Mariner Mars 1964 Handbook

Total Page:16

File Type:pdf, Size:1020Kb

Mariner Mars 1964 Handbook NATIONALAERONAUTICSANDSPACEADMINISTRATION MARINER MARS 1964 HANDBOOK RobertVanBuren JETPROPULSIONLABORATORY CaliforniaInstituteofTechnology December1, 1965 JPLTechnicalMemorandum33-265 Copyright© 1965 Jet PropulsionLaboratory California Institute of Technology Prepared under Contract No. NAS7-100 National Aerenauticsand Space Administration Preface This book presents a compilation of significant technical data relative to Mariner Mars 1964. Its purpose is to collect, in one location, a wide variety of statistical information that would otherwise be scattered throughout a large number of miscellaneous documents. The information presented here pertains primarily to the Mariner spacecraft, itself; it does not include the Launch Vehicle System, the ground support equipment, the Deep Space Network System, or other areas of the total Mariner Mars 1964 project. The primary Mariner Mars ]964 mission is considered in this book to have ended on October 1, 1965. Historical data are carried only to that date, although some orbital parame. ters are projected to 1967 and 1971 in the tables and figures. It is expected that the user of this handbook will have somefamiliarity with the terminology, operational procedures, and engineering concepts related to an interplanetary space- craft project and, specifically, to the Mariner Mars 1964 proj- ect. The handbook's function is more to remind those who already know than to instruct those who don't. A list of documentspertaining to the Mariner Mars 1964 mission is included (Table 25) for reference purposes. The list is complete as of the publication date of this handbook, but many articles and reports are still being prepared and will continueto be published for sometime to come. CONTENTS AbsorptivityStandard ..................................... 1 Acquisition(see Sun Acquisition,Star Acquisition) Albedo (see Mars) Alpha Particles (see Scientific Data, CosmicRay Telescope) Altitude ............................................... 1 Antenna (see High-GainAntenna, Low-GainAntenna) Aphelion (see Orbit Data) AstronomicalUnit (see Orbit Data) Atmosphere,Martian (see Scientific Data) Attitude Control ......................................... 2 Battery (see Power) Bays ................................................. 3 Bibliography(see Table 25) Bit Rate ............................................... 3 Black Space Picture Sequence .............................. 3 Booster Regulators (see Power) CanopusAcquisition(see Star Acquisition) Canopus-Probe-SunAngles .................................. 4 Canopus Tracker ........................................ 4 Cavity Amplifier (see Radio) Celestial Latitude, Mariner IV .............................. 5 Celestial Longitude, Earth ................................. 6 Celestial Longitude, Mariner IV ............................. 6 Celestial Longitude, Mars ................................. 6 Center of Gravity (see Spacecraft) Central Computer and Sequencer ............................ 7 Chronology(see Dates, Event Times) Clock (see Central Computer and Sequencer) Clock Angle ............................................ 8 ClosestApproachto Mars .................................. 8 CognizantEngineers and Scientists (see Personnel) Command Subsystem ..................................... 8 Commands ............................................. 9 Communication .......................................... 11 Communication Times, One Way ............................. 11 Computer (see Central Computer and Sequencer) Cone Angle ............................................ ] 1 Conjunction (see Orbit Data) Contractors (see Table 24) Cosmic Dust Detector ..................................... 12 Cosmic RayTelescope ..................................... 12 Cost Information ........................................ 14 Cover Drop ............................................. ]5 CONTENTS(Cont'd) Cruise Mode ............................................ 15 . Cyclics ............................................... 16 Data (see Telemetry) Data Automation Subsystem ................................ 16 Data Encoder Subsystem ................................... 16 Data Modes (see Telemetry) Dates ................................................. 16 DC-15 Canopus Gate Override Event .......................... 18 Deimos(see Mars) Detectors (see Canopus Tracker, Earth Detector) Dimensions ............................................ 18 Dipole Moment of Earth ................................... 19 Dipole Moment of Mars (see Scientific Data) Distance of Mariner IV from Earth ........................... 19 Distance of Mariner IV from Center of Mars .................... 19 Distance of Mariner IV from Sun ............................ 