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REPORT RESUMES ED 019 218 88 SE 004 494 A RESOURCE BOOK OF AEROSPACE ACTIVITIES, K-6. LINCOLN PUBLIC SCHOOLS, NEBR. PUB DATE 67 EDRS PRICEMF.41.00 HC-S10.48 260P. DESCRIPTORS- *ELEMENTARY SCHOOL SCIENCE, *PHYSICAL SCIENCES, *TEACHING GUIDES, *SECONDARY SCHOOL SCIENCE, *SCIENCE ACTIVITIES, ASTRONOMY, BIOGRAPHIES, BIBLIOGRAPHIES, FILMS, FILMSTRIPS, FIELD TRIPS, SCIENCE HISTORY, VOCABULARY, THIS RESOURCE BOOK OF ACTIVITIES WAS WRITTEN FOR TEACHERS OF GRADES K-6, TO HELP THEM INTEGRATE AEROSPACE SCIENCE WITH THE REGULAR LEARNING EXPERIENCES OF THE CLASSROOM. SUGGESTIONS ARE MADE FOR INTRODUCING AEROSPACE CONCEPTS INTO THE VARIOUS SUBJECT FIELDS SUCH AS LANGUAGE ARTS, MATHEMATICS, PHYSICAL EDUCATION, SOCIAL STUDIES, AND OTHERS. SUBJECT CATEGORIES ARE (1) DEVELOPMENT OF FLIGHT, (2) PIONEERS OF THE AIR (BIOGRAPHY),(3) ARTIFICIAL SATELLITES AND SPACE PROBES,(4) MANNED SPACE FLIGHT,(5) THE VASTNESS OF SPACE, AND (6) FUTURE SPACE VENTURES. SUGGESTIONS ARE MADE THROUGHOUT FOR USING THE MATERIAL AND THEMES FOR DEVELOPING INTEREST IN THE REGULAR LEARNING EXPERIENCES BY INVOLVING STUDENTS IN AEROSPACE ACTIVITIES. INCLUDED ARE LISTS OF SOURCES OF INFORMATION SUCH AS (1) BOOKS,(2) PAMPHLETS, (3) FILMS,(4) FILMSTRIPS,(5) MAGAZINE ARTICLES,(6) CHARTS, AND (7) MODELS. GRADE LEVEL APPROPRIATENESS OF THESE MATERIALSIS INDICATED. (DH) 4:14.1,-) 1783 1490 ,r- 6e tt*.___.Vhf 1842 1869 LINCOLN PUBLICSCHOOLS A RESOURCEBOOK OF AEROSPACEACTIVITIES U.S. DEPARTMENT OF HEALTH, EDUCATION & WELFARE OFFICE OF EDUCATION K-6) THIS DOCUMENT HAS BEEN REPRODUCED EXACTLY AS RECEIVED FROM THE PERSON OR ORGANIZATION ORIGINATING IT.POINTS OF VIEW OR OPINIONS STATED DO NOT NECESSARILY REPRESENT OFFICIAL OFFICE OF EDUCATION POSITION OR POLICY. 1919 O O Vj A PROJECT FUNDED UNDER TITLE HIELEMENTARY AND SECONDARY EDUCATION ACT A RESOURCE BOOK OF AEROSPACE ACTIVITIES (K-6) The work presentedor reported herein was performed pursuant to a Grant from the U. -
EPSC-DPS2011-1845, 2011 EPSC-DPS Joint Meeting 2011 C Author(S) 2011
EPSC Abstracts Vol. 6, EPSC-DPS2011-1845, 2011 EPSC-DPS Joint Meeting 2011 c Author(s) 2011 Analysis of mineralogy of an effusive volcanic lunar dome in Marius Hills, Oceanus Procellarum. A.S. Arya, Guneshwar Thangjam, R.P. Rajasekhar, Ajai Space Applications Centre, Indian Space Research Organization, Ahmedabad-380 015 (India). Email:[email protected] Abstract found on the lunar surface. As a part of initiation of the study of mineralogy of MHC, an effusive dome Domes are analogous to the terrestrial shield located in the south of Rima Galilaei, near the volcanoes and are among the important volcanic contact of Imbrian and Eratosthenian geological units features found on the lunar surface indicative of is taken up for the present study. The morphology, effusive vents of primary volcanism within Mare rheology and the possible dike parameters have regions. Marius Hills Complex (MHC) is one of the already been studied and reported [5]. most important regions on the entire lunar surface, having a complex geological setting and largest distribution of volcanic constructs with an abundant number of volcanic features like domes, cones and rilles. The mineralogical study of an effusive dome located in the south of Rima Galilaei, near the contact of Imbrian and Eratosthenian geological units is done using hyperspectral band parameters and spectral plots so as to understand the compositional variation, the nature of the volcanism and relate it to the rheology of the dome. Fig. 1: Distribution of dome in MHC (Red-the dome under study, Green- from Virtual Moon Atlas, Magenta [6]) and the Study area showing the dome under study on M3 1. -
OMNI Magazine Interview, July 1992)
