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Mathématiques Et Espace
Atelier disciplinaire AD 5 Mathématiques et Espace Anne-Cécile DHERS, Education Nationale (mathématiques) Peggy THILLET, Education Nationale (mathématiques) Yann BARSAMIAN, Education Nationale (mathématiques) Olivier BONNETON, Sciences - U (mathématiques) Cahier d'activités Activité 1 : L'HORIZON TERRESTRE ET SPATIAL Activité 2 : DENOMBREMENT D'ETOILES DANS LE CIEL ET L'UNIVERS Activité 3 : D'HIPPARCOS A BENFORD Activité 4 : OBSERVATION STATISTIQUE DES CRATERES LUNAIRES Activité 5 : DIAMETRE DES CRATERES D'IMPACT Activité 6 : LOI DE TITIUS-BODE Activité 7 : MODELISER UNE CONSTELLATION EN 3D Crédits photo : NASA / CNES L'HORIZON TERRESTRE ET SPATIAL (3 ème / 2 nde ) __________________________________________________ OBJECTIF : Détermination de la ligne d'horizon à une altitude donnée. COMPETENCES : ● Utilisation du théorème de Pythagore ● Utilisation de Google Earth pour évaluer des distances à vol d'oiseau ● Recherche personnelle de données REALISATION : Il s'agit ici de mettre en application le théorème de Pythagore mais avec une vision terrestre dans un premier temps suite à un questionnement de l'élève puis dans un second temps de réutiliser la même démarche dans le cadre spatial de la visibilité d'un satellite. Fiche élève ____________________________________________________________________________ 1. Victor Hugo a écrit dans Les Châtiments : "Les horizons aux horizons succèdent […] : on avance toujours, on n’arrive jamais ". Face à la mer, vous voyez l'horizon à perte de vue. Mais "est-ce loin, l'horizon ?". D'après toi, jusqu'à quelle distance peux-tu voir si le temps est clair ? Réponse 1 : " Sans instrument, je peux voir jusqu'à .................. km " Réponse 2 : " Avec une paire de jumelles, je peux voir jusqu'à ............... km " 2. Nous allons maintenant calculer à l'aide du théorème de Pythagore la ligne d'horizon pour une hauteur H donnée. -
MIRA Ceticeti Periodieke Uitgave Van Volkssterrenwacht MIRA Vzw
België - Belgique P.B. 1850 Grimbergen 2/2676 ISSN-nummer 1783-4406 MIRA CetiCeti Periodieke uitgave van Volkssterrenwacht MIRA vzw Abdijstraat 22, 1850 Grimbergen - tel: 02 / 269 12 80 • Jaargang 14 nr 1 • Internet: http://www.mira.be/ - fax: 02 / 269 10 75 Verschijnt driemaandelijks:MIRA Ceti - januari januari -- maart 20102010 Verantwoordelijke uitgever: Felix Verbelen Afgiftekantoor: Grimbergen 1 Bosstraat 9, 1910 Kampenhout 1 NIEUW IN DE BIBILIOTHEEK Voor wie het nog niet mocht weten: MIRA is ook de trotse bezitter van een heus “Informatie– en documenta- tiecentrum”: één ruime leeszaal en één collectiezaal. De collectie omvat ondertussen meer dan 1500 uitleenbare werken (boeken vooral, maar ook video, cd-rom, dvd,…) en vele honderden ingebonden jaargangen van tijd- schriften. Er staat ook een pc ter beschikking waarop u niet enkel de collectie kan doorzoeken, dvd‟s raadple- gen, maar ook scannen en surfen op het internet. De MIRA-bib. is geopend elke woensdag (14-18h) en vrijdag (19-22h). Andere dagen kunnen ook, maar dan volgens afspraak. Men betaalt een éénmalige waarborg van 25 euro, maar voor de leden is de uitleen zelf gratis. ENKELE INTERESSANTE AANWINSTEN VAN DE LAATSTE MAANDEN • Boek; nr. 1852, categorie 800, Auteur: Sharpe, Michael ―Space. The ultimate frontier‖ Uitgeverij: TAJ Books, Cobham UK, 2006, ISBN: "978-1-84406-078-8 Groot, groter, grootst… Maar groter dan dit boek zal u alvast niet vinden: 60cm hoog, 40cm breed, 160 pagina‟s dik. Niet bruikbaar als bedliteratuur, maar wel schitterend als naslagwerk (als u een grote studeertafel heeft tenminste). Een héél uitvoerig geïllustreerd en zeer compleet overzicht van de ruimtevaart: alle missies tot eind 2005 worden stuk voor stuk besproken, ook de minder gekende testvluch- ten, met bij elke missie één of meerdere fraaie foto‟s. -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
