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Large Impact Basins on Mercury: Global Distribution, Characteristics, and Modification History from MESSENGER Orbital Data Caleb I
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 117, E00L08, doi:10.1029/2012JE004154, 2012 Large impact basins on Mercury: Global distribution, characteristics, and modification history from MESSENGER orbital data Caleb I. Fassett,1 James W. Head,2 David M. H. Baker,2 Maria T. Zuber,3 David E. Smith,3,4 Gregory A. Neumann,4 Sean C. Solomon,5,6 Christian Klimczak,5 Robert G. Strom,7 Clark R. Chapman,8 Louise M. Prockter,9 Roger J. Phillips,8 Jürgen Oberst,10 and Frank Preusker10 Received 6 June 2012; revised 31 August 2012; accepted 5 September 2012; published 27 October 2012. [1] The formation of large impact basins (diameter D ≥ 300 km) was an important process in the early geological evolution of Mercury and influenced the planet’s topography, stratigraphy, and crustal structure. We catalog and characterize this basin population on Mercury from global observations by the MESSENGER spacecraft, and we use the new data to evaluate basins suggested on the basis of the Mariner 10 flybys. Forty-six certain or probable impact basins are recognized; a few additional basins that may have been degraded to the point of ambiguity are plausible on the basis of new data but are classified as uncertain. The spatial density of large basins (D ≥ 500 km) on Mercury is lower than that on the Moon. Morphological characteristics of basins on Mercury suggest that on average they are more degraded than lunar basins. These observations are consistent with more efficient modification, degradation, and obliteration of the largest basins on Mercury than on the Moon. This distinction may be a result of differences in the basin formation process (producing fewer rings), relaxation of topography after basin formation (subduing relief), or rates of volcanism (burying basin rings and interiors) during the period of heavy bombardment on Mercury from those on the Moon. -
Polygonal Impact Craters on Mercury G
43rd Lunar and Planetary Science Conference (2012) 1083.pdf POLYGONAL IMPACT CRATERS ON MERCURY G. T. Weihs1, J. J. Leitner1;2 and M. G. Firneis1;2, 1Institute of Astronomy, University of Vienna, Tuerkenschanzstrasse 17, A-1180 Vienna, Austria; 2Research Platform: ExoLife, University of Vienna, Austria; [email protected] Introduction: A polygonal impact crater (PIC) is a Table 1: List of PICs found on Mercury crater, which shape in plan view is more or less angular, and the rims are composed of several straight segments Quadr.Crater Diameter [km]Latitude [◦]Longitude [◦] [1]. Analyzing the images transmitted back to Earth by H01 Nizami 76.88 70.38 167.12 the spacecrafts Mariner 10 and MESSENGER, polyg- H01 Saikaku 64.06 71.89 178 onal impact craters with at least two straight rim seg- H01 Van Dijck 101.23 75.48 166.89 H02 Monteverdi 133.57 64.5 80.88 ments, were detected on Mercury. H02 Rubens 158.79 60.81 78.27 PICs on Mercury: The search for polygonal impact H02 Stravinsky 129.07 51.97 78.91 craters was carried out, using the database in [2]: In a H03 Verdi 144.55 64.25 169.62 H05 Hokusai 114.03 57.76 343.1 first step each of the 15 quadrangle-maps was optically H06 Al-jahiz 82.86 1.42 21.66 scanned for impact craters with at least two straight H06 Chaikovskij 171.02 7.9 50.87 rims. In a second step the data preparation was resulting H06 Hiroshige 138.42 -13.33 26.97 in a set of two images per PIC, one with marked straight H06 Kuiper 62.32 -11.32 31.4 H06 Lermontov 165.82 15.27 48.91 rims and an original one for the purpose of comparison. -
Final Report
Final Report Project No: 282703 Project Acronym: NEOShield Project Full Name: A Global Approach to Near-Earth Object Impact Threat Mitigation Final Report Period covered: from 01/01/2012 to 31/05/2015 Date of preparation: 06/07/2015 Start date of project: 01/01/2012 Date of submission (SESAM): 05/08/2015 Project coordinator name: Project coordinator organisation name: Prof. Alan Harris DEUTSCHES ZENTRUM FUER LUFT - UND RAUMFAHRT EV Version: 2 Final Report PROJECT FINAL REPORT Grant Agreement number: 282703 Project acronym: NEOShield Project title: A Global Approach to Near-Earth Object Impact Threat Mitigation Funding Scheme: FP7-CP-FP Project starting date: 01/01/2012 Project end date: 31/05/2015 Name of the scientific representative of the Prof. Alan Harris DEUTSCHES ZENTRUM project's coordinator and organisation: FUER LUFT - UND RAUMFAHRT EV Tel: +493067055324 Fax: +493067055303 E-mail: [email protected] Project website address: www.neoshield.net Project No.: 282703 Page - 2 of 44 Period number: 3rd Ref: 282703_NEOShield_Final_Report-13_20150805_154413_CET.pdf Final Report Please note that the contents of the Final Report can be found in the attachment. 