ALIEN CITY ON MARS? TiTil W i^ -A Im; SCENES Lji U *' Ul EDITOR IN CHIEF & DESIGN DIRECTOR: BOB GUCCIONE PRESIDENT a C.O.O.: KATHY KEETON VP/EDITOR' KEITH FERRELL EXECUTIVE VP/GBAPHICS DIRECTOR- FRANK DEVINO MANAGING EDITOR: CAROLINE DARK ART DIRECTOR: CATHRYN MEZZO First Word Continuum By Dana Rohrabacher 42 Fighting for Opening the X-Files U.S. patent rights By David Bischoff S Mulder and Scully know Communications something is m out there—and so do their Funds many fans. A behind- By Linda Marsa the-scenes lool< at this fas- Cashing in on collectibles cinating and m increasingly popular Electronic Universe new show. By Grsgg Keizer ArchiTreIc Medicine Designing Generations By Anita Bartholomew By Herman Zimmerman m and Philip Thomas Edgerly .Sounds Boldly going where By Steve Nadis few. production designers Sounds of the silent have gone before: 22 designing the Star Trek Eanii By Melanie Menagh Choices Fiction: S.4 Dying Virtual Realities [Vlichael IVlarshall Smith By Tom Dworetzl<y 7^ 23 Cartoon Feature Artificial Intelligence . By Steve Nadis Interview: 32 Richard hioa gland Mind By Steve Nadis By Steve Nadis A close-up lool< at the Hallucinations, man behind delusions, the face on Mars and schizophrenia SS 33 Tsuneo Sanda's cover painting, On Patrol, made possible by Antimatter the PI" I p Edge ly Age cy n a'^sar qt on witi ZD^sgn Copyrght Pa amount PcturesCorporaticn Games (Additional art rred t"^ page 110) By bi, iff Morris SR1''6ril7'iBn FIRST UUORD INVENTING AMERICA: Patent laws and the protection of individual rights By Dana Rohrabacher merica's greatest asset side. -
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. -
Impact Cratering
6 Impact cratering The dominant surface features of the Moon are approximately circular depressions, which may be designated by the general term craters … Solution of the origin of the lunar craters is fundamental to the unravel- ing of the history of the Moon and may shed much light on the history of the terrestrial planets as well. E. M. Shoemaker (1962) Impact craters are the dominant landform on the surface of the Moon, Mercury, and many satellites of the giant planets in the outer Solar System. The southern hemisphere of Mars is heavily affected by impact cratering. From a planetary perspective, the rarity or absence of impact craters on a planet’s surface is the exceptional state, one that needs further explanation, such as on the Earth, Io, or Europa. The process of impact cratering has touched every aspect of planetary evolution, from planetary accretion out of dust or planetesimals, to the course of biological evolution. The importance of impact cratering has been recognized only recently. E. M. Shoemaker (1928–1997), a geologist, was one of the irst to recognize the importance of this process and a major contributor to its elucidation. A few older geologists still resist the notion that important changes in the Earth’s structure and history are the consequences of extraterres- trial impact events. The decades of lunar and planetary exploration since 1970 have, how- ever, brought a new perspective into view, one in which it is clear that high-velocity impacts have, at one time or another, affected nearly every atom that is part of our planetary system. -
Project: Apollo 8
v ._. I / I NATIONAL AERONAUTICS AND SPACE ADMINISTRATION TELS WO 2-4155 NEWS WASHINGTON,D.C.20546 • WO 3-6925 FOR RELEASE: SUNDAY December 15, 1968 RELEASE NO: 68.208 P PROJECT: APOLLO 8 R E contents GENERAL RELEASE----------~-------~·~-~-~--~~----~----~-~--~-l-lO MISSION OBJECTIVES------------------------------------------11 SEQUENCE OF EVENTS-------------~-------------~----~----~--~~12-14 5 Launch W1ndow~~-~----~--~-~--~-------~-----~---------w--~-14 MISSION DESCRIPTION-----------------------------------------15-19 FLIGHT PLAN--~---~-----·------------~------~----~---~----~--20-23 ALTERNATE MISSIONS---------------------------------~--------24-26 5 ABORT MODES-----~--------------~--~--~------------~---~~--~-27~29 PHOTOGRAPHIC TASKS------------------------------------------30-32 SPACECRAFT STRUCTURE SYSTEMS--------------------------------33-37 SATURN V LAUNCH VEHICLE-------------------------------------38-50 APOLLO 8 LAUNCH OPERATIONS----------------------------------51.64 MISSION CONTROL CENTER--------------------------------------65-66 MANNED SPACE FLIGHT NETWORK---------------------------------67-71 APOLLO 8 RECOVERY-------------------------------------------72-73 APOLLO 8 CREW-------------~--~--~~-~~---~---~~~-------------74-86 K LUNAR DESCRIPTION-------------------------------------------87-88 APOLLO PROGRAM MANAGEMENT/CONTRACTORS---~-------------------39-94 I APOLLO 8 GLOSSARY-------- -----------------------------------95-101 T -0- 12/6/68 NATIONAL AERONAUTICS AND SPACE ADMINISTRATION WO 2-4155 NEWS WASHINGTON, D.C. 20546 TELS. -
