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Curiosity's Candidate Field Site in Gale Crater, Mars
Curiosity’s Candidate Field Site in Gale Crater, Mars K. S. Edgett – 27 September 2010 Simulated view from Curiosity rover in landing ellipse looking toward the field area in Gale; made using MRO CTX stereopair images; no vertical exaggeration. The mound is ~15 km away 4th MSL Landing Site Workshop, 27–29 September 2010 in this view. Note that one would see Gale’s SW wall in the distant background if this were Edgett, 1 actually taken by the Mastcams on Mars. Gale Presents Perhaps the Thickest and Most Diverse Exposed Stratigraphic Section on Mars • Gale’s Mound appears to present the thickest and most diverse exposed stratigraphic section on Mars that we can hope access in this decade. • Mound has ~5 km of stratified rock. (That’s 3 miles!) • There is no evidence that volcanism ever occurred in Gale. • Mound materials were deposited as sediment. • Diverse materials are present. • Diverse events are recorded. – Episodes of sedimentation and lithification and diagenesis. – Episodes of erosion, transport, and re-deposition of mound materials. 4th MSL Landing Site Workshop, 27–29 September 2010 Edgett, 2 Gale is at ~5°S on the “north-south dichotomy boundary” in the Aeolis and Nepenthes Mensae Region base map made by MSSS for National Geographic (February 2001); from MOC wide angle images and MOLA topography 4th MSL Landing Site Workshop, 27–29 September 2010 Edgett, 3 Proposed MSL Field Site In Gale Crater Landing ellipse - very low elevation (–4.5 km) - shown here as 25 x 20 km - alluvium from crater walls - drive to mound Anderson & Bell -
The Evolution of a Heterogeneous Martian Mantle: Clues from K, P, Ti, Cr, and Ni Variations in Gusev Basalts and Shergottite Meteorites
Earth and Planetary Science Letters 296 (2010) 67–77 Contents lists available at ScienceDirect Earth and Planetary Science Letters journal homepage: www.elsevier.com/locate/epsl The evolution of a heterogeneous Martian mantle: Clues from K, P, Ti, Cr, and Ni variations in Gusev basalts and shergottite meteorites Mariek E. Schmidt a,⁎, Timothy J. McCoy b a Dept. of Earth Sciences, Brock University, St. Catharines, ON, Canada L2S 3A1 b Dept. of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, DC 20560-0119, USA article info abstract Article history: Martian basalts represent samples of the interior of the planet, and their composition reflects their source at Received 10 December 2009 the time of extraction as well as later igneous processes that affected them. To better understand the Received in revised form 16 April 2010 composition and evolution of Mars, we compare whole rock compositions of basaltic shergottitic meteorites Accepted 21 April 2010 and basaltic lavas examined by the Spirit Mars Exploration Rover in Gusev Crater. Concentrations range from Available online 2 June 2010 K-poor (as low as 0.02 wt.% K2O) in the shergottites to K-rich (up to 1.2 wt.% K2O) in basalts from the Editor: R.W. Carlson Columbia Hills (CH) of Gusev Crater; the Adirondack basalts from the Gusev Plains have more intermediate concentrations of K2O (0.16 wt.% to below detection limit). The compositional dataset for the Gusev basalts is Keywords: more limited than for the shergottites, but it includes the minor elements K, P, Ti, Cr, and Ni, whose behavior Mars igneous processes during mantle melting varies from very incompatible (prefers melt) to very compatible (remains in the shergottites residuum). -
Preliminary Mission Analysis and Orbit Design for Next Mars Exploration
Trans. JSASS Aerospace Tech. Japan Vol. 8, No. ists27, pp. Tk_7-Tk_12, 2010 Topics Preliminary Mission Analysis and Orbit Design for Next Mars Exploration By Naoko OGAWA 1), Mutsuko Y. MORIMOTO1), Yuichi TSUDA1,2), Tetsuya YAMADA1,2), Kazuhisa FUJITA1,3), Tomohiro YAMAGUCHI4), Yasuhiro KAWAKATSU1,2), Takashi KUBOTA1,2) and Jun’ichiro KAWAGUCHI1,2) 1)JAXA Space Exploration Center, Japan Aerospace Exploration Agency, Sagamihara, Japan 2)Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan 3)Aerospace Research and Development Directorate, Japan Aerospace Exploration Agency, Tokyo, Japan 4)The Graduate University for Advanced Studies, Sagamihara, Japan (Received July 21st, 2009) Japan has launched many interplanetary spacecraft for exploration of solar system bodies including Mars. Now we are planning the next Mars mission in the late 2010’s. This paper describes the preliminary