20 Distance Traveled Along Heliocentic Arc by Mariner IV ............ 21 Documents(see Table 25) Earth Clock Angle Through1971 (see Fig. 42) Earth Detector .......................................... 22 Earth Dipole Moment ..................................... 22 Earth-Probe-Sun Angle ..................................... 22 Ecliptic ............................................... 22 Electrons (see Scientific Data, Trapped Radiation Detector, Cosmic RayTelescope) Encounter ............................................. 22 End of Mission .......................................... 23 Engineering Change Requests ............................... 23 Environmental Tests ...................................... 24 Escape Velocity ......................................... 24 Event Times, GMT ........................................ 24 Exciters (see Radio) Experimenters (see Table 7) Fields and Particles ...................................... 31 Fields of View .......................................... 31 Frequency (see Radio) Fuel (see Propulsion) Gas (see Attitude Control) Gravitational Constant (see Orbit Data) Greenwich Mean Times of Mission Events (see Event Times) Gyro Control Subsystem ................................... 32 Helium Magnetometer ..................................... 32 High-Gain Antenna ........................................ 33 CONTENTS(Cent'd) Injection (see Event Times) Instruments, Field and Particles (see Cosmic Dust Detector, Cosmic Ray Telescope, Helium Magnetometer, Ionization Chamber, Solar Plasma Probe, Trapped Radiation Detector; see also Scientific Data from Mariner IV, Telemetry) Interferometer Effect (see Fig. 26) Investigators (see Table 7) Ionization Chamber ...................................... 34 Latitude (see Celestial Latitude) Launch Data for Mariner III ................................ 34 Launch Data for Mariner IV ................................ 34 Life Tests ............................................. 35 Longitude (see Celestial Longitude) Look Angles ............................................ 35 Louvers (see Temperature Control) Low-Gain Antenna ........................................ 36 Magnetic Fields ......................................... 37 Magnetometer (see Helium Magnetometer) Maneuver Inhibit Sequence ................................ 3'7 Mariner III ............................................. 37 Mars ................................................. 38 Mass (see Scientific Data) Materials (see Spacecraft Structure, Absorptivity Standard) Measurements (see Scientific Data, Telemetry; see also Cosmic Dust Detector, Cosmic Ray Telescope, Helium Magnetometer, Ionization Chamb3r, Solar Plasma Probe, Trapped Radiation Detector, and Figs. 10-13, 22, and 24-33) Midcourse Maneuver ..................................... 40 Midcourse Motor (see Propulsion) MT-1 Canopus Cone Angle Update Event ....................... 42 MT-2 Canopus Cone Angle Update Event ....................... 42 MT-3 Canopus Cone Angle Update Event ....................... 43 MT-4 Canopus Cone Angle Update Event ....................... 43 MT-5 Changeover to High-Gain Antenna ........................ 44 MT-6 Changeover to 81/3 bps ............................... 44 MT-7 Event (see Encounter) MT-8 Event (see Event Times) MT-9 Event (see Event Times) Narrow-Angle Acquisition (see Event Times, Narrow-Angle Mars Gate) Narrow-Angle Mars Gate ................................... 45 NASA Quarterly Reviews (see Dates) Occultation Experiment .................................... 46 Opposition (see Orbit Data) Orbit Data, Mariner III .................................... 46 Orbit Data, Mariner IV .................................... 47 vii CONTENTS(Cont'd) Parking Orbit (see LaunchData) Part Failure Summary(see Table 26) Parts, Numberof (see Spacecraft) Perihelion (see Orbit Data) Personnel ............................................. 49 Phobos(see Mars) Photographs(see Picture Data) Picture Data ........................................... 54 Planetary Acquisition (see Wide-AngleAcquisition) Planetary Scan Platform ................................... 57 Plasma Probe (see Solar Plasma Probe) Post-Injection Propulsion System (see Propulsion) Power Subsystem ........................................ 58 Principal Investigators (see Table 7) Problem/Failure Reports .................................. 59 Propulsion System ....................................... 59 Protons (see Scientific Data, TrappedRadiation Detector, Cosmic Ray Telescope) Publications (see Table 25) Pyrotechnics ........................................... 60 Quarterly Reviews, NASA (see Dates) Radiation (see Cosmic Ray Telescope, Ionization Chamber, Scientific Datafrom Mariner IV, Trapped Radiation Detector) Radio ................................................. 61 Range (see Orbit Data) Receiver (see Radio)
