps Scale: 1:250,000 Projection: Transverse Mercator Sheet Size: 25.5”x 26.5” The Lunar Topographic Orthophotmaps and Lunar Orthophotomaps Series are the first comprehensive and continuous mapping to be accomplished from Apollo Mission 15-17 mapping photographs. This series is also the first major effort to apply recent advances in orthophotography to lunar mapping. Presently developed maps of this series were designed to support initial lunar scientific investigations primarily employing results of Apollo Mission 15-17 data. Individual maps of this series cover 4 degrees of lunar latitude and 5 degrees of lunar longitude consisting of 1/16 of the area of a 1:1,000,000 scale Lunar Astronautical Chart (LAC) (Section 4.2.1). Their apha-numeric identification (example – LTO38B1) consists of the designator LTO for topographic orthophoto editions or LO for orthophoto editions followed by the LAC number in which they fall, followed by an A, B, C or D designator defining the pertinent LAC quadrant and a 1, 2, 3, or 4 designator defining the specific sub-quadrant actually covered. The following designation (250) identifies the sheets as being at 1:250,000 scale. The LTO editions display 100-meter contours, 50-meter supplemental contours and spot elevations in a red overprint to the base, which is lithographed in black and white. LO editions are identical except that all relief information is omitted and selenographic graticule is restricted to border ticks, presenting an umencumbered view of lunar features imaged by the photographic base. -
SMART-1 Lunar Highlights Bernard H
SMART-1 lunar highlights Bernard H. Foing & SMART-1 Project & Operations team, SMART-1 Science Technology Working Team, SMART-1 Impact Campaign Team http://sci.esa.int/smart-1/, www.esa.int BHF 2007 Europe to the Moon: spacecraft, launch, operations (ESA+ industry) Instruments PIs + TIs from 5 countries Co-Is from 13 ESA + 6 non European countries BHF 2007 Solar Electric Primary Propulsion: 7 g thrust, 60 liters Xenon to the Moon BHF 2007 SMART-1: With Sun power to the Moon on 60 liters of fuel BHF 2007 Solar Electric Propulsion to the Moon – Launched 27 Sept 2003 as Auxiliary passenger on Ariane 5 into Geostationary Transfer Orbit – Spiral out cruise (13.5 month): – lunar capture 15 November 2004, spiral down – arrival 15 March 05 science(450 -2900 km): commissioned spacecraft/instruments at Moon, nominal science mission March-July 05 – reboosting 2 aug-15 Sept 05 to increase orbit lifetime for extension phase until Aug 2006 BHF 2007 AMIE /SMART-1 End August 2006 Earth set & rise from the Moon X AMIE /SMART-1 May 21st, 2004 Earth view from ~70’000 km BHF 2007 First European Far Side Image of The Moon by AMIE/SMART-1 North Pole 12 Nov. 2004 BHF 2007 Moon Phase & Mission Extension MISSION EXTENSION Apolune Perilune Moon Radius BHF 2007 Sun SMART-1 light Reflecte d Sun Triple junction solar cells Multicolor microcamera light KA-band antenna Laser Link Communication X-Ray Spectrometer On-board computer Lithium ion batteries Infrared Spectrometer OBAN Platform Autonomy Technologies Miniaturisation BHF 2007 SMART-1 Science and Exploration Themes -
The Moon After Apollo
ICARUS 25, 495-537 (1975) The Moon after Apollo PAROUK EL-BAZ National Air and Space Museum, Smithsonian Institution, Washington, D.G- 20560 Received September 17, 1974 The Apollo missions have gradually increased our knowledge of the Moon's chemistry, age, and mode of formation of its surface features and materials. Apollo 11 and 12 landings proved that mare materials are volcanic rocks that were derived from deep-seated basaltic melts about 3.7 and 3.2 billion years ago, respec- tively. Later missions provided additional information on lunar mare basalts as well as the older, anorthositic, highland rocks. Data on the chemical make-up of returned samples were extended to larger areas of the Moon by orbiting geo- chemical experiments. These have also mapped inhomogeneities in lunar surface chemistry, including radioactive anomalies on both the near and far sides. Lunar samples and photographs indicate that the moon is a well-preserved museum of ancient impact scars. The crust of the Moon, which was formed about 4.6 billion years ago, was subjected to intensive metamorphism by large impacts. Although bombardment continues to the present day, the rate and size of impact- ing bodies were much greater in the first 0.7 billion years of the Moon's history. The last of the large, circular, multiringed basins occurred about 3.9 billion years ago. These basins, many of which show positive gravity anomalies (mascons), were flooded by volcanic basalts during a period of at least 600 million years. In addition to filling the circular basins, more so on the near side than on the far side, the basalts also covered lowlands and circum-basin troughs. -
