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(Sptpang Coil.) [I49] I50 Bulletin American Museum of Natural History
Article VIII.-CATALOGUE OF METEORITES IN THE COLLECTION OF THE AMERICAN MUSEUM OF NATURAL HISTORY, TO JULY i, I896. By E. 0. HOVEY. 'T'he Collection of Meteorites in the Arnerican Museum of Natural History consists of fifty-five slabs, fragments and com- plete individuals, representing twenty-six falls and finds. The foundation of the mineralogical department of the Museum was laid in I874 by the purchase of the collection of S. C. H. Bailey, in which there were a few meteorites. More were acquired with the portion of the Norman Spang Collection of Minerals which was purchased in I89I, and other meteorites have been bought by the Museum from time to time, or have been presented to it by friends. The soujrce from which each specimen came has been indicated in the following cataloguLe. This publication is made to assist. the large number of persons who have become interested in knowing the extent to which the material of various falls and finds has been distributed among collections and the present location of specimens. AEROSIDERITES. (IRON METEORI ES.) Cat. Date of NAME AND Weight No. Discovery. DE;SCRIPTION. in grams. 18 1784 Tejupilco, Toluca Valley, Mexico. A complete individual, the surface of which has scaled off somewhat. A polished and etched surface shows coarse Widmanstatten figures. 1153. (Bailey Co/i.) 17841 Xiquipilco, Toluca Valley, Mexico. A complete individual of ellipsoidal form, which had been used as a pounder by the natives. 564. (Sptpang Coil.) [I49] I50 Bulletin American Museum of Natural History. [Vol. VIII, AEROSIDERITES.-Continued. Cat. Date of NAME AND DESCRIPTION. -
Iron Meteorites Are Made of Fe-Ni Metal Phases with Such Minor Minerals As Schrebersite, Troilite, Cohenite and Other Fe-Ni Carbides
Bulk elemental analyses of iron meteorites by using INAA and LA-ICPMS. N. Shirai1, A. Yamaguchi2, M. K. Haba2, T. Ojima2, M. Ebiahra1 and H. Kojima2, 1Tokyo Metropolitan Univer- sity, 2National Institute of Polar Research. Introduction: Iron meteorites are made of Fe-Ni metal phases with such minor minerals as schrebersite, troilite, cohenite and other Fe-Ni carbides. As most iron meteorites are believed to be samples from the metallic core of differentiated planetesimals, petrological, mineralogical and chemi- cal studies of iron meteorites are fundamental for unraveling the process of planetary differentiation. Based on the structures, iron meteorites are originally classified into hexahedrites, octahedrites and ataxites. Hexahedrites and ataxites are nearly made of kamacite and taenite, respectively. Octahedrites consist of kamacite and taenite, and they are further divided into six subgroups on the basis of the width of the kamcite from finest (>0.2 mm) to coarsest (>3.3 mm). Almost all iron meteorites are classified into octahedrites. The chemical clas- sification of iron meteorites is based on their trace element compositions (Ni, Ga, Ge and Ir). Bulk elemental abundances for iron meteorites have been obtained by using neutron activation analysis (NAA). Other analytical methods such as laser ablation inductively coupled plasma mass spectrometry (LA-ICPMS) have not been very often applied to iron meteorites. In this study, we present simple and effective procedures for the chemical classification of iron meteorites by using INAA and LA-ICPMS. Based on the analytical data obtained by two analytical techniques, we discuss the accuracy and the precision of our data and how promisingly our analytical methods can be applied to classifica- tion of iron meteorites.r 9, 2016 (12:00 pm, JST) Experimental: Canyon Diablo (IAB), Toluca (IAB), Cape York (IIIAB), Muonionalusta (IVA) and Dronino (ungrouped) were analyzed by using two analytical methods (INAA and LA-ICPMS). -
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. -
Warfare in a Fragile World: Military Impact on the Human Environment