Stars and Telescopes : a Resource Book for Teachers of Lower School Science
Edith Cowan University Research Online ECU Publications Pre. 2011 1981 Stars and telescopes : a resource book for teachers of lower school science Clifton L. Smith Follow this and additional works at: https://ro.ecu.edu.au/ecuworks Part of the Science and Mathematics Education Commons Smith, C. (1981). Stars and telescopes : a resource book for teachers of lower school science. Nedlands, Australia: Nedlands College of Advanced Education. This Book is posted at Research Online. https://ro.ecu.edu.au/ecuworks/7034 Edith Cowan University Copyright Warning You may print or download ONE copy of this document for the purpose of your own research or study. The University does not authorize you to copy, communicate or otherwise make available electronically to any other person any copyright material contained on this site. You are reminded of the following: Copyright owners are entitled to take legal action against persons who infringe their copyright. A reproduction of material that is protected by copyright may be a copyright infringement. Where the reproduction of such material is done without attribution of authorship, with false attribution of authorship or the authorship is treated in a derogatory manner, this may be a breach of the author’s moral rights contained in Part IX of the Copyright Act 1968 (Cth). Courts have the power to impose a wide range of civil and criminal sanctions for infringement of copyright, infringement of moral rights and other offences under the Copyright Act 1968 (Cth). Higher penalties may apply, and higher damages may be awarded, for offences and infringements involving the conversion of material into digital or electronic form. -
Physics Abstracts CLASSIFICATION and CONTENTS (PACC)
Physics Abstracts CLASSIFICATION AND CONTENTS (PACC) 0000 general 0100 communication, education, history, and philosophy 0110 announcements, news, and organizational activities 0110C announcements, news, and awards 0110F conferences, lectures, and institutes 0110H physics organizational activities 0130 physics literature and publications 0130B publications of lectures(advanced institutes, summer schools, etc.) 0130C conference proceedings 0130E monographs, and collections 0130K handbooks and dictionaries 0130L collections of physical data, tables 0130N textbooks 0130Q reports, dissertations, theses 0130R reviews and tutorial papers;resource letters 0130T bibliographies 0140 education 0140D course design and evaluation 0140E science in elementary and secondary school 0140G curricula, teaching methods,strategies, and evaluation 0140J teacher training 0150 educational aids(inc. equipment,experiments and teaching approaches to subjects) 0150F audio and visual aids, films 0150H instructional computer use 0150K testing theory and techniques 0150M demonstration experiments and apparatus 0150P laboratory experiments and apparatus 0150Q laboratory course design,organization, and evaluation 0150T buildings and facilities 0155 general physics 0160 biographical, historical, and personal notes 0165 history of science 0170 philosophy of science 0175 science and society 0190 other topics of general interest 0200 mathematical methods in physics 0210 algebra, set theory, and graph theory 0220 group theory(for algebraic methods in quantum mechanics, see -
