DOCSLIB.ORG

(Nasa-Cr-157784) (Lunar Magnetic Peemeability

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
(Nasa-Cr-157784) (Lunar Magnetic Peemeability FINAL REPORT NASA GRANT NSG-2075 Covering the Period September i, 1975 To August 31, 1978 (NASA-CR-157784) (LUNAR MAGNETIC N79-10985 PEEMEABILITY, MAGNETIC FIELDS, AND ELECTRICAL CONDUCTIVITY TEMPERATURE] Final Report, I Sep. 1975 - 31 Aug. 1978 Unclas Jpanta Clra, Univ.)- 131 p_BC _A07/MF, A011 63/91 -35816Th . Submitted by Curtis W. Parkin Principal Investigator Department of Physics University of Santa Clara Santa Clara, California TABLE OF CONTENTS Page I. INTRODUCTION .... ......... 1i II. SCIENTIFIC RESULTS ............... ............ .... .. 2 A. Electrical Conductivity Temperature, and Structure of the Lunar Crust and Deep Interior .......... ............ 2 B. Lunar Magnetic Permeability and Iron Abundance; Limits on Size of a Highly Conducting.Lunar Core ...... ...... ..... 6 C. Lunar Remanent Magnetic Fields: Present-Day Properties; Interaction with the Solar wind; Thermoelectric Origin Model 8 III. PUBLICATIONS AND PRESENTED PAPERS . ........ ......... .... 12 APPENDIX - Publications Listed in Section III .......... 1 4 I. INTRODUCTION In the time period 1969-1972 a total of five magnetometers were deployed on the lunar surface during four Apollo missions. Data from these instru­ ments, along with simultaneous measurements from other experiments on the moon and in lunar orbit, have been used to study properties of the lunar interior and the lunar environment. The principal scientific results result­ ing from analyses of the magnetic field data are discussed in Section II. The results are presented in the following main categories: (1) Lunar elec­ trical conductivity, temperature, and structure; (2) Lunar magnetic permeabil­ ity, iron abundance, and core size limits; (3) the Local remanent magnetic fields, their interaction with the solar wind, and a thermoelectric genera­ tion model for their origin. In Section III relevant publications and presented papers are listed. Copies of publications resulting from the research funded by this grant are-included in the appendix. I. SCIENTIFIC RESULTS Magnetometers placed on the lunar surface and in orbit about the moon have returned a wealth of information about the moon which was not anticipated prior to the Apollo manned lunar missions. Analyses of lunar magnetic data have been used to study the following properties of the moon: Electrical conductivity, temperature, and structure of the lunar crust and deep interior; Lunar magnetic permeability and iron abundance, and inferred limits on size of a highly conducting lunar core; and-Lunar surface remanent magnetic fields: present-day properties, interaction with the solar wind, and origin by thermo­ electric generation. A. Electrical Conductivity "Temperature, and Structure of the Lunar Crust and Deep Interior Electrical conductivity of the lunar interior can be studied by analysis of two types of global induction fields: the poloidal field due to eddy currents driven by-time-varying external magnetic fields, and the toroidal -field due to unipolar currents driven through the moon by the motional solar. wind VxB electric field. Poloidal field induction has been used by many researchers to investigate lunar electrical conductivity, and to date poloidal induction analysis has yielded the most accurate conductivity informa­ tion at depths greater than 200 km. At shallower depths where the poloidal technique is limited by instrumental frequency response and number of measure­ ment sites, a toroidal induction analysis technique is used to determine the-­ upper limit of conductivity of the lunar crust. Since the conductivity is related to temperature, a global temperature profile can be calculated for an assumed compositional model of the lunar interior. Furthermore, structural properties of the-lunar interior can be inferred from characteristics of conductivity and temperature profiles and correlations with results from other geophysical instruments on the moon. 1. Conductivity at depths greater than 200 km. When the moon is in the solar wind, lunar eddy current fields form an induced lunar magnetosphere which is distorted in a complex manner due to flow of solar wind plasma past the moon. The eddy current field is compressed on the day side of the moon and is swept