DOCSLIB.ORG

NASA Goddard Space Flight Center, Greenbelt, MD Contact: [email protected]

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
NASA Goddard Space Flight Center, Greenbelt, MD Contact: David.M.Hollibaughbaker@Nasa.Gov Updated Catalogs of Peak-Ring Basins and Protobasins on Mars David M.H. Baker; NASA Goddard Space Flight Center, Greenbelt, MD Contact: [email protected] A catalog of craters ≥1 km on Mars from Robbins et al. [2] was used to survey all craters >50 km on the planet (N=2,070) in a manner similar to [5,6] for the Moon and Mercury. Motivation: II. Basin Images Datasets used included MOLA gridded topography and a global THEMIS daytime IR mosaic [7]. During the survey, each crater was identified as having a rim crest in addition to a single interior ring of peaks (peak-ring basin), an interior ring of peaks plus a central peak (protobasin), a central peak only (complex crater), or no interior structure (unclassified). • The morphology of peak-ring basins (exhibiting a rim crest and interior peak Schiaparelli; 446 km Schroeter; 292 km Galle; 223 km Kepler; 222 km Secchi; 217 km Kaiser; 202 km Lowell; 199 km Phillips; 185 km ring) in the complex crater to basin transition on the Moon and Mercury have been well characterized based on data from recent missions to these planetary bodies [e.g., 1]. • Although global crater catalogs have recently been produced for Mars [e.g., 2], the detailed characteristics of the crater to basin transition on Mars has not been fully re-examined since basin ring catalogs and measurements were produced over two decades ago by Pike and Spudis [3], among others. • Here, previous basin catalogs [3] and the global crater catalog of Robbins Unnamed; 180 km Molesworth; 175 km Proctor; 167 km Becquerel; 165 km Ptolemaeus; 165 km Dejnev 152 km Unnamed; 103 km Mie; 101 km et al. [2] are re-analyzed using topographic and image datasets to provide updated catalogs of peak-ring basins and protobasins on Mars. • These updated catalogs are important for comparisons with other planetary Galle; 223km bodies [1], constraining basin formation models, and understanding the Peak-Ring Basins (16) original morphology of the abundant degraded craters on Mars. Findings: Herschel; 298 km Lyot; 220 km Gale; 154 km Bakhuysen; 153 km Holden; 153 km Liu Hsin; 135 km Barnard; 121 km Bjerknes; 89 km • A total of 16 peak-ring basins and 8 protobasins were identified, ranging in rim-crest diameter from 101 to 446 km (peak-ring basins) and 89 to 298 km (protobasins). exposed peak (possibly larger) • Nine of these basins are newly added to the catalog and not included in the previous catalog of [3]. Nine basins from [3] are also removed from the present catalogs, as current topography and image data do not support the Protobasins (8) presence of interior rings within these basins. • Although it has a larger surface area, Mars has nearly an order of magnitude fewer peak-ring basins than Mercury (N=110), which can be attributed to the planet’s much higher resurfacing and erosion rates. III. The Updated Basin Catalogs for Mars Peak-ring and/ 1000 • Like Mercury, the rim-crest diameters of both complex craters with central or central-peak peaks and protobasins overlap those of peak-ring basins over a much larger Updated basin catalogs. Below: Number of basins and craters with interior diameters versus 100 range than on the Moon. Name Lat. Lon. Dr Dpr Dcp structures as a fraction of the total crater populations [2]. rim-crest diameters • As noted by previous researchers, protobasins, such as Lyot, occur at Peak-Ring Basins Note the low