Annual Reports, Town of Acton, Massachusetts
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General Index
General Index Italicized page numbers indicate figures and tables. Color plates are in- cussed; full listings of authors’ works as cited in this volume may be dicated as “pl.” Color plates 1– 40 are in part 1 and plates 41–80 are found in the bibliographical index. in part 2. Authors are listed only when their ideas or works are dis- Aa, Pieter van der (1659–1733), 1338 of military cartography, 971 934 –39; Genoa, 864 –65; Low Coun- Aa River, pl.61, 1523 of nautical charts, 1069, 1424 tries, 1257 Aachen, 1241 printing’s impact on, 607–8 of Dutch hamlets, 1264 Abate, Agostino, 857–58, 864 –65 role of sources in, 66 –67 ecclesiastical subdivisions in, 1090, 1091 Abbeys. See also Cartularies; Monasteries of Russian maps, 1873 of forests, 50 maps: property, 50–51; water system, 43 standards of, 7 German maps in context of, 1224, 1225 plans: juridical uses of, pl.61, 1523–24, studies of, 505–8, 1258 n.53 map consciousness in, 636, 661–62 1525; Wildmore Fen (in psalter), 43– 44 of surveys, 505–8, 708, 1435–36 maps in: cadastral (See Cadastral maps); Abbreviations, 1897, 1899 of town models, 489 central Italy, 909–15; characteristics of, Abreu, Lisuarte de, 1019 Acequia Imperial de Aragón, 507 874 –75, 880 –82; coloring of, 1499, Abruzzi River, 547, 570 Acerra, 951 1588; East-Central Europe, 1806, 1808; Absolutism, 831, 833, 835–36 Ackerman, James S., 427 n.2 England, 50 –51, 1595, 1599, 1603, See also Sovereigns and monarchs Aconcio, Jacopo (d. 1566), 1611 1615, 1629, 1720; France, 1497–1500, Abstraction Acosta, José de (1539–1600), 1235 1501; humanism linked to, 909–10; in- in bird’s-eye views, 688 Acquaviva, Andrea Matteo (d. -
DMAAC – February 1973
LUNAR TOPOGRAPHIC ORTHOPHOTOMAP (LTO) AND LUNAR ORTHOPHOTMAP (LO) SERIES (Published by DMATC) Lunar Topographic Orthophotmaps and Lunar Orthophotomaps Scale: 1:250,000 Projection: Transverse Mercator Sheet Size: 25.5”x 26.5” The Lunar Topographic Orthophotmaps and Lunar Orthophotomaps Series are the first comprehensive and continuous mapping to be accomplished from Apollo Mission 15-17 mapping photographs. This series is also the first major effort to apply recent advances in orthophotography to lunar mapping. Presently developed maps of this series were designed to support initial lunar scientific investigations primarily employing results of Apollo Mission 15-17 data. Individual maps of this series cover 4 degrees of lunar latitude and 5 degrees of lunar longitude consisting of 1/16 of the area of a 1:1,000,000 scale Lunar Astronautical Chart (LAC) (Section 4.2.1). Their apha-numeric identification (example – LTO38B1) consists of the designator LTO for topographic orthophoto editions or LO for orthophoto editions followed by the LAC number in which they fall, followed by an A, B, C or D designator defining the pertinent LAC quadrant and a 1, 2, 3, or 4 designator defining the specific sub-quadrant actually covered. The following designation (250) identifies the sheets as being at 1:250,000 scale. The LTO editions display 100-meter contours, 50-meter supplemental contours and spot elevations in a red overprint to the base, which is lithographed in black and white. LO editions are identical except that all relief information is omitted and selenographic graticule is restricted to border ticks, presenting an umencumbered view of lunar features imaged by the photographic base. -
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 -
User Guide to 1:250,000 Scale Lunar Maps