downstream and confined to the "cavity" on the lunar night side. Because of the complexity, early analysis -included a theory fortransient response of a sphere in a vacuum to model lunar response as measured on the lunar night side. An analysis-was also applied to time series magnetometer data taken on the lunar day side using a theory for transient response of a sphere immersed in a completely confining plasma. The most thorough and accurate analysis, using time-dependent poloidal response of a sphere in a vacuum, has been applied to data measured in the geomagnetic tail where plasma confinement effects are minimized. Two basic techniques have been applied to analysis of poloidal induction data measured with the moon ingtbe geomagnetic tail. The-first method used simultaneous measurements by the Apollo 12 lunar surface magnetometer (which measures total response field at the lunar surface) and an Explorer 35 orbiting magnetometer (which measures the externaldriving field). The second uses simultaneous measurements of- the total response field by-two surface magnetometers (Apollo 15 and 16 LSM's) and one close-orbiting-magnetometer (Apollo 16 subsatellite). The first-technique has been applied to the single largest transient measured with the moon in the geomagnetic tail; both techniques are applicable to aggregate "transient eventst9 made up of a linear superposition of -smaller events, Results of the different poloidal induction analysis techniques have been consistent, and an evolution-of improved computer analysis capabilities and use of more data as'it has become available, have yielded the following characteristics of the conductivity profile: The lunar conductivity rises rapidly with depth in the crust.to %,10- 3 nhhos/meter at a 200 to 300 km depth, which corresponds to the upper-mantle boundary reported in seismic results.- From 300 to 900 km depth the conductivity rises more gradually to 3xlO 2 mhos/m. 2. Conductivity of lunar crust; at depths less than 200 km. Studies of crustal conductivity have been completed using toroidal induction analysis. In the toroidal mode a unipolar current J is driven by an electric field -T E = VXBE which is produced as the solar magnetic field BE' frozen in the solar plasma, sweeps by the moon. V is the velocity of the moon relative to the solar plasma. Corresponding to the induced current JTis the toroidal field B which has a magnitude inversely proportional-to the total resistance to -=T current flow through.the moon; the magnitude of T (or likewise, AT) is limited by the region-of lowest conductivity in the current path, that is, the lunar crust0 An upper limit on the electrical conductivity of the lunar crust has been determined from upper limits on toroidal induction intthe moon by the solar wind VxB electric field. The toroidal induction theory is used for the spherically symmetric case of the induction field totally confined to the lunar interior or near-surface regions by a highly conducting plasma. Components of toroidal field are calculated by subtracting components of the external field BE measured by the Explorer 35-Ames magnetometer, from the total field B measured by the Apollo 12 lunar surface magnetometer By comparing the appropriate components of toroidal magnetic field and electric field, the upper limit of the proportionality factor relating these variables is determined. The qualityBTy,= BAy - BEy is compared to the electric field 5 component, Ez, which, is the largest of the three components for average solar wind conditions. These data are linearly correlated, with a least-squares slope A = C-6.2 ± 4.3) x 10- 2 sec/m, where the'limits include only random statistical measurement errors. Estimates of systematic instrumental errors are based upon comparisons between Apollo 12 LSM, Explorer 35-Ames, and r, Explorer 35-Goddard magnetometers. From this comparison we estimate the systematic error inherent in the analysis. W hen systematic ,errors due to uncertainties in instrumental gain factors are included, the upper limit slop becomes A - 2x10 - 7 sec/m. This factor is related to the average crustal conductivity upper limit of 0'crust"u10- 8 mhos/m for an assumed crustal thickness of 80 km. Wenote that the average crust conductivity is not a strong function of crust thickness for thicknesses 'U 80 km (e.g., a 100 km crust would correspond to a l.2x10 upper limit, and a 60 km crust would correspond to about 7x10- 7 mhos/m.) A very thin outer shell of even lower conductivity (indicated by radar and sample measurements for depths up to lb1 km) are consistent with this upper limit. The surface conductivity upper limit, derived from toroidal induction-analysis, places an important con­ straint on the previous lunar conductivity profile obtained from poloidal induction analysis: it lowers the previous crust conductivity limit nearly four orders of magnitude. Electrical conductivity profile results of the lunar interior are summarized in Figure 1. 