number of craters and basins on Mars with for peak-ring basins Schiaparelli -2.51 16.80 446 239 -- recognizable interior peaks or rings due the higher erosion anomalously large diameters on Mars compared to Mercury and the Moon. Schroeter -1.90 55.99 292 142 -- and protobasins on The effect of volatiles on the basin-formation process is often used to explain Galle -50.65 -30.88 223 102 -- and resurfacing rates on the planet. This is most evident Mars only. Data from 10 Protobasin Kepler -46.75 141.16 222 120 -- Protobasin CP when compared with the Moon and Mercury (below). Ring or (km) DiameterPeak this feature, but more modeling work is needed to fully explore this problem. Secchi -57.85 101.97 217 115 -- Pike and Spudis [3] Peak-Ring Basin Kaiser -46.16 19.11 202 98 -- 1 (PS87) are shown for PS87 Peak-Ring Basin PS87 Protobasin Lowell -51.95 -81.37 199 96 -- Other 0.9 comparison. 1 Acknowledgements Phillips -66.33 -44.79 185 104 -- Peak-ring basins 50 500 Unnamed -39.34 76.83 180 90 -- Protobasins Rim-crest Diameter (km) Support from a NASA Postdoctoral Program Fellowship is gratefully acknowledged. 0.8 Molesworth -27.49 149.21 175 80 -- Complex Craters Proctor -47.57 29.69 167 81 -- Becquerel 21.89 -7.94 165 72 -- 0.7 Ratios of peak-ring 0.8 References: [1] Baker, D.M.H. and Head, J.W. (2013) Planet. Space Sci. 86, 91–116. [2] Ptolemaeus -45.89 -157.73 165 76 -- 0.7 Robbins, S.J. and Hynek, B.M. (2012) J. Geophys. Res. 117, E05004. [3] Pike, R.J. and Spudis, Dejnev -25.14 -164.64 152 68 -- 0.6 diameter to rim- Unnamed -9.07 150.51 103 33 -- crest diameter for P.D. (1987) Earth Moon Planets 39, 129–194. [4] Allen, C.C. (2015) LPSC 46, no. 2787. [5] 0.5 0.6 Mie 48.12 139.69 101 30 -- peak-ring basins Baker, D.M.H. et al. (2011) Icarus 214, 377–393. [6] Baker, D.M.H. et al. (2011) Planet. Space Protobasins 0.5 Sci. 59, 1932–1948. [7] Edwards, C.S., et al. (2011) J. Geophys. Res. 116, E10008. Herschel -14.48 129.89 298 148 40 0.4 and protobasins crest Ratiocrest - 0.4 Lyot 50.46 29.31 220 106 33 0.3 on Mars only. The Gale -5.37 137.81 154 87 18 0.3 Bakhuysen -22.97 15.76 153 57 29 ratio increases with Ring/Rim Holden -26.04 -34.02 153 58 21 0.2 increasing basin 0.2 Liu Hsin -53.20 -171.51 135 41 19 Peak-Ring Basin size. The same 0.1 Barnard -61.08 61.55 121 50 12 0.1 Protobasin Fraction of Total Crater Population Fraction of Total Bjerknes -43.06 171.48 89 34 14 occurs on the Moon 0.0 0 50 150 250 350 450 Dr: rim-crest diameter (km); Dpr=peak-ring and Mercury (see 75 125 175 225 275 325 375 425 475 525 575 625 Rim-crest Diameter (km) diameter (km); Dcp: central-peak diameter (km). I. Global Distribution Rim-crest Diameter Bin Center (km) below). Peak-ring basins and protobasins are mainly located within the cratered southern highlands of Mars. Below is an equidistant cylindrical map of MOLA colored topography on a MOLA hillshade basemap. A) Peak-ring diameters versus 1000 IV. Comparisons with the Moon and Mercury Mars rim-crest diameters for peak-ring Mercury Number of basins and craters as a basins and protobasins on Mars, Moon Table of basin summary statistics, comparing the fraction of total crater populations [1]. the Moon [1,5], and Mercury Moon [1,5], Mercury [1,6] and Mars. Mars has the Moon [1,6]. The data fall along a similar 1 100 lowest population of preserved peak-ring basins even Other power-law trend. 