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Low Thrust Manoeuvres to Perform Large Changes of RAAN Or Inclination in LEO
Facoltà di Ingegneria Corso di Laurea Magistrale in Ingegneria Aerospaziale Master Thesis Low Thrust Manoeuvres To Perform Large Changes of RAAN or Inclination in LEO Academic Tutor: Prof. Lorenzo CASALINO Candidate: Filippo GRISOT July 2018 “It is possible for ordinary people to choose to be extraordinary” E. Musk ii Filippo Grisot – Master Thesis iii Filippo Grisot – Master Thesis Acknowledgments I would like to address my sincere acknowledgments to my professor Lorenzo Casalino, for your huge help in these moths, for your willingness, for your professionalism and for your kindness. It was very stimulating, as well as fun, working with you. I would like to thank all my course-mates, for the time spent together inside and outside the “Poli”, for the help in passing the exams, for the fun and the desperation we shared throughout these years. I would like to especially express my gratitude to Emanuele, Gianluca, Giulia, Lorenzo and Fabio who, more than everyone, had to bear with me. I would like to also thank all my extra-Poli friends, especially Alberto, for your support and the long talks throughout these years, Zach, for being so close although the great distance between us, Bea’s family, for all the Sundays and summers spent together, and my soccer team Belfiga FC, for being the crazy lovable people you are. A huge acknowledgment needs to be address to my family: to my grandfather Luciano, for being a great friend; to my grandmother Bianca, for teaching me what “fighting” means; to my grandparents Beppe and Etta, for protecting me -
Observing from Space Orbits, Constraints, Planning, Coordination
Observing from Space Orbits, constraints, planning, coordination Integral XMM-Newton Jan-Uwe Ness European Space Astronomy Centre (ESAC) Villafranca del Castillo, Spain On behalf of the Integral and XMM-Newton Science Operations Centres Slide 1 Observing from Space - Orbits http://sci.esa.int/integral/59688-integral-fifteen-years-in-orbit/ Slide 2 Observing from Space - Orbits Highly elliptical Earth orbit: XMM-Newton, Integral, Chandra Slide 3 Observing from Space - Orbits Low-Earth orbit: ~1.5 hour, examples: Hubble Space Telescope Swift NuSTAR Fermi Earth blocking, especially low declination objects Only short snapshots of a few 100s possible No long uninterrupted observations Only partial overlap with Integral/XMM possible Slide 4 Observing from Space - Orbits Orbit around Lagrange point L2 past: future: Herschel James Webb Planck Athena present: Gaia Slide 5 Observing from Space – Constraints Motivations for constraints: • Safety of space-craft and instruments • Contamination by bright optical/X-ray sources or straylight from them • Functionality of star Tracker • Power supply (solar panels) • Thermal stability (avoid heat from the sun) • Ground contact for remote commanding and downlink of data Space-specific constraints in bold orange Slide 6 Observing from Space – Constraints Examples for constraints: • No observations while passing through radiation belts • Orientation of space craft to sun • Large avoidance angles around Sun and anti-Sun, Moon, Earth, Bright planets • No slewing over Moon and Earth (planets ok) • Availability -
THE AVALANCHE DEPOSITS in LUNAR CRATER REINER. V.V.Shevchenko1,2, P.C.Pinet1, S.Chevrel1, Y.Daydou1, T.P.Skobeleva2, O.I.Kvaratskhelia3, C.Rosemberg1
