XIII Annual SOCHIAS Meeting__
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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. -
FY08 Technical Papers by GSMTPO Staff
AURA/NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation July 23, 2008 Revised as Complete and Submitted December 23, 2008 NGC 660, ~13 Mpc from the Earth, is a peculiar, polar ring galaxy that resulted from two galaxies colliding. It consists of a nearly edge-on disk and a strongly warped outer disk. Image Credit: T.A. Rector/University of Alaska, Anchorage NATIONAL OPTICAL ASTRONOMY OBSERVATORY NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation December 23, 2008 TABLE OF CONTENTS EXECUTIVE SUMMARY ............................................................................................................................. 1 1 SCIENTIFIC ACTIVITIES AND FINDINGS ..................................................................................... 2 1.1 Cerro Tololo Inter-American Observatory...................................................................................... 2 The Once and Future Supernova η Carinae...................................................................................................... 2 A Stellar Merger and a Missing White Dwarf.................................................................................................. 3 Imaging the COSMOS...................................................................................................................................... 3 The Hubble Constant from a Gravitational Lens.............................................................................................. 4 A New Dwarf Nova in the Period Gap............................................................................................................ -
Star Formation and Galaxy Evolution of the Local Universe Based on HIPASS
Star formation and galaxy evolution of the Local Universe based on HIPASS Oiwei Ivy Wong Submitted in total fulfilment of the requirements of the Degree of Doctor of Philosophy School of Physics University of Melbourne December, 2007 Abstract This thesis investigates the star formation and galaxy evolution of the nearby Local Volume based on Neutral Hydrogen (HI) studies. A large portion of this thesis con- sists of work with the Northern extension of the HI Parkes All Sky Survey (HIPASS). HIPASS is an HI survey of the entire Southern sky up to a declination of +25.5 de- grees (including the Northern extension) using the Parkes 64-metre radio telescope. I have also produced a catalogue of the optical counterparts corresponding to the galaxies found in Northern HIPASS. From this optical catalogue, we also conclude that we did not find any isolated dark galaxies. The other half of my thesis consists of work with the SINGG and SUNGG projects. SINGG is the Survey for Ioniza- tion in Neutral Gas Galaxies and SUNGG is the Survey of Ultraviolet emission in Neutral Gas Galaxies. Both SINGG and SUNGG are selected from HIPASS and are star formation studies in the H-alpha and ultraviolet (UV), respectively. My work in the SINGG-SUNGG collaboration is mostly based on SUNGG. Using the results of SUNGG, I measured the local luminosity density and the cosmic star formation rate density (SFRD) of the Local Universe. Using far-infrared (FIR) observations from IRAS, the FIR luminosity density was also calculated. Combining the FUV luminosity density and the FIR luminosity density, the bolometric SFRD of the Lo- cal Universe was estimated. -
The Detection of 13CO and Other Apparent Abundance Anomalies In
The Detection of 13CO and Other Apparent Abundance Anomalies in the Secondary Stars of Long-Period Cataclysmic Variables Thomas E. Harrison1,2, Heather L. Osborne2 Department of Astronomy New Mexico State University, Box 30001, MSC 4500, Las Cruces, NM 88003-8001 Steve B. Howell WIYN Observatory and National Optical Astronomy Observatories, 950 North Cherry Avenue, Tucson, AZ 85726 Accepted for publication in the Astronomical Journal on 18 February, 2004 1Visiting Astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. 2Visiting Astronomer at the Infrared Telescope Facility, which is operated by the University arXiv:astro-ph/0402470v1 19 Feb 2004 of Hawaii under contract from the National Aeronautics and Space Administration. Subject headings: cataclysmic variablesstars: infrared spectrastars: individual (V442 Centauri, SY Cancri, RU Pegasi, CH Ursae Majoris, MU Centauri, TT Crateris, AC Cancri, EM Cygni, V426 Ophiuchi, SS Cygni, BV Puppis, AH Herculis) Received ; accepted –2– ABSTRACT We present moderate resolution (R ≥ 1,800) infrared K-band spectra of twelve long-period (Porb ≥ 6 hr) cataclysmic variables. We detect absorption lines from the photospheres of the secondary stars in every system, even though two of them were undergoing outbursts. We have attempted to assign spectral types to each of the secondary stars, and these classifications are generally consistent with previous determinations/estimates. We find evidence for abundance anomalies that include enhancements and/or deficits for all of the species commonly found in K-band spectra of G- and K-type dwarfs. -
