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Technology Today Spring 2014
Spring 2014 TECHNOLOGY today® Southwest Research Institute® San Antonio, Texas Spring 2014 • Volume 35, No.2 TECHNOLOGY today COVER Director of Communications Dr. Tim Martin Editor Joe Fohn TECHNOLOGY Assistant Editor today Deborah Deffenbaugh Contributors Deb Schmid Tracey S. Whelan Design Scott Funk Photography Larry Walther Circulation Darlene Herring D019274_4431 Southwest Research Institute San Antonio, Texas About the cover A portable solar cell atop a rotating fixture has a Technology Today (ISSN 1528-431X) is published three times "moth-eye" light-absorbing coating applied inside each year and distributed free of charge. The publication a vacuum deposition chamber. discusses some of the more than 1,000 research and develop- ment projects under way at Southwest Research Institute. The materials in Technology Today may be used for educational and informational purposes by the public and the media. Credit to Southwest Research Institute should be given. This authorization does not extend to property rights such as patents. Commercial and promotional use of the contents in Technology Today without the express written consent of Southwest Research Institute is prohibited. The information published in Technology Today does not necessarily reflect the position or policy of Southwest Research Institute or its clients, and no endorsements should be made or inferred. Address correspondence to the editor, Communications Department, Southwest Research Institute, P.O. Drawer 28510, San Antonio, Texas 78228-0510, or e-mail [email protected]. To be placed on the mailing list or to make address changes, call (210) 522-2257 or fax (210) 522-3547, or visit update.swri.org. © 2014 Southwest Research Institute. -
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 -
Litteratur Och Kritiker Fornvännen 1926, S
Litteratur och kritiker http://kulturarvsdata.se/raa/fornvannen/html/1926_litt Fornvännen 1926, s. Ingår i: samla.raa.se Litteratur och kritiker. L. M. BAÄTH, Hälsingborgs Historia 1. Forntiden och den äldre medeltiden. Hälsingborg 1925, 310 sid. Inom Hälsingborgs stadsfullmäktige väcktes 1911 förslag om utgivandet av en historisk redogörelse över stadens utveckling sedan dess stadsfullmäktige- institutions tillkomst, vilken tanke omsider resulterade i -utgivandet av en minnesskrift 1913. Emellertid hade planer varit å färde att komma med ett bre dare lagt arbete över stadens historia frän äldsta tider. Detta större verk skulle omfatta en allmän del och en speciell med statistik. Första delen av den av arkivarien Bäåth redigerade allmänna avdelningen föreligger nu i en diger och vackert utstyrd volym, som sysslar med stadens historia från urtiden till den nordiska äldre medeltidens slut. UNO SUNDELIUS rikt illustrerade skildring av Hälsingborgstraktens geolo giska historia bygger till stor del pä originalmaterial och blir särskilt beträffande kvartärtiden instruktiv därigenom att de lokala företeelserna ständigt ses i sitt samband med de mera omfattande, som gälla hela Skandinavien och Nordeu ropa. För arkeologer (och även andra icke geologiska fackmän) föreligger här en förträfflig orientering över de viktiga och intressanta istidsfenomenen, och i innehållsrika noter refereras de ledande istidsforskarnas divergerande åsikter om huvudproblemen. En litteraturförteckning jämte 5 kartor komplettera beskriv ningen. Antikvarien B. SCHNITTGERS -
Technology Today Spring 2016
Spring 2016 HIDDEN STRUCTURES REVEALED THE METHANE SwRI WINS CYGNSS DETECTORS R&D 100 CONSTELLATION 10 CHALLENGE 18AWARDS 22TECHNOLOGYCOMPLETE TODAY 13 AVIATION FUEL TESTING To meet the needs of the Department of Defense, the Energy Institute, and the aviation industry, SwRI maintains facilities to qualify fuel filters, develop new test methods, and enhance aviation fuel technology. The coalescer-separator shown removes dirt and water contaminants from fuel in both commercial and military fuel handling systems. SwRI works with industry organizations to develop and improve quality standards. The Institute also helps industry develop advanced sensing technologies and fuel handling equipment. AVIATION FUEL FILTRATION AVIATION FUEL MONITORS AVIATION FUEL COALESCERS AVIATION FUEL ADDITIVES WATER MAPPING TEST JET FUEL ELECTRONIC