3. Lunar temperature'and structure. The lunar temperature profile has been inferred from the electrical conductivity profile along with the experi­ mentally known dependence of the conductivity on the temperature for materials used to model the composition.of the lunar interior. For the thermal profile corresponding to the conductivity profile in Figure 1, assuming
Load more

Recommended publications
  • LCROSS (Lunar Crater Observation and Sensing Satellite) Observation Campaign: Strategies, Implementation, and Lessons Learned
    Space Sci Rev DOI 10.1007/s11214-011-9759-y LCROSS (Lunar Crater Observation and Sensing Satellite) Observation Campaign: Strategies, Implementation, and Lessons Learned Jennifer L. Heldmann · Anthony Colaprete · Diane H. Wooden · Robert F. Ackermann · David D. Acton · Peter R. Backus · Vanessa Bailey · Jesse G. Ball · William C. Barott · Samantha K. Blair · Marc W. Buie · Shawn Callahan · Nancy J. Chanover · Young-Jun Choi · Al Conrad · Dolores M. Coulson · Kirk B. Crawford · Russell DeHart · Imke de Pater · Michael Disanti · James R. Forster · Reiko Furusho · Tetsuharu Fuse · Tom Geballe · J. Duane Gibson · David Goldstein · Stephen A. Gregory · David J. Gutierrez · Ryan T. Hamilton · Taiga Hamura · David E. Harker · Gerry R. Harp · Junichi Haruyama · Morag Hastie · Yutaka Hayano · Phillip Hinz · Peng K. Hong · Steven P. James · Toshihiko Kadono · Hideyo Kawakita · Michael S. Kelley · Daryl L. Kim · Kosuke Kurosawa · Duk-Hang Lee · Michael Long · Paul G. Lucey · Keith Marach · Anthony C. Matulonis · Richard M. McDermid · Russet McMillan · Charles Miller · Hong-Kyu Moon · Ryosuke Nakamura · Hirotomo Noda · Natsuko Okamura · Lawrence Ong · Dallan Porter · Jeffery J. Puschell · John T. Rayner · J. Jedadiah Rembold · Katherine C. Roth · Richard J. Rudy · Ray W. Russell · Eileen V. Ryan · William H. Ryan · Tomohiko Sekiguchi · Yasuhito Sekine · Mark A. Skinner · Mitsuru Sôma · Andrew W. Stephens · Alex Storrs · Robert M. Suggs · Seiji Sugita · Eon-Chang Sung · Naruhisa Takatoh · Jill C. Tarter · Scott M. Taylor · Hiroshi Terada · Chadwick J. Trujillo · Vidhya Vaitheeswaran · Faith Vilas · Brian D. Walls · Jun-ihi Watanabe · William J. Welch · Charles E. Woodward · Hong-Suh Yim · Eliot F. Young Received: 9 October 2010 / Accepted: 8 February 2011 © The Author(s) 2011.
    [Show full text]
  • January 2019 Cardanus & Krafft
    A PUBLICATION OF THE LUNAR SECTION OF THE A.L.P.O. EDITED BY: Wayne Bailey [email protected] 17 Autumn Lane, Sewell, NJ 08080 RECENT BACK ISSUES: http://moon.scopesandscapes.com/tlo_back.html FEATURE OF THE MONTH – JANUARY 2019 CARDANUS & KRAFFT Sketch and text by Robert H. Hays, Jr. - Worth, Illinois, USA September 24, 2018 04:40-05:04 UT, 15 cm refl, 170x, seeing 7/10, transparence 6/6. I drew these craters and vicinity on the night of Sept. 23/24, 2018. The moon was about 22 hours before full. This area is in far western Oceanus Procellarum, and was favorably placed for observation that night. Cardanus is the southern one of this pair and is of moderate depth. Krafft to the north is practically identical in size, and is perhaps slightly deeper. Neither crater has a central peak. Several small craters are near and within Krafft. The crater just outside the southeast rim of Krafft is Krafft E, and Krafft C is nearby within Krafft. The small pit to the west is Krafft K, and Krafft D is between Krafft and Cardanus. Krafft C, D and E are similar sized, but K is smaller than these. A triangular-shaped swelling protrudes from the north side of Krafft. The tiny pit, even smaller than Krafft K, east of Cardanus is Cardanus E. There is a dusky area along the southwest side of Cardanus. Two short dark strips in this area may be part of the broken ring Cardanus R as shown on the. Lunar Quadrant map.