Lunar and Planetary Science XXXVIII (2007) 1066.pdf THE AVALANCHE DEPOSITS IN LUNAR CRATER REINER. V.V.Shevchenko1,2, P.C.Pinet1, S.Chevrel1, Y.Daydou1, T.P.Skobeleva2, O.I.Kvaratskhelia3, C.Rosemberg1. 1UMR 5562 “Dynamique Terrestre et Planet- aire”/CNRS/UPS, Observatoire Midi-Pyrenees, Toulouse, 31400 France; 2Sternberg Astronomical Institute, Mos- cow University, Moscow, 119992, Russia, 3Abastumany Astrophysical Observatory, Georgian Academy of Sci- ences, Georgia. [email protected] Introduction: Space weathering processes on the Fig. 3 represents the Clementine image of the cra- Moon affect the optical properties of an exposed lunar ter Reiner. soil. The main spectral/optical effects of space weath- ering are a reduction of reflectance, attenuation of the 1-μm ferrous absorption band, and a red-sloped con- tinuum creation [1]. Lucey et al. [2 - 4] proposed to estimate the maturity of lunar soils from Clementine UVVIS data using a method which decorrelates the effects of variations in Fe2+ concentration from the effects of soil maturity. The method calculates optical maturity defined as parameter OMAT [5]. Pinet et al. [6] used the method to analyse the ‘Reiner-γ – Reiner’ region on the basis of Clementine spectral image data. Crater Reiner: Crater Reiner is located in western Oceanus Procellarum. Diameter of the crater is 30 km, its depth is 2.4 km and its central peak height is about 700 m (Fig. 1). Fig.3 Evidence of avalanching and of other downslope movement of material is clearly visible on the inner walls of the crater. In general, freshly exposed lunar material is brighter than undisturbed materials nearby. -
USGS Open-File Report 2005-1190, Table 1
TABLE 1 GEOLOGIC FIELD-TRAINING OF NASA ASTRONAUTS BETWEEN JANUARY 1963 AND NOVEMBER 1972 The following is a year-by-year listing of the astronaut geologic field training trips planned and led by personnel from the U.S. Geological Survey’s Branches of Astrogeology and Surface Planetary Exploration, in collaboration with the Geology Group at the Manned Spacecraft Center, Houston, Texas at the request of NASA between January 1963 and November 1972. Regional geologic experts from the U.S. Geological Survey and other governmental organizations and universities s also played vital roles in these exercises. [The early training (between 1963 and 1967) involved a rather large contingent of astronauts from NASA groups 1, 2, and 3. For another listing of the astronaut geologic training trips and exercises, including all attending and the general purposed of the exercise, the reader is referred to the following website containing a contribution by William Phinney (Phinney, book submitted to NASA/JSC; also http://www.hq.nasa.gov/office/pao/History/alsj/ap-geotrips.pdf).] 1963 16-18 January 1963: Meteor Crater and San Francisco Volcanic Field near Flagstaff, Arizona (9 astronauts). Among the nine astronaut trainees in Flagstaff for that initial astronaut geologic training exercise was Neil Armstrong--who would become the first man to step foot on the Moon during the historic Apollo 11 mission in July 1969! The other astronauts present included Frank Borman (Apollo 8), Charles "Pete" Conrad (Apollo 12), James Lovell (Apollo 8 and the near-tragic Apollo 13), James McDivitt, Elliot See (killed later in a plane crash), Thomas Stafford (Apollo 10), Edward White (later killed in the tragic Apollo 1 fire at Cape Canaveral), and John Young (Apollo 16). -
No. 40. the System of Lunar Craters, Quadrant Ii Alice P
NO. 40. THE SYSTEM OF LUNAR CRATERS, QUADRANT II by D. W. G. ARTHUR, ALICE P. AGNIERAY, RUTH A. HORVATH ,tl l C.A. WOOD AND C. R. CHAPMAN \_9 (_ /_) March 14, 1964 ABSTRACT The designation, diameter, position, central-peak information, and state of completeness arc listed for each discernible crater in the second lunar quadrant with a diameter exceeding 3.5 km. The catalog contains more than 2,000 items and is illustrated by a map in 11 sections. his Communication is the second part of The However, since we also have suppressed many Greek System of Lunar Craters, which is a catalog in letters used by these authorities, there was need for four parts of all craters recognizable with reasonable some care in the incorporation of new letters to certainty on photographs