SENSOR MIL PRF 52308J ELECTRONIC SENSORS aviationturbinefuels.swri.org DM018200_6585 12 SPRING 2016 • VOLUME 37, NO. 1 Executive Director of Communications ON THE COVER Tim Martin, Ph.D. Editor 2 Hidden Structures Revealed Deb Schmid Flight control surfaces include the flaps, tabs, Assistant Editor and spoilers that allow a pilot to adjust and Rob Leibold control an aircraft’s flight attitude. Using the Contributors Institute’s recently aquired powerful CT Barbara Bowen scanner, SwRI engineers imaged the aluminum Robert Crowe honeycomb control surface to visualize its Deborah Deffenbaugh D021911 internal structure. This 3-D visualization shows Maria Stothoff a bonding layer running through the structure. Design 8 New Horizons News Jessica Vidal Photography 10 The Methane Detectors Challenge Larry Walther Ian McKinney 14 Consortia News Circulation Stephanie Paredes 16 Pluto-Jupiter Infographic 18 SwRI Wins R&D 100 Awards Technology Today (ISSN 1528-431X) is published 19 TechBytes three times each year and distributed free of charge. -
Moore Et Al., 1977
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 98, NO. E2, PAGES 3413-3429, FEBRUARY 25, 1993 SOIL TEXTURE AND GRANULOMETRY AT THE SURFACE OF MARS Audouin Dollfus and Marc Deschamps Observatoire de Paris, Meudon, France James R. Zimbelman Center for Earth and Planetary Sciences, National Air and Space Museum Smithsonian Institution, Washington, D. C. The physical behavior of the Martian surface soil has been characterized remotely by both photopolarimetry and radiometry. The degree of linear polarization defines a coefficient b which is related to the top surface soil texture and is calibrated in terms of grain size, or as a fraction of the area exhibiting uncovered clean rocks. This coefficient b was recorded with the instrument VPM (Visual Polarimeter Mars) on board Soviet orbiter MARS 5 in 1974. The radiometric thermal inertia coefficient I is essentially a measurement of the soil compaction, or an effective average particle size in the soil texture, through the few decimeters below the top surface sensed by polarimetry. The instrument IBTM (Infra Bed Thermal Mapper) was used on board the Viking spacecraft between 1976 and 1982. The polarimetric scans raked a strip covering two contrasting regions, the dark-hued Mare Erythraeum and the light-hued Thaumasia. Over these wide areas, several smaller typical terrains were characterized by the three parameters A (albedo), b (related to top surface grain size) and I (underlaying compaction or block size). The large dark region Erythraeum is characterized everywhere by a uniform polarization response, despite the large geomorphological diversity of the surface. The values of A and b indicate a ubiquitous coating or mantling with small dark grains of albedo 12.7%, with a radius of 10 to 20 urn. -
Topographic Map of Mars
U.S. DEPARTMENT OF THE INTERIOR OPEN-FILE REPORT 02-282 U.S. GEOLOGICAL SURVEY Prepared for the NATIONAL AERONAUTICS AND SPACE ADMINISTRATION 180° 0° 55° –55° Russell Stokes 150°E NOACHIS 30°E 210°W 330°W 210°E NOTES ON BASE smooth global color look-up table. Note that the chosen color scheme simply 330°E Darwin 150°W This map is based on data from the Mars Orbiter Laser Altimeter (MOLA) 30°W — 60° represents elevation changes and is not intended to imply anything about –60° Chalcoporous v (Smith and others 2001), an instrument on NASA’s Mars Global Surveyor Milankovic surface characteristics (e.g. past or current presence of water or ice). These two (MGS) spacecraft (Albee and others 2001). The image used for the base of this files were then merged and scaled to 1:25 million for the Mercator portion and Rupes map represents more than 600 million measurements gathered between 1999 1:15,196,708 for the two Polar Stereographic portions, with a resolution of 300 and 2001, adjusted for consistency (Neumann and others 2001 and 2002) and S dots per inch. The projections have a common scale of 1:13,923,113 at ±56° TIA E T converted to planetary radii. These have been converted to elevations above the latitude. N S B LANI O A O areoid as determined from a martian gravity field solution GMM2 (Lemoine Wegener a R M S s T u and others 2001), truncated to degree and order 50, and oriented according to IS s NOMENCLATURE y I E t e M i current standards (see below). -