    [Show full text]
  • Planetary Surfaces
    Chapter 4 PLANETARY SURFACES 4.1 The Absence of Bedrock A striking and obvious observation is that at full Moon, the lunar surface is bright from limb to limb, with only limited darkening toward the edges. Since this effect is not consistent with the intensity of light reflected from a smooth sphere, pre-Apollo observers concluded that the upper surface was porous on a centimeter scale and had the properties of dust. The thickness of the dust layer was a critical question for landing on the surface. The general view was that a layer a few meters thick of rubble and dust from the meteorite bombardment covered the surface. Alternative views called for kilometer thicknesses of fine dust, filling the maria. The unmanned missions, notably Surveyor, resolved questions about the nature and bearing strength of the surface. However, a somewhat surprising feature of the lunar surface was the completeness of the mantle or blanket of debris. Bedrock exposures are extremely rare, the occurrence in the wall of Hadley Rille (Fig. 6.6) being the only one which was observed closely during the Apollo missions. Fragments of rock excavated during meteorite impact are, of course, common, and provided both samples and evidence of co,mpetent rock layers at shallow levels in the mare basins. Freshly exposed surface material (e.g., bright rays from craters such as Tycho) darken with time due mainly to the production of glass during micro- meteorite impacts. Since some magnetic anomalies correlate with unusually bright regions, the solar wind bombardment (which is strongly deflected by the magnetic anomalies) may also be responsible for darkening the surface [I].
    [Show full text]
  • General Index
    General Index Italicized page numbers indicate figures and tables. Color plates are in- cussed; full listings of authors’ works as cited in this volume may be dicated as “pl.” Color plates 1– 40 are in part 1 and plates 41–80 are found in the bibliographical index. in part 2. Authors are listed only when their ideas or works are dis- Aa, Pieter van der (1659–1733), 1338 of military cartography, 971 934 –39; Genoa, 864 –65; Low Coun- Aa River, pl.61, 1523 of nautical charts, 1069, 1424 tries, 1257 Aachen, 1241 printing’s impact on, 607–8 of Dutch hamlets, 1264 Abate, Agostino, 857–58, 864 –65 role of sources in, 66 –67 ecclesiastical subdivisions in, 1090, 1091 Abbeys. See also Cartularies; Monasteries of Russian maps, 1873 of forests, 50 maps: property, 50–51; water system, 43 standards of, 7 German maps in context of, 1224, 1225 plans: juridical uses of, pl.61, 1523–24, studies of, 505–8, 1258 n.53 map consciousness in, 636, 661–62 1525; Wildmore Fen (in psalter), 43– 44 of surveys, 505–8, 708, 1435–36 maps in: cadastral (See Cadastral maps); Abbreviations, 1897, 1899 of town models, 489 central Italy, 909–15; characteristics of, Abreu, Lisuarte de, 1019 Acequia Imperial de Aragón, 507 874 –75, 880 –82; coloring of, 1499, Abruzzi River, 547, 570 Acerra, 951 1588; East-Central Europe, 1806, 1808; Absolutism, 831, 833, 835–36 Ackerman, James S., 427 n.2 England, 50 –51, 1595, 1599, 1603, See also Sovereigns and monarchs Aconcio, Jacopo (d. 1566), 1611 1615, 1629, 1720; France, 1497–1500, Abstraction Acosta, José de (1539–1600), 1235 1501; humanism linked to, 909–10; in- in bird’s-eye views, 688 Acquaviva, Andrea Matteo (d.
