Crater Mountain Hike Through a Volcanic Wonderland
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Glossary Glossary
Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts. -
UNITED STATES DISTRICT COURT NORTHERN DISTRICT of INDIANA SOUTH BEND DIVISION in Re FEDEX GROUND PACKAGE SYSTEM, INC., EMPLOYMEN
USDC IN/ND case 3:05-md-00527-RLM-MGG document 3279 filed 03/22/19 page 1 of 354 UNITED STATES DISTRICT COURT NORTHERN DISTRICT OF INDIANA SOUTH BEND DIVISION ) Case No. 3:05-MD-527 RLM In re FEDEX GROUND PACKAGE ) (MDL 1700) SYSTEM, INC., EMPLOYMENT ) PRACTICES LITIGATION ) ) ) THIS DOCUMENT RELATES TO: ) ) Carlene Craig, et. al. v. FedEx Case No. 3:05-cv-530 RLM ) Ground Package Systems, Inc., ) ) PROPOSED FINAL APPROVAL ORDER This matter came before the Court for hearing on March 11, 2019, to consider final approval of the proposed ERISA Class Action Settlement reached by and between Plaintiffs Leo Rittenhouse, Jeff Bramlage, Lawrence Liable, Kent Whistler, Mike Moore, Keith Berry, Matthew Cook, Heidi Law, Sylvia O’Brien, Neal Bergkamp, and Dominic Lupo1 (collectively, “the Named Plaintiffs”), on behalf of themselves and the Certified Class, and Defendant FedEx Ground Package System, Inc. (“FXG”) (collectively, “the Parties”), the terms of which Settlement are set forth in the Class Action Settlement Agreement (the “Settlement Agreement”) attached as Exhibit A to the Joint Declaration of Co-Lead Counsel in support of Preliminary Approval of the Kansas Class Action 1 Carlene Craig withdrew as a Named Plaintiff on November 29, 2006. See MDL Doc. No. 409. Named Plaintiffs Ronald Perry and Alan Pacheco are not movants for final approval and filed an objection [MDL Doc. Nos. 3251/3261]. USDC IN/ND case 3:05-md-00527-RLM-MGG document 3279 filed 03/22/19 page 2 of 354 Settlement [MDL Doc. No. 3154-1]. Also before the Court is ERISA Plaintiffs’ Unopposed Motion for Attorney’s Fees and for Payment of Service Awards to the Named Plaintiffs, filed with the Court on October 19, 2018 [MDL Doc. -
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. -
June 21 2017 Regular Meeting
Northern Inyo Hospital June 21 2017 Regular Meeting June 21 2017 Regular Meeting - June 21 2017 Regular Meeting Agenda, June 21 2017 Regular Meeting Draft Agenda, June 21 2017 Regular Meeting...........................................................3 Budget, Fiscal Year 2017-2018 Budget, 2017-2018 Fiscal Year ...................................................................................6 Nursing Department Policies and Procedures Licensure of Nursing Personnel Policy and Procedure.........................................38 Language Access Services Program Policy and Procedure.................................40 Annual Policy and Procedure Approvals Annual Policy and Procedure Approvals ................................................................44 Board Resolution 17-01, Appropriations Limit Board Resolution 17-02, Annual Appropriations Limit ..........................................50 Board Resolution 17-02, 401(A) Retirement Plan Contribution Board Resolution 17-02, 401(A) Plan Contribution ................................................51 Radiology Services Agreement Radiology Services Agreement................................................................................52 Email Use Policy and Procedure Electronic Communications (Email) Use Policy and Procedure...........................74 NIHD Password Policy NIHD Password Policy and Procedure ....................................................................79 Workplace Violence Prevention Policy and Procedure Workplace Violence Prevention Policy and Procedure .........................................80 -
June 9, 2020 LIST of ABSENTEE VOTERS HOLDING BALLOTS – NAMES
WARSAW CENTRAL SCHOOL BUDGET/BOARD VOTE – June 9, 2020 LIST OF ABSENTEE VOTERS HOLDING BALLOTS – NAMES Abbasey, Salman Aumer, Andrew J. Bauer, James E. Abbott, John Axtell, Paula A. Bauer, Janet M. Ackerman, James Backlas, Frederick A. Jr Bauer, Michael Ackerman, Susan M. Bagg , Robert L. Bauer, Michelle Adolf, Jeremy J. Bagg, Kenneth G. Baxter, Susan Agrawal, Rajendra Bagg, Patty Bayliss, Bruce A. Aguado, Andrew E. Bagley, Raymond F. Bayoumi, Ahmed Ahl, Florence Bailey, Betty J. Beach, Douglas A. Aker, James D. Bailey, Judith L. Beach, Robert L. Akin, Claudia J. Bailey, Lyndsay Beals, Duane M. Alband, Jeffrey L. Bailey, Richard L. Beals, Shane Alcaraz, Christina M. Bailey, Stephen Beardsley, Peter G. Alderson, Donald P. Bailey, Stephen Beck, Michael J. Aldinger, Suzanne Bailey, Tara L. Beckstrand, Benjamine C. Aldrich, Heather L. Baize, Mary A. Beckstrand, Denise C. Aldrich, Jordan A. Baker, Arlene W. Beilein, Paul T. Aldrich, Kathryn J. Baker, Charles O. Beinhauer, Joseph F. Alexander, Christopher J. Baker, Frederic Belden, Barbara A. Alexander, Tara Baker, Gregory S. Belden, James C. Allen, Patricia A. Baker, Karen Bell, David K. Allison, Eddie R. Baker, Kirk E. Bell, Kathleen D. Almeter, David J Baker, Kristina Bell, Lorraine F. Almeter, George Anna Baker, Nichlos Bell, Milda Almeter, Nathan A. Baker, Peggy J. Bell, Mildred E. Almeter, Steven A. Baker, Roger O. Bellaire, Donald Ames, Gregory K. Baker, Shawn R. Bellaire, Donald W. Sr Ames, Richard A. Bakowski, Christopher Belles, Cody J. Andalora, Ingeburg Ballard, Joanne R. Bellinger, Heather Andalora, Orah Ballerstein, Lisa Bender, Gloria Andrews, Lee H. Ballew, Marjorie Bender, Sidney Antinore, Hope Bannister, Jeffrey H. -