4.1 Final publishable summary report Executive Summary NEOShield was conceived to address realistic options for preventing the collision of a naturally occurring celestial body (near-Earth object, NEO) with the Earth. Three deflection techniques, which appeared to be the most realistic and feasible at the time of the European Commission’s call in 2010, form the focus of NEOShield efforts: the kinetic impactor, in which a spacecraft transfers momentum to an asteroid by impacting it at a very high velocity; blast deflection, in which an explosive, such as a nuclear device, is detonated near, on, or just beneath the surface of the object; and the gravity tractor, in which a spacecraft hovering under power in close proximity to an asteroid uses the gravitational force between the asteroid and itself to tow the asteroid onto a safe trajectory relative to the Earth. -
IAU Mercurian Nomenclature
Appendix 1 IAU Mercurian Nomenclature 1. IAU Nomenclature Rules Since its inception in Brussels in 1919 [1], the International Astronomical Union (IAU) has gradually developed a planetary nomenclature system that has evolved from a purely classically based system into a quite so- phisticated attempt to broaden the cultural base of the names approved for planetary bodies and surface features. At present, name selection is guided by 11 rules (quoted verbatim below) in addition to conventions decided upon by nomenclature task groups for individual Solar System bodies. The general rules are as follows1: 1. Nomenclature is a tool and the first consideration should be to make it simple, clear, and unambiguous. 2. In general, official names will not be given to features whose longest di- mensions are less than 100 metres, although exceptions may be made for smaller features having exceptional scientific interest. 3. The number of names chosen for each body should be kept to a minimum. Features should be named only when they have special scientific inter- est, and when the naming of such features is useful to the scientific and cartographic communities at large. 4. Duplication of the same surface feature name on two or more bodies, and of the same name for satellites and minor planets, is discouraged. Duplications may be allowed when names are especially appropriate and the chances for confusion are very small. 5. Individual names chosen for each body should be expressed in the language of origin. Transliteration for various alphabets should be given, but there will be no translation from one language to another. -
Open File Report 88-4. Seismic Hazards of Western
WASHINGTON DIVISION OF GEOLOGY AND EARTH RESOURCES Raymond LMrnaais, State o.ologlst SEISMIC HAZARDS OF WESTERN WASHINGTON AND SELECTED ADJACENT AREAS BIBUOGRAPHY AND INDEX 1855-JUNE 1988 compiled by CONNIE J. MANSON WASHINGTON DMSION OF GEOLOGY AND EARTH RESOURCES OPEN FILE REPORT 88-4 September 1988 Prepared for the U. S. Geological Survey's Regional Eartbqtµike Hazards Aesasment of the Puget Sound-Portland Area program This report has not been edited or reviewed for conformity wi1h Division of Geology and Earth Resources standards and nomenclature llr!cBI lloy!e • Commlssioner of Public Lands -iiciiuii~Al1 Slaams • ~ CONTENTS Preface ........................... _. .........•................ v Author bibliography ......•.....•...•...••.• ~·~··············l Subject index ......•. ............................................. 263 ~' Subject index tenns •....•••....•...•.•..•.......•......... 996 ILLUSTRATION Map showing the study area for the bibliography of seismic hazards of western Washington and adjacent areas ...................................................... ,x PREFACE This bibliography and index of materials pertinent to the study of earthquake hazards in western Washington was prepared in support of the U.S. Geological Survey's Regional Earthquake Hazards Assessment of the Puget Sound-Portland Area program. Scope Geograehic:. The prpject's entral ge?graph~c foc~s is the Puget Lowland, primarily Whatcom, Skagit,7 Snohomish, King, K1tsap, Thurston, Pierce, Mason, Clark, Cowlitz, Grays Harbor. and Island Counties, and the metropolitan -
Apply Today for Fall 2019!
