July 2019 Medicine’S Lunar Legacies • René T
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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. -
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. -
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. -
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. -
Deep Carbon Emissions from Volcanoes Michael R
Reviews in Mineralogy & Geochemistry Vol. 75 pp. 323-354, 2013 11 Copyright © Mineralogical Society of America Deep Carbon Emissions from Volcanoes Michael R. Burton Istituto Nazionale di Geofisica e Vulcanologia Via della Faggiola, 32 56123 Pisa, Italy [email protected] Georgina M. Sawyer Laboratoire Magmas et Volcans, Université Blaise Pascal 5 rue Kessler, 63038 Clermont Ferrand, France and Istituto Nazionale di Geofisica e Vulcanologia Via della Faggiola, 32 56123 Pisa, Italy Domenico Granieri Istituto Nazionale di Geofisica e Vulcanologia Via della Faggiola, 32 56123 Pisa, Italy INTRODUCTION: VOLCANIC CO2 EMISSIONS IN THE GEOLOGICAL CARBON CYCLE Over long periods of time (~Ma), we may consider the oceans, atmosphere and biosphere as a single exospheric reservoir for CO2. The geological carbon cycle describes the inputs to this exosphere from mantle degassing, metamorphism of subducted carbonates and outputs from weathering of aluminosilicate rocks (Walker et al. 1981). A feedback mechanism relates the weathering rate with the amount of CO2 in the atmosphere via the greenhouse effect (e.g., Wang et al. 1976). An increase in atmospheric CO2 concentrations induces higher temperatures, leading to higher rates of weathering, which draw down atmospheric CO2 concentrations (Ber- ner 1991). Atmospheric CO2 concentrations are therefore stabilized over long timescales by this feedback mechanism (Zeebe and Caldeira 2008). This process may have played a role (Feulner et al. 2012) in stabilizing temperatures on Earth while solar radiation steadily increased due to stellar evolution (Bahcall et al. 2001). In this context the role of CO2 degassing from the Earth is clearly fundamental to the stability of the climate, and therefore to life on Earth. -
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. -
Salubrious Living
Salubrious Living 00. Salubrious Living - Introduction 01. The Search for Youth 02. The Myth of Medical Progress 03. The Hygienic System 04. The Nature of Disease 05. The Foods of Civilization 06. The Foods of Primitive Man 07. Don't Cook Your Foods 08. The Fruitarian Diet 09. How to Plan Your Meals 10. The Best Sources of Minerals and Vitamins 11. Soil and Food 12. Nature's Supreme Healing Agency 13. The Value of Heliotherapy 14. Building Strength and Health Through Exercise 15. Some Common Ailments 16. Why Lose Your Teeth? 17. Better Vision Without Glasses 18. Building Strong Feet 19. Keep Your Hair 20. The Needs of Infants and Growing Children 21. To Build Beauty You Must Build Health 22. Eugenics and the Survival of the White Race Author: Ben Klassen Format: Paperback Creativity Book Publisher Pub. Date: 1982 Food Chart Copyright © 2003 by World Church of Creativity Salubrious Living - Introduction The term "Salubrious Living" is a nomenclature I have coined as part and parcel of a very important facet of our religious creed and program set forth by the CHURCH OF THE CREATOR. The word "salubrious" comes from the Latin word "salubris" meaning "healthy; wholesome; sound; useful; vigorous". Webster's dictionary defines the English derivative "salubrious" as: 1. favorable to, or promoting health or well being; invigorating; 2. spiritually wholesome; conducive to good results". It is in this context of fully promoting the health and well being of the White Race that we use this term in its true literal meaning. We of the CHURCH OF THE CREATOR want to differentiate this term from "Natural Hygiene popularly used for many decades by health practitioners devoted to this worthy art and science. -
INDEX to 1915-1919 Obituaries in the Canton Repository