mission analysis and orbit design for this plan. The combined exploration by several spacecraft requires complicated and careful consideration, different from those for single-probe missions. Mission plans to realize required configuration by a single launch and simple simulation results are reported. Key Words: Mars, Mission Analysis, Orbit Design, MELOS 1. Introduction 2.1.1. Meteorological orbiter for martian climate One orbiter of the two, called hereafter as the meteorological In 2008, Japan Aerospace Exploration Agency (JAXA) orbiter, aims understanding of the interaction between the has established a novel working group toward a novel Mars atmosphere and subsurface ice, and atmospheric dynamics. exploration program named MELOS, an acronym for “Mars Global, high-resolution and continuous mapping of water vapor, Exploration with Lander-Orbiter Synergy”1). As its name clouds, dusts and atmospheric temperature will be performed indicates, this is an ambitious mission composed of several with imaging cameras from the apoapsis of its highly elliptic landers and orbiters, schematically illustrated in Fig. -
The Meridiani Face on Mars
The Meridiani Face on Mars Greg Orme* School of Arts and Science, University of Queensland, Brisbane, Australia *Corresponding author: Greg Orme, School of Arts and Science, Undergraduate Science Student, University of Queensland, Brisbane, Australia, Tel: 07-33656195; E-mail: [email protected] Received: September 11, 2016; Accepted: November 25, 2016; Published: December 25, 2016 Abstract The Meridian Face has some similar features to the Cydonia and Crowned Faces such as having a crown. It is similar to the Nefertiti formation in that it seems to be made of dark soil, dunes in this case. Some dark dune fields can migrate large distances in Meridiani Planum, others remain confined in larger craters perhaps by shielding them from the wind. This can allow for the formation to be very old and remain intact. The similarity between the Crowned Face in the King’s Valley Libya Montes and the Meridiani Face was originally shown with an overall. The implicit hypothesis was that a new overlay would match the two faces even more closely, this has been borne out with the Crowned Face HiRise image and the Meridiani Face CTX image. Keywords: Meridiani planum; Barchan dune; Aeolian process; pareidolia; Dune migration Introduction The Meridiani Face was discovered around early June 2007 by a Mars researcher Terry James, (FIG. 1). The null hypothesis is that this is a random dune formation, an example of people’s innate ability to see faces [1]. It is proposed that this is falsified by the shape of these dunes, to be artificial they would have had to be moved to their current positions. -
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, -
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. -
Mineralogy of the Inverted Channel on the Floor of Miyamoto Crater, Mars
40th Lunar and Planetary Science Conference (2009) 1236.pdf MINERALOGY OF THE INVERTED CHANNEL ON THE FLOOR OF MIYAMOTO CRATER, MARS. G. A. Marzo1, T. L. Roush1, N. L. Lanza2, P. C. McGuire3, H. E. Newsom2, A. M. Olilla2, S. M. Wiseman4, 1NASA Ames Research Center, Space Science and Astrobiology Division (MS245-3, Moffett Field, CA 94035, giuseppe.a.- [email protected]), 2Institute of Meteoritics, University of New Mexico, 3Institute for Geosciences, Department of Planetary Science and Remote Sensing, Freie Universitaet, Berlin, Germany, 4Department of Earth and Planetary Sciences, Washington University. Introduction: Miyamoto crater is a 160-km-dia- verted channel and offers a unique opportunity to fur- meter impact crater of Noachian age located southwest ther investigate the mineralogical characteristics of this of Meridiani Planum whose north and north-eastern features and its surroundings. half is buried beneath light-toned layered rock, over- lain by a thin regolith of sand, granules, and hematitic spherules [1]. The regional geologic history of the Me- ridiani Planum region has been extensively studied [2- 6] and is interpreted to have begun with formation of the ancient cratered crust and a subsequent major fluvi- al episode carved an extensive valley network, origin- ating from an area located south of the Schiaparelli im- pact basin [5]. The north-eastern portion of the crater is buried by a plain forming unit composed of layered sedimentary rock covered with a thin sand sheet. The extent of the plains unit corresponds with occurrences of crystalline gray hematite [7] which hosts the landing site of the MER Opportunity rover [8]. -