Apply Today for Fall 2019! TENNESSEE STATE UNIVERSITY, founded in 1912, is Nashville’s only public university, and is a comprehensive, urban, co-educational, land-grant university. TSU has earned a top 20 ranking for Historically Black Colleges and Universities according to U.S. News and World Report, and is rated as one of the top universities in the country by Washington Monthly. Visit us online at tnstate.edu. TENNESSEE STATE UNIVERSITY offers: 38 bachelor’s degree programs 24 master’s degree programs 7 doctoral degrees in biological sciences, computer information systems engineering, psychology, public administration, curriculum and instruction, educational administration and supervision, and physical therapy THINK SERVE WORK Office of the President March 26, 2019 Dear Honor Students and Faculty: Congratulations to each of you for your outstanding achievements in academic excellence. We salute you in our Honors Convocation today for your hard work, dedication and determination to continue the legacy of excellence at Tennessee State University. We are very proud of the number of Dean’s List students (2,397) and President’s List students (283) who are being recognized today for their outstanding academic achievements. We are also honored to have State Senator Raumesh Akbari as our convocation speaker. This year’s theme is “Saluting Academic Excellence, Service, and Leadership: Mobilizing High Achievers to be Global Citizens, and Change Agents.” As President of Tennessee State University, and like you a former student in our University Honors College, I commend you for maintaining a high grade point average and for serving as role models to your peers. Your leadership is distinctive and your commitment is unparalleled. -
The Tectonics of Mercury
P1: aaa Trim: 174mm × 247mm Top: 0.553in Gutter: 0.747in CUUK632-02 CUUK632-Watters ISBN: 978 0 521 76573 2 June 26, 2009 20:13 2 The tectonics of Mercury T. R. Watters Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington and F. Nimmo Department of Earth and Planetary Sciences, University of California, Santa Cruz Summary Mercury has a remarkable number of landforms that express widespread defor- mation of the planet’s crustal materials. Deformation on Mercury can be broadly described as either distributed or basin-localized. The distributed deformation on Mercury is dominantly compressional. Crustal shortening is reflected by three land- forms, lobate scarps, high-relief ridges, and wrinkle ridges. Lobate scarps are the expression of surface-breaking thrust faults and are widely distributed on Mercury. High-relief ridges are closely related to lobate scarps and appear to be formed by high-angle reverse faults. Wrinkle ridges are landforms that reflect folding and thrust faulting and are found largely in smooth plains material within and exterior to the Caloris basin. The Caloris basin has an array of basin-localized tectonic features. Basin-concentric wrinkle ridges in the interior smooth plains material are very similar to those found in lunar mascon basins. The Caloris basin also has the only clear evidence of broad-scale, extensional deformation. Extension of the interior plains materials is expressed as a complex pattern of basin-radial and basin-concentric graben. The graben crosscut the wrinkle ridges in Caloris, suggesting that they are among the youngest tectonic features on Mercury. -
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Yapici Phd Submission
CROSS-BORDER M&A DEAL INCOMPLETION: INSTITUTIONAL PROCESSES AND OUTCOMES by Nilufer Yapici A Dissertation submitted to the Faculty of the College of Business in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy Florida Atlantic University Boca Raton, FL August 2014 ACKNOWLEDGEMENTS The author wishes to express her sincere thanks and love to her husband, Yapici, Herrmann and Peterson families and her friends for their support and encouragement throughout the writing of this dissertation. The author is grateful to her advisor and committee for providing guidance along the process. The encouragement of entire management faculty in Florida Atlantic University is greatly appreciated. iii ABSTRACT Author: Nilufer Yapici Title: Cross-border M&A Bid Incompletion: Institutional Processes and Outcomes Institution: Florida Atlantic University Dissertation Advisor: Bryant A. Hudson Degree: Doctor of Philosophy Year: 2014 My objective in this dissertation was to understand the processes leading to incompletion of the high profile cross-border deals. A conceptual framework was developed which suggests that announcement of a cross-border merger and acquisition (M&A) deal starts a string of institutional processes that leads to incompletion of the bid. I proposed that less powerful host country actors threatened by the MNC’s bid proposal politicize the transaction turning the deal into a transgression. These actors publicize this transgression, initiating a scandal, to gather support of multiple audiences in their attempts to thwart the threat that the MNC poses. Thanks to their efforts in appealing to audiences and publicization of the deal as a transgression, these actors mobilize audiences who reveal hostile reaction against the MNC and the proposed bid. -