Recommended publications
  • MARS an Overview of the 1985–2006 Mars Orbiter Camera Science
    MARS MARS INFORMATICS The International Journal of Mars Science and Exploration Open Access Journals Science An overview of the 1985–2006 Mars Orbiter Camera science investigation Michael C. Malin1, Kenneth S. Edgett1, Bruce A. Cantor1, Michael A. Caplinger1, G. Edward Danielson2, Elsa H. Jensen1, Michael A. Ravine1, Jennifer L. Sandoval1, and Kimberley D. Supulver1 1Malin Space Science Systems, P.O. Box 910148, San Diego, CA, 92191-0148, USA; 2Deceased, 10 December 2005 Citation: Mars 5, 1-60, 2010; doi:10.1555/mars.2010.0001 History: Submitted: August 5, 2009; Reviewed: October 18, 2009; Accepted: November 15, 2009; Published: January 6, 2010 Editor: Jeffrey B. Plescia, Applied Physics Laboratory, Johns Hopkins University Reviewers: Jeffrey B. Plescia, Applied Physics Laboratory, Johns Hopkins University; R. Aileen Yingst, University of Wisconsin Green Bay Open Access: Copyright 2010 Malin Space Science Systems. This is an open-access paper distributed under the terms of a Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Abstract Background: NASA selected the Mars Orbiter Camera (MOC) investigation in 1986 for the Mars Observer mission. The MOC consisted of three elements which shared a common package: a narrow angle camera designed to obtain images with a spatial resolution as high as 1.4 m per pixel from orbit, and two wide angle cameras (one with a red filter, the other blue) for daily global imaging to observe meteorological events, geodesy, and provide context for the narrow angle images. Following the loss of Mars Observer in August 1993, a second MOC was built from flight spare hardware and launched aboard Mars Global Surveyor (MGS) in November 1996.
    [Show full text]
  • Sinuous Ridges in Chukhung Crater, Tempe Terra, Mars: Implications for Fluvial, Glacial, and Glaciofluvial Activity Frances E.G
    Sinuous ridges in Chukhung crater, Tempe Terra, Mars: Implications for fluvial, glacial, and glaciofluvial activity Frances E.G. Butcher, Matthew Balme, Susan Conway, Colman Gallagher, Neil Arnold, Robert Storrar, Stephen Lewis, Axel Hagermann, Joel Davis To cite this version: Frances E.G. Butcher, Matthew Balme, Susan Conway, Colman Gallagher, Neil Arnold, et al.. Sinuous ridges in Chukhung crater, Tempe Terra, Mars: Implications for fluvial, glacial, and glaciofluvial activity. Icarus, Elsevier, 2021, 10.1016/j.icarus.2020.114131. hal-02958862 HAL Id: hal-02958862 https://hal.archives-ouvertes.fr/hal-02958862 Submitted on 6 Oct 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. 1 Sinuous Ridges in Chukhung Crater, Tempe Terra, Mars: 2 Implications for Fluvial, Glacial, and Glaciofluvial Activity. 3 Frances E. G. Butcher1,2, Matthew R. Balme1, Susan J. Conway3, Colman Gallagher4,5, Neil 4 S. Arnold6, Robert D. Storrar7, Stephen R. Lewis1, Axel Hagermann8, Joel M. Davis9. 5 1. School of Physical Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6 6AA, UK. 7 2. Current address: Department of Geography, The University of Sheffield, Sheffield, S10 8 2TN, UK ([email protected]).
    [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]
  • Mariner to Mercury, Venus and Mars
    NASA Facts National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, CA 91109 Mariner to Mercury, Venus and Mars Between 1962 and late 1973, NASA’s Jet carry a host of scientific instruments. Some of the Propulsion Laboratory designed and built 10 space- instruments, such as cameras, would need to be point- craft named Mariner to explore the inner solar system ed at the target body it was studying. Other instru- -- visiting the planets Venus, Mars and Mercury for ments were non-directional and studied phenomena the first time, and returning to Venus and Mars for such as magnetic fields and charged particles. JPL additional close observations. The final mission in the engineers proposed to make the Mariners “three-axis- series, Mariner 10, flew past Venus before going on to stabilized,” meaning that unlike other space probes encounter Mercury, after which it returned to Mercury they would not spin. for a total of three flybys. The next-to-last, Mariner Each of the Mariner projects was designed to have 9, became the first ever to orbit another planet when two spacecraft launched on separate rockets, in case it rached Mars for about a year of mapping and mea- of difficulties with the nearly untried launch vehicles. surement. Mariner 1, Mariner 3, and Mariner 8 were in fact lost The Mariners were all relatively small robotic during launch, but their backups were successful. No explorers, each launched on an Atlas rocket with Mariners were lost in later flight to their destination either an Agena or Centaur upper-stage booster, and planets or before completing their scientific missions.