    [Show full text]
  • Workshop on Lunar Volcanic Glasses: Scientific and Resource Potential
    WORKSHOP ON LUNAR VOLCANIC GLASSES: SCIENTIFIC AND RESOURCE POTENTIAL t)--- LPI Technical Report Number 90~02 .. LUNAR AND PLANETARY INSTITUTE 3303 NASA ROAD 1 HOUSTON, TEXAS 77058-4399 WORKSHOP ON LUNAR VOLCANIC GLASSES: SCIENTIFIC AND RESOlTRCE POTENTIAL Edited by John W. Delano and Grant H. Heiken Held at Lunar and Planetary Institute Houston, Texas October 10 - 11, 1989 Sponsored by Lunar and Planetary Institute Lunar and Planetary Sample Team Lunar and Planetary Institute 3303 NASA Road 1 Houston, Texas 77058-4399 LPI Technical Report Number 90-02 Compiled in 1990 by the LUNAR AND PLANETARY INSTITUTE The Institute is operated by Universities Space Research Association under Contract NASW-4066 with the National Aeronautics and Space Administration. Material in this document may be copied without restraint for library, abstract service, educational, or personal research purposes; however, republication of any portion requires the written permission of the authors as well as appropriate acknowledgment of this publication. This report may be cited as: Delano J. W. and Heiken G. H., eds. (1990) Workshop on Lunar Volcanic Glasses: Scientific alld Resource Potelltial. LPI Tech. Rpt. 90-02. Lunar and Planetary Institute, Houston. 74 pp. Papers in this report may be cited as: Author A. A. (1990) Title of paper. In Workshop Oil Lunar Volcanic Glasses: Scientific alld Resource Potelltial (J. W. Delano and G. H. Heiken, eds.), pp. xx-yy. LPI Tech. Rpt. 90-02. Lunar and Planetary Institute, Houston. This report is distributed by: ORDER DEPARTMENT Lunar and Planetary Institute 3303 NASA Road 1 Houston, TX 77058-4399 Mail order requestors will be ill voiced for the cost ofshippillg and halldling.
    [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]
  • 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]
  • Vegetative Ecology of a Montane Mire, Crater Lake National
    AJ ABSTRACT OF THE THESIS OF Susan Cornelia Seyer for the degree of Master of Science in Botany and Plant Pathology presented on December 14, 1979 Title: VEGETATIVE ECOLOGY OF A MONTANE MIRE, CRATER LAKE NATIONAL PARK, OREGON Redacted for Privacy Abstract approved: Jerry F. Franklin Mires, or peat-producing ecosystems, dominated by sedges, shrubs, and brown mosses, are common features in Cascade subalpine regions, occurring where moisture accumulates in small basins or on poorly-drained slopes. Although descriptions and classifications have been developed for mire vegetation in much of the world, there is little information of even a descriptive nature for these montane mires in Oregon and Washington. This thesis reports on phytosocia- logical structure, env'ironental relations, and successional trends in one such mire in the Oregon Cascade mountains. To characterize the general phytosociological structure of the mire vegetation at Sphagnum Bog, Crater Lake National Park, quantitative species cover data were used in conjunction with a Braun-Blanquet tabular analysis and two-dimensional stand ordinations, reciprocal averaging and a Bray-Curtis polar ordination. Defined community types correspond to physiognomic types as follows: Carex rostrata (reedswamp); Eleocharis pauciflora-Carex limosa, Eleocharis pauciflora/bryophytes (low sedge fens); Carex sichensis (tall sedge fen); Vaccinium/ Aulacomnium palustre, Vaccinium occidentala/Carex sitchensis (shrub thickets; Alnus incana/Brachythacium sp. and Salix barclayi (marginal carrs).Phases were defined when appropriate. A vegetation map was made to illustrate the locations and extent of the variouscommunities. Comparisons with other montane mires in thearea determined that the physiognomic units defined are repeatable when appropriate habitat conditions are present, and that they usually includemany of the same characteristic species, the dominant mosses being particularly constant.
    [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]
  • Why NASA Consistently Fails at Congress
    W&M ScholarWorks Undergraduate Honors Theses Theses, Dissertations, & Master Projects 6-2013 The Wrong Right Stuff: Why NASA Consistently Fails at Congress Andrew Follett College of William and Mary Follow this and additional works at: https://scholarworks.wm.edu/honorstheses Part of the Political Science Commons Recommended Citation Follett, Andrew, "The Wrong Right Stuff: Why NASA Consistently Fails at Congress" (2013). Undergraduate Honors Theses. Paper 584. https://scholarworks.wm.edu/honorstheses/584 This Honors Thesis is brought to you for free and open access by the Theses, Dissertations, & Master Projects at W&M ScholarWorks. It has been accepted for inclusion in Undergraduate Honors Theses by an authorized administrator of W&M ScholarWorks. For more information, please contact [email protected]. The Wrong Right Stuff: Why NASA Consistently Fails at Congress A thesis submitted in partial fulfillment of the requirement for the degree of Bachelors of Arts in Government from The College of William and Mary by Andrew Follett Accepted for . John Gilmour, Director . Sophia Hart . Rowan Lockwood Williamsburg, VA May 3, 2013 1 Table of Contents: Acknowledgements 3 Part 1: Introduction and Background 4 Pre Soviet Collapse: Early American Failures in Space 13 Pre Soviet Collapse: The Successful Mercury, Gemini, and Apollo Programs 17 Pre Soviet Collapse: The Quasi-Successful Shuttle Program 22 Part 2: The Thin Years, Repeated Failure in NASA in the Post-Soviet Era 27 The Failure of the Space Exploration Initiative 28 The Failed Vision for Space Exploration 30 The Success of Unmanned Space Flight 32 Part 3: Why NASA Fails 37 Part 4: Putting this to the Test 87 Part 5: Changing the Method.