INDEX To 1915-1919 Obituaries in the Canton Repository Published by the Stark County District Library of Canton, Ohio 2005 Index to 1915-1919 Obituaries in the Canton Repository The following is an alphabetical listing, by the deceased’s surname, of obituaries that appeared in the Canton, Ohio newspaper, The Repository. It was compiled by the library staff during the course of the year in the hope that it would be a useful tool to genealogy, as well as other researchers. To use this index, simply locate the name of the person whose obituary you wish to find. The entries will appear as follows: Miller William A. (Estella M.) Mrs. 1924 Jan. 13 30 The first column is the name of the deceased. The second gives the date on which the item appeared. And the third tells the page number containing the obituary. You may find one name with multiple listings showing different dates and locations in the paper. This indicates consecutive listings for that individual. I encourage you to view each for additional information. Index to 1915-1919 Obituaries in the Canton Repository Surname Given Name Maiden Title Year Mth Day Pg ? Mary 1918 Apr. 18 15 Aaron Benjamin 1918 Nov. 27 2 Abbott Lawrence C. 1919 Mar. 14 24 Abels infant 1919 July 16 6 Abherve Minnie Jacobs Mrs. 1918 Dec. 13 33 Abrams Leo 1917 Apr. 24 2 Abt Leo 1918 Apr. 27 1 Abvrezis Macone 1917 Sept. 17 2 Acker L. E. 1918 Jan. 13 26 Acker Leonard E. 1918 Jan. 12 5 Acker Sarah Mrs. -
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. -
A Study About a Lunar Dome Near Hortensius: Morphometry and Mode of Formation
47th Lunar and Planetary Science Conference (2016) 1005.pdf A study about a lunar dome near Hortensius: Morphometry and mode of formation. M. Wirths1, R. Lena2 , A. Mallama3 - Geologic Lunar Research (GLR) Group. 1km 67 Camino Observatorio, Baja California, Mexico; [email protected]; 2 Via Cartesio 144, sc. D, 00137 Rome, Italy; [email protected]; 314012 Lancaster Lane, Bowie, MD, 20715, USA, [email protected] Introduction: Lunar mare domes formed during the later stages of volcanic episode on the Moon, char- acterized by a decreasing rate of lava extrusion and comparably low eruption temperatures, resulted in the formation of effusive domes. Important clusters of lu- nar domes are observed in the Hortensius/Milichius/T. Mayer region in Mare Insularum and in Mare Tranquillitatis around the craters Arago and Cauchy. The region west of Copernicus extending from Hortensius to Milichius and to Tobias Mayer contains large numbers of lunar domes and cones, evidence of past volcanism on the lunar surface [1-3]. A compre- hensive map of the area was produced by GLR group, including the six lunar domes north of Hortensius and three lower domes to the south of Hortensius [4]. Fig. 1. Telescopic image acquired on May 1, 2012, at 03:44 In this contribution we provide an analysis of an- UT with a 450 mm aperture Starmaster driven Dobsonian other low dome to the east of Hortensius, termed H11, (M. Wirths). Morphometric properties of the domes H1-H7 located at 26.87° W and 6.88° N and with a prominent have been examined in previous studies [1, 3]. -
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. -
Effusive Lunar Domes in Mare Tranquillitatis: Morphometry and Mode of Emplacement
Lunar and Planetary Science XXXIX (2008) 1107.pdf EFFUSIVE LUNAR DOMES IN MARE TRANQUILLITATIS: MORPHOMETRY AND MODE OF EMPLACEMENT. K. C. Pau1, R. Lena2, C. Wöhler3, M. T. Bregante4, G. Sbarufatti5 – Geologic Lunar Research (GLR) Group. 1Flat 20A, Fook Chak House, Tung Fai Gardens, 17 Po Yan Street, Sheung Wan, Hong Kong; [email protected]; 2Via Cartesio 144, sc. D, 00137 Rome, Italy; [email protected]; 3Daimler Group Research, P. O. Box 2360, D-89013 Ulm, Germany; [email protected]; 4Via Antica Romana Occ. 13, 16039 Sestri Levante Genova, Italy; [email protected]; 5Via Cabrini 10, 26842 Caselle Landi, Lodi, Italy; [email protected] Introduction: Lunar mare domes are smooth low by a low Titanium content, while the youngest lavas features with gentle convex upward profiles. They are erupted in this region are spectrally blue (high circular to elliptical in shape. Isolated domes may be Titanium content) [4,5]. The Carrel complex largely found in almost all maria, but significant concentra- represents the eastern rim of a ruined crater nearly tions occur in the Hortensius region, Oceanus Procel- completely buried by mare lava. In the Clementine larum, and Mare Tranquillitatis [1]. These domes are colour ratio image, the crater ruin and ejecta from commonly interpreted as shield volcanoes or laccoliths Carrel have the same reddish color as the mare surface [2]. Recent studies about lunar domes are based on the around Jansen. The soil around Ca1 and also C13 is evaluation of their spectrophotometric and morpho- spectrally bluish, indicating a moderate TiO2 content, metric properties, rheologic parameters, and their clas- while the dome A7 appears strongly blue, indicating sification based on the spectral properties and three- basalts of high TiO2 content (Figs.