Science Concept 3: Key Planetary Processes Are Manifested in the Diversity of Lunar Crustal Rocks
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GEOLOGIC MAPPING OF THE LUNAR SOUTH POLE QUADRANGLE (LQ-30). S.C. Mest1,2, D.C. Ber- man1, and N.E. Petro2, 1Planetary Science Institute, 1700 E. Ft. Lowell, Suite 106, Tucson, AZ 85719-2395 ([email protected]); 2Planetary Geodynamics Laboratory, Code 698, NASA GSFC, Greenbelt, MD 20771. Introduction: In this study we use recent image, the surface [7]. Impact craters display morphologies spectral and topographic data to map the geology of the ranging from simple to complex [7-9,24] and most lunar South Pole quadrangle (LQ-30) at 1:2.5M scale contain floor deposits distinct from surrounding mate- [1-7]. The overall objective of this research is to con- rials. Most of these deposits likely consist of impact strain the geologic evolution of LQ-30 (60°-90°S, 0°- melt; however, some deposits, especially on the floors ±180°) with specific emphasis on evaluation of a) the of the larger craters and basins (e.g., Antoniadi), ex- regional effects of impact basin formation, and b) the hibit low albedo and smooth surfaces and may contain spatial distribution of ejecta, in particular resulting mare. Higher albedo deposits tend to contain a higher from formation of the South Pole-Aitken (SPA) basin density of superposed impact craters. and other large basins. Key scientific objectives in- Antoniadi Crater. Antoniadi crater (D=150 km; clude: 1) Determining the geologic history of LQ-30 69.5°S, 172°W) is unique for several reasons. First, and examining the spatial and temporal variability of Antoniadi is the only lunar crater that contains both a geologic processes within the map area. -
Geoscience and a Lunar Base
" t N_iSA Conference Pubhcatmn 3070 " i J Geoscience and a Lunar Base A Comprehensive Plan for Lunar Explora, tion unclas HI/VI 02907_4 at ,unar | !' / | .... ._-.;} / [ | -- --_,,,_-_ |,, |, • • |,_nrrr|l , .l -- - -- - ....... = F _: .......... s_ dd]T_- ! JL --_ - - _ '- "_r: °-__.......... / _r NASA Conference Publication 3070 Geoscience and a Lunar Base A Comprehensive Plan for Lunar Exploration Edited by G. Jeffrey Taylor Institute of Meteoritics University of New Mexico Albuquerque, New Mexico Paul D. Spudis U.S. Geological Survey Branch of Astrogeology Flagstaff, Arizona Proceedings of a workshop sponsored by the National Aeronautics and Space Administration, Washington, D.C., and held at the Lunar and Planetary Institute Houston, Texas August 25-26, 1988 IW_A National Aeronautics and Space Administration Office of Management Scientific and Technical Information Division 1990 PREFACE This report was produced at the request of Dr. Michael B. Duke, Director of the Solar System Exploration Division of the NASA Johnson Space Center. At a meeting of the Lunar and Planetary Sample Team (LAPST), Dr. Duke (at the time also Science Director of the Office of Exploration, NASA Headquarters) suggested that future lunar geoscience activities had not been planned systematically and that geoscience goals for the lunar base program were not articulated well. LAPST is a panel that advises NASA on lunar sample allocations and also serves as an advocate for lunar science within the planetary science community. LAPST took it upon itself to organize some formal geoscience planning for a lunar base by creating a document that outlines the types of missions and activities that are needed to understand the Moon and its geologic history. -
Chandrayaan-2 Completes a Year Around the Moon
