DOCSLIB.ORG

Galileo Imaging Observations of Lunar Maria and Related Deposits

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Galileo Imaging Observations of Lunar Maria and Related Deposits JOURNALOF GEOPHYSICALRESEARCH, VOL. 98, NO. E9, PAGES17,183-17,205, SEPTEMBER 25, 1993 Galileo Imaging Observationsof Lunar Maria and Related Deposits RONALDGREELEY, 1 STEVEN D. KADEL,1 DAVIDA. WILLIAMS,1 LISA R. GADDIS,2 JAMESW. HEAD,3 ALFREDS. MCEWEN,2 SCOTT L. MURCHIE,3 ]•NGELBERT NAGEL, 4 GERHARD NEUKUM, 4 CARLEM. PIETERS,3 JESSICA M. SUNSHINE,3 ROLAND WAGNER? AND MICHAEL J. S. BELTON5 The Galileo spacecraftimaged parts of the westernlimb and far side of the Moon in December 1990. Ratios of 0.41/0.56 gin filter images from the Solid State hnaging (SSI) experiment provided information on the titanium content of mare deposits' ratios of the 0.76/0.99 gm imagesindicated 1gin absorptions associated with Fe 2+ in maficminerals. Mare ages were derived froin crater statistics obtained from Lunar Orbiter images. Results on mare coinpositionsin western Oceanus Procellarum and the Humorurn basin are consistent with previous Earth-basedobservations, thus providing confidence in the use of Galileo data to extract compositional information. Mare units in the Grimaldi and Riccioli basins range in age froin 3.25 to 3.48 Ga and consistof medium- to medium-high titanium (<4 to 7% TiO2) content lavas. The Schiller-Zucchius basin shows a higher 0.76/0.99 gm ratio than the surroundinghighlands, indicating a potentially higher mafic mineral content consistentwith previous interpretationsthat the area includesmare depositsblanketed by highland ejecta and light plains materials. The oldest mare materials in the Orientale basin occur in south-central Mare Orientale and are 3.7 Ga old; youngestmare materials are in Lacus Autumni and are 2.85 Ga old; theseunits are medium- to medium-hightitanium (<4 to 7% TiO2) basalts. Thus, volcanism was active in Orientale for 0.85 Ca, but lavas were relatively constant in composition. Galileo data suggestthat Mendel-Rydberg mare is similar to Mare Orientale; cryptomareare presentas well. Thus, the mare lavas on the westernlimb and far side (to 178øE) are remarkably uniform in coinposition,being generally of medium- to medium-high titanium content and having relatively low 0.76/0.99 gin ratios. This region of the Moon is between two postulatedlarge impact structures,the Procellarum and the South Pole-Aitken basins, and may have a relatively thick crust. In areas underlain by an inferred thinner crust, i.e., zones within large basins (as at Apollo), titanium content is often higher. However, no mare deposits with titanium abundancesapproaching those of the high-titanium (9 to 14% TiO2) Apollo 11 and 17 basaltsnor of the high-titanium regions of central Oceanus Procellarum are seenon the westernlimb or easternfar side. Light plains depositsare generallyindistinct froin the surroundinghighlands in the SSI data and are inferred to be derived primarily from the same material that forins the highlands. Some of the light plains are too young to be related to basin-forming impacts, suggesting possible volcanic origin. Dark mantle deposit compositionsderived from SSI data are consistentwith Earth-basedobservations of similar near-sidedeposits and are interpretedto be pyroclasticmaterials. However,the modernitc albedo and 1 gin absorption of the dark mantle deposit on the southwest margin of the Orientale basin suggestit is a local pyroclasticdeposit contaminated with underlyinghighland materials from the Orientale impact. 1. INTRODUCTION 1Departmentof Geology,Arizona State University, Tempe. The Galileo flyby of the Moon in 1990 [Belton et al., 2U.S.Geological Survey, Flagstaff, Arizona. 1992]acquired the first new spacecraftlunar data in 15 years 3Departmentof Geological Sciences, Brown University, and includedobservations of far-side regionswith modem Providence, Rhode Island. instruments.Galileo missionobjectives for the Moon were 4GermanAerospace Research Establishment (DLR), outlinedby Fanale [1990] and preliminaryresults from the Institute for Planetary Exploration, Berlin/ Solid StateImaging (SSI) experimentwere givenby Belton Oberpfaffenhofen,Germany. et al. [1992]. 