    [Show full text]
  • Martian Perched Craters and Large Ejecta Volume: Evidence for Episodes of Deflation in the Northern Lowlands
    Meteoritics & Planetary Science 41, Nr 10, 1647–1658 (2006) Abstract available online at http://meteoritics.org Martian perched craters and large ejecta volume: Evidence for episodes of deflation in the northern lowlands Sandrine MERESSE1*, François COSTARD1, Nicolas MANGOLD1, David BARATOUX2, and Joseph M. BOYCE3 1Laboratoire IDES-Orsay, Université Paris-Sud, UMR 8148, Bat 509, 91405 Orsay, France 2Observatoire Midi-Pyrénées, UMR 5562, 31400 Toulouse, France 3Hawai’i Institute of Geophysics and Planetology, University of Hawai’i at Manoa, Honolulu, Hawai’i, USA *Corresponding author. E-mail: [email protected] (Received 28 October 2005; revision accepted 30 June 2006) Abstract–The northern lowland plains, such as those found in Acidalia and Utopia Planitia, have high percentages of impact craters with fluidized ejecta. In both regions, the analysis of crater geometry from Mars Orbiter Laser Altimeter (MOLA) data has revealed large ejecta volumes, some exceeding the volume of excavation. Moreover, some of the crater cavities and fluidized ejecta blankets of these craters are topographically perched above the surrounding plains. These perched craters are concentrated between 40 and 70°N in the northern plains. The atypical high volumes of the ejecta and the perched craters suggest that the northern lowlands have experienced one or more episodes of resurfacing that involved deposition and erosion. The removal of material, most likely caused by the sublimation of ice in the materials and their subsequent erosion and transport by the wind, is more rapid on the plains than on the ejecta blankets. The thermal inertia difference between the ejecta and the surrounding plains suggests that ejecta, characterized by a lower thermal inertia, protect the underneath terrain from sublimation.
    [Show full text]
  • Orbital Evidence for More Widespread Carbonate- 10.1002/2015JE004972 Bearing Rocks on Mars Key Point: James J
    PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Orbital evidence for more widespread carbonate- 10.1002/2015JE004972 bearing rocks on Mars Key Point: James J. Wray1, Scott L. Murchie2, Janice L. Bishop3, Bethany L. Ehlmann4, Ralph E. Milliken5, • Carbonates coexist with phyllosili- 1 2 6 cates in exhumed Noachian rocks in Mary Beth Wilhelm , Kimberly D. Seelos , and Matthew Chojnacki several regions of Mars 1School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA, 2The Johns Hopkins University/Applied Physics Laboratory, Laurel, Maryland, USA, 3SETI Institute, Mountain View, California, USA, 4Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA, 5Department of Geological Sciences, Brown Correspondence to: University, Providence, Rhode Island, USA, 6Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA J. J. Wray, [email protected] Abstract Carbonates are key minerals for understanding ancient Martian environments because they Citation: are indicators of potentially habitable, neutral-to-alkaline water and may be an important reservoir for Wray, J. J., S. L. Murchie, J. L. Bishop, paleoatmospheric CO2. Previous remote sensing studies have identified mostly Mg-rich carbonates, both in B. L. Ehlmann, R. E. Milliken, M. B. Wilhelm, Martian dust and in a Late Noachian rock unit circumferential to the Isidis basin. Here we report evidence for older K. D. Seelos, and M. Chojnacki (2016), Orbital evidence for more widespread Fe- and/or Ca-rich carbonates exposed from the subsurface by impact craters and troughs. These carbonates carbonate-bearing rocks on Mars, are found in and around the Huygens basin northwest of Hellas, in western Noachis Terra between the Argyre – J.