CORE https://ntrs.nasa.gov/search.jsp?R=19750010068Metadata, citation 2020-03-22T22:26:24+00:00Z and similar papers at core.ac.uk Provided by NASA Technical Reports Server USER GUIDE TO 1:250,000 SCALE LUNAR MAPS (NASA-CF-136753) USE? GJIDE TO l:i>,, :LC h75- lu1+3 SCALE LUNAR YAPS (Lumoalcs Feseclrch Ltu., Ottewa (Ontario) .) 24 p KC 53.25 CSCL ,33 'JIACA~S G3/31 11111 DANNY C, KINSLER Lunar Science Instltute 3303 NASA Road $1 Houston, TX 77058 Telephone: 7131488-5200 Cable Address: LUtiSI USER GUIDE TO 1: 250,000 SCALE LUNAR MAPS GENERAL In 1972 the NASA Lunar Programs Office initiated the Apollo Photographic Data Analysis Program. The principal point of this program was a detailed scientific analysis of the orbital and surface experiments data derived from Apollo missions 15, 16, and 17. One of the requirements of this program was the production of detailed photo base maps at a useable scale. NASA in conjunction with the Defense Mapping Agency (DMA) commenced a mapping program in early 1973 that would lead to the production of the necessary maps based on the need for certain areas. This paper is designed to present in outline form the neces- sary background informatiox or users to become familiar with the program. MAP FORMAT * The scale chosen for the project was 1:250,000 . The re- search being done required a scale that Principal Investigators (PI'S) using orbital photography could use, but would also serve PI'S doing surface photographic investigations. Each map sheet covers an area four degrees north/south by five degrees east/west. -
Odd Year Nur-Rn-Lic-30550 G
LicenseNumber FirstName MiddleName LastName RenewalGroup NUR-LPN-LIC-6174 DOLORES ROSE AABERG 2019 - ODD YEAR NUR-RN-LIC-30550 GRETCHEN ELLEN AAGAARD-SHIVELY 2019 - ODD YEAR NUR-RN-LIC-128118 CAMBRIA LAUREN AANERUD 2019 - ODD YEAR NUR-RN-LIC-25862 SOPHIA SABINA AANSTAD 2018 - EVEN YEAR NUR-APRN-LIC-124944 ERIN EDWARD AAS 2018 - EVEN YEAR NUR-RN-LIC-105371 ERIN EDWARD AAS 2018 - EVEN YEAR NUR-RN-LIC-34536 BRYON AAS 2019 - ODD YEAR NUR-RN-LIC-39208 JULIA LYNN AASEN 2018 - EVEN YEAR NUR-APRN-LIC-130522 LORI ANN AASEN 2019 - ODD YEAR NUR-RN-LIC-130520 LORI ANN AASEN 2019 - ODD YEAR NUR-RN-LIC-21015 DEBBIE ABAR 2018 - EVEN YEAR NUR-APRN-LIC-130757 LUKE G ABAR 2018 - EVEN YEAR NUR-RN-LIC-130756 LUKE GORDON ABAR 2019 - ODD YEAR NUR-RN-LIC-31911 AIMEE KRISTINE ABBOTT 2018 - EVEN YEAR NUR-RN-LIC-29448 DENISE M ABBOTT 2018 - EVEN YEAR NUR-RN-LIC-131150 SARAH FRANCES ABBOTT 2018 - EVEN YEAR NUR-LPN-LIC-31701 ANGIE ABBOTT 2019 - ODD YEAR NUR-LPN-LIC-33325 HEIDI ABBOTT 2019 - ODD YEAR NUR-LPN-LIC-4920 LORI ANN ABBOTT 2019 - ODD YEAR NUR-LPN-LIC-97426 DAYMON ABBOTT Expired - 2018 - EVEN YEAR NUR-RN-LIC-13260 ROBERT C ABBOTT Expired - 2018 - EVEN YEAR NUR-RN-LIC-17858 MONICA MAY ABDALLAH 2018 - EVEN YEAR NUR-RN-LIC-48890 STEVEN P ABDALLAH 2019 - ODD YEAR NUR-APRN-LIC-101391 LANEICE LORRAINE ABDEL-SHAKUR Expired - 2018 - EVEN YEAR NUR-RN-LIC-101333 LANEICE LORRAINE ABDEL-SHAKUR Expired - 2018 - EVEN YEAR NUR-RN-LIC-96606 RENDI L ABEL 2018 - EVEN YEAR NUR-RN-LIC-97338 LAURA ANN ABEL 2019 - ODD YEAR NUR-RN-LIC-69876 LACEY ANN ABELL 2019 - ODD YEAR NUR-RN-LIC-131932 -
Testing Impact Numerical Model Setups for Simple Craters
EPSC Abstracts Vol. 12, EPSC2018-889, 2018 European Planetary Science Congress 2018 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2018 Testing impact numerical model setups for simple craters Prieur Nils (1), Tobias Rolf (1) and Stephanie Werner (1) (1) University of Oslo, Dept. of Geosciences, Centre for Earth Evolution and Dynamics CEED, Norway, ([email protected]) Abstract dilatancy) to describe the material model, allowing us to test easily different model setups. The impact To investigate the challenges in testing impact velocity is here held constant to a value of U = 12.7 numerical model setups we selected three of the most km/s, which is a rather reasonable average impact velocity for the Moon (including the vertical common setups used in the impact cratering o community. For each of these setups, we carried