    [Show full text]
  • Evidence for Impact-Generated Deposition
    EVIDENCE FOR IMPACT-GENERATED DEPOSITION ON THE LATE EOCENE SHORES OF GEORGIA by ROBERT SCOTT HARRIS (Under the direction of Michael F. Roden) ABSTRACT Modeling demonstrates that the Late Eocene Chesapeake Bay impact would have been capable of depositing ejecta in east-central Georgia with thicknesses exceeding thirty centimeters. A coarse sand layer at the base of the Upper Eocene Dry Branch Formation was examined for shocked minerals. Universal stage measurements demonstrate that planar fabrics in some fine to medium sand-size quartz grains are parallel to planes commonly exploited by planar deformation features (PDF’s) in shocked quartz. Possible PDF’s are observed parallel to {10-13}, {10-11}, {10-12}, {11-22} and {51-61}. Petrographic identification of shocked quartz is supported by line broadening in X-ray diffraction experiments. Other impact ejecta recognized include possible ballen quartz, maskelynite, and reidite-bearing zircon grains. The layer is correlative with an unusual diamictite that contains goethite spherules similar to altered microkrystites. It may represent an impact-generated debris flow. These discoveries suggest that the Chesapeake Bay impact horizon is preserved in Georgia. The horizon also should be the source stratum for Georgia tektites. INDEX WORDS: Chesapeake Bay impact, Upper Eocene, Shocked quartz, Impact shock, Shocked zircon, Impact, Impact ejecta, North American tektites, Tektites, Georgiaites, Georgia Tektites, Planar deformation features, PDF’s, Georgia, Geology, Coastal Plain, Stratigraphy, Impact stratigraphy, Impact spherules, Goethite spherules, Diamictite, Twiggs Clay, Dry Branch Formation, Clinchfield Sand, Irwinton Sand, Reidite, Microkrystite, Cpx Spherules, Impact debris flow EVIDENCE FOR IMPACT-GENERATED DEPOSITION ON THE LATE EOCENE SHORES OF GEORGIA by ROBERT SCOTT HARRIS B.
    [Show full text]
  • The Royalston Community Newsletter
    THE ROYALSTON COMMUNITY NEWSLETTER December 2020 Volume XXII IssueX January 2021 A Publication of the Friends of the Phinehas S. Newton Library, Royalston, Massachusetts Calendar of Events December 1 Monday December 18 Friday National Ugly Sweater Day NORAD follows Santa’s travels this month, and can be seen on-line at http://www.noradsanta.org. This December 21 Monday special mission of the North American Aerospace Defense Predawn Ursid Meteor Shower continues from about a Command at Peterson Air Force Base in Colorado goes live week ago, peaking this morning through tomorrow, and depart- December 1, providing information and games to help every- ing shortly after Christmas. The remains of the Tuttle Comet will one gear up for the big night. produce a “shooting star” every six to ten minutes, but there have been bursts of up to 25 in a single hour. December 4 Friday 6 pm South Village Tree Lighting and Gazebo Dedi- 5:02 a.m. Winter Solstice – First Day of Winter (Day- cation sponsored by The Royalston South Village Revital- light hours begin to increase!) ization group. All are welcome. Hot chocolate and cookies. Music provided by Larry Trask and Rene Lake. Memorial December 25 Friday Christmas Day ornaments from the Ladies’ Benevolent Society will be hung on the tree. To get yours, call Laurie Deveneau at 978-249- December 26 Saturday First Day of Kwanzaa 5807. The 120 Drawing will be held and a special guest in a red suit will visit. In case of inclement weather, the event will December 29 Tuesday be held on the following Friday, December 11.
    [Show full text]