The Brightest Stars Seite 1 Von 9
The Brightest Stars Seite 1 von 9 The Brightest Stars This is a list of the 300 brightest stars made using data from the Hipparcos catalogue. The stellar distances are only fairly accurate for stars well within 1000 light years. 1 2 3 4 5 6 7 8 9 10 11 12 13 No. Star Names Equatorial Galactic Spectral Vis Abs Prllx Err Dist Coordinates Coordinates Type Mag Mag ly RA Dec l° b° 1. Alpha Canis Majoris Sirius 06 45 -16.7 227.2 -8.9 A1V -1.44 1.45 379.21 1.58 9 2. Alpha Carinae Canopus 06 24 -52.7 261.2 -25.3 F0Ib -0.62 -5.53 10.43 0.53 310 3. Alpha Centauri Rigil Kentaurus 14 40 -60.8 315.8 -0.7 G2V+K1V -0.27 4.08 742.12 1.40 4 4. Alpha Boötis Arcturus 14 16 +19.2 15.2 +69.0 K2III -0.05 -0.31 88.85 0.74 37 5. Alpha Lyrae Vega 18 37 +38.8 67.5 +19.2 A0V 0.03 0.58 128.93 0.55 25 6. Alpha Aurigae Capella 05 17 +46.0 162.6 +4.6 G5III+G0III 0.08 -0.48 77.29 0.89 42 7. Beta Orionis Rigel 05 15 -8.2 209.3 -25.1 B8Ia 0.18 -6.69 4.22 0.81 770 8. Alpha Canis Minoris Procyon 07 39 +5.2 213.7 +13.0 F5IV-V 0.40 2.68 285.93 0.88 11 9. Alpha Eridani Achernar 01 38 -57.2 290.7 -58.8 B3V 0.45 -2.77 22.68 0.57 144 10. -
Spectropolarimetry As a Probe of Stellar Winds
Spectropolarimetry as a Probe of Stellar Winds Timothy James Harries Thesis submitted for the degree of Doctor of Philosophy in the Faculty of Science of the University of London. UCL Department of Physics & Astronomy U n iv e r s it y • C o l l e g e • L o n d o n February 1995 ProQuest Number: 10045605 All rights reserved INFORMATION TO ALL USERS The quality of this reproduction is dependent upon the quality of the copy submitted. In the unlikely event that the author did not send a complete manuscript and there are missing pages, these will be noted. Also, if material had to be removed, a note will indicate the deletion. uest. ProQuest 10045605 Published by ProQuest LLC(2016). Copyright of the Dissertation is held by the Author. All rights reserved. This work is protected against unauthorized copying under Title 17, United States Code. Microform Edition © ProQuest LLC. ProQuest LLC 789 East Eisenhower Parkway P.O. Box 1346 Ann Arbor, Ml 48106-1346 Abstract The use of spectropolarimetry as a diagnostic probe of stellar-wind structure is inves tigated by using high-quality observations and state-of-the-art analytical and numerical models. The winds of late-type giant stars are studied through the highly polarized 6830Â and 7088Â Raman-scattered emission hnes that are observed in many symbiotic systems. A spectropolarimetric survey of 28 symbiotic stars is presented. A Monte-Carlo code is developed in order to aid interpretation of the hnes and the parameter sensitivity of the Raman hne polarization spectrum is investigated. -
Stars and Their Spectra: an Introduction to the Spectral Sequence Second Edition James B
Cambridge University Press 978-0-521-89954-3 - Stars and Their Spectra: An Introduction to the Spectral Sequence Second Edition James B. Kaler Index More information Star index Stars are arranged by the Latin genitive of their constellation of residence, with other star names interspersed alphabetically. Within a constellation, Bayer Greek letters are given first, followed by Roman letters, Flamsteed numbers, variable stars arranged in traditional order (see Section 1.11), and then other names that take on genitive form. Stellar spectra are indicated by an asterisk. The best-known proper names have priority over their Greek-letter names. Spectra of the Sun and of nebulae are included as well. Abell 21 nucleus, see a Aurigae, see