19680012850.Pdf
Research in Space Science SA0 Special Report No. 268 AN ANALYSIS OF THE MARINER 4 PHOTOGRAPHY OF MARS Clark R. Chapman, James €3. Pollack, and Carl Sagan February 14, 1968 % Smithsonian Institution A s tr o phy s ica1 Ob s e rvat ory Cambridge, Massachusetts 02138 708-1 1 TABLE OF CONTENTS Section Page ABSTRACT...... ........................... vi INTRODUCTION ............................. 1 A NEW REDUCTION OF THE CRATERING STATISTICS. 3 CRATER EROSION AND OBLITERATION . 17 SOURCES OF IMPACT CRATERS. 23 5 MAJOR TOPOGRAPHICAL FEATURES AS POSSIBLE CRATERS.................................. 33 6 EROSION MECHANISMS . 35 7 CRATERS AS SOURCES OF DUS-T . 51 8 CRATERAGES .............................. 53 9 VARIATION OF CRATER DENSITIES WITH POSITION ONMARS.. ................................ 55 10 RECOMMENDATIONS FOR FUTURE WORK. 59 11 ACKNOWLEDGMENTS . 61 REFERENCES ............................... 62 APPENDIXA ............................... ~-1 APPENDIXB ............................... B-1 BIOGRAPHICAL NOTES . LIST OF ILLUSTRATIONS Figure Page 1 Low-quality reproduction of Picture 4 of the Mariner 4 photographic sequence. 5 2 Sketch of the position of cataloged craters (Appendices A and B), Picture 4 of the Mariner 4 photographic sequence. 6 3 Low-quality reproduction of Picture 7 of the Mariner 4 photographic sequence. 7 4 Sketch of the position of cataloged craters (Appendices A and B), Picture 7 of the Mariner 4 photographic sequence. 8 5 Low-quality reproduction of Picture 11 of the Mariner 4 photographic sequence. 9 6 Sketch of the position of cataloged craters (Appendices A and B), Picture 11 of the Mariner 4 photographic sequence. 10 7 Diameter-frequency plot for Pictures 7 through 14, Qualities A and B (left); Pictures 7 to 11, Qualities A and B (center); and Pictures 7 and 11, Qualities A and B (right) . -
Communications in Observations
ISSN 0917-7388 COMMUNICATIONS IN CMO Since 1986 MARS No.375 25 August 2010 OBSERVATIONS No.01 PublishedbytheInternational Society of the Mars Observers Observing Red Surfaces on Mars in Violet Light (from 2005 apparition) By Christophe PELLIER he reason that amateur observers use blue fil‐ no effect on the images. Tters to observe Mars is that, owing to contrast 2. The UV filter effects, the visibility of white clouds is much en‐ (Schuler ‐ shown for in‐ hanced. In short wavelengths, the ochre surface of formation) passes light the planet absorbs light and appears darker, while from before 350 nm to water clouds continue to reflect these wavelengths. around 400 nm (the « U » Some observers have also experimented with violet band). This has often or UV filters, which prove to be even more effective been used to reveal spe‐ in bringing out these contrasts, as they produce a cialdetailssuchasthe further darkening of the martian soils and lead to so‐call ultraviolet mark‐ enhanced white clouds. When this was done during ings in the clouds of the 2005 apparition, much unexpected detail was Venus. revealed. The first ISMO paper reviews the appear‐ 3. The W47 transmission is based on an old ance of anomalous dark markings seen on images gelatin filter from Kodak. Curiously, the official taken with filters such as the Wratten 47 and makes transmission curve does not agree with the ob‐ some attempts to explain the situation. served specifications, as instead of the putative peak near 440 nm in blue light, the actual peak lies in the Filter techniques near‐UV around 390 nm! 1 The W47 has become The transmission curves of different blue filters are popularwithamateursinrecentyearsforimaging presented on Fig. -
Appendix:. Maps of the Terrestrial Planets
APPENDIX Maps of the Terrestrial Planets Mercury SOUTH POLAR REGION SCALE 1 8388000 AT 56' LATITUDE POLAR STEREOGRAPHIC PROJECTION i \ \ \ \ .. \. 200 KILOMETERS 400 600 800 1000 NORTH POLAR REGION Mercury North 0 ZW KILOMETERS 400 600 800 1000 2W0 257. I 550. , 140. / / f30. r20. * / - - I +I". 1 1 / / / I North -GO'7 South SCALE 1 50000MO llmm 50 kml AT 0 LlT4TUDE MERCATOR PROlECTlON CONTOUR PLANET ELEVATION RADIUS l~~lornererrl IU~lometerrl 6063 Earth North Pole 278 South Pole 279 Earth Moon ' 1 "'rnl",,, , 'f 4 .I-.%, + I/>, ,,, /!v~00xu3 \\' 345 ! , , , 15 (15WI 0 NORTH POLAR REGION Moon Mars NORTH POLAR REGION Polar cap 81 11apparld on August 4. 