List of Targets for the Lunar II Observing Program (PDF File)
Task or Task Description or Target Name Wood's Rükl Target LUNAR # 100 Atlas Catalog (chart) Create a sketch/map of the visible lunar surface: 1 Observe a Full Moon and sketch a large-scale (prominent features) L-1 map depicting the nearside; disk of visible surface should be drawn 2 at L-1 3 least 5-inches in diameter. Sketch itself should be created only by L-1 observing the Moon, but maps or guidebooks may be used when labeling sketched features. Label all maria, prominent craters, and major rays by the crater name they originated from. (Counts as 3 observations (OBSV): #1, #2 & #3) Observe these targets; provide brief descriptions: 4 Alpetragius 55 5 Arago 35 6 Arago Alpha & Arago Beta L-32 35 7 Aristarchus Plateau L-18 18 8 Baco L-55 74 9 Bailly L-37 71 10 Beer, Beer Catena & Feuillée 21 11 Bullialdus, Bullialdus A & Bullialdus B 53 12 Cassini, Cassini A & Cassini B 12 13 Cauchy, Cauchy Omega & Cauchy Tau L-48 36 14 Censorinus 47 15 Crüger 50 16 Dorsae Lister & Smirnov (A.K.A. Serpentine Ridge) L-33 24 17 Grimaldi Basin outer and inner rings L-36 39, etc. 18 Hainzel, Hainzel A & Hainzel C 63 19 Hercules, Hercules G, Hercules E 14 20 Hesiodus A L-81 54, 64 21 Hortensius dome field L-65 30 22 Julius Caesar 34 23 Kies 53 24 Kies Pi L-60 53 25 Lacus Mortis 14 26 Linne 23 27 Lamont L-53 35 28 Mairan 9 29 Mare Australe L-56 76 30 Mare Cognitum 42, etc. -
Water on the Moon, III. Volatiles & Activity
Water on The Moon, III. Volatiles & Activity Arlin Crotts (Columbia University) For centuries some scientists have argued that there is activity on the Moon (or water, as recounted in Parts I & II), while others have thought the Moon is simply a dead, inactive world. [1] The question comes in several forms: is there a detectable atmosphere? Does the surface of the Moon change? What causes interior seismic activity? From a more modern viewpoint, we now know that as much carbon monoxide as water was excavated during the LCROSS impact, as detailed in Part I, and a comparable amount of other volatiles were found. At one time the Moon outgassed prodigious amounts of water and hydrogen in volcanic fire fountains, but released similar amounts of volatile sulfur (or SO2), and presumably large amounts of carbon dioxide or monoxide, if theory is to be believed. So water on the Moon is associated with other gases. Astronomers have agreed for centuries that there is no firm evidence for “weather” on the Moon visible from Earth, and little evidence of thick atmosphere. [2] How would one detect the Moon’s atmosphere from Earth? An obvious means is atmospheric refraction. As you watch the Sun set, its image is displaced by Earth’s atmospheric refraction at the horizon from the position it would have if there were no atmosphere, by roughly 0.6 degree (a bit more than the Sun’s angular diameter). On the Moon, any atmosphere would cause an analogous effect for a star passing behind the Moon during an occultation (multiplied by two since the light travels both into and out of the lunar atmosphere). -
ASTR110G Astronomy Laboratory Exercises C the GEAS Project 2020
ASTR110G Astronomy Laboratory Exercises c The GEAS Project 2020 ASTR110G Laboratory Exercises Lab 1: Fundamentals of Measurement and Error Analysis ...... ....................... 1 Lab 2: Observing the Sky ............................... ............................. 35 Lab 3: Cratering and the Lunar Surface ................... ........................... 73 Lab 4: Cratering and the Martian Surface ................. ........................... 97 Lab 5: Parallax Measurements and Determining Distances ... ....................... 129 Lab 6: The Hertzsprung-Russell Diagram and Stellar Evolution ..................... 157 Lab 7: Hubble’s Law and the Cosmic Distance Scale ........... ..................... 185 Lab 8: Properties of Galaxies .......................... ............................. 213 Appendix I: Definitions for Keywords ..................... .......................... 249 Appendix II: Supplies ................................. .............................. 263 Lab 1 Fundamentals of Measurement and Error Analysis 1.1 Introduction This laboratory exercise will serve as an introduction to all of the laboratory exercises for this course. We will explore proper techniques for obtaining and analyzing data, and practice plotting and analyzing data. We will discuss a scientific methodology for conducting exper- iments in which we formulate a question, predict the behavior of the system based on likely solutions, acquire relevant data, and then compare our predictions with the observations. You will have a chance to plan a short experiment,