    [Show full text]
  • Sinuous Ridges in Chukhung Crater, Tempe Terra, Mars: Implications for Fluvial, Glacial, and Glaciofluvial Activity
    This is a repository copy of Sinuous ridges in Chukhung crater, Tempe Terra, Mars: Implications for fluvial, glacial, and glaciofluvial activity. White Rose Research Online URL for this paper: http://eprints.whiterose.ac.uk/166644/ Version: Published Version Article: Butcher, F.E.G. orcid.org/0000-0002-5392-7286, Balme, M.R., Conway, S.J. et al. (6 more authors) (2021) Sinuous ridges in Chukhung crater, Tempe Terra, Mars: Implications for fluvial, glacial, and glaciofluvial activity. Icarus, 357. 114131. ISSN 0019-1035 https://doi.org/10.1016/j.icarus.2020.114131 Reuse This article is distributed under the terms of the Creative Commons Attribution (CC BY) licence. This licence allows you to distribute, remix, tweak, and build upon the work, even commercially, as long as you credit the authors for the original work. More information and the full terms of the licence here: https://creativecommons.org/licenses/ Takedown If you consider content in White Rose Research Online to be in breach of UK law, please notify us by emailing [email protected] including the URL of the record and the reason for the withdrawal request. [email protected] https://eprints.whiterose.ac.uk/ Journal Pre-proof Sinuous ridges in Chukhung crater, Tempe Terra, Mars: Implications for fluvial, glacial, and glaciofluvial activity Frances E.G. Butcher, Matthew R. Balme, Susan J. Conway, Colman Gallagher, Neil S. Arnold, Robert D. Storrar, Stephen R. Lewis, Axel Hagermann, Joel M. Davis PII: S0019-1035(20)30473-5 DOI: https://doi.org/10.1016/j.icarus.2020.114131 Reference: YICAR 114131 To appear in: Icarus Received date: 2 June 2020 Revised date: 19 August 2020 Accepted date: 28 September 2020 Please cite this article as: F.E.G.
    [Show full text]
  • Seasonal Melting and the Formation of Sedimentary Rocks on Mars, with Predictions for the Gale Crater Mound
    Seasonal melting and the formation of sedimentary rocks on Mars, with predictions for the Gale Crater mound Edwin S. Kite a, Itay Halevy b, Melinda A. Kahre c, Michael J. Wolff d, and Michael Manga e;f aDivision of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA bCenter for Planetary Sciences, Weizmann Institute of Science, P.O. Box 26, Rehovot 76100, Israel cNASA Ames Research Center, Mountain View, California 94035, USA dSpace Science Institute, 4750 Walnut Street, Suite 205, Boulder, Colorado, USA eDepartment of Earth and Planetary Science, University of California Berkeley, Berkeley, California 94720, USA f Center for Integrative Planetary Science, University of California Berkeley, Berkeley, California 94720, USA arXiv:1205.6226v1 [astro-ph.EP] 28 May 2012 1 Number of pages: 60 2 Number of tables: 1 3 Number of figures: 19 Preprint submitted to Icarus 20 September 2018 4 Proposed Running Head: 5 Seasonal melting and sedimentary rocks on Mars 6 Please send Editorial Correspondence to: 7 8 Edwin S. Kite 9 Caltech, MC 150-21 10 Geological and Planetary Sciences 11 1200 E California Boulevard 12 Pasadena, CA 91125, USA. 13 14 Email: [email protected] 15 Phone: (510) 717-5205 16 2 17 ABSTRACT 18 A model for the formation and distribution of sedimentary rocks on Mars 19 is proposed. The rate{limiting step is supply of liquid water from seasonal 2 20 melting of snow or ice. The model is run for a O(10 ) mbar pure CO2 atmo- 21 sphere, dusty snow, and solar luminosity reduced by 23%.
    [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]
  • Atoll Research Bulletin
    HARLES H. LAMOOREW No. 86 February 28, 1965 BOTANY DEPT. UNlVERSllY OF HAWAII HONOLULU 14. HAWAII ATOLL RESEARCH BULLETIN Geography and land ecology of CZ;Pperton Idand by ~arie-H6l;ne Sachet Issued by THE PACIFIC SCIENCE BOARD National Academy of Sciences-National Research Council Washington, D.C., U.S.A. ATOU RESEARCH lNlUXTN ---..------------- NO. 86 Geography and land ecology of Clipperton Island by Marie -&'lbne Sachet Issued by PACITE EClENCE BOARD National Academcy of Sciences-4?a'tlonal Research Council Washington, D. C. February 28, 1962 It is a pleasure to conmend the far-sighted policy of the Of'fice of Naval Research, with its emphasis on basic research, as a result of which a grant has made possible the continuation of the Coral Atoll Program of the Pacific Science Board. It is of interest to note, historically, that much of the f'unda- mntal Infomaation on atolls of the Pacific was gathered by the U. S. Navy's South Pacific Exploring Ekpedition, over one hundred years ago, under the cormnand of Captain Charles kfillres. The continuing nature of such scientific interest by the Navy is shotm by the support for the Pacific Science Board ' s research programs during the past fourteen years. me preparation and issuance of the Atoll Research Bulletin is assisted by fbds from Contract N70nr-2300(12). The sole responsibility for all statements made by authors of papers in the Atoll Research Bulletin rests with them, and they do not necessarily represent the views of the Pacific Science Board or of the editors of the Bulletin.