Capella Abell 78 nucleus, 327* ε Aurigae, 178, 186 Achernar, 9, 243, 264, 274 z Aurigae, 177, 186 Acrux, see Alpha Crucis Z Aurigae, 186, 269* Adhara, see Epsilon Canis Majoris AB Aurigae, 255 Albireo, 26 Alcor, 26, 177, 241, 243, 272* Barnard’s Star, 129–130, 131 Aldebaran, 9, 27, 80*, 163, 165 Betelgeuse, 2, 9, 16, 18, 20, 73, 74*, 79, Algol, 20, 26, 176–177, 271*, 333, 366 80*, 88, 104–105, 106*, 110*, 113, Altair, 9, 236, 241, 250 115, 118, 122, 187, 216, 264 a Andromedae, 273, 273* image of, 114 b Andromedae, 164 BDþ284211, 285* g Andromedae, 26 Bl 253* u Andromedae A, 218* a Boo¨tis, see Arcturus u Andromedae B, 109* g Boo¨tis, 243 Z Andromedae, 337 Z Boo¨tis, 185 Antares, 10, 73, 104–105, 113, 115, 118, l Boo¨tis, 254, 280, 314 122, 174* s Boo¨tis, 218* 53 Aquarii A, 195 53 Aquarii B, 195 T Camelopardalis, -
Annual Report / Rapport Annuel / Jahresbericht 1996
Annual Report / Rapport annuel / Jahresbericht 1996 ✦ ✦ ✦ E U R O P E A N S O U T H E R N O B S E R V A T O R Y ES O✦ 99 COVER COUVERTURE UMSCHLAG Beta Pictoris, as observed in scattered light Beta Pictoris, observée en lumière diffusée Beta Pictoris, im Streulicht bei 1,25 µm (J- at 1.25 microns (J band) with the ESO à 1,25 microns (bande J) avec le système Band) beobachtet mit dem adaptiven opti- ADONIS adaptive optics system at the 3.6-m d’optique adaptative de l’ESO, ADONIS, au schen System ADONIS am ESO-3,6-m-Tele- telescope and the Observatoire de Grenoble télescope de 3,60 m et le coronographe de skop und dem Koronographen des Obser- coronograph. l’observatoire de Grenoble. vatoriums von Grenoble. The combination of high angular resolution La combinaison de haute résolution angu- Die Kombination von hoher Winkelauflö- (0.12 arcsec) and high dynamical range laire (0,12 arcsec) et de gamme dynamique sung (0,12 Bogensekunden) und hohem dy- (105) allows to image the disk to only 24 AU élevée (105) permet de reproduire le disque namischen Bereich (105) erlaubt es, die from the star. Inside 50 AU, the main plane jusqu’à seulement 24 UA de l’étoile. A Scheibe bis zu einem Abstand von nur 24 AE of the disk is inclined with respect to the l’intérieur de 50 UA, le plan principal du vom Stern abzubilden. Innerhalb von 50 AE outer part. Observers: J.-L. Beuzit, A.-M. -
Atlas Menor Was Objects to Slowly Change Over Time
C h a r t Atlas Charts s O b by j Objects e c t Constellation s Objects by Number 64 Objects by Type 71 Objects by Name 76 Messier Objects 78 Caldwell Objects 81 Orion & Stars by Name 84 Lepus, circa , Brightest Stars 86 1720 , Closest Stars 87 Mythology 88 Bimonthly Sky Charts 92 Meteor Showers 105 Sun, Moon and Planets 106 Observing Considerations 113 Expanded Glossary 115 Th e 88 Constellations, plus 126 Chart Reference BACK PAGE Introduction he night sky was charted by western civilization a few thou - N 1,370 deep sky objects and 360 double stars (two stars—one sands years ago to bring order to the random splatter of stars, often orbits the other) plotted with observing information for T and in the hopes, as a piece of the puzzle, to help “understand” every object. the forces of nature. The stars and their constellations were imbued with N Inclusion of many “famous” celestial objects, even though the beliefs of those times, which have become mythology. they are beyond the reach of a 6 to 8-inch diameter telescope. The oldest known celestial atlas is in the book, Almagest , by N Expanded glossary to define and/or explain terms and Claudius Ptolemy, a Greco-Egyptian with Roman citizenship who lived concepts. in Alexandria from 90 to 160 AD. The Almagest is the earliest surviving astronomical treatise—a 600-page tome. The star charts are in tabular N Black stars on a white background, a preferred format for star form, by constellation, and the locations of the stars are described by charts. -
