Lunar Features Named After Chinese
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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. -
EPSC2013-167, 2013 European Planetary Science Congress 2013 Eeuropeapn Planetarsy Science Ccongress C Author(S) 2013
EPSC Abstracts Vol. 8, EPSC2013-167, 2013 European Planetary Science Congress 2013 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2013 Scientific Characterization of Mare Moscoviense Region of Interest A. Calzada (1) and S.C. Mest (2,3) (1) Department of Earth and Planetary Sciences Birkbeck, University of London, Malet Street, Bloomsbury, London WC1E 7HX (2) Planetary Science Institute, 1700 E. Ft. Lowell, Suite 106, Tucson, AZ 85719-2395 and (3) Planetary Geodynamics Laboratory, Code 698, NASA GSFC, Greenbelt, MD 20771 Abstract NASA´s Constellation Program has identified 50 Regions of Interest (ROI) with high scientific value in preparation for an eventual return to the Moon [1]. These 50 locations are geological diverse and geographically distributed to achieve a variety of goals and objectives and described by LEAG [2]. In order to evaluate its scientific interest, Mare Moscoviense (MMos) ROI was characterized using digital images and data provided by NASA´s Clementine and Lunar Reconnaissance (LRO) Missions as well as ArcGISTM v.10.1 software to create a geomorphologic and geologic map. The cartography and the input were analyzed to propose a set of three hypothetical traverses for future human or robotic expeditions within an area up to distances of 5, 10 and 20 km from the ROI location. The traverses has no constrains regarding Figure 1 LRO WAC Image from Mare Moscoviense basin. Red schedule, distances or topography. Experiments box indicates the studied area. Credits: NASA/JPL/MSSS proposed vary from petrologic and geochemical characterization such as samples and drill cores to 2. Cartography geophysical experiments using gravimetry, magnetometry and seismicity methods. -
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 -
THE STUDY of SATURN's RINGS 1 Thesis Presented for the Degree Of
1 THE STUDY OF SATURN'S RINGS 1610-1675, Thesis presented for the Degree of Doctor of Philosophy in the Field of History of Science by Albert Van Haden Department of History of Science and Technology Imperial College of Science and Teohnology University of London May, 1970 2 ABSTRACT Shortly after the publication of his Starry Messenger, Galileo observed the planet Saturn for the first time through a telescope. To his surprise he discovered that the planet does.not exhibit a single disc, as all other planets do, but rather a central disc flanked by two smaller ones. In the following years, Galileo found that Sa- turn sometimes also appears without these lateral discs, and at other times with handle-like appendages istead of round discs. These ap- pearances posed a great problem to scientists, and this problem was not solved until 1656, while the solution was not fully accepted until about 1670. This thesis traces the problem of Saturn, from its initial form- ulation, through the period of gathering information, to the final stage in which theories were proposed, ending with the acceptance of one of these theories: the ring-theory of Christiaan Huygens. Although the improvement of the telescope had great bearing on the problem of Saturn, and is dealt with to some extent, many other factors were in- volved in the solution of the problem. It was as much a perceptual problem as a technical problem of telescopes, and the mental processes that led Huygens to its solution were symptomatic of the state of science in the 1650's and would have been out of place and perhaps impossible before Descartes. -
Robert Ayuso and Klaus Schulz Convenors September 14-16, 1992
DEPARTMENT OF THE INTERIOR UNITED STATES GEOLOGICAL SURVEY Informal Notes: WORKSHOP ON THE APPLICATION OF ISOTOPE SYSTEMS TO GEOLOGICAL PROBLEMS Robert Ayuso and Klaus Schulz Convenors September 14-16, 1992 Auditorium National Center Reston, Virginia 22092 Open-File Report 92-525 September 1992 This report is preliminary and has not been edited or reviewed for conformity with U.S. Geological Survey editorial standards and stratigraphic nomenclature. Any use of trade names is for descriptive purposes only and does not imply endorsement by the uses. List of Titles, Presenters, and Authors Page Introduction 1 Schedule of meeting 3 Innovative uses ofPb isotopic measurements: Dating stromatolites and tracing sand dunes by J. N. Aleinikoff (U.S. Geological Survey, Box 