5NationalOptical Astronomy Observatories, Tucson, Arizona. Someof the key scienceobjectives focused on lunar maria andrelated deposits. Although mare materials represent <1% of the lunar crust [Head, 1976], they provideinsight into Copyright1993 by the AmericanGeophysical Union. crustalevolution, thermal history, and the Moon's interior. Consequently,information on the locationand composition Paper number 93JE01000. of mare deposits,combined with agesderived from impact 0148-0227/93/93 JE01000505.00 crater statistics, enable better understandingof magma 17,183 17,184 GREELEYET AL.: GALILEOIMAGING OBSERVATIONS OF LUNARMARIA evolution and lunar volcanis•n. Although much has been only areascovered by •naturemare soilscan be classifiedfor learnedabout maria in thelast 25 years(reviewed by Headand TiO2, regions of young crater ejecta were not assessed. Wilson [1992]), compositionaldata for much of the surface Table 1 gives the classification used here for titanium are lacking. Multispecu'aldata obtainedfrom Earth provide contents. A comparisonof our classificationscheme with insight into surfacecompositions [Pieters, 1991], but are others,from both the spectraland petrologicperspective, is limited to the near side. Galileo provided the first given in Table 2. opportunity to collect multispectral data for parts of the Albedois broadlyindicative of lithologicdifferences among westernli•nb and far side. Our approachwas to obtain data mare, highland,and fresh cratermaterials [Pieters et al., this on near-sidemaria previouslyobserved and for which re,note issue]. Unlike normal albedo(reflectance at 0ø phaseangle) sensingdata were calibratedusing Alx)11o s,-unples [Pieters et usedby Pieters [1978], we determinedalbedo using the al., this issue]. This enabled calibration of SSI data to assess 0.56 gm filter (normalized to MH0 and 20ø phase angle mare compositionsfor the westernlimb and far side. [Pieters et al., this issue]). Aremsanalyzed (Figures la and lb m•dPlate 1) includemare Mafic minerals, such as pyroxene, produce strong deposits, light plains materials, and dark mantle deposits absorptionsnear 1 gm [e.g., Pieters, 1978]. The Galileo SSI (DMD). In each area we assessedthe local stratigraphy, 0.76/0.99 gm ratio, usedhere to estimate1 gm absorption obtainedcrater countsto determineages (except for DMD), strength,is influencedby soil maturity, grain size, viewing derived spectral characteristics, and interpreted the geometry,glass content, and the model abundances of Fe 2+ compositionsof the deposits. bearing minerals. However, by studying only areas of mature, uncont,'uninatedmare soils it is possibleto use the 2. DATA CHARACTERISTICSAND PROCESSING 0.76/0.99 grn ratio as an indicationof the relativeamount of maficminerals and Fe 2+ bearing glass present in mareunits. The Galileo imagingsequence [Belton et al., 1992] began at the easternterminator over the Apollo 12 and 14 landing 2.2. Data Correlation to Previous Studies sites, continued across the western near side, and extended to To assessSSI datafor analyzinglunar maria, we compared the far side to 178øE. The highestresolution images were SSI and Earth-based spectral information for parts of -3.5 Pan/pixel,centered at 7øS 25øW; the lowest resolution O. Procellarum and M. Humorurn [e.g., Whitaker, 1972; images analyzed were -7.6 Pan/pixelfor the Apollo basin. Pieters et al., 1975; McCord et al., 1976]. O. Procellarum These imageswere processedwith photometric,phase angle, mafia appearto be associatedwith eitherthe "mega-Imbriuln" and radiometric calibrations [McEwen et al., this issue], and basin [Spudis et al., 1988] or the Procellarum basin geometric control, and were reprojectedto a standardmap [Cadogan, 1974, 1981]. The formation of the postulated format with subpixelregistration applied. The result was a Procellarum basin would have had an enoHnous effect on the highly correlated data set of multispectral mosaicsin five Moon [Wilhelms,1987] and may haveresulted in thinningof wavelengths (0.41, 0.56, 0.66, 0.78, 0.99 [.tm). These the near-sidelithosphere, crustal deformation, mare extrusion, mosaicsserved as the primary data sourcefor thisstudy. and perhapsthickening of far-side crust [Cadogan, 1974, 1981]. 