Curriculum Vitae Stephan Robert Mccandliss
August 2015 Curriculum Vitae Stephan Robert McCandliss Research Professor - JHU [email protected] Johns Hopkins University tel: 410-516-5272 Department of Physics & Astronomy fax: 410-516-8260 Baltimore, Maryland 21218 http://www.pha.jhu.edu/~stephan Familial History 1955/09/07 Born Salinas California 1989/01/01 Married Ann Marie McCandliss (nee Selander) 1989/11/10 Daughter Rachel Pearl McCandliss 1992/05/26 Son Ian Frederick McCandliss Education 1988 Ph.D. Astrophysics University of Colorado, Boulder 1981 B.S. Physics University of Washington, Seattle 1981 B.S. Astronomy University of Washington, Seattle Work History 2015 – present Director, Center for Astrophysical Sciences Johns Hopkins University 2010 – present Research Professor Johns Hopkins University 2002 – 2010 Principal Research Scientist Johns Hopkins University 1994 – 2002 Research Scientist Johns Hopkins University 1988 – 1994 Associate Research Scientist Johns Hopkins University 1981 – 1988 Ph.D. Candidate University of Colorado, Boulder 1977 – 1981 Reader and Lab Assistant University of Washington, Seattle Primary Research Interests The ionization history of the universe. Spectral signatures of dust, molecules and atoms in astrophysical environments. Rapid-response space science missions and enabling low-cost access to space. Space-based astronomical instrumentation. Service 2013 HST Cycle 21 Proposal Review Panel 2011 NASA APRA/SAT UV/Vis Review Panel Chair 2011 NSF Astronomy Advanced Technology and Instrumentation Opt/IR Panel 2008 – present Astrophysics Sounding Rocket -
CHEMICAL and KINEMATIC ANALYSIS of CN-STRONG METAL-POOR FIELD STARS in LAMOST DR3 Baitian Tang1, Chao Liu2, J
Draft version December 6, 2018 Preprint typeset using LATEX style emulateapj v. 12/16/11 CHEMICAL AND KINEMATIC ANALYSIS OF CN-STRONG METAL-POOR FIELD STARS IN LAMOST DR3 Baitian Tang1, Chao Liu2, J. G. Fernandez-Trincado´ 3,4,11, Doug Geisler3,5,6, Jianrong Shi2, Olga Zamora7,8, Guy Worthey9, and Edmundo Moreno10 1School of Physics and Astronomy, Sun Yat-sen University, Zhuhai 519082, China; [email protected] 2Key Lab of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China 3Departamento de Astronom´ıa,Casilla 160-C, Universidad de Concepci´on,Concepci´on,Chile 4Institut Utinam, CNRS UMR 6213, Universit´eBourgogne-Franche-Comt´e,OSU THETA Franche-Comt´e,Observatoire de Besan¸con, BP 1615, 25010 Besan¸conCedex, France 5Instituto de Investigaci´onMultidisciplinario en Ciencia y Tecnologa, Universidad de La Serena. Avenida Ra´ulBitr´anS/N, La Serena, Chile 6Departamento de F´ısica y Astronom´ıa, Facultad de Ciencias, Universidad de La Serena. Av. Juan Cisternas 1200, La Serena, Chile 7Instituto de Astrof´ısicade Canarias, 38205 La Laguna, Tenerife, Spain 8Departamento de Astrof´ısica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain 9Department of Physics and Astronomy, Washington State University, Pullman, WA 99163-2814, USA 10Instituto de Astronom´ıa,Universidad Nacional Aut´onomade M´exico,Apdo. Postal 70264, M´exicoD.F., 04510, M´exicoand 11Instituto de Astronom´ıay Ciencias Planetarias, Universidad de Atacama, Copayapu 485, Copiap´o,Chile. Draft version December 6, 2018 ABSTRACT The large amount of chemical and kinematic information available in large spectroscopic surveys have inspired the search for chemically peculiar stars in the field.