Radar Sounder Evidence of Thick, Porous Sediments in Meridiani
PUBLICATIONS Geophysical Research Letters RESEARCH LETTER Radar sounder evidence of thick, porous sediments 10.1002/2017GL074431 in Meridiani Planum and implications Key Points: for ice-filled deposits on Mars • The MARSIS radar sounder has detected subsurface echoes deep Thomas R. Watters1 , Carl J. Leuschen2, Bruce A. Campbell1 , Gareth A. Morgan1 , within the Meridiani Planum deposits 3 1 4 5 • The time delay between surface and Andrea Cicchetti , John A. Grant , Roger J. Phillips , and Jeffrey J. Plaut subsurface echoes is consistent with 1 2 deposits having a low bulk value of Center for Earth and Planetary Studies, Smithsonian Institution, Washington, District of Columbia, USA, Center for Remote the real dielectric constant Sensing of Ice Sheets, University of Kansas, Lawrence, Kansas, USA, 3Infocom Department, La Sapienza University of Rome, • New compaction relationships for Rome, Italy, 4Department of Earth and Planetary Sciences and McDonnell Center for the Space Sciences, Washington Mars indicate that a low dielectric University, St. Louis, Missouri, USA, 5Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA constant can be accounted for without invoking pore-filling water ice Abstract Meridiani Planum is one of the most intensely studied regions on Mars, yet little is known about Supporting Information: the physical properties of the deposits below those examined by the Opportunity rover. We report the • Supporting Information S1 detection of subsurface echoes within the Meridiani Planum deposits from data obtained by the Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) instrument. The delay time between the Correspondence to: T. R. Watters, surface and subsurface returns is indicative of materials with a real dielectric constant of 3.6 ± 0.6. -
Landing Site Selection and Miyamoto Crater, Mars – Why No Hydrothermal Deposits? H
LANDING SITE SELECTION AND MIYAMOTO CRATER, MARS – WHY NO HYDROTHERMAL DEPOSITS? H. E. Newsom1, N. L. Lanza1, A. M. Ollila1, S. M. Wiseman2, T. L. Roush3, G. A. Marzo3, L. L. Tor- nabene4, L. S. Crumpler5, C. H. Okubo6, M. M. Osterloo7, V. E. Hamilton8, and S. P. Schwenzer. 1Univ. of New Mexico, Inst. of Meteoritics, MSC03-2050, Albuquerque, NM 87131, USA, ([email protected]), 2Dept. of Earth & Planet. Sci., Washington Univ., St. Louis, MO, USA, 3NASA Ames Research Center, Moffett Field, CA, USA, 4Lunar & Planetary Laboratory, Univ. of Arizona, Tucson, AZ, USA, 5New Mexico Museum of Natural History & Science, Albuquerque, NM, USA 6U.S. Geological Survey, Flagstaff, AZ, USA, 7Hawai'i Institute of Geophysics & Planetology, Univ.of Hawai'i at Manoa, Honolulu, HI, USA, 8Southwest Research Inst., Boulder, CO, USA, 9Lunar and Planetary Institute, USRA, 3600 Bay Area Blvd., Houston TX 77058, USA;. unnamed crater in Nili Fosse, and Miyamoto crater [1]. Miyamoto crater is a 160-km-diameter impact crater of Noachian age (Fig. 1). The floor of the Miyamoto cra- ter, southwest of Meridiani Planum is a potential site for studying aqueous processes on Mars. The crater floor contains raised curvilinear features that are sug- gestive of past fluvial activity. Unfortunately, the po- tential for identifying and studying hydrothermal depo- sits in this location has been handicapped by the lack of high resolution CRISM data from the crater rim, due to the focus of providing data only on potential landing site ellipses. A search for evidence of hydrothermal activity in crater rims and central uplifts could provide important alternative targets for future rovers and sam- ple return missions. -
Geophysical and Remote Sensing Study of Terrestrial Planets