and having diameters avoid confusion. Accordingly, the Greek letters greater than 3.5 kilometers. Thus it is a continua- added by us are always different from those that tion of Comm. LPL No. 30 of September 1963. The have been suppressed. Observers who wish may use format is the same except for some minor changes the omitted symbols of Blagg and Miiller without to improve clarity and legibility. The information in fear of ambiguity. the text of Comm. LPL No. 30 therefore applies to The photographic coverage of the second quad- this Communication also. rant is by no means uniform in quality, and certain Some of the minor changes mentioned above phases are not well represented. Thus for small cra- have been introduced because of the particular ters in certain longitudes there are no good determi- nature of the second lunar quadrant, most of which nations of the diameters, and our values are little is covered by the dark areas Mare Imbrium and better than rough estimates. -
Glossary Glossary
Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts. -
General Disclaimer One Or More of the Following Statements May Affect
General Disclaimer One or more of the Following Statements may affect this Document This document has been reproduced from the best copy furnished by the organizational source. It is being released in the interest of making available as much information as possible. This document may contain data, which exceeds the sheet parameters. It was furnished in this condition by the organizational source and is the best copy available. This document may contain tone-on-tone or color graphs, charts and/or pictures, which have been reproduced in black and white. This document is paginated as submitted by the original source. Portions of this document are not fully legible due to the historical nature of some of the material. However, it is the best reproduction available from the original submission. Produced by the NASA Center for Aerospace Information (CASI) ^i e I !emote sousing sad eeolegio Studies of the llaistary Crusts Bernard Ray Hawke Prince-1 Investigator a EL r Z^ .99 University of Hawaii Hawaii Institute of Geophysics Planetary Geosciences Division Honolulu, Hawaii 96822 ^y 1i i W. December 1983 (NASA —CR-173215) REMOTE SENSING AND N84-17092 GEOLOGIC STUDIES OF THE PLANETARY CRUSTS Final Report ( Hawaii Inst. of Geophysics) 14 p HC A02/MF 101 CSCL 03B Unclas G3/91 11715 Gy -2- ©R1GNAL OF POOR QUALITY Table of Contents Page I. Remote Sensing and Geologic Studies cf Volcanic Deposits . • . 3 A. Spectral reflectance studies of dark-haloed craters. • . 3 B. Remote s^:sing studies of regions which were sites of ancient volcanisa . 3 C. [REEP basalt deposits in the Imbrium Region. -
Intentos Argentinos Para Probar La Teor´Ia De La Relatividad
Asociaci´on Argentina de Astronom´ıa BAAA, Vol. 50, 2007 G. Dubner, M. Rovira, A. Piatti & F. A. Bareilles, eds. PRESENTACION´ ORAL Intentos argentinos para probar la Teor´ıa de la Relatividad Santiago Paolantonio1 & Edgardo R. Minitti2 (1) Museo Astron´omico Sarmiento-Gould, Observatorio Astron´omico, Universidad Nacional de C´ordoba, Argentina (2) Observatorio Astron´omico, Universidad Nacional de C´ordoba, Argentina Abstract. Astrophysics research at the Argentinean National Observa- tory (Cordoba) began during the period when Dr. Charles Perrine was its Director (1909-1936). In 1911 Perrine was invited by Dr. Freundlich (Berlin Observatory) to carry out observations in Brazil during the solar eclipse that would take place on October 10, 1912, with the aim of verify- ing Einstein’s theory of relativity. With numerous instruments specially designed and constructed in Cordoba, the expedition took place. How- ever, an inopportune rain made fail all the project. Poor weather condi- tions made also fail two new attempts, one in Teodesy (Ukraine; August 21, 