out component of a 45 impact angle). simulations where the projectile diameters are varied. We focus only on simple craters on the lunar surface The three setups investigated are relatively different, (i.e., craters with diameters smaller than 14-31 km the first one (#1) describes best granular or [1]). Preliminary results are presented and discussed brecciated target [6], while the second [7] (#2) and in the second part of this abstract. third (#3) describes best the behavior of rocks [8]. Model parameters which might affect the most the final crater geometry and morphology are listed 1. Introduction below. In addition, we list two other important A crucial step in impact numerical modeling is to factors: the crater diameter interval over which the directly compare results with observations in order to setups have been used, and the datasets against which test and quantify how well a model reproduces the the setup have been tested. -
Methane Release on Early Mars by Atmospheric Collapse and Atmospheric Reinflation
Methane release on Early Mars by atmospheric collapse and atmospheric reinflation Edwin S. Kite1, Michael A. Mischna2, Peter Gao3,4, Yuk L. Yung2,5, Martin Turbet6,7,* 1. University of Chicago ([email protected]), Chicago, IL 60637. 2. Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109. 3. NASA Ames Research Center, Mountain View, CA 94035. 4. University of California, Berkeley, CA 94720. 5. California Institute of Technology, Pasadena, CA 91125. 6. Laboratoire de Météorologie Dynamique, IPSL, Sorbonne Universités, UPMC Univ Paris 06, CNRS, Paris 75005, France. 7. Observatoire Astronomique de l’Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland. * Currently Marie Sklodowska-Curie Fellow, Geneva Astronomical Observatory. Abstract. A candidate explanation for Early Mars rivers is atmospheric warming due to surface release of H2 or CH4 gas. However, it remains unknown how much gas could be released in a single event. We model the CH4 release by one mechanism for rapid release of CH4 from clathrate. By modeling how CH4-clathrate release is affected by changes in Mars’ obliquity and atmospheric composition, we find that a large fraction of total outgassing from CH4 clathrate occurs following Mars’ first prolonged atmospheric collapse. This atmosphere-collapse-initiated CH4-release mechanism has three stages. (1) Rapid collapse of Early Mars’ carbon dioxide atmosphere initiates a slower shift of water ice from high ground to the poles. (2) Upon subsequent CO2-atmosphere re-inflation and CO2-greenhouse warming, low-latitude clathrate decomposes and releases methane gas. (3) Methane can then perturb atmospheric chemistry and surface temperature, until photochemical processes destroy the methane. -
Final Program
8–12 JANUARY 2018 KISSIMMEE, FL SEIZING THE NEXT DIGITAL TRANSFORMATION See what’s in Check pages 169-172 for details. scitech.aiaa.org #aiaaSciTech A CLEAR VISION FOR THE FUTURE. AT LOCKHEED MARTIN, WE’RE ENGINEERING A BETTER TOMORROW.® Lockheed Martn Skunk Works® has been a trusted partner in creatng revolutonary aircraf and technologies for nearly 75 years. It took a clear vision to produce the world’s fastest jet aircraf, frst producton stealth fghter and highest fying manned aircraf. And it’s that same vision that will allow Skunk Works to contnue developing the world’s most advanced aircraf well into the future. Learn more at lockheedmartn.com/skunkworks © 2017 LOCKHEED MARTIN CORPORATION Contents Contents ............................................................3 Please be advised that AIAA’s partner for our forums is no longer supporting the conference Organizing Committee ...................................4 app. The full program can be found online here: http://aiaa-mst18.abstractcentral.com/itin.jsp Welcome ...........................................................5 or by scanning the QR code. AIAA is currently investigating a new conference app for future Sponsors and Supporters ...............................6 forums and would like your feedback regarding tools you would like to see included in the app. Pre-Forum Activities .......................................7 AIAA staff will be in the HUB on Wednesday, 0930–1130 hrs, to gather feedback from attendees. Please join us. Forum Overview ........................................... -