2.1. SpectralAnalysis Whitford-Starkand Head [1977, 1980] mappedthe lava Pieters et al. [this issue] discuss the calibration of Galileo flows in O. Procellarum,the youngestof which is the Sharp images to extract spectral data and the limitations of the Formation. Pieters [1978] and Pieters et al. [1980] found derived information. Imaging sequenceswere designedto this unit to be 3-11 wt % TiO2. The Hermann Formation, obtain data over stand,'u'dsites for Earth-basedmultispectral the next youngestunit, coversnearly half of O. Procellarum analyses,including one in Mare Humoruln (designatedMH0). and is <3 wt % TiO2 [Pieters, 1978]. The Telemann Pieters[1978] outlineda four-par,'uneterclassification scheme Formationunderlies both the Sharpand HermannFormations for lunar basaltsbased on telescopicspectral reflectance data, and is <2wt % TiO2 [Pieters, 1978]. The Repsold includingthe 0.40/0.56 gm (UV/VIS) ratio, normalalbedo, Formation is the oldest unit, covers -1% of northwestern 1 gm absorption band strength, and 2 gm absorption O. Procellarum,and is 3-6 wt % TiO2 [Pieters, 1978]. The stxength. This scheme was adapted here, but without the boundariesof theseunits are clearly distinguishedon a color latterparmeter becauseGalileo lacksa 2 gm filter. map of the SSI 0.41/0.56 gm ratio (Plate 2)
Load more

Recommended publications
  • Mission to Jupiter
    This book attempts to convey the creativity, Project A History of the Galileo Jupiter: To Mission The Galileo mission to Jupiter explored leadership, and vision that were necessary for the an exciting new frontier, had a major impact mission’s success. It is a book about dedicated people on planetary science, and provided invaluable and their scientific and engineering achievements. lessons for the design of spacecraft. This The Galileo mission faced many significant problems. mission amassed so many scientific firsts and Some of the most brilliant accomplishments and key discoveries that it can truly be called one of “work-arounds” of the Galileo staff occurred the most impressive feats of exploration of the precisely when these challenges arose. Throughout 20th century. In the words of John Casani, the the mission, engineers and scientists found ways to original project manager of the mission, “Galileo keep the spacecraft operational from a distance of was a way of demonstrating . just what U.S. nearly half a billion miles, enabling one of the most technology was capable of doing.” An engineer impressive voyages of scientific discovery. on the Galileo team expressed more personal * * * * * sentiments when she said, “I had never been a Michael Meltzer is an environmental part of something with such great scope . To scientist who has been writing about science know that the whole world was watching and and technology for nearly 30 years. His books hoping with us that this would work. We were and articles have investigated topics that include doing something for all mankind.” designing solar houses, preventing pollution in When Galileo lifted off from Kennedy electroplating shops, catching salmon with sonar and Space Center on 18 October 1989, it began an radar, and developing a sensor for examining Space interplanetary voyage that took it to Venus, to Michael Meltzer Michael Shuttle engines.
    [Show full text]
  • Modeling and Adjustment of THEMIS IR Line Scanner Camera Image Measurements
    Modeling and Adjustment of THEMIS IR Line Scanner Camera Image Measurements by Brent Archinal USGS Astrogeology Team 2255 N. Gemini Drive Flagstaff, AZ 86001 [email protected] As of 2004 December 9 Version 1.0 Table of Contents 1. Introduction 1.1. General 1.2. Conventions 2. Observations Equations and Their Partials 2.1. Line Scanner Camera Specific Modeling 2.2. Partials for New Parameters 2.2.1. Orientation Partials 2.2.2. Spatial Partials 2.2.3. Partials of the observations with respect to the parameters 2.2.4. Parameter Weighting 3. Adjustment Model 4. Implementation 4.1. Input/Output Changes 4.1.1. Image Measurements 4.1.2. SPICE Data 4.1.3. Program Control (Parameters) Information 4.2. Computational Changes 4.2.1. Generation of A priori Information 4.2.2. Partial derivatives 4.2.3. Solution Output 5. Testing and Near Term Work 6. Future Work Acknowledgements References Useful web sites Appendix I - Partial Transcription of Colvin (1992) Documentation Appendix II - HiRISE Sensor Model Information 1. Introduction 1.1 General The overall problem we’re solving is that we want to be able to set up the relationships between the coordinates of arbitrary physical points in space (e.g. ground points) and their coordinates on line scanner (or “pushbroom”) camera images. We then want to do a least squares solution in order to come up with consistent camera orientation and position information that represents these relationships accurately. For now, supported by funding from the NASA Critical Data Products initiative (for 2003 September to 2005 August), we will concentrate on handling the THEMIS IR camera system (Christensen et al., 2003).