One-year completion of Chandrayaan-2 Lunar orbit insertion (August 20, 2019) Chandrayaan-2 completes a year around the Moon The Moon provides the best linkage to understand Earth’s early history and offers an undisturbed record of the inner Solar system environment. It could also be a base for future human space exploration of the solar system and a unique laboratory, unlike any on Earth, for fundamental physics investigations. In spite of several missions to the Moon, there remains several unanswered questions. Continued high resolution studies of its surface, sub-surface/interior and its low-density exosphere, are essential to address diversities in lunar surface composition and to trace back the origin and evolution of the Moon. The clear evidence from India’s first mission to the Moon, Chandrayaan-1, on the extensive presence of surface water and the indication for sub- surface polar water-ice deposits, argues for more focused studies on the extent of water on the surface, below the surface and in the tenuous lunar exosphere, to address the true origin and availability of water on Moon. With the goal of expanding the lunar scientific knowledge through detailed studies of topography, mineralogy, surface chemical composition, thermo-physical characteristics and the lunar exosphere, Chandrayaan-2 was launched on 22nd July 2019 and inserted into the lunar orbit on 20th August 2019, exactly one year ago. Though the soft-landing attempt was not successful, the orbiter, which was equipped with eight scientific instruments, was successfully placed in the lunar orbit. The orbiter completed more than 4400 orbits around the Moon and all the instruments are currently performing well. -
No. 40. the System of Lunar Craters, Quadrant Ii Alice P
NO. 40. THE SYSTEM OF LUNAR CRATERS, QUADRANT II by D. W. G. ARTHUR, ALICE P. AGNIERAY, RUTH A. HORVATH ,tl l C.A. WOOD AND C. R. CHAPMAN \_9 (_ /_) March 14, 1964 ABSTRACT The designation, diameter, position, central-peak information, and state of completeness arc listed for each discernible crater in the second lunar quadrant with a diameter exceeding 3.5 km. The catalog contains more than 2,000 items and is illustrated by a map in 11 sections. his Communication is the second part of The However, since we also have suppressed many Greek System of Lunar Craters, which is a catalog in letters used by these authorities, there was need for four parts of all craters recognizable with reasonable some care in the incorporation of new letters to certainty on photographs and having diameters avoid confusion. Accordingly, the Greek letters greater than 3.5 kilometers. Thus it is a continua- added by us are always different from those that tion of Comm. LPL No. 30 of September 1963. The have been suppressed. Observers who wish may use format is the same except for some minor changes the omitted symbols of Blagg and Miiller without to improve clarity and legibility. The information in fear of ambiguity. the text of Comm. LPL No. 30 therefore applies to The photographic coverage of the second quad- this Communication also. rant is by no means uniform in quality, and certain Some of the minor changes mentioned above phases are not well represented. Thus for small cra- have been introduced because of the particular ters in certain longitudes there are no good determi- nature of the second lunar quadrant, most of which nations of the diameters, and our values are little is covered by the dark areas Mare Imbrium and better than rough estimates. -
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. -
Technical Note
NASA TN D-1493 O5 C,/ 1-4 I Q LOAJN' ? < TECHNICAL NOTE D-1493 ENVIRONMENTAL PROBLEMS OF SPACE FLIGHT STRUCTURES H. METEOROID HAZARD Prepared by John R. Davidson and Paul E. Sandorff in collaboration with the NASA Research Advisory Committee on Missile and Space Vehicle Structures Langley Research Center Langley Station, Hampton, Va. NATIONAL AERONAUTICS AND SPACE ADMINISTRATION WASHINGTON January 1963 TECH LIBRARY KAFB, NM Illllllll TABLE OF CONTENTS 0153^57 Page PREFACE li MEMBERS OF THE NASA RESEARCH ADVISORY COMMITTEE ON MISSILE AND SPACE VEHICLE STRUCTURES in SUMMARY 1 INTRODUCTION 1 SYMBOLS -. 