User Guide To
USER GUIDE TO 1 2 5 0 , 000 S CA L E L U NA R MA P S DANNY C. KINSLER Lunar Science Institute 3303 NASA Road #1 Houston, TX 77058 Telephone: 713/488-5200 Cable Address: LUNSI The Lunar Science Institute is operated by the Universities Space Research Association under Contract No. NSR 09-051-001 with the National Aeronautics and Space Administration. This document constitutes LSI Contribution No. 206 March 1975 USER GUIDE TO 1 : 250 , 000 SCALE LUNAR MAPS GENERAL In 1 972 the NASA Lunar Programs Office initiated the Apoll o Photographic Data Analysis Program. The principal point of this program was a detail ed scientific analysis of the orbital and surface experiments data derived from Apollo missions 15, 16, and 17 . One of the requirements of this program was the production of detailed photo base maps at a useabl e scale . NASA in conjunction with the Defense Mapping Agency (DMA) commenced a mapping program in early 1973 that would lead to the production of the necessary maps based on the need for certain areas . This paper is desi gned to present in outline form the neces- sary background information for users to become familiar with the program. MAP FORMAT The scale chosen for the project was 1:250,000* . The re- search being done required a scale that Principal Investigators (PI's) using orbital photography could use, but would also serve PI's doing surface photographic investigations. Each map sheet covers an area four degrees north/south by five degrees east/west. The base is compiled from vertical Metric photography from Apollo missions 15, 16, and 17. -
Scientific Exploration of Near-Earth Objects Via the Orion Crew Exploration Vehicle
Meteoritics & Planetary Science 44, Nr 12, 1825–1836 (2009) Abstract available online at http://meteoritics.org Scientific exploration of near-Earth objects via the Orion Crew Exploration Vehicle Paul A. ABELL1, 2*, David J. KORSMEYER3, Rob R. LANDIS3, Thomas D. JONES4, Daniel R. ADAMO5, David D. MORRISON6, Lawrence G. LEMKE7, Andrew A. GONZALES7, Robert GERSHMAN8, Theodore H. SWEETSER8, Lindley L. JOHNSON9, and Ed LU10 1Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, Texas 77058, USA 2Planetary Science Institute, 1700 E. Fort Lowell, Tucson, Arizona 85719, USA 3Intelligent Systems Division, NASA Ames Research Center, Moffett Field, California 94035, USA 4Association of Space Explorers, 1150 Gemini Avenue, Houston, Texas 77058, USA 5Trajectory Consultant, 4203 Moonlight Shadow Court, Houston, Texas 77059, USA 6NASA Astrobiology Institute, NASA Ames Research Center, Moffett Field, California 94035, USA 7NASA Ames Research Center, Moffett Field, California 94035, USA 8Jet Propulsion Laboratory, Pasadena, California 91109, USA 9Planetary Science Division, NASA Headquarters, Washington, D.C. 20546, USA 10Google Inc., 1600 Amphitheatre Parkway, Mountain View, California 94043, USA *Corresponding author. E-mail: [email protected] (Received 20 December 2008; revision accepted 13 September 2009) Abstract–A study in late 2006 was sponsored by the Advanced Projects Office within NASA’s Constellation Program to examine the feasibility of sending the Orion Crew Exploration Vehicle (CEV) to a near-Earth object (NEO). The ideal mission profile would involve two or three astronauts on a 90 to 180 day flight, which would include a 7 to 14 day stay for proximity operations at the target NEO. This mission would be the first human expedition to an interplanetary body beyond the Earth- Moon system and would prove useful for testing technologies required for human missions to Mars and other solar system destinations. -