0.9 Peak-ring basins though it has the greatest surface area. Protobasins Protobasins 0.8 Ring Diameter (km) also occur at anomalously large diameters on Mars. Complex Craters 0.7 Ratios of peak-ring diameter 0.6 A) Moon Mercury Mars to rim-crest diameter for peak- Gravitational acceleration (m/s2) 1.62 3.70 3.69 0.5 10 50 500 2 7 7 8 0.4 ring basins and protobasins on Surface area (km ) 3.8 x 10 7.5 x 10 1.4 x 10 Rim-crest Diameter (km) Mean impact velocity (km/s) 19.4 42.5 10.6 0.3 the Moon (B) and Mercury (C). 0.2 Peak-ring basins (Npr) 17 110 16 Note the similarly increasing 2 -7 -6 -7 0.1 Npr/km 4.5 x 10 1.5 x 10 1.1 x 10 Crater Population Fraction of Totlal ratios with basin size, suggesting Geometric mean diameter (km) 343 172 188 0 75 125 175 225 275 325 375 425 475 525 575 625 a continuum in process forming Minimum diameter (km) 207 84 101 Rim-crest Diameter Bin Center (km) Peak-ring basins and protobasins Maximum diameter (km) 582 320 446 protobasins and peak-ring basins. Onset diameter, method 1 (km) 206 109 (+23,-19) 132 (+35,-28) Mercury 0.8 0.8 Complex craters >50 km with central peaks 1 Other Moon Mercury Onset diameter, method 2 (km) 227 103 102 0.7 0.7 0.9 Peak-ring basins Protobasins (Nproto) 3 70 8 Protobasins 0.8 0.6 0.6 2 -8 -7 -8 Complex Craters Nproto/km 7.9 x 10 9.4 x 10 5.7 x 10 0.7 0.5 Geometric mean diameter (km) 157 92 155 0.5 0.6 crest Ratiocrest - Minimum diameter (km) 137 50 89 Ratiocrest 0.4 - 0.4 Maximum diameter (km) 170 195 298 0.5 0.3 0.3 0.4 Complex Craters ≥ 50 km (Ncpc) 430 682 311 Ring/Rim Ring/Rim 2 -5 -6 -6 0.2 Ncpc/km 1.1 x 10 9.1 x 10 2.2 x 10 0.3 0.2 Peak-Ring Basin Peak-Ring Basin 0.1 Geometric mean diameter (km) 75 70 75 0.2 0.1 Protobasin B) Protobasin C) Minimum diameter (km) 50 50 50 0.1 0.0 Maximum diameter (km) 205 168 182 Crater Population Fraction of Total 0.0 50 150 250 350 0 50 150 250 350 450 550 650 Rim-crest Diameter (km) 75 125 175 225 275 325 375 425 475 525 575 625 Rim-crest Diameter (km) Rim-crest Diameter Bin Center (km).
Load more

Recommended publications
  • Imaginative Geographies of Mars: the Science and Significance of the Red Planet, 1877 - 1910
    Copyright by Kristina Maria Doyle Lane 2006 The Dissertation Committee for Kristina Maria Doyle Lane Certifies that this is the approved version of the following dissertation: IMAGINATIVE GEOGRAPHIES OF MARS: THE SCIENCE AND SIGNIFICANCE OF THE RED PLANET, 1877 - 1910 Committee: Ian R. Manners, Supervisor Kelley A. Crews-Meyer Diana K. Davis Roger Hart Steven D. Hoelscher Imaginative Geographies of Mars: The Science and Significance of the Red Planet, 1877 - 1910 by Kristina Maria Doyle Lane, B.A.; M.S.C.R.P. Dissertation Presented to the Faculty of the Graduate School of The University of Texas at Austin in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy The University of Texas at Austin August 2006 Dedication This dissertation is dedicated to Magdalena Maria Kost, who probably never would have understood why it had to be written and certainly would not have wanted to read it, but who would have been very proud nonetheless. Acknowledgments This dissertation would have been impossible without the assistance of many extremely capable and accommodating professionals. For patiently guiding me in the early research phases and then responding to countless followup email messages, I would like to thank Antoinette Beiser and Marty Hecht of the Lowell Observatory Library and Archives at Flagstaff. For introducing me to the many treasures held deep underground in our nation’s capital, I would like to thank Pam VanEe and Ed Redmond of the Geography and Map Division of the Library of Congress in Washington, D.C. For welcoming me during two brief but productive visits to the most beautiful library I have seen, I thank Brenda Corbin and Gregory Shelton of the U.S.