Recent Slprt•• books World Armaments and Disarmament: SIPRI Yearbook 1979 World Armaments and Disarmament: SIPRI Yearbooks 1968-1979, Cumulative Index Nuclear Energy and Nuclear Weapon Proliferation Other related •• 8lprt books Ecological Consequences of the Second Ihdochina War Weapons of Mass Destruction and the Environment Publish~d on behalf of SIPRI by Taylor & Francis Ltd 10-14 Macklin Street London WC2B 5NF Distributed in the USA by Crane, Russak & Company Inc 3 East 44th Street New York NY 10017 USA and in Scandinavia by Almqvist & WikseH International PO Box 62 S-101 20 Stockholm Sweden For a complete list of SIPRI publications write to SIPRI Sveavagen 166 , S-113 46 Stockholm Sweden Stoekholol International Peace Research Institute Warfare in a Fragile World Military Impact onthe Human Environment Stockholm International Peace Research Institute SIPRI is an independent institute for research into problems of peace and conflict, especially those of disarmament and arms regulation. It was established in 1966 to commemorate Sweden's 150 years of unbroken peace. The Institute is financed by the Swedish Parliament. The staff, the Governing Board and the Scientific Council are international. As a consultative body, the Scientific Council is not responsible for the views expressed in the publications of the Institute. Governing Board Dr Rolf Bjornerstedt, Chairman (Sweden) Professor Robert Neild, Vice-Chairman (United Kingdom) Mr Tim Greve (Norway) Academician Ivan M£ilek (Czechoslovakia) Professor Leo Mates (Yugoslavia) Professor -
The Islamic Traditions of Cirebon
the islamic traditions of cirebon Ibadat and adat among javanese muslims A. G. Muhaimin Department of Anthropology Division of Society and Environment Research School of Pacific and Asian Studies July 1995 Published by ANU E Press The Australian National University Canberra ACT 0200, Australia Email: [email protected] Web: http://epress.anu.edu.au National Library of Australia Cataloguing-in-Publication entry Muhaimin, Abdul Ghoffir. The Islamic traditions of Cirebon : ibadat and adat among Javanese muslims. Bibliography. ISBN 1 920942 30 0 (pbk.) ISBN 1 920942 31 9 (online) 1. Islam - Indonesia - Cirebon - Rituals. 2. Muslims - Indonesia - Cirebon. 3. Rites and ceremonies - Indonesia - Cirebon. I. Title. 297.5095982 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 or otherwise, without the prior permission of the publisher. Cover design by Teresa Prowse Printed by University Printing Services, ANU This edition © 2006 ANU E Press the islamic traditions of cirebon Ibadat and adat among javanese muslims Islam in Southeast Asia Series Theses at The Australian National University are assessed by external examiners and students are expected to take into account the advice of their examiners before they submit to the University Library the final versions of their theses. For this series, this final version of the thesis has been used as the basis for publication, taking into account other changes that the author may have decided to undertake. In some cases, a few minor editorial revisions have made to the work. The acknowledgements in each of these publications provide information on the supervisors of the thesis and those who contributed to its development. -
New Chryse and the Provinces
New Chryse and the Provinces The city of New Chryse is actually several connected cities. The Upper City is located on a break in the crater rim, looking down past a steep rock to the Lower City. Inside the da Vinci crater rim lies the Inner City, also known as the Old City – Red Era tunnels and cave shelters, as well as several nanocomposite towers and cupolas on Mona Lys Ridge looking down on the lower parts of the city. The Lower city lies in a valley sloping down to the Harbour City, which fills a crater 20 kilometres to the East. The Harbour City crater is connected to Camiling Bay and the sea through two canyons and is very well protected from both wind and ice. South of the Lower City and Harbour City lies The Slopes, a straight slope into the sea that is covered with sprawl and slums. Mona Lys Ridge is a mixture of palatial estates surrounded by gardens, imposing official imperial buildings and towering ancient structures used by the highest ranks of the Empire. The central imperial administration and especially the Council is housed in the Deimos Needle, a diamondoid tower that together with its sibling the Phobos Needle dominate the skyline. Escalators allow swift and discreet transport down to the lower levels of the city, and can easily be defended by the police force. North of Mona Lys lies a secluded garden city for higher administrators, guild officials and lesser nobility. The Inner City is to a large extent part of Mona Lys, although most of the inhabitants of Mona Lys do not care much for the dusty old tunnels and hidden vaults – that is left to the Guild of Antiquarians who maintain and protect it. -
Magnetized Impact Craters