1972 SOUTH POLAR REGION Polar cap as 11 sSWrd on February 28 1972 287 Mars 4u-t-t PLAt$ITIA F South SCALE 1 25.0m.0m A7 0' LATITUDE 1 12.549 CCO IT M' LATITUDE MERCITOR PROJLCTON m lorn ern CONTOUR lNTERYltL I KlLOMETRE 288 REFERENCES CHAPTER 1 Burns, J. A., 1976. Consequences of tidal slowing of Mercury: Icarus, v. 28, pp. 453-458. Beatty, J. K., B. O'Leary, and A. Chaikin, 1981. The New Solar Carr, M. H., L. S. Crumpler, J. A. Cutts, R. Greeley, J. E. System: Sky Publishing Corp., Cambridge, Mass. Guest, and H. Masursky, 1977. Martian impact craters and Shoemaker, E. M., 1962. Interpretation of lunar craters: Physics emplacement of ejecta by surface flow: J. Geophys. Res., v. 82, and Astronomy of the Moon (Kopal, Z., ed.), Academic Press, p. 4055. N.Y., pp. 283-359. Chapman, C. R., 1976. Chronology of terrestrial planet evolu- Shoemaker, E. -
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 -
Topographic Map of Mars Any Use of Trade, Product, Or Firm Names in This Publication Is for Descriptive Purposes Only and Does Not Imply Endorsement by the U.S
U.S. DEPARTMENT OF THE INTERIOR Prepared for the GEOLOGIC INVESTIGATIONS SERIES I–2782 U.S. GEOLOGICAL SURVEY NATIONAL AERONAUTICS AND SPACE ADMINISTRATION SHEET 1 OF 2 180° 0° 55° NOTES ON BASE between maps and quadrangles, and most closely resembles lighting conditions –55° This map is based on data from the Mars Orbiter Laser Altimeter (MOLA; found on imagery. The DEM values were then mapped to a smooth global color RussellRussell StokesStokes look-up table. Note that the chosen color scheme simply represents elevation us 150 Smith and others, 2001), an instrument on NASA’s Mars Global Surveyor NOACHISN O A C H I S o E E orousor 30 ° 210 ° E changes and is not intended to imply anything about surface characteristics (for ° p 330 ° E 210 W (MGS) spacecraft (Albee and others, 2001). The image used for the base of this 330 o ° ° W ° W DarwinDarwin lc ° W 150 example, past or current presence of water or ice). These two files were then 30 ha s map represents more than 600 million measurements gathered between 1999 and ChalcopC pe 60° merged and scaled to 1:25 million for the Mercator portion and 1:15,196,708 for –60° u v 2001, adjusted for consistency (Neumann and others, 2001, 2003) and converted R MilankovicMilankovic to planetary radii. These have been converted to elevations above the areoid as the two Polar Stereographic portions, with a resolution of 300 dots per inch. The determined from a martian gravity field solution GMM-2B (Lemoine and others, projections have a common scale of 1:13,923,113 at ±56° latitude. -
IAU INFORMATION BULLETIN No 83
IAU / INFORMATION BULLETIN No 83 file:///Users/luis/Desktop/IB/IB83.html Home | News | FAQ | Organization | Activities | Contact INFORMATION BULLETIN No. 83 January 1999 Preface 1.Faits Divers 2.Main Deadlines in 1999-2000 3.The XXIVth General Assembly 4.News from Divisions 5.Executive Committee 6.Scientific Meetings in 1999 7.Policy statement on enviromental challenges to Astronomy 8.Policy statement on Near Earth Object research 9.IAU working rules, as revised at the 71st EC meeting 10.The IAU archives 1919-1970 11.Educational Activites 12.Relations to other organizations 13.Membership 14.Publications 15.Other meetings on astronomical topics 16.Announcements PREFACE The activities of the IAU form a sort of tidal-wave pattern, with highs at the General Assemblies and lows midway between. Thus, this Information Bulletin appears at what should be "low ebb". In fact, there has been no noticeable decrease in the workload of the Secretariat, but the direction of the flow is changing perceptibly: With the Highlights and Transactions volumes from the last GA off to print, and a first Web page and meeting proposal forms for the next GA now in place, the outgoing tide from Kyoto is over and the incoming tide for Manchester picking up. With a Secretariat staff of only two, those individuals are crucial for the work of the Union in general and the General Secretary in particular. We are fortunate that, with almost no gap since the departure of Julie Saucedo on June 30, we have been able to recruit a very capable successor, Jodi Greenberg. Jodi is from the USA, but has lived for long periods in South America, mostly Ecuador and Colombia, as well as in Ukraine, Hungary, and France before settling in Paris.