    [Show full text]
  • 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.
    [Show full text]
  • March 21–25, 2016
    FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk,
    [Show full text]
  • Naval Juniorreserve ()Hiders
    DOCUMENT RESUME ED 219 280 SE 038 787 e $ . AUTHOR ' Omans, S. E.; And Others TITLE Workbook for Naval Science 3: An Illustrated Workbook for the NJROTC Sjudent. Focus. on the Trained Person. Technical Report 124. INSTITUTION University of Central Florida, Orlando.. -, SPONS AGENCY Naval %Training Analysis and Evaluation Group, Orlando, Fla. PUB DATE May f2 GRANT N61339-79-D-0105 4 NOTE if 348p.- 4 ,EDRS PRICE MF01/PC14 Plus Postage. DESCRIPTORS Astronomy; Electricity; High Schools; Instructional -Materials; *Leadership; Meteotiology; Military Science; *Military Training; *Physical Sciences; ( *Remedial Reading; *Secondary School Science; Workbooks' _ IDENTIFIERS Navaleistory; *Naval JuniorReserve ()Hiders . ,-..\ Traiffing torps , '-'--..... ..,. ABSTRACT This workbook (first in a series of three) - supplements the textbook of the third year Naval Junior Reserve Officers Training Corps (NJROTC),program and is designed for NJROTC students who do not have the reading skillsOlecessary to fully benefit from the regular curriculum materidls. The workbook is written at the eighth-grade readability level as detprmined by a Computer Readability Editing System'analysis. In addition to its use in the NJROTC program, the wdrkbook may be useful in 'several remedial programs such as Academic Remedial Training(ART) and;the Verbal' Skills Curriculum,\Jzoth of which are offered at each 'of the three . RecruitTraining Com?nands to recruits deficient in reading or oral English skills.' Topics' in the workbook include naval history (1920-1945), leadership.characteristiCs, meteorology, astronomy, sand introductory electricity.'Exercises-include'vocabulary development, matching, concept application, and -extending Yearning actrties. (Author/JN) V 1' ****************************.0***,*************************************** * * Reproductions suppled'bi EDRS are the best that can be made. from- the oryiginal% document.
    [Show full text]
  • GSA TODAY • Radon in Water, P
    Vol. 8, No. 11 November 1998 INSIDE • Field Guide Editor, p. 5 GSA TODAY • Radon in Water, p. 10 • Women Geoscientists, p. 12 A Publication of the Geological Society of America • 1999 Annual Meeting, p. 31 Gas Hydrates: Greenhouse Nightmare? Energy Panacea or Pipe Dream? Bilal U. Haq, National Science Foundation, Division of Ocean Science, Arlington, VA 22230 ABSTRACT Recent interest in methane hydrates has resulted from the recognition that they may play important roles in the global carbon cycle and rapid climate change through emissions of methane from marine sediments and permafrost into the atmosphere, and in causing mass failure of sediments and structural changes on the continental slope. Their presumed large volumes are also consid- ered to be a potential source for future exploitation of methane as a resource. Natural gas hydrates occur widely on continental slope and rise, stabilized in place by high hydrostatic pressure and frigid bottom-temperature condi- tions. Change in these conditions, Figure 1. This seismic profile, over the landward side of Blake Ridge, crosses a salt diapir; the profile has either through lowering of sea level or been processed to show reflection strength. The prominent bottom simulating reflector (BSR) swings increase in bottom-water temperature, upward over the diapir because of the higher conductivity of the salt. Note the very strong reflections of may trigger the following sequence of gas accumulations below the gas-hydrate stability zone and the “blanking” of energy above it. Bright events: dissociation of the hydrate at its Spots along near-vertical faults above the diapir represent conduits for gas venting.