2 METEOROID ENVIRONMENT ^ Asteroidal Particles ; . k Cometary Particles 5 Tektites 8 Pertubation Forces 9 Observations of Meteors From the Earth 10 Satellites and Space Probes 15 Research in Progress 18 INTERACTION BETWEEN METEOROID ENVIRONMENT AND STRUCTURE 19 Historical Aspects of the Plate Perforation Problem 19 Physical Description of High-Speed Impact Phenomena 20 Modern Theories of Penetration 22 Experimental Data .__ 26 PROTECTION METHODS 30 Types of Structural Damage 30 Application of Meteoroid Flux Data and Impact Data to Design Problems 30 RESEARCH IN PROGRESS 36 Ground Research 36 Flight Test Research 36 RECOMMENDED METEOROID RESEARCH PROGRAM 36 REFERENCES kO BIBLIOGRAPHY 1*7 TABLES 49 FIGURES 61 PREFACE The exploration, study, and definition of the environmental conditions which exist in space beyond the earth's atmosphere form an essential part of the current space-age effort. The development of this science is of especial interest to the vehicle structures designer, who must make decisions today that will establish the capability and efficiency of the space hardware in use 5 °r 10 years hence. -
General Disclaimer One Or More of the Following Statements May Affect
General Disclaimer One or more of the Following Statements may affect this Document This document has been reproduced from the best copy furnished by the organizational source. It is being released in the interest of making available as much information as possible. This document may contain data, which exceeds the sheet parameters. It was furnished in this condition by the organizational source and is the best copy available. This document may contain tone-on-tone or color graphs, charts and/or pictures, which have been reproduced in black and white. This document is paginated as submitted by the original source. Portions of this document are not fully legible due to the historical nature of some of the material. However, it is the best reproduction available from the original submission. Produced by the NASA Center for Aerospace Information (CASI) ^i e I !emote sousing sad eeolegio Studies of the llaistary Crusts Bernard Ray Hawke Prince-1 Investigator a EL r Z^ .99 University of Hawaii Hawaii Institute of Geophysics Planetary Geosciences Division Honolulu, Hawaii 96822 ^y 1i i W. December 1983 (NASA —CR-173215) REMOTE SENSING AND N84-17092 GEOLOGIC STUDIES OF THE PLANETARY CRUSTS Final Report ( Hawaii Inst. of Geophysics) 14 p HC A02/MF 101 CSCL 03B Unclas G3/91 11715 Gy -2- ©R1GNAL OF POOR QUALITY Table of Contents Page I. Remote Sensing and Geologic Studies cf Volcanic Deposits . • . 3 A. Spectral reflectance studies of dark-haloed craters. • . 3 B. Remote s^:sing studies of regions which were sites of ancient volcanisa . 3 C. [REEP basalt deposits in the Imbrium Region. -
Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
June 9, 2020 LIST of ABSENTEE VOTERS HOLDING BALLOTS – NAMES
WARSAW CENTRAL SCHOOL BUDGET/BOARD VOTE – June 9, 2020 LIST OF ABSENTEE VOTERS HOLDING BALLOTS – NAMES Abbasey, Salman Aumer, Andrew J. Bauer, James E. Abbott, John Axtell, Paula A. Bauer, Janet M. Ackerman, James Backlas, Frederick A. Jr Bauer, Michael Ackerman, Susan M. Bagg , Robert L. Bauer, Michelle Adolf, Jeremy J. Bagg, Kenneth G. Baxter, Susan Agrawal, Rajendra Bagg, Patty Bayliss, Bruce A. Aguado, Andrew E. Bagley, Raymond F. Bayoumi, Ahmed Ahl, Florence Bailey, Betty J. Beach, Douglas A. Aker, James D. Bailey, Judith L. Beach, Robert L. Akin, Claudia J. Bailey, Lyndsay Beals, Duane M. Alband, Jeffrey L. Bailey, Richard L. Beals, Shane Alcaraz, Christina M. Bailey, Stephen Beardsley, Peter G. Alderson, Donald P. Bailey, Stephen Beck, Michael J. Aldinger, Suzanne Bailey, Tara L. Beckstrand, Benjamine C. Aldrich, Heather L. Baize, Mary A. Beckstrand, Denise C. Aldrich, Jordan A. Baker, Arlene W. Beilein, Paul T. Aldrich, Kathryn J. Baker, Charles O. Beinhauer, Joseph F. Alexander, Christopher J. Baker, Frederic Belden, Barbara A. Alexander, Tara Baker, Gregory S. Belden, James C. Allen, Patricia A. Baker, Karen Bell, David K. Allison, Eddie R. Baker, Kirk E. Bell, Kathleen D. Almeter, David J Baker, Kristina Bell, Lorraine F. Almeter, George Anna Baker, Nichlos Bell, Milda Almeter, Nathan A. Baker, Peggy J. Bell, Mildred E. Almeter, Steven A. Baker, Roger O. Bellaire, Donald Ames, Gregory K. Baker, Shawn R. Bellaire, Donald W. Sr Ames, Richard A. Bakowski, Christopher Belles, Cody J. Andalora, Ingeburg Ballard, Joanne R. Bellinger, Heather Andalora, Orah Ballerstein, Lisa Bender, Gloria Andrews, Lee H. Ballew, Marjorie Bender, Sidney Antinore, Hope Bannister, Jeffrey H. -