Short Range Transit Plan – 2009 (PDF)
Eastern Sierra Transit Authority Short Range Transit Plan Volume 1 Service and Financial Plan Final Report January 2009 Eastern Sierra Transit Authority Short Range Transit Plan Table of Contents Executive Summary ......................................................................... ES-1 Short Range Transit Plan Objectives ....................................................................... ES-1 Overview of Existing Services.................................................................................... ES-1 Transit Needs .............................................................................................................. ES-1 Transit Dependent Population ...........................................................................ES-1 Tourist and Visitor Market ................................................................................ES-2 Seamless Transit System ...................................................................................ES-3 ESTA Mission, Goals and Performance Standards................................................. ES-3 395 Corridor Services................................................................................................. ES-4 Rural Transit Services................................................................................................ ES-5 Bishop Local Services................................................................................................. ES-6 Mammoth Local Services.......................................................................................... -
A Study About the Temporal Constraints on the Martian Yardangs’ Development in Medusae Fossae Formation
remote sensing Article A Study about the Temporal Constraints on the Martian Yardangs’ Development in Medusae Fossae Formation Jia Liu 1,2 , Zongyu Yue 1,3,*, Kaichang Di 1,3 , Sheng Gou 1,4 and Shengli Niu 4 1 State Key Laboratory of Remote Sensing Science, Aerospace Information Research Institute, Chinese Academy of Sciences, Beijing 100101, China; [email protected] (J.L.); [email protected] (K.D.); [email protected] (S.G.) 2 University of Chinese Academy of Sciences, Beijing 100049, China 3 CAS Center for Excellence in Comparative Planetology, Hefei 230026, China 4 State Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology, Macau 999078, China; [email protected] * Correspondence: [email protected]; Tel.: +86-10-64889553 Abstract: The age of Mars yardangs is significant in studying their development and the evolution of paleoclimate conditions. For planetary surface or landforms, a common method for dating is based on the frequency and size distribution of all the superposed craters after they are formed. However, there is usually a long duration for the yardangs’ formation, and they will alter the superposed craters, making it impossible to give a reliable dating result with the method. An indirect method by analyzing the ages of the superposed layered ejecta was devised in the research. First, the layered ejecta that are superposed on and not altered by the yardangs are identified and mapped. Then, the ages of the layered ejecta are derived according to the crater frequency and size distribution on them. These ages indicate that the yardangs ceased development by these times, and the ages are valuable for studying the evolution of the yardangs. -
First International Conference on Mars Polar Science and Exploration
FIRST INTERNATIONAL CONFERENCE ON MARS POLAR SCIENCE AND EXPLORATION Held at The Episcopal Conference Center at Carnp Allen, Texas Sponsored by Geological Survey of Canada International Glaciological Society Lunar and Planetary Institute National Aeronautics and Space Administration Organizers Stephen Clifford, Lunar and Planetary Institute David Fisher, Geological Survey of Canada James Rice, NASA Ames Research Center LPI Contribution No. 953 Compiled in 1998 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. Abstracts in this volume may be cited as Author A. B. (1998) Title of abstract. In First International Conference on Mars Polar Science and Exploration, p. xx. LPI Contribution No. 953, Lunar and Planetary Institute, Houston. This report is distributed by ORDER DEPARTMENT Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1 113 Mail order requestors will be invoiced for the cost of shipping and handling. LPI Contribution No. 953 iii Preface This volume contains abstracts that have been accepted for presentation at the First International Conference on Mars Polar Science and Exploration, October 18-22? 1998. The Scientific Organizing Committee consisted of Terrestrial Members E. Blake (Icefield Instruments), G. Clow (U.S. Geologi- cal Survey, Denver), D. Dahl-Jensen (University of Copenhagen), K. Kuivinen (University of Nebraska), J. -
Binary Asteroids and the Formation of Doublet Craters