A Study About the Temporal Constraints on the Martian Yardangs’ Development in Medusae Fossae Formation
remote sensing Article A Study about the Temporal Constraints on the Martian Yardangs’ Development in Medusae Fossae Formation Jia Liu 1,2 , Zongyu Yue 1,3,*, Kaichang Di 1,3 , Sheng Gou 1,4 and Shengli Niu 4 1 State Key Laboratory of Remote Sensing Science, Aerospace Information Research Institute, Chinese Academy of Sciences, Beijing 100101, China; [email protected] (J.L.); [email protected] (K.D.); [email protected] (S.G.) 2 University of Chinese Academy of Sciences, Beijing 100049, China 3 CAS Center for Excellence in Comparative Planetology, Hefei 230026, China 4 State Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology, Macau 999078, China; [email protected] * Correspondence: [email protected]; Tel.: +86-10-64889553 Abstract: The age of Mars yardangs is significant in studying their development and the evolution of paleoclimate conditions. For planetary surface or landforms, a common method for dating is based on the frequency and size distribution of all the superposed craters after they are formed. However, there is usually a long duration for the yardangs’ formation, and they will alter the superposed craters, making it impossible to give a reliable dating result with the method. An indirect method by analyzing the ages of the superposed layered ejecta was devised in the research. First, the layered ejecta that are superposed on and not altered by the yardangs are identified and mapped. Then, the ages of the layered ejecta are derived according to the crater frequency and size distribution on them. These ages indicate that the yardangs ceased development by these times, and the ages are valuable for studying the evolution of the yardangs. -
A Study About a Lunar Dome Near Hortensius: Morphometry and Mode of Formation
47th Lunar and Planetary Science Conference (2016) 1005.pdf A study about a lunar dome near Hortensius: Morphometry and mode of formation. M. Wirths1, R. Lena2 , A. Mallama3 - Geologic Lunar Research (GLR) Group. 1km 67 Camino Observatorio, Baja California, Mexico; [email protected]; 2 Via Cartesio 144, sc. D, 00137 Rome, Italy; [email protected]; 314012 Lancaster Lane, Bowie, MD, 20715, USA, [email protected] Introduction: Lunar mare domes formed during the later stages of volcanic episode on the Moon, char- acterized by a decreasing rate of lava extrusion and comparably low eruption temperatures, resulted in the formation of effusive domes. Important clusters of lu- nar domes are observed in the Hortensius/Milichius/T. Mayer region in Mare Insularum and in Mare Tranquillitatis around the craters Arago and Cauchy. The region west of Copernicus extending from Hortensius to Milichius and to Tobias Mayer contains large numbers of lunar domes and cones, evidence of past volcanism on the lunar surface [1-3]. A compre- hensive map of the area was produced by GLR group, including the six lunar domes north of Hortensius and three lower domes to the south of Hortensius [4]. Fig. 1. Telescopic image acquired on May 1, 2012, at 03:44 In this contribution we provide an analysis of an- UT with a 450 mm aperture Starmaster driven Dobsonian other low dome to the east of Hortensius, termed H11, (M. Wirths). Morphometric properties of the domes H1-H7 located at 26.87° W and 6.88° N and with a prominent have been examined in previous studies [1, 3]. -
Glossary of Lunar Terminology
Glossary of Lunar Terminology albedo A measure of the reflectivity of the Moon's gabbro A coarse crystalline rock, often found in the visible surface. The Moon's albedo averages 0.07, which lunar highlands, containing plagioclase and pyroxene. means that its surface reflects, on average, 7% of the Anorthositic gabbros contain 65-78% calcium feldspar. light falling on it. gardening The process by which the Moon's surface is anorthosite A coarse-grained rock, largely composed of mixed with deeper layers, mainly as a result of meteor calcium feldspar, common on the Moon. itic bombardment. basalt A type of fine-grained volcanic rock containing ghost crater (ruined crater) The faint outline that remains the minerals pyroxene and plagioclase (calcium of a lunar