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • Warren and Taylor-2014-In Tog-The Moon-'Author's Personal Copy'.Pdf
    This article was originally published in Treatise on Geochemistry, Second Edition published by Elsevier, and the attached copy is provided by Elsevier for the author's benefit and for the benefit of the author's institution, for non- commercial research and educational use including without limitation use in instruction at your institution, sending it to specific colleagues who you know, and providing a copy to your institution’s administrator. All other uses, reproduction and distribution, including without limitation commercial reprints, selling or licensing copies or access, or posting on open internet sites, your personal or institution’s website or repository, are prohibited. For exceptions, permission may be sought for such use through Elsevier's permissions site at: http://www.elsevier.com/locate/permissionusematerial Warren P.H., and Taylor G.J. (2014) The Moon. In: Holland H.D. and Turekian K.K. (eds.) Treatise on Geochemistry, Second Edition, vol. 2, pp. 213-250. Oxford: Elsevier. © 2014 Elsevier Ltd. All rights reserved. Author's personal copy 2.9 The Moon PH Warren, University of California, Los Angeles, CA, USA GJ Taylor, University of Hawai‘i, Honolulu, HI, USA ã 2014 Elsevier Ltd. All rights reserved. This article is a revision of the previous edition article by P. H. Warren, volume 1, pp. 559–599, © 2003, Elsevier Ltd. 2.9.1 Introduction: The Lunar Context 213 2.9.2 The Lunar Geochemical Database 214 2.9.2.1 Artificially Acquired Samples 214 2.9.2.2 Lunar Meteorites 214 2.9.2.3 Remote-Sensing Data 215 2.9.3 Mare Volcanism
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • The Economic Impact of Physics Research in the UK: Satellite Navigation Case Study
    The economic impact of physics research in the UK: Satellite Navigation Case Study A report for STFC November 2012 Contents Executive Summary................................................................................... 3 1 The science behind satellite navigation......................................... 4 1.1 Introduction ................................................................................................ 4 1.2 The science................................................................................................ 4 1.3 STFC’s role in satellite navigation.............................................................. 6 1.4 Conclusions................................................................................................ 8 2 Economic impact of satellite navigation ........................................ 9 2.1 Introduction ................................................................................................ 9 2.2 Summary impact of GPS ........................................................................... 9 2.3 The need for Galileo................................................................................. 10 2.4 Definition of the satellite navigation industry............................................ 10 2.5 Methodological approach......................................................................... 11 2.6 Upstream direct impacts .......................................................................... 12 2.7 Downstream direct impacts.....................................................................
    [Show full text]
  • JPL to Map the Moon on India Mission
    I n s i d e May 19, 2006 Volume 36 Number 10 News Briefs ............... 2 Griffin Visits Lab ............ 3 Special Events Calendar ...... 2 Passings, Letters ........... 4 Spitzer Sees Comet Breakup... 2 Retirees, Classifieds ......... 4 Jet Propulsion Laborator y A JPL state-of-the-art imaging spectrometer that will provide the first high-resolution spectral map of the JPL to entire lunar surface successfully completed its critical design review this week. The Moon Mineralogy Mapper, also known as “M3,” is one of two in- materials across the surface at high spatial resolution. This data map the struments that NASA is contributing to India’s first mission to the moon, will provide a much-needed long-term baseline for future exploration scheduled to launch in late 2007 or early 2008. By mapping the mineral activities. composition of the lunar surface, the mission will both provide clues to The mission’s observations will address several important scientific moon the early development of the solar system and guide future astronauts to issues, including early evolution of the solar system; fundamental stores of precious resources. processes acting on planets that shape their character; assessment of on India Chandrayaan-1 is India’s first deep-space mission as well as its first potential impact hazards to Earth; and assessment of space resources. lunar mission. “The entire M3 team feels honored to be able to partici- From its vantage point in orbit around the moon, the spacecraft will mission pate,” said Project Manager Tom Glavich of JPL. measure the sunlight reflected by all of the rocks and soil over which The instrument is well on its way to being delivered to the Chandray- it passes.