25046, Mail Stop 963, Denver Federal Center, Denver, CO 80225) 7 Pb-Nd-O isotopic compositions of igneous rocks: Implications for petrogenesis and terrane correlation, Cape Breton Island, Nova Scotia, Canada by R. Ayuso (U.S. Geological Survey, 954 National Center, Reston, VA 22092), S. Barr, F. Longstaffe, and E. Hegner 15 The use ofK-Ar and ^Ar/^Ar techniques to date multiple thermal events: An example from the Bayan Obo Fe-Nb-REE ore deposit, China by J. E. Conrad (U.S. Geological Survey, 345 Middlefield Road, Mail Stop 901, Menlo Park, CA 94025) 24 Lead isotopic composition of galena from Malaysia, an S-type granite terrane by B. R. Doe (U.S. Geological Survey, 104 National Center, Reston, VA 22092) 28 Mass spectrometric measurements of234^!/23^ and 230Th/238U and dating late Quaternary carbonates by R. L. Edwards (University of Minnesota, Department of Geology and Geophysics, Minneapolis, MN 55455) 63 Nd isotopes as tracers of the origin and evolution of the continental lithosphere by G. -
Remote Sensing
remote sensing Article Reevaluating Mare Moscoviense And Its Vicinity Using Chang’e-2 Microwave Sounder Data Zhiguo Meng 1,2,3,4, Shengbo Chen 1, Yongzhi Wang 1,2,3,* , Tianxing Wang 2 , Zhanchuan Cai 3, Yuanzhi Zhang 4 , Yongchun Zheng 4 and Shuo Hu 1 1 College of Geoexploration Science and Technology, Jilin University, Changchun 130026, China; [email protected] (Z.M.); [email protected] (S.C.); [email protected] (S.H.) 2 State Key Laboratory of Remote Sensing Science, Institute of Remote Sensing and Digital Earth, Chinese Academy of Sciences, Beijing 100101, China; [email protected] 3 State Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology, Macau, China; [email protected] 4 Key Laboratory of Lunar and Deep-space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China; [email protected] (Y.Z.); [email protected] (Y.Z.) * Correspondence: [email protected]; Tel.: +86-4318-850-2362 Received: 5 December 2019; Accepted: 5 February 2020; Published: 6 February 2020 Abstract: Mare Moscoviense (148◦E, 27◦N) is one of the few large maria on the lunar farside, with the thinnest crust and a positive gravity anomaly. In this paper, the Chang’E-2 Microwave Sounder (CELMS) data was employed to study the microwave thermal emission features of mare basalts in Moscoviense Basin. The time angle and linear interpolation method are used to generate the brightness temperature (TB) maps at noon and night, as well as the TB difference (dTB) map. The obtained important results are as follows. -
An Examination of Mare Age Based On
An Examination of Mare Age Based On Cratering Density The Chenango Forks Lunar Research Team: Sharon Hartzell, Jackson Haskell, Benjamin Daniels, Sarah Maximowicz, and Sarah Andrus Objective Cooled basaltic lava flows, known as maria, cover approximately sixteen percent of the lunar surface. The determination of absolute and relative ages of maria is an important question in lunar research, because it provides insight into the geologic history of the lunar environment. Many samples returned from the Apollo and Luna missions have been absolutely dated using radiogenic techniques. However, not all samples returned from the moon have been radiogenically dated. Furthermore, returned samples represent only a small portion of each visited mare. One of the major challenges facing lunar researches is the fact that most maria are still unvisited. The lack of complete data from visited maria in combination with the absence of data from unvisited maria has compelled lunar researchers to rely on remote techniques for relative dating. The overriding goal of our research was to develop and utilize a method for analyzing the ages of the twenty‐three lunar maria. Approach •Areas of the twenty‐three lunar maria were analyzed in three distinct investigations. Investigation 1: Total crater count to determine cratering densities, and comparison of densities to absolute age Investigation 2: Analysis of crater weathering in relation to age Investigation 3: Analysis of crater size in relation to age •A relative age map was created to display the distribution of the maria on the moon’s surface. The •Analysis of age dist ributions within individual mari a revealed several interesting trends: Investigation 1 map itself was obtained from Google Moon, and the maria were highlighted based on the scale Method displayed below. -
Special Supplement to the Bulletin of the American Meteorological Society Vol