crater that has been largely erased by some feldspar). Mare basalts are rich in iron and titanium, later action, usually lava flooding. while highland basalts are high in aluminum. glacis A gently sloping bank; an old term for the outer breccia A rock composed of a matrix oflarger, angular slope of a crater's walls. stony fragments and a finer, binding component. graben A sunken area between faults. caldera A type of volcanic crater formed primarily by a highlands The Moon's lighter-colored regions, which sinking of its floor rather than by the ejection of lava. are higher than their surroundings and thus not central peak A mountainous landform at or near the covered by dark lavas. Most highland features are the center of certain lunar craters, possibly formed by an rims or central peaks of impact sites. -
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 -
The Composition of the Lunar Crust: Radiative Transfer Modeling and Analysis of Lunar Visible and Near-Infrared Spectra
THE COMPOSITION OF THE LUNAR CRUST: RADIATIVE TRANSFER MODELING AND ANALYSIS OF LUNAR VISIBLE AND NEAR-INFRARED SPECTRA 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 GEOLOGY AND GEOPHYSICS DECEMBER 2009 By Joshua T.S. Cahill Dissertation Committee: Paul G. Lucey, Chairperson G. Jeffrey Taylor Patricia Fryer Jeffrey J. Gillis-Davis Trevor Sorensen Student: Joshua T.S. Cahill Student ID#: 1565-1460 Field: Geology and Geophysics Graduation date: December 2009 Title: The Composition of the Lunar Crust: Radiative Transfer Modeling and Analysis of Lunar Visible and Near-Infrared Spectra 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 Geology and Geophysics. Dissertation Committee: Names Signatures Paul G. Lucey, Chairperson ____________________________ G. Jeffrey Taylor ____________________________ Jeffrey J. Gillis-Davis ____________________________ Patricia Fryer ____________________________ Trevor Sorensen ____________________________ ACKNOWLEDGEMENTS I must first express my love and appreciation to my family. Thank you to my wife Karen for providing love, support, and perspective. And to our little girl Maggie who only recently became part of our family and has already provided priceless memories in the form of beautiful smiles, belly laughs, and little bear hugs. The two of you provided me with the most meaningful reasons to push towards the "finish line". I would also like to thank my immediate and extended family. Many of them do not fully understand much about what I do, but support the endeavor acknowledging that if it is something I’m willing to put this much effort into, it must be worthwhile. -
South Pole-Aitken Basin
Feasibility Assessment of All Science Concepts within South Pole-Aitken Basin INTRODUCTION While most of the NRC 2007 Science Concepts can be investigated across the Moon, this chapter will focus on specifically how they can be addressed in the South Pole-Aitken Basin (SPA). SPA is potentially the largest impact crater in the Solar System (Stuart-Alexander, 1978), and covers most of the central southern farside (see Fig. 8.1). SPA is both topographically and compositionally distinct from the rest of the Moon, as well as potentially being the oldest identifiable structure on the surface (e.g., Jolliff et al., 2003). Determining the age of SPA was explicitly cited by the National Research Council (2007) as their second priority out of 35 goals. A major finding of our study is that nearly all science goals can be addressed within SPA. As the lunar south pole has many engineering advantages over other locations (e.g., areas with enhanced illumination and little temperature variation, hydrogen deposits), it has been proposed as a site for a future human lunar outpost. If this were to be the case, SPA would be the closest major geologic feature, and thus the primary target for long-distance traverses from the outpost. Clark et al. (2008) described four long traverses from the center of SPA going to Olivine Hill (Pieters et al., 2001), Oppenheimer Basin, Mare Ingenii, and Schrödinger Basin, with a stop at the South Pole. This chapter will identify other potential sites for future exploration across SPA, highlighting sites with both great scientific potential and proximity to the lunar South Pole.