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. -
August 2017 Posidonius P & Luther
A PUBLICATION OF THE LUNAR SECTION OF THE A.L.P.O. EDITED BY: Wayne Bailey [email protected] 17 Autumn Lane, Sewell, NJ 08080 RECENT BACK ISSUES: http://moon.scopesandscapes.com/tlo_back.html FEATURE OF THE MONTH – AUGUST 2017 POSIDONIUS P & LUTHER Sketch and text by Robert H. Hays, Jr. - Worth, Illinois, USA March 5, 2017 01:28-01:48; UT, 15 cm refl, 170x, seeing 7-8/10. I drew these craters on the evening of March 4/5, 2017 while the moon was hiding some Hyades stars. This area is in northeast Mare Serenitatis west of Posidonius itself. Posidonius P is the largest crater on this sketch. The smaller crater south of P is Posidonius F and Posidonius G is the tiny pit to the north. There is a halo around Posidonius G, but this crater is noticeably north of the halo's center. A very low round swelling is northeast of Posidonius G. Luther is the crater well to the west of Posidonius P. All four of these craters are crisp, symmetric features, differing only in size. There are an assortment of elevations near Luther. The peak Luther alpha is well to the west of Luther, and showed dark shadowing at this time. All of the other features near Luther are more subtle than Luther alpha. One mound is between Luther and Luther alpha. Two more mounds are north of Luther, and a low ridge is just east of this crater. A pair of very low mounds are south of Luther. These are the vaguest features depicted here, and may be too conspicuous on the sketch. -
Chenangoforks2.Pdf
• Rilles – Lunar Rilles are long, narrow, depressions formed by lava flows, resembling channels. • Rugged Terra – Rugged terra are mountainous regions of the moon. • Wrinkle Ridges – Wrinkle Ridges are created through compression of tectonic plates within the maria. • Graben – Graben are formed from the stress of two fault lines. • Scarps – A displacement of land beside a fault. • Fault – A fault is a fracture on the surface. Grabens Rilles Scarps Fault Rugged Terra Wrinkle Ridge •Scarp‐ A type of fault. It is the displacement of land alongside a fault. • Mare Ridge‐ The raised edges of a mare impact basin. •Trough‐ A depression that is characterized by its shallow ridges • Lineament‐ A linear expression used to characterize a fault lined valley •The wrinkle ridge structures that deform and interrupt the mare basalts are commonly asymmetrical, with the steeper side bounded by a complex scarp composed of multiple overlapping lobate scarp segments that may have rounded crests that make them resemble mare ridges. •Lobate scarps are thrust faults that occur primarily in the Moon's lunar highlands. •a graben is a depressed block of land bordered by parallel faults. •Graben is German for ditch. •A graben is the result of a block of land being downthrown producing a valley with a distinct scarp on each side. •Graben often occur side-by-side with horsts. Horst and graben structures are indicative of tensional forces and crustal stretching. •Horsts are parallel blocks that remain between graben, the bounding faults of a horst typically dip away from the center line of the horst. •Also known as a Dark halo craterlets •Dark-halo craters are formed when an impact unearths lower albedo material from below the surface, then deposits this darker ejecta around the main crater.