Icarus xxx (2011) xxx–xxx Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Predicted and observed magnetic signatures of martian (de)magnetized impact craters ⇑ Benoit Langlais a, , Erwan Thébault b a CNRS UMR 6112, Université de Nantes, Laboratoire de Planétologie et Géodynamique, 2 Rue de la Houssinière, F-44000 Nantes, France b CNRS UMR 7154, Institut de Physique du Globe de Paris, Équipe de Géomagnétisme, 1 Rue Cuvier, F-75005 Paris, France article info abstract Article history: The current morphology of the martian lithospheric magnetic field results from magnetization and Received 3 May 2010 demagnetization processes, both of which shaped the planet. The largest martian impact craters, Hellas, Revised 6 January 2011 Argyre, Isidis and Utopia, are not associated with intense magnetic fields at spacecraft altitude. This is Accepted 6 January 2011 usually interpreted as locally non- or de-magnetized areas, as large impactors may have reset the mag- Available online xxxx netization of the pre-impact material. We study the effects of impacts on the magnetic field. First, a care- ful analysis is performed to compute the impact demagnetization effects. We assume that the pre-impact Keywords: lithosphere acquired its magnetization while cooling in the presence of a global, centered and mainly Mars, Surface dipolar magnetic field, and that the subsequent demagnetization is restricted to the excavation area cre- Mars, Interior Impact processes ated by large craters, between 50- and 500-km diameter. Depth-to-diameter ratio of the transient craters Magnetic fields is set to 0.1, consistent with observed telluric bodies. Associated magnetic field is computed between 100- and 500-km altitude. -
The Mineralogical Magazine Journal
THE MINERALOGICAL MAGAZINE AND JOURNAL OF THE MINERALOGICAL SOCIETY. 1~o. 40. OCTOBER 1889. Vol. VIII. On the Meteorites which have been found iu the Desert of Atacama and its neighbourhood. By L. FLETCHER, M.A., F.R.S., Keeper of Minerals in the British Museum. (With a Map of the District, Plate X.) [Read March 12th and May 7th, ]889.J 1. THE immediate object of the present paper is to place on record J- the history and characters of several Atacama meteorites of which no description has yet been published; but incidentally it is con- venient at the same time to consider the relationship of these masses to others from the same region, which either have been already described, or at least are stated to be preserved in one or more of the known Meteo. rite-Collections. 2. The term " Desert of Atacama " is generally applied to that part of western South America which lies between the towns of Copiapo and Cobija, about 330 miles distant from each other, and which extends island as far as the Indian hamlet of Antofagasta, about 180 miles from 224 L. FLETCHER ON THE METEORITES OF ATACAMA. the coast. The Atacama meteorites preserved in the Collections have been found at several places widely separated throughout the Desert. 3. A critical examination of the descriptive literature, and a compari- son of the manuscript and printed meteorite-lists, which have been placed at my service, lead to the conclusion that all the meteoritic frag- ments from Atacama now preserved in the known Collections belong to one or other of at most thirteen meteorites, which, for reasons given below, are referred to in this paper under the following names :-- 1. -
Hi-Resolution Map Sheet
Controlled Mosaic of Enceladus Hamah Sulci Se 400K 43.5/315 CMN, 2018 GENERAL NOTES 66° 360° West This map sheet is the 5th of a 15-quadrangle series covering the entire surface of Enceladus at a 66° nominal scale of 1: 400 000. This map series is the third version of the Enceladus atlas and 1 270° West supersedes the release from 2010 . The source of map data was the Cassini imaging experiment (Porco et al., 2004)2. Cassini-Huygens is a joint NASA/ESA/ASI mission to explore the Saturnian 350° system. The Cassini spacecraft is the first spacecraft studying the Saturnian system of rings and 280° moons from orbit; it entered Saturnian orbit on July 1st, 2004. The Cassini orbiter has 12 instruments. One of them is the Cassini Imaging Science Subsystem 340° (ISS), consisting of two framing cameras. The narrow angle camera is a reflecting telescope with 290° a focal length of 2000 mm and a field of view of 0.35 degrees. The wide angle camera is a refractor Samad with a focal length of 200 mm and a field of view of 3.5 degrees. Each camera is equipped with a 330° 300° large number of spectral filters which, taken together, span the electromagnetic spectrum from 0.2 60° 320° 310° to 1.1 micrometers. At the heart of each camera is a charged coupled device (CCD) detector 60° consisting of a 1024 square array of pixels, each 12 microns on a side. MAP SHEET DESIGNATION Peri-Banu Se Enceladus (Saturnian satellite) 400K Scale 1 : 400 000 43.5/315 Center point in degrees consisting of latitude/west longitude CMN Controlled Mosaic with Nomenclature Duban 2018 Year of publication IMAGE PROCESSING3 Julnar Ahmad - Radiometric correction of the images - Creation of a dense tie point network 50° - Multiple least-square bundle adjustments 50° - Ortho-image mosaicking Yunan CONTROL For the Cassini mission, spacecraft position and camera pointing data are available in the form of SPICE kernels. -