1914), and the other in Tucacas (Venezuela; February 3, 1916). Suc- cessful observations and verification of Einstein’s predictions finally took place in 1919, during an eclipse observed in Brazil. The Argentinean Observatory was unfortunately absent in such opportunity. Resumen. Durante la direcci´on del Dr. Charles Perrine (1909-1936) se inician en el Observatorio Nacional Argentino los trabajos relacionados con la Astrof´ısica. En 1911, Perrine es contactado por el Dr. Freundlich del Observatorio de Berl´ın, quien le propone realizar observaciones para verificar la Teor´ıa de la Relatividad en el eclipse del 10 de octubre de 1912 que ocurrir´ıa en Brasil. -
Regolith Compaction and Its Implications for the Formation Mechanism of Lunar Swirls
EPSC Abstracts Vol. 13, EPSC-DPS2019-1608-1, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Regolith Compaction and its Implications for the Formation Mechanism of Lunar Swirls Christian Wöhler (1), Megha Bhatt (2), Arne Grumpe (1), Marcel Hess (1), Alexey A. Berezhnoy (3), Vladislav V. Shevchenko (3) and Anil Bhardwaj (2) (1) Image Analysis Group, TU Dortmund University, Otto-Hahn-Str. 4, 44227 Dortmund, Germany, (2) Physical Research Laboratory, Ahmedabad, 380009, India, (3) Sternberg Astronomical Institute, Universitetskij pr., 13, Moscow State University, 119234 Moscow, Russia ([email protected]) Abstract The brightening of the regolith at Reiner Gamma could be a result of reduced space-weathering due to In this study we have examined spectral trends of magnetic shielding [3] and/or due to soil compaction Reiner Gamma (7.5°N, 59°W) using the Moon [5]. According to the model of [9], the spectral Mineralogy Mapper (M3) [1] observations. We variation due to soil compaction is a change in albedo derived maps of solar wind induced OH/H2O and a with negligible effect on spectral slope and compaction index map of the Reiner Gamma swirl. absorption band depths. To quantify soil compaction Our results suggest that the combination of soil at Reiner Gamma, we empirically defined the compaction and magnetic shielding can explain the compaction index c as a positive real number given observed spectral trends. These new findings support by c = M / RSE, where M is the reflectance the hypothesis of swirl formation by interaction modulation at 1.579 µm between a bright on-swirl between a comet and the uppermost regolith layer. -
École De Paris Tableaux Modernes Photographies Aviation Conquête Spatiale
EXPERTISES – VENTES AUX ENCHÈRES École de Paris Tableaux modernes Photographies Aviation Conquête spatiale Paris - Hôtel Drouot - 8 et 9 octobre 2019 EXPERTISES – VENTES AUX ENCHÈRES VENTE AUX ENCHÈRES PUBLIQUES Hôtel Drouot Richelieu salle 6 9, rue Drouot à Paris IXe Mardi 8 octobre 2019 à 14 h École de Paris Tableaux Modernes Mercredi 9 octobre 2019 à 14 h Photographies Aviation Conquête spatiale Reproduction des œuvres sur : www.ogerblanchet.fr - www.jj-mathias.fr Expositions publiques : Le lundi 7 octobre de 11 h à 18 heures Le mardi 8 octobre de 11 h à 12 heures Le mercredi 9 octobre de 11 h à 12 heures EXPERTISES – VENTES AUX ENCHÈRES 22 rue Drouot - 75009 Paris 01 42 46 96 95 - [email protected] ASSISTÉS DES EXPERTS Pour les lots 5 à 10 Pour l’École de Paris Éric SCHOELLER Christophe ZAGRODKI Tél. +33 (0)6 11 86 39 64 Tél. +33 (0)1 43 21 44 52 [email protected] [email protected] Pour les lots 38, 82 à 136, 252, 253, 281 à 287, Pour les autographes et manuscrits 289 à 314 M. Jean-Emmanuel RAUX Cabinet PERAZZONE-BRUN Arts et Autographes 4, rue Favart - 75002 9 rue de l’Odéon - 75006 Paris Tél. +33 (0)1 42 60 45 45 01 43 25 60 48 - [email protected] Pour les photographies M. Serge PLANTUREUX 80 Rue Taitbout - 75009 Paris Tél. +33 (0)6 50 85 60 74 - [email protected] AVERTISSEMENT Concernant l’état des œuvres décrites dans le présent catalogue, des rapports d’état sont disponibles sur simple demande Pour les estampes, sauf mention contraire, les dimensions sont celles de la cuvette pour les gravures et du sujet pour les lithographies J.J. -