J. Blunden, D. S. Arndt, and M. O. Baringer, Eds. Associate Eds. H. J. Diamond, A. J. Dolman, R. L. Fogt, B. D. Hall, M. Jeffries, J. M. Levy, J. M. Renwick, J. Richter-Menge, P. W. Thorne, L. A. Vincent, and K. M. Willett Special Supplement to the Bulletin of the American Meteorological Society Vol. 92, No. 6, June 2011 STATE OF THE CLIMATE IN 2010 STATE OF THE CLIMATE IN 2010 JUNE 2011 | S1 HOW TO CITE THIS DOCUMENT __________________________________________________________________________________________ Citing the complete report: Blunden, J., D. S. Arndt, and M. O. Baringer, Eds., 2011: State of the Climate in 2010. Bull. Amer. Meteor. Soc., 92 (6), S1 –S266. Citing a chapter (example): Fogt, R. L., Ed., 2011: Antarctica [in “State of the Climate in 2010”]. Bull. Amer. Meteor. Soc., 92 (6), S161 –S171. Citing a section (example): Wovrosh, A. J., S. Barreira, and R. L. Fogt, 2011: [Antarctica] Circulation [in “State of the Climate in 2010”]. Bull. Amer. Meteor. Soc., 92 (6), S161 –S163. S2 | JUNE 2011 Editor & Author Affiliations (ALPHABETICAL BY NAME ) Achberger, Christine, Earth Sciences Centre, University of Belward, Alan S., Global Environment Monitoring Unit, IES, EC Gothenburg, Gothenburg, Sweden Joint Research Centre, Ispra, Italy Ackerman, Steven A., CIMSS University of Wisconsin - Madi- Benedetti, Angela, European Centre for Medium-Range son, Madison, Wisconsin Weather Forecasts, Reading, United Kingdom Ahlstrøm, A., Geological Survey of Denmark and Greenland Berrisford, Paul, NCAS-Climate, European Centre for Medi- (GEUS), -
Reader 19 05 19 V75 Timeline Pagination
Plant Trivia TimeLine A Chronology of Plants and People The TimeLine presents world history from a botanical viewpoint. It includes brief stories of plant discovery and use that describe the roles of plants and plant science in human civilization. The Time- Line also provides you as an individual the opportunity to reflect on how the history of human interaction with the plant world has shaped and impacted your own life and heritage. Information included comes from secondary sources and compila- tions, which are cited. The author continues to chart events for the TimeLine and appreciates your critique of the many entries as well as suggestions for additions and improvements to the topics cov- ered. Send comments to planted[at]huntington.org 345 Million. This time marks the beginning of the Mississippian period. Together with the Pennsylvanian which followed (through to 225 million years BP), the two periods consti- BP tute the age of coal - often called the Carboniferous. 136 Million. With deposits from the Cretaceous period we see the first evidence of flower- 5-15 Billion+ 6 December. Carbon (the basis of organic life), oxygen, and other elements ing plants. (Bold, Alexopoulos, & Delevoryas, 1980) were created from hydrogen and helium in the fury of burning supernovae. Having arisen when the stars were formed, the elements of which life is built, and thus we ourselves, 49 Million. The Azolla Event (AE). Hypothetically, Earth experienced a melting of Arctic might be thought of as stardust. (Dauber & Muller, 1996) ice and consequent formation of a layered freshwater ocean which supported massive prolif- eration of the fern Azolla. -
Constraining the Evolutionary History of the Moon and the Inner Solar System: a Case for New Returned Lunar Samples
Space Sci Rev (2019) 215:54 https://doi.org/10.1007/s11214-019-0622-x Constraining the Evolutionary History of the Moon and the Inner Solar System: A Case for New Returned Lunar Samples Romain Tartèse1 · Mahesh Anand2,3 · Jérôme Gattacceca4 · Katherine H. Joy1 · James I. Mortimer2 · John F. Pernet-Fisher1 · Sara Russell3 · Joshua F. Snape5 · Benjamin P. Weiss6 Received: 23 August 2019 / Accepted: 25 November 2019 / Published online: 2 December 2019 © The Author(s) 2019 Abstract The Moon is the only planetary body other than the Earth for which samples have been collected in situ by humans and robotic missions and returned to Earth. Scien- tific investigations of the first lunar samples returned by the Apollo 11 astronauts 50 years ago transformed the way we think most planetary bodies form and evolve. Identification of anorthositic clasts in Apollo 11 samples led to the formulation of the magma ocean concept, and by extension the idea that the Moon experienced large-scale melting and differentiation. This concept of magma oceans would soon be applied to other terrestrial planets and large asteroidal bodies. Dating of basaltic fragments returned from the Moon also showed that a relatively small planetary body could sustain volcanic