    [Show full text]
  • The Stratigraphy and Evolution of Lower Mount Sharp from Spectral
    PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE The stratigraphy and evolution of lower Mount Sharp 10.1002/2016JE005095 from spectral, morphological, and thermophysical Key Points: orbital data sets • We have developed a stratigraphy for lower Mount Sharp using analyses of A. A. Fraeman1, B. L. Ehlmann1,2, R. E. Arvidson3, C. S. Edwards4,5, J. P. Grotzinger2, R. E. Milliken6, new spectral, thermophysical, and 2 7 morphologic orbital data products D. P. Quinn , and M. S. Rice • Siccar Point group records a period of 1 2 deposition and exhumation that Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA, Division of Geological and followed the deposition and Planetary Sciences, California Institute of Technology, Pasadena, California, USA, 3Department of Earth and Planetary exhumation of the Mount Sharp Sciences, Washington University in St. Louis, St. Louis, Missouri, USA, 4United States Geological Survey, Flagstaff, Arizona, group USA, 5Department of Physics and Astronomy, Northern Arizona University, Flagstaff, Arizona, USA, 6Department of Earth, • Late state silica enrichment and redox 7 interfaces within lower Mount Sharp Environmental and Planetary Sciences, Brown University, Providence, Rhode Island, USA, Geology Department, Physics were pervasive and widespread in and Astronomy Department, Western Washington University, Bellingham, Washington, USA space and/or in time Abstract We have developed a refined geologic map and stratigraphy for lower Mount Sharp using coordinated analyses of new spectral, thermophysical, and morphologic orbital data products. The Mount Correspondence to: A. A. Fraeman, Sharp group consists of seven relatively planar units delineated by differences in texture, mineralogy, and [email protected] thermophysical properties.
    [Show full text]
  • Composition of Mars, Michelle Wenz
    The Composition of Mars Michelle Wenz Curiosity Image NASA Importance of minerals . Role in transport and storage of volatiles . Ex. Water (adsorbed or structurally bound) . Control climatic behavior . Past conditions of mars . specific pressure and temperature formation conditions . Constrains formation and habitability Curiosity Rover at Mount Sharp drilling site, NASA image Missions to Mars . 44 missions to Mars (all not successful) . 21 NASA . 18 Russia . 1 ESA . 1 India . 1 Japan . 1 joint China/Russia . 1 joint ESA/Russia . First successful mission was Mariner 4 in 1964 Credit: Jason Davis / astrosaur.us, http://utprosim.com/?p=808 First Successful Mission: Mariner 4 . First image of Mars . Took 21 images . No evidence of canals . Not much can be said about composition Mariner 4, NASA image Mariner 4 first image of Mars, NASA image Viking Lander . First lander on Mars . Multispectral measurements Viking Planning, NASA image Viking Anniversary Image, NASA image Viking Lander . Measured dust particles . Believed to be global representation . Computer generated mixtures of minerals . quartz, feldspar, pyroxenes, hematite, ilmenite Toulmin III et al., 1977 Hubble Space Telescope . Better resolution than Mariner 6 and 7 . Viking limited to three bands between 450 and 590 nm . UV- near IR . Optimized for iron bearing minerals and silicates Hubble Space Telescope NASA/ESA Image featured in Astronomy Magazine Hubble Spectroscopy Results . 1994-1995 . Ferric oxide absorption band 860 nm . hematite . Pyroxene 953 nm absorption band . Looked for olivine contributions . 1042 nm band . No significant olivine contributions Hubble Space Telescope 1995, NASA Composition by Hubble . Measure of the strength of the absorption band . Ratio vs.
    [Show full text]