    [Show full text]
  • Workshop on Mars Telescopic Observations
    WORKSHCPON MARS TELESCOPIC OBSERVATIONS 90' 180'-;~~~~~~------------------..~~------------~~----..~o~,· 270' LPI Technical Report Number 95-04 Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPIITR--95-04 WORKSHOP ON MARS TELESCOPIC OBSERVATIONS Edited by J. F. Bell III and J. E. Moersch Held at Cornell University, Ithaca, New York August 14-15, 1995 Sponsored by Lunar and Planetary Institute Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPI Technical Report Number 95-04 LPIITR--95-04 Compiled in 1995 by LUNAR AND PLANETARY INSTITUTE The Institute is operated by the Universities Space Research Association under Contract No. NASW-4574 with the National Aeronautics and Space Administration. Material in this volume may be copied without restraint for library, abstract service, education, or personal research purposes; however, republication of any paper or portion thereof requires the written permission of the authors as well as the appropriate acknowledgment of this publication. This report may be cited as Bell J. F.III and Moersch J. E., eds. (1995) Workshop on Mars Telescopic Observations. LPI Tech. Rpt. 95-04, Lunar and Planetary Institute, Houston. 33 pp. This report is distributed by ORDER DEPARTMENT Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Mail order requestors will be invoiced for the cost ofshipping and handling. Cover: Orbits of Mars (outer ellipse) and Earth (inner ellipse) showing oppositions of the planet from 1954to 1999. From C. Aammarion (1954) The Flammarion Book ofAstronomy, Simon and Schuster, New York. LPl Technical Report 95-04 iii Introduction The Mars Telescopic Observations Workshop, held August 14-15, 1995, at Cornell University in Ithaca, New York, was organized and planned with two primary goals in mind: The first goal was to facilitate discussions among and between amateur and professional observers and to create a workshop environment fostering collaborations and comparisons within the Mars ob­ serving community.
    [Show full text]
  • In T Er Na Sj O Nale O Per a Sj O
    Internasjonale operasjoner rapport første halvår 2013 INTERNASJONALE OPERASJONER 02 forsvaret — internasjonale operasjoner innholD Forsvarets operative hovedkvarter Forsvarets operative hovedkvarter i Bodø er ansvarlig for den daglige oppfølgingen av Forsvarets operasjoner både i Norge og i utlandet. Gjennom rapportering og jevnlig besøk i de internasjonale operasjonene, får hovedkvarteret en god situasjonsforståelse. s. 48 ∫ europa miNerydderstyrkeN Norske mineryddere deltar aktivt i jakten på sjøminer, torpedoer og luftbomber som ligger igjen etter verdenskrigene. s. 42 ∫ aFrika deN demokratiske repuBLikkeNkoNGo Forsvaret er til stede med én offiser i bidraget som skal beskytte sivilbefolk- ningen i den demokratiske republikkenkongo.dette er FNs største fredsbeva- rende styrke. Deltakelse i internasjonale Forsvaret i kroner 2013 operasjoner styrker forsvarets evne til å operere sammen meD våre allierte, noe som er en forutsetning for et i miLLioNer kroNer: effektivt forsvar av norge. driFtnorge ForsvarssjeF Harald sunde 73 % 24 % driFtnorge investering 25 055 investering 8382 operasjoner 3 % i utlandet operasjoner i utlandet 1096 tallene viser de midlene som det er budsjettert med for hele 2013 til de internasjonale operasjonene i adenbukta, afghanistan, Bosnia-Hercegovina, kongo, kosovo, midtøsten og sør-sudan. Forsvaret 2013 INTERNASJONALE OPERASJONER 03 s. 52 ∫ europa luFtovervåkiNg med hovedkvarter i tyskland bidrar 24 nord- menn for å sikre luftrom- Innsats ute, met over europa og sørge s. 54 ∫ s. 50 ∫ for varsling. europa sikkerhet hjemme europa traNsportFly iNato Forsvarets viktigste oppgave er å forsvare Norge. Norge har sammen med For å løse denne oppgaven må Forsvaret først BosNia-HercegoviNa elleve andre land gått til og fremst drive realistisk trening og øving, alene den unge nasjonen skal innkjøp av tre enorme og med våre allierte, under norske forhold.