Lunar Topographical Studies Section Banded Craters Program
Lunar Topographical Studies Section Banded Craters Program These highly stylized drawings are intended only to give a general impression of each Group In the March 1955 Journal of the British Astronomical Association, K. W. Abineri and A. P. Lenham published a paper in which they suggested that banded craters could be grouped into the following five categories: Group 1 - (Aristarchus type) Craters are very bright, quite small, and have fairly small dark floors leaving broad bright walls. The bands, on the whole, apparently radiate from near the centre of the craters. These craters are often the centres of simple bright ray systems. Group 2 - (Conon type) Rather dull craters with large dark floors and narrow walls. Very short bands show on the walls but cannot be traced on the floors. The bands, despite their shortness, appear radial to the crater centre. Group 3 - (Messier type) A broad east-west band is the main feature of the floors. Group 4 - (Birt type) Long, usually curved, bands radiate from a non-central dull area. The brightness and size are similar to the Group 1 craters. Group 5 - (Agatharchides A type) One half of the floor is dull and the bands radiate from near the wall inside this dull section and are visible on the dull and bright parts of the floor. 1 BANDED CRATERS BY NAMED FEATURE NAMED FEATURE LUNAR LONG. LUNAR LAT. GROUP (Unnamed Feature) E0.9 S18.0 1 (Unnamed Feature) E4.8 N23.4 4 (Unnamed Feature) W45.4 S23.6 3 (Unnamed Feature) E56.6 N38.3 1 Abbot (Apollonius K) E54.8 N5.6 1 Abenezra A (Mayfair A) E10.5 22.8S 2 -
Spectroscopic and Theoretical Constraints on the Differentiation of Planetesimals a Dissertation Submitted to the Graduate Divis
SPECTROSCOPIC AND THEORETICAL CONSTRAINTS ON THE DIFFERENTIATION OF PLANETESIMALS A DISSERTATION SUBMITTED TO THE GRADUATE DIVISION OF THE UNIVERSITY OF HAWAI‘I IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN ASTRONOMY AUGUST 2009 By Nicholas A. Moskovitz Dissertation Committee: E. Gaidos, Chairperson R. Jedicke N. Haghighipour D. Jewitt S. Krot We certify that we have read this dissertation and that, in our opinion, it is satisfactory in scope and quality as a dissertation for the degree of Doctor of Philosophy in Astronomy. DISSERTATION COMMITTEE Chairperson ii c Copyright 2009 by Nicholas A. Moskovitz All Rights Reserved iii Gei˘ wo˘ de jiar¯ en.´ iv Acknowledgements Whatever weaknesses may be present in the following pages, they undoubtedly would have been far greater without support, insight and inspiration from numerous individuals. First and foremost, I am deeply grateful to my advisor Eric Gaidos whose intelligence, patience and deep curiosity have helped to guide me through the intellectual rigors of completing this dissertation. I want to extend a special thanks to Robert Jedicke who, through his enthusiasm and thoughtful insight, has been an invaluable contributor to this work. Thanks are due to the rest of my committee members (David Jewitt, Nader Haghighipour and Sasha Krot) for their helpful perspectives and for tactfully listening to my sometimes outlandish ideas. Many of my peers have been instrumental (in small ways and large) to the completion of this dissertation. To those who fall into the ubiquitous category of “too many to mention”, I thank you for your support. Others have been absolutely essential in their contributions to this work and I would be remiss if I did not recognize them individually.