ICARUS 124, 372±391 (1996) ARTICLE NO. 0215 Binary Asteroids and the Formation of Doublet Craters WILLIAM F. BOTTKE,JR. Division of Geological and Planetary Sciences, California Institute of Technology, Mail Code 170-25, Pasadena, California 91125 E-mail: [email protected] AND H. JAY MELOSH Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona 85721 Received April 29, 1996; revised August 14, 1996 found we could duplicate the observed fraction of doublet cra- At least 10% (3 out of 28) of the largest known impact craters ters found on Earth, Venus, and Mars. Our results suggest on Earth and a similar fraction of all impact structures on that any search for asteroid satellites should place emphasis Venus are doublets (i.e., have a companion crater nearby), on km-sized Earth-crossing asteroids with short-rotation formed by the nearly simultaneous impact of objects of compa- periods. 1996 Academic Press, Inc. rable size. Mars also has doublet craters, though the fraction found there is smaller (2%). These craters are too large and too far separated to have been formed by the tidal disruption 1. INTRODUCTION of an asteroid prior to impact, or from asteroid fragments dispersed by aerodynamic forces during entry. We propose that Two commonly held paradigms about asteroids and some fast rotating rubble-pile asteroids (e.g., 4769 Castalia), comets are that (a) they are composed of non-fragmented after experiencing a close approach with a planet, undergo tidal chunks of rock or rock/ice mixtures, and (b) they are soli- breakup and split into multiple co-orbiting fragments. -
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 -
Geologic Studies of Planetary Surfaces Using Radar Polarimetric Imaging 2
Geologic studies of planetary surfaces using radar polarimetric imaging 2 4 Lynn M. Carter NASA Goddard Space Flight Center 8 Donald B. Campbell 9 Cornell University 10 11 Bruce A. Campbell 12 Smithsonian Institution 13 14 14 Abstract: Radar is a useful remote sensing tool for studying planetary geology because it is 15 sensitive to the composition, structure, and roughness of the surface and can penetrate some 16 materials to reveal buried terrain. The Arecibo Observatory radar system transmits a single 17 sense of circular polarization, and both senses of circular polarization are received, which allows 18 for the construction of the Stokes polarization vector. From the Stokes vector, daughter products 19 such as the circular polarization ratio, the degree of linear polarization, and linear polarization 20 angle are obtained. Recent polarimetric imaging using Arecibo has included Venus and the 21 Moon. These observations can be compared to radar data for terrestrial surfaces to better 22 understand surface physical properties and regional geologic evolution. For example, 23 polarimetric radar studies of volcanic settings on Venus, the Moon and Earth display some 24 similarities, but also illustrate a variety of different emplacement and erosion mechanisms. 25 Polarimetric radar data provides important information about surface properties beyond what can 26 be obtained from single-polarization radar. Future observations using polarimetric synthetic 27 aperture radar will provide information on roughness, composition and stratigraphy that will 28 support a broader interpretation of surface evolution. 29 2 29 1.0 Introduction 30 31 Radar polarimetry has the potential to provide more information about surface physical 32 properties than single-polarization backscatter measurements, and has often been used in remote 33 sensing observations of Solar System objects. -
Tectonic Evolution of Northwestern Imbrium of the Moon That Lasted In
Daket et al. Earth, Planets and Space (2016) 68:157 DOI 10.1186/s40623-016-0531-0 FULL PAPER Open Access Tectonic evolution of northwestern Imbrium of the Moon that lasted in the Copernican Period Yuko Daket1* , Atsushi Yamaji1, Katsushi Sato1, Junichi Haruyama2, Tomokatsu Morota3, Makiko Ohtake2 and Tsuneo Matsunaga4 Abstract The formation ages of tectonic structures and their spatial distributions were studied in the northwestern Imbrium and Sinus Iridum regions using images obtained by Terrain Camera and Multiband Imager on board the SELENE spacecraft and the images obtained by Narrow Angle Camera on board LRO. The formation ages of mare ridges are constrained by the depositional ages of mare basalts, which are either deformed or dammed by the ridges. For this purpose, we defined stratigraphic units and determined their depositional ages by crater counting. The degradation levels of craters dislocated by tectonic structures were also used to determine the youngest limits of the ages of the tectonic activities. As a result, it was found that the contractions to form mare ridges lasted long after the deposition of the majority of the mare basalts. There are mare ridges that were tectonically active even in the Copernican Period. Those young structures are inconsistent with the mascon tectonics hypothesis, which attributes tectonic deforma- tions to the subsidence of voluminous basaltic fills. The global cooling or the cooling of the Procellarum KREEP Ter- rane region seems to be responsible for them. In addition, we found a graben that was active after the Eratosthenian Period. It suggests that the global or regional cooling has a stress level low enough to allow the local extensional tectonics.