NASA Process for Limiting Orbital Debris
NASA-HANDBOOK NASA HANDBOOK 8719.14 National Aeronautics and Space Administration Approved: 2008-07-30 Washington, DC 20546 Expiration Date: 2013-07-30 HANDBOOK FOR LIMITING ORBITAL DEBRIS Measurement System Identification: Metric APPROVED FOR PUBLIC RELEASE – DISTRIBUTION IS UNLIMITED NASA-Handbook 8719.14 This page intentionally left blank. Page 2 of 174 NASA-Handbook 8719.14 DOCUMENT HISTORY LOG Status Document Approval Date Description Revision Baseline 2008-07-30 Initial Release Page 3 of 174 NASA-Handbook 8719.14 This page intentionally left blank. Page 4 of 174 NASA-Handbook 8719.14 This page intentionally left blank. Page 6 of 174 NASA-Handbook 8719.14 TABLE OF CONTENTS 1 SCOPE...........................................................................................................................13 1.1 Purpose................................................................................................................................ 13 1.2 Applicability ....................................................................................................................... 13 2 APPLICABLE AND REFERENCE DOCUMENTS................................................14 3 ACRONYMS AND DEFINITIONS ...........................................................................15 3.1 Acronyms............................................................................................................................ 15 3.2 Definitions ......................................................................................................................... -
Landed Science at a Lunar Crustal Magnetic Anomaly
Landed Science at a Lunar Crustal Magnetic Anomaly David T. Blewett, Dana M. Hurley, Brett W. Denevi, Joshua T.S. Cahill, Rachel L. Klima, Jeffrey B. Plescia, Christopher P. Paranicas, Benjamin T. Greenhagen, Lauren Jozwiak, Brian A. Anderson, Haje Korth, George C. Ho, Jorge I. Núñez, Michael I. Zimmerman, Pontus C. Brandt, Sabine Stanley, Joseph H. Westlake, Antonio Diaz-Calderon, R. Ter ik Daly, and Jeffrey R. Johnson Space Science Branch, Johns Hopkins University Applied Physics Lab, USA Lunar Science for Landed Missions Workshop – January, 2018 1 Lunar Magnetic Anomalies • The lunar crust contains magnetized areas, a few tens to several hundred kilometers across, known as "magnetic anomalies". • The crustal fields are appreciable: Strongest anomalies are ~10-20 nT at 30 km altitude, perhaps a few hundred to 1000 nT at the surface. Lunar Prospector magnetometer Btot map (Richmond & Hood 2008 JGR) over LROC WAC 689-nm mosaic 2 Lunar Magnetic Anomalies: Formation Hypotheses • Magnetized basin ejecta: ambient fields amplified by compression as impact-generated plasma converged on the basin antipode (Hood and co-workers) Lunar Prospector magnetometer Btot (Richmond & Hood 2008 JGR) over LROC WAC 689- nm mosaic 3 Lunar Magnetic Anomalies: Formation Hypotheses • Magnetized basin ejecta: ambient fields amplified by compression as impact-generated plasma converged on the basin antipode (Hood and co-workers) • Magnetic field impressed on the surface by plasma interactions when a cometary coma struck the Moon (Schultz) Lunar Prospector magnetometer Btot (Richmond & Hood 2008 JGR) over LROC WAC 689- nm mosaic 4 Lunar Magnetic Anomalies: Formation Hypotheses • Magnetized basin ejecta: ambient fields amplified by compression as impact-generated plasma converged on the basin antipode (Hood and co-workers) • Magnetic field impressed on the surface by plasma interactions when a cometary coma struck the Moon (Schultz) • Magmatic intrusion or impact melt magnetized in an early lunar dynamo field (e.g., Purucker et al.