GEOPHYSICAL AND REMOTE SENSING STUDY OF TERRESTRIAL PLANETS A Dissertation Presented to The Academic Faculty By Lujendra Ojha In Partial Fulfillment Of the Requirements for the Degree Doctor of Philosophy in Earth and Atmospheric Sciences Georgia Institute of Technology August, 2016 COPYRIGHT © 2016 BY LUJENDRA OJHA GEOPHYSICAL AND REMOTE SENSING STUDY OF TERRESTRIAL PLANETS Approved by: Dr. James Wray, Advisor Dr. Ken Ferrier School of Earth and Atmospheric School of Earth and Atmospheric Sciences Sciences Georgia Institute of Technology Georgia Institute of Technology Dr. Joseph Dufek Dr. Suzanne Smrekar School of Earth and Atmospheric Jet Propulsion laboratory Sciences California Institute of Technology Georgia Institute of Technology Dr. Britney Schmidt School of Earth and Atmospheric Sciences Georgia Institute of Technology Date Approved: June 27th, 2016. To Rama, Tank, Jaika, Manjesh, Reeyan, and Kali. ACKNOWLEDGEMENTS Thanks Mom, Dad and Jaika for putting up with me and always being there. Thank you Kali for being such an awesome girl and being there when I needed you. Kali, you are the most beautiful girl in the world. Never forget that! Thanks Midtown Tavern for the hangovers. Thanks Waffle House for curing my hangovers. Thanks Sarah Sutton for guiding me into planetary science. Thanks Alfred McEwen for the continued support and mentoring since 2008. Thanks Sue Smrekar for taking me under your wings and teaching me about planetary geodynamics. Thanks Dan Nunes for guiding me in the gravity world. Thanks Ken Ferrier for helping me study my favorite planet. Thanks Scott Murchie for helping me become a better scientist. Thanks Marion Masse for being such a good friend and a mentor. -
Regimes of Truth in the X-Files
Edith Cowan University Research Online Theses: Doctorates and Masters Theses 1-1-1999 Aliens, bodies and conspiracies: Regimes of truth in The X-files Leanne McRae Edith Cowan University Follow this and additional works at: https://ro.ecu.edu.au/theses Part of the Film and Media Studies Commons Recommended Citation McRae, L. (1999). Aliens, bodies and conspiracies: Regimes of truth in The X-files. https://ro.ecu.edu.au/ theses/1247 This Thesis is posted at Research Online. https://ro.ecu.edu.au/theses/1247 Edith Cowan University Research Online Theses: Doctorates and Masters Theses 1999 Aliens, bodies and conspiracies : regimes of truth in The -fiX les Leanne McRae Edith Cowan University Recommended Citation McRae, L. (1999). Aliens, bodies and conspiracies : regimes of truth in The X-files. Retrieved from http://ro.ecu.edu.au/theses/1247 This Thesis is posted at Research Online. http://ro.ecu.edu.au/theses/1247 Edith Cowan University Copyright Warning You may print or download ONE copy of this document for the purpose of your own research or study. The University does not authorize you to copy, communicate or otherwise make available electronically to any other person any copyright material contained on this site. You are reminded of the following: Copyright owners are entitled to take legal action against persons who infringe their copyright. A reproduction of material that is protected by copyright may be a copyright infringement. Where the reproduction of such material is done without attribution of authorship, with false attribution of authorship or the authorship is treated in a derogatory manner, this may be a breach of the author’s moral rights contained in Part IX of the Copyright Act 1968 (Cth). -
Free Pascal and Lazarus Programming Textbook
This page deliberately left blank. In the series: ALT Linux library Free Pascal and Lazarus Programming Textbook E. R. Alekseev O. V. Chesnokova T. V. Kucher Moscow ALT Linux; DMK-Press Publishers 2010 i UDC 004.432 BBK 22.1 A47 Alekseev E.R., Chesnokova O.V., Kucher T.V. A47 Free Pascal and Lazarus: A Programming Textbook / E. R. Alekseev, O. V. Chesnokova, T. V. Kucher M.: ALTLinux; Publishing house DMK-Press, 2010. 440 p.: illustrated.(ALT Linux library). ISBN 978-5-94074-611-9 Free Pascal is a free implementation of the Pascal programming language that is compatible with Borland Pascal and Object Pascal / Delphi, but with additional features. The Free Pascal compiler is a free cross-platform product implemented on Linux and Windows, and other operating systems. This book is a textbook on algorithms and programming, using Free Pascal. The reader will also be introduced to the principles of creating graphical user interface applications with Lazarus. Each topic is accompanied by 25 exercise problems, which will make this textbook useful not only for those studying programming independently, but also for teachers in the education system. The book’s website is: http://books.altlinux.ru/freepascal/ This textbook is intended for teachers and students of junior colleges and universities, and the wider audience of readers who may be interested in programming. UDC 004.432 BBK 22.1 This book is available from: The <<Alt Linux>> company: (495) 662-3883. E-mail: [email protected] Internet store: http://shop.altlinux.ru From the publishers <<Alians-kniga>>: Wholesale purchases: (495) 258-91-94, 258-91-95.