    [Show full text]
  • Table of Exposures
    Table of Exposures Dole UT Focal Emulsion Exposure Moon's age Plate Nos. ralio sec. days 08.11.65 2132· f/29 Kodak 0.250 Plole 0.4 15.3 7e/2 08.01.66 2228 f/24 Kodak 0.250 Plate 0.31 17.0 3b, 15e 31.01.66 1947 1/24 Kodak 0.250 Plale 0.3 10.1 5b 02.02.66 1944 f/24 Kodak 0.250 Plote 0.25 12.1 7b, 8b 06.02.66 2326 1/24 Kodak 0.250 Plole 0.2 16.3 14c,16b 05.03.66 2259 1/41 IIford Zenith Plole 0.1 13 .5 lOe/l 27.04.66 2152 1/24 lIford G.30 Plate 0.5 6.9 150 28.04.66 2046 f/30 lIford G.30 Pia Ie 0.8 7.9 10,130 23.05.66 2033 f/24 Kodak 0.250 Plole 0.7 3.4 15e/2 23.05,66 2034 f/24 Kodak 0.250 Plate 0.7 3.4 3e/2,4b 23.05.66 2036 1/24 Kodak 0.250 Plate 0.7 3.4 16e 28.05.66 2122 1/30 IIford G.30 Plole 0.8 8.4 140 29.05.66 2103 1/30 IIford G.30 Plate 0.8 9.4 2e 23.06.66 2109 f/24 lIford G.30 Pia Ie 1.0 5.0 160 06.08.66 0211 f/30 Illord G.30 Pia Ie 0.7 18.9 2b 06.08.66 0215 1/30 IIford G.30 Plale 0.7 18.9 lb, 13b 09.08.66 0315 1/30 IIlord G.30 Plate 1.1 23.8 50,60 09.08.66 03 17 1/30 Ilford G.30 Plate 1.1 23.8 90, 91/2, 11 b, 12e/l 06.
    [Show full text]
  • Highresolution Local Gravity Model of the South Pole of the Moon From
    GeophysicalResearchLetters RESEARCH LETTER High-resolution local gravity model of the south pole 10.1002/2014GL060178 of the Moon from GRAIL extended mission data 1,2 2 2,3 2 Key Points: Sander Goossens , Terence J. Sabaka , Joseph B. Nicholas , Frank G. Lemoine , • We present a high-resolution gravity David D. Rowlands2, Erwan Mazarico2,4, Gregory A. Neumann2, model of the south pole of the Moon David E. Smith4, and Maria T. Zuber4 • Improved correlations with topography to higher degrees than 1CRESST, University of Maryland Baltimore County, Baltimore, Maryland, USA, 2NASA Goddard Space Flight Center, global models 3 4 • Improved fits to the data and Greenbelt, Maryland, USA, Emergent Space Technologies, Greenbelt, Maryland, USA, Department of Earth, Atmospheric reduced striping that is present in and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Massachusetts, USA global models Abstract We estimated a high-resolution local gravity field model over the south pole of the Moon Supporting Information: using data from the Gravity Recovery and Interior Laboratory’s extended mission. Our solution consists of • Readme • Figures S1 adjustments with respect to a global model expressed in spherical harmonics. The adjustments are • Figures S2 expressed as gridded gravity anomalies with a resolution of 1/6◦ by 1/6◦ (equivalent to that of a degree • Figures S3 and order 1080 model in spherical harmonics), covering a cap over the south pole with a radius of 40◦.The • Figures S4 • Figures S5 gravity anomalies have been estimated from a short-arc analysis using only Ka-band range-rate (KBRR) • Figures S6 data over the area of interest.
    [Show full text]
  • Testing Hypotheses for the Origin of Steep Slope of Lunar Size-Frequency Distribution for Small Craters
    CORE Metadata, citation and similar papers at core.ac.uk Provided by Springer - Publisher Connector Earth Planets Space, 55, 39–51, 2003 Testing hypotheses for the origin of steep slope of lunar size-frequency distribution for small craters Noriyuki Namiki1 and Chikatoshi Honda2 1Department of Earth and Planetary Sciences, Kyushu University, Hakozaki 6-10-1, Higashi-ku, Fukuoka 812-8581, Japan 2The Institute of Space and Astronautical Science, Yoshinodai 3-1-1, Sagamihara 229-8510, Japan (Received June 13, 2001; Revised June 24, 2002; Accepted January 6, 2003) The crater size-frequency distribution of lunar maria is characterized by the change in slope of the population between 0.3 and 4 km in crater diameter. The origin of the steep segment in the distribution is not well understood. Nonetheless, craters smaller than a few km in diameter are widely used to estimate the crater retention age for areas so small that the number of larger craters is statistically insufficient. Future missions to the moon, which will obtain high resolution images, will provide a new, large data set of small craters. Thus it is important to review current hypotheses for their distributions before future missions are launched. We examine previous and new arguments and data bearing on the admixture of endogenic and secondary craters, horizontal heterogeneity of the substratum, and the size-frequency distribution of the primary production function. The endogenic crater and heterogeneous substratum hypotheses are seen to have little evidence in their favor, and can be eliminated. The primary production hypothesis fails to explain a wide variation of the size-frequency distribution of Apollo panoramic photographs.
    [Show full text]