    [Show full text]
  • Water on the Moon, III. Volatiles & Activity
    Water on The Moon, III. Volatiles & Activity Arlin Crotts (Columbia University) For centuries some scientists have argued that there is activity on the Moon (or water, as recounted in Parts I & II), while others have thought the Moon is simply a dead, inactive world. [1] The question comes in several forms: is there a detectable atmosphere? Does the surface of the Moon change? What causes interior seismic activity? From a more modern viewpoint, we now know that as much carbon monoxide as water was excavated during the LCROSS impact, as detailed in Part I, and a comparable amount of other volatiles were found. At one time the Moon outgassed prodigious amounts of water and hydrogen in volcanic fire fountains, but released similar amounts of volatile sulfur (or SO2), and presumably large amounts of carbon dioxide or monoxide, if theory is to be believed. So water on the Moon is associated with other gases. Astronomers have agreed for centuries that there is no firm evidence for “weather” on the Moon visible from Earth, and little evidence of thick atmosphere. [2] How would one detect the Moon’s atmosphere from Earth? An obvious means is atmospheric refraction. As you watch the Sun set, its image is displaced by Earth’s atmospheric refraction at the horizon from the position it would have if there were no atmosphere, by roughly 0.6 degree (a bit more than the Sun’s angular diameter). On the Moon, any atmosphere would cause an analogous effect for a star passing behind the Moon during an occultation (multiplied by two since the light travels both into and out of the lunar atmosphere).
    [Show full text]
  • Glossary of Lunar Terminology
    Glossary of Lunar Terminology albedo A measure of the reflectivity of the Moon's gabbro A coarse crystalline rock, often found in the visible surface. The Moon's albedo averages 0.07, which lunar highlands, containing plagioclase and pyroxene. means that its surface reflects, on average, 7% of the Anorthositic gabbros contain 65-78% calcium feldspar. light falling on it. gardening The process by which the Moon's surface is anorthosite A coarse-grained rock, largely composed of mixed with deeper layers, mainly as a result of meteor­ calcium feldspar, common on the Moon. itic bombardment. basalt A type of fine-grained volcanic rock containing ghost crater (ruined crater) The faint outline that remains the minerals pyroxene and plagioclase (calcium of a lunar crater that has been largely erased by some feldspar). Mare basalts are rich in iron and titanium, later action, usually lava flooding. while highland basalts are high in aluminum. glacis A gently sloping bank; an old term for the outer breccia A rock composed of a matrix oflarger, angular slope of a crater's walls. stony fragments and a finer, binding component. graben A sunken area between faults. caldera A type of volcanic crater formed primarily by a highlands The Moon's lighter-colored regions, which sinking of its floor rather than by the ejection of lava. are higher than their surroundings and thus not central peak A mountainous landform at or near the covered by dark lavas. Most highland features are the center of certain lunar craters, possibly formed by an rims or central peaks of impact sites.