Thedatabook.Pdf
THE DATA BOOK OF ASTRONOMY Also available from Institute of Physics Publishing The Wandering Astronomer Patrick Moore The Photographic Atlas of the Stars H. J. P. Arnold, Paul Doherty and Patrick Moore THE DATA BOOK OF ASTRONOMY P ATRICK M OORE I NSTITUTE O F P HYSICS P UBLISHING B RISTOL A ND P HILADELPHIA c IOP Publishing Ltd 2000 All rights reserved. No part of this publication may be reproduced, stored in a retrieval system or transmitted in any form or by any means, electronic, mechanical, photocopying, recording or otherwise, without the prior permission of the publisher. Multiple copying is permitted in accordance with the terms of licences issued by the Copyright Licensing Agency under the terms of its agreement with the Committee of Vice-Chancellors and Principals. British Library Cataloguing-in-Publication Data A catalogue record for this book is available from the British Library. ISBN 0 7503 0620 3 Library of Congress Cataloging-in-Publication Data are available Publisher: Nicki Dennis Production Editor: Simon Laurenson Production Control: Sarah Plenty Cover Design: Kevin Lowry Marketing Executive: Colin Fenton Published by Institute of Physics Publishing, wholly owned by The Institute of Physics, London Institute of Physics Publishing, Dirac House, Temple Back, Bristol BS1 6BE, UK US Office: Institute of Physics Publishing, The Public Ledger Building, Suite 1035, 150 South Independence Mall West, Philadelphia, PA 19106, USA Printed in the UK by Bookcraft, Midsomer Norton, Somerset CONTENTS FOREWORD vii 1 THE SOLAR SYSTEM 1 -
A Pre-Caloris Synchronous Rotation for Mercury Arxiv:1112.2384V1 [Astro
A pre-Caloris synchronous rotation for Mercury Mark A. Wieczorek,1∗ Alexandre C. M. Correia,2 Mathieu Le Feuvre,3 Jacques Laskar,4 Nicolas Rambaux5 1Institut de Physique du Globe de Paris, Univ Paris Diderot 4 avenue de Neptune, 94100 Saint-Maur des Fosses,´ France 2Departamento de F´ısica da Universidade de Aveiro, Campus Universitario´ de Santiago 3810-193 Aveiro, Portugal 3Laboratoire de Planetologie´ et Geodynamique,´ Universite´ de Nantes, France 2 rue de la Houssiniere,` BP 92208, 44322 Nantes Cedex 3, France 4Astronomie et Systemes` Dynamiques, IMCCE-CNRS UMR8028 Observatoire de Paris, 77 avenue Denfert-Rochereau, 75014 Paris, France 5Universite´ Pierre et Marie Curie–Paris 6; IMCCE-CNRS UMR8028 Observatoire de Paris, 77 avenue Denfert-Rochereau, 75014 Paris, France ∗To whom correspondence should be addressed; E-mail: [email protected]. The planet Mercury is locked in a spin-orbit resonance where it rotates three times about its spin axis for every two orbits about the Sun [1, 2]. The current explanation for this unique state assumes that the initial rotation of this planet was prograde and rapid, and that tidal torques decelerated the planetary spin to this resonance [3–6]. When core- mantle boundary friction is accounted for, capture into the 3/2 resonance occurs with a 26% probability, but the most probable outcome is capture into one of the higher-order arXiv:1112.2384v1 [astro-ph.EP] 11 Dec 2011 resonances [7]. Here we show that if the initial rotation of Mercury were retrograde, this planet would be captured into synchronous rotation with a 68% probability. Strong spa- tial variations of the impact cratering rate would have existed at this time, and these are shown to be consistent with the distribution of pre-Calorian impact basins observed by Mariner 10 and MESSENGER. -
1 2 3 Large Impact Basins on Mercury
1 2 3 4 Large impact basins on Mercury: Global distribution, characteristics, and modification 5 history from MESSENGER orbital data 6 7 8 Caleb I. Fassett1, James W. Head2, David M. H. Baker2, Maria T. Zuber3, David E. Smith3,4, 9 Gregory A. Neumann4, Sean C. Solomon5, Christian Klimczak5, Robert G. Strom6, Clark R. 10 Chapman7, Louise M. Prockter8, Roger J. Phillips7, Jürgen Oberst9, Frank Preusker9 11 12 13 14 1Department of Astronomy, Mount Holyoke College, South Hadley, Massachusetts, USA. 15 2Department of Geological Sciences, Brown University, Providence, Rhode Island, USA. 16 3Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of 17 Technology, Cambridge, Massachusetts, USA. 18 4NASA Goddard Space Flight Center, Greenbelt, Maryland, USA. 19 5Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, D.C., 20 USA. 21 6Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA. 22 7Department of Space Sciences, Southwest Research Institute, Boulder, Colorado, USA. 23 8The Johns Hopkins University Applied Physics Laboratory, Laurel, Maryland, USA. 24 9Institute of Planetary Research, German Aerospace Center, Berlin, Germany. 25 26 27 For submission to JGR Planets Special Section on MESSENGER 28 v.17 29 June 4, 2012 30 31 Abstract 32 33 The formation of large impact basins (diameter D ≥ 300 km) was an important process in the 34 early evolution of Mercury and influenced the planet’s topography, stratigraphy, and crustal 35 structure. We catalog and characterize this basin population on Mercury from global 36 observations by the MESSENGER spacecraft, and we use the new data to evaluate basins 37 suggested on the basis of the Mariner 10 flybys.