activity for more than a billion years after its formation. Finally, studies of the lunar regolith showed that in addition to contain- ing a treasure trove of the Moon’s history, it also provided us with a rich archive of the past 4.5 billion years of evolution of the inner Solar System. Further investigations of samples returned from the Moon over the past five decades led to many additional discoveries, but also raised new and fundamental questions that are difficult to address with currently avail- able samples, such as those related to the age of the Moon, duration of lunar volcanism, the Role of Sample Return in Addressing Major Questions in Planetary Sciences Edited by Mahesh Anand, Sara Russell, Yangting Lin, Meenakshi Wadhwa, Kuljeet Kaur Marhas and Shogo Tachibana B R. -
Nomenclature for Lunar Features at the Chang'e-3 Landing Site
Acta Geochim (2017) 36(2):213–223 DOI 10.1007/s11631-017-0159-1 ORIGINAL ARTICLE Nomenclature for lunar features at the Chang’e-3 landing site Zhoubin Zhang1,2 · Chunlai Li1,2,3 · Wei Zuo1,2,3 · Xingguo Zeng1,2 Received: 22 December 2016 / Revised: 15 February 2017 / Accepted: 9 April 2017 / Published online: 27 April 2017 © Science Press, Institute of Geochemistry, CAS and Springer-Verlag Berlin Heidelberg 2017 Abstract Nomenclatures for lunar features always published after some necessary approval procedures by the accompany the progresses of human lunar exploration, International Astronomical Union. which has an important dual meaning in culture and sci- ence. The naming of lunar features not only can Keywords Moon · Chang’e-3 · Landing site · Lunar commemorate the outstanding contributions of academics, feature nomenclature masters in various fields, and popularize the traditional cultures of ethnic groups all over the world, but also have a critical function of providing accurate indicative informa- 1 Introduction tion on features with special morphology, origin, nature and scientific value. However, nomenclature for features at Planetary nomenclature, like terrestrial nomenclature, is the Chang’e-3 landing site, which has a more arbitrary used to uniquely identify a feature on the surface of a form without many constrains posed by a uniformed sys- planet or satellite so that the feature can be easily located, tem, is unlike the features for other morphological units. described, and discussed. Nomenclature for lunar features This paper originated from the actual needs for the originated in the seventeenth century, as early scientists in description of scientific exploration activities, interpreta- that era used telescopes to observe the lunar surface, named tion of scientific research and dissemination of scientific the remarkable features on the lunar surface according to results. -
Russell Priest Ship Catalog
Russell Priest Catalogue Name Type Company Flag YOB Tonnage Desc. Colour B/W 1ST LT BALDOMERO LOPEZ US URR USN USA 1985 40846 GRT 50 LET SSSR GRF 1973 13518 GRT A,S,MAYNE DRG MELBOUR AUS A.D.GEOPOTES DSH VOLKER D GBR 1972 4122 GRT A.D.McKENZIE DBD MELBOUR AUS GRT A.HAZER BBU 1978 25635 GRT A.M.VELLA DCH PORT OF AUS 1972 4122 GRT A.P.MOLLER TTA A.P.MOLL DIS 1984 28010 GRT A.P.MOLLER TTA A.P.MOLL DNK 1966 52673 GRT AAGTEKERK GGC UNITED N NLD 1943 8149 GRT AALSMEERGRACHT GGC SPLIETHO NLD 1992 7949 GRT AALTJE-JACOBA GGC WAGENBO 1995 1576 GRT AARO GGC ELLERMA GBR 1960 2468 GRT AASFJORD BBU TORKELSE NIS 1978 3086 GRT ABADESA TTA HOULDER GBR 1962 13571 GRT ABAKAN TTA 1971 14106 GRT ABBEKERK GGC UNITED N NLD 1946 8336 GRT ABBEYDALE TTA RFA GBR 1937 8299 GRT ABDALLAH BNOU YASSINE GRF SOCIETE MAR 1978 3086 GRT ABDOUN DISCOVERY TTA 1977 45587 GRT ABEL TASMAN GGC H.C.SLEIG AUS 1957 2681 GRT ABEL TASMAN MPR TT LINE AUS 1975 19212 GRT ABEL TASMAN GGC H.C.SLEIG AUS 1916 2053 GRT ABERDEEN TTA CHEVRON BHS 1996 47274 GRT ABERDEEN MPR G.THOMPS GBR 1881 3684 GRT ABERSEA GGC JONES BR AUS 1913 818 GRT ABIDA TTA SHELL TA NLD 1958 12226 GRT ABILITY GGC EVERARD GBR 1943 881 GRT ABINSI MPR ELDER DE GBR 1908 6327 GRT ABITIBI CLAIBORNE GGC 1986 7580 GRT ABITIBI ORINOCO GGC 1986 7580 GRT ABLE GENERAL GGC 1985 4337 GRT ABLE REEFER GRF SNG 1961 2683 GRT ABOSSO MPR ELDER DE GBR 1935 11329 GRT ABRAHAM LINCOLN GGC US GOVER USA 1919 7660 GRT ABRAHAM LINCOLN USS (CVN7 CVN USN USA 1989 102000 DISP ABRAM SCHULTE TTA SCHULTE CYP 2004 41503 GRT ABSIRTO GGC ITA 1943 7176 GRT ABU DHABI UCC 1998 48154 GRT ABU EGILA GGC EGY 1984 10022 GRT ABU ZEMNIA URR 1983 10022 GRT ABUJA GGC 1995 5999 GRT Thursday, 31 January 2013 Page 1 of 449 Name Type Company Flag YOB Tonnage Desc.