THE CHANTICLEER Jacksonville State University Jacksonville
Jacksonville State University JSU Digital Commons Chanticleer Historical Newspapers 1985-01-11 Chanticleer | Vol 32, Issue 15 Jacksonville State University Follow this and additional works at: https://digitalcommons.jsu.edu/lib_ac_chanty Recommended Citation Jacksonville State University, "Chanticleer | Vol 32, Issue 15" (1985). Chanticleer. 871. https://digitalcommons.jsu.edu/lib_ac_chanty/871 This Book is brought to you for free and open access by the Historical Newspapers at JSU Digital Commons. It has been accepted for inclusion in Chanticleer by an authorized administrator of JSU Digital Commons. For more information, please contact [email protected]. C Entertainment THE CHANTICLEER Jacksonville State university Jacksonville. Alabama Vol. &No. W January 11, 1985 Mild controversy erupts over - senate resolution By JAN DICKINSON A resolution calling for a faculty-wide vote of "no confidence" in Resident Theron Montgomery was presented to the Faculty Senate at its December 10 meeting, two days before Montgomery anriounced his resignation to the Board of Trustees. Now the sponsor of the resolution, Dr. Gene Blanton, of the English Department, says that he intends to withdraw the resolution at the January 14 meeting of the senate. 13lanton stated in the January 6 edition of the Anniston Star that, because of comments made by several members of the Board of bstees, the wssibility of dropping the resolution was strong. According to that article, trustee Paul Carpenter said, "It (the vote) wouid make absolutely no difference in my opinion. We have studied the entire situation, and we are satisfied with the decision." Another board member, Dwaine Luce, stated, "....the bard is responsible for running the school, and the faculty is responsible for iristructing the students." Echoing the sentiments of Carpenter, he added, "'I'he board has inade its decision and the board, in my pinion, will stand by its decision." According to Dr. -
Possible Origin of Chlorobenzene Detected by SAM Instrument at Gale Crater, Mars: Synergy of Iron Oxides and Perchlorate and Consequences for Organic Matter Analysis
Eighth International Conference on Mars (2014) 1201.pdf Possible origin of chlorobenzene detected by SAM instrument at Gale crater, Mars: synergy of iron oxides and perchlorate and consequences for organic matter analysis. P. Francois1, P. Coll1, C. Szopa2, T. Georgelin3, A. Buch4, C. Freissinet5,6, I. Belmahdi4, A. McAdam5, J. Eigenbrode5, D. Glavin5, S. Kashyap5, A. R. Navarro- Gonzalez7, P. Mahaffy5 and M. Cabane2. [email protected]. 1LISA, Univ. Paris-Est Créteil, Univ. Denis Diderot & CNRS 94010 Créteil, France 2LATMOS, Univ. Pierre et Marie Curie, Univ. Versailles Saint- Quentin & CNRS, 75005 Paris, France 3LRS, Univ. Pierre et Marie Curie, Ivry sur Seine, France 4LGPM, Ecole Centrale de Paris, 92295 Châtenay-Malabry 5NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 6NASA Postdoctoral Program Administered by Oak Ridge Associated Universities, Oak Ridge, Tennessee 37831, USA 7Universidad Nacional Autónoma de México, México, D.F. 04510, Mexico Introduction: The Sample Analysis at Mars rates [5]. Apart from an oxychlorine phase, CB sam- (SAM) instrument on the Curiosity rover is designed to ples also contain iron oxides (e.g. hematite, magnetite) determine the inventory of organic and inorganic vola- [6] which could oxidize organic compounds and cata- tiles thermally evolved from solid samples notably by lyze their decomposition leading to differences in the using a combination of evolved gas analysis (EGA) amount and/or nature of the observed pyrolysis prod- and pyrolysis gas chromatography mass spectrometry ucts [7, 8]. A synergy between oxychlorine phases and (pyr-GC-MS) [1]. Multiple portions from three solid iron oxides in the presence of a carbon source can samples have been analyzed by SAM : a scoop of ba- potentially lead to the formation of CBZ, without any saltic sand at Rocknest (RN) and two drilled samples of specific need for aromatic precursors. -
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