    [Show full text]
  • Appendix I Lunar and Martian Nomenclature
    APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei
    [Show full text]
  • The Role of External Factors in the Variability of the Structure of the Zooplankton Community of Small Lakes (South-East Kazakhstan)
    water Article The Role of External Factors in the Variability of the Structure of the Zooplankton Community of Small Lakes (South-East Kazakhstan) Moldir Aubakirova 1,2,*, Elena Krupa 3 , Zhanara Mazhibayeva 2, Kuanysh Isbekov 2 and Saule Assylbekova 2 1 Faculty of Biology and Biotechnology, Al-Farabi Kazakh National University, Almaty 050040, Kazakhstan 2 Fisheries Research and Production Center, Almaty 050016, Kazakhstan; mazhibayeva@fishrpc.kz (Z.M.); isbekov@fishrpc.kz (K.I.); assylbekova@fishrpc.kz (S.A.) 3 Institute of Zoology, Almaty 050060, Kazakhstan; [email protected] * Correspondence: [email protected]; Tel.: +7-27-3831715 Abstract: The variability of hydrochemical parameters, the heterogeneity of the habitat, and a low level of anthropogenic impact, create the premises for conserving the high biodiversity of aquatic communities of small water bodies. The study of small water bodies contributes to understanding aquatic organisms’ adaptation to sharp fluctuations in external factors. Studies of biological com- munities’ response to fluctuations in external factors can be used for bioindication of the ecological state of small water bodies. In this regard, the purpose of the research is to study the structure of zooplankton of small lakes in South-East Kazakhstan in connection with various physicochemical parameters to understand the role of biological variables in assessing the ecological state of aquatic Citation: Aubakirova, M.; Krupa, E.; ecosystems. According to hydrochemical data in summer 2019, the nutrient content was relatively Mazhibayeva, Z.; Isbekov, K.; high in all studied lakes. A total of 74 species were recorded in phytoplankton. The phytoplankton Assylbekova, S. The Role of External abundance varied significantly, from 8.5 × 107 to 2.71667 × 109 cells/m3, with a biomass from 0.4 Factors in the Variability of the to 15.81 g/m3.
    [Show full text]
  • Carnegie Institution of Washington Monograph Series
    BTILL UMI Carnegie Institution of Washington Monograph Series BT ILL UMI 1 The Carnegie Institution of Washington, D. C. 1902. Octavo, 16 pp. 2 The Carnegie Institution of Washington, D. C. Articles of Incorporation, Deed of Trust, etc. 1902. Octavo, 15 pp. 3 The Carnegie Institution of Washington, D. C. Proceedings of the Board of Trustees, January, 1902. 1902. Octavo, 15 pp. 4 CONARD, HENRY S. The Waterlilies: A Monograph of the Genus Nymphaea. 1905. Quarto, [1] + xiii + 279 pp., 30 pls., 82 figs. 5 BURNHAM, S. W. A General Catalogue of Double Stars within 121° of the North Pole. 1906. Quarto. Part I. The Catalogue. pp. [2] + lv + 1–256r. Part II. Notes to the Catalogue. pp. viii + 257–1086. 6 COVILLE, FREDERICK VERNON, and DANIEL TREMBLY MACDOUGAL. Desert Botani- cal Laboratory of the Carnegie Institution. 1903. Octavo, vi + 58 pp., 29 pls., 4 figs. 7 RICHARDS, THEODORE WILLIAM, and WILFRED NEWSOME STULL. New Method for Determining Compressibility. 1903. Octavo, 45 pp., 5 figs. 8 FARLOW, WILLIAM G. Bibliographical Index of North American Fungi. Vol. 1, Part 1. Abrothallus to Badhamia. 1905. Octavo, xxxv + 312 pp. 9 HILL, GEORGE WILLIAM, The Collected Mathematical Works of. Quarto. Vol. I. With introduction by H. POINCARÉ. 1905. xix + 363 pp. +errata, frontispiece. Vol. II. 1906. vii + 339 pp. + errata. Vol. III. 1906. iv + 577 pp. Vol. IV. 1907. vi + 460 pp. 10 NEWCOMB, SIMON. On the Position of the Galactic and Other Principal Planes toward Which the Stars Tend to Crowd. (Contributions to Stellar Statistics, First Paper.) 1904. Quarto, ii + 32 pp.
    [Show full text]