Dynamics and Mass of the Shapley Supercluster, the Largest Bound Structure in the Local Universe A
mega-telescopes and their IR instru- modern techniques such as radial ve- such systems with evolutionary models mentation it will be possible to in- locities, planetary occultations (transits) of our own solar system. vestigate the physical characteristics and micro-lensing. Once ALMA is avail- of these objects, particularly those in able we will be able to undertake mo- The present article could not have orbit around nearby stars which will al- lecular line observations of the atmos- been written without the contribution of low us to obtain their masses. ALMA pheres of planets and other bodies the FONDAP Centre of Excellence will be a perfect instrument for the fol- which will give new knowledge of plan- Director, Guido Garay, and of its P.I. low-up studies of brown dwarfs found in etary “weather”, the structure of atmos- Members. I thankfully acknowledge the these studies. pheric wind and the variations in chem- contribution from M.T. Ruiz, Director of • Extrasolar planets and proto-plane- ical constituents. Studies of proto-plan- the Astronomy Department at Universi- tary disks. – One of the great appeals etary disks will be carried out using the dad de Chile; L. Infante, Chairman of of astronomy is undoubtedly its poten- recently available IR facilities. ALMA, the Pontificia Universidad Católica de tial to help us understand the origin of with its sensitivity and resolving power, Chile Department of Astronomy and our planet. The Centre will foster the will be the ideal instrument to provide Astrophysics; W. Gieren, Head of the development of the area of planetary definite answers regarding the forma- Astronomy Group at the Universidad de science, currently non-existent in the tion and evolution of proto-planetary Concepción Physics Department; L. -
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. -
Be Stars Seen by Space Photometry
Be Stars Seen by Space Photometry Thomas Rivinius1, Dietrich Baade2 and Alex C. Carciofi3 1. ESO | European Organisation for Astronomical Research in the Southern Hemisphere, Casilla 19001, Santiago 19, Chile 2. ESO | European Organisation for Astronomical Research in the Southern Hemisphere, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 3. Instituto de Astronomia, Geof´ısica e Ci^encias Atmosf´ericas, Universidade de S~ao Paulo, 05508-900, S~ao Paulo, SP, Brazil Classical Be stars are introduced as object class and their particular potential for space based photometry is highlighted. A brief summary of the various types of variability observed in Be stars makes clear that an interpretation of every single frequency as a pulsation mode falls short, instead there are as well purely circumstellar variations and those that originate in the immediate stellar to cir- cumstellar interaction region. In particular the latter offer great potential, as they are linked to one of the few remaining great riddles of Be stars, namely how they feed their disks. 1 Introduction The class of Be stars is simply defined as those non-supergiant B stars that at least once have shown Balmer line emission (see Rivinius et al., 2013, for a review). While this definition is very valuable for bulk classification of stars for which no high quality data is available, e.g., in the Magellanic Clouds, it is also very broad: Any circumstellar gas close to a B star and above some threshold density will produce line emission. In an attempt at a taxonomy that reflects our knowledge on how the gas was put and is kept close to the star (e.g., magnetically confined, an accretion disk, or a decretion disk), the class was subdivided. -
Astrophysical Plasma Modeling of the Hot Universe
Astrophysical plasma modeling of the hot Universe Advances and challenges in high-resolution X-ray spectroscopy Astrophysical plasma modeling of the hot Universe Advances and challenges in high-resolution X-ray spectroscopy Proefschrift ter verkrijging van de graad van Doctor aan de Universiteit Leiden, op gezag van de Rector Magnificus prof. mr. C. J. J. M. Stolker, volgens besluit van het College voor Promoties te verdedigen op donderdag 7 juni 2018 klokke 10:00 uur door Junjie Mao geboren te Ningbo, China in 1988 Promotiecommissie: Promotor: Prof. dr. J. S. Kaastra Co-promotor: Dr. J. de Plaa (SRON) Overige leden: Prof. dr. H. Röttgering Prof. dr. J. Schaye Prof. dr. W. R. Jaffe Prof. dr. G. Branduardi-Raymont (University College London) Prof. dr. F. B. S. Paerels (Columbia University) To Lilan our active family nucleus with her inflows and outflows © 2018 Junjie Mao Cover design by Junjie Mao Image credit: Adobe Spark Contents 1 Introduction 1 1.1 Hot astrophysical plasmas in X-rays . 2 1.2 Active Galactic Nuclei and circumnuclear media . 3 1.3 Intracluster media and chemical enrichment . 9 1.4 Plasma code and atomic data . 13 1.5 This thesis . 15 References. 18 2 Parameterization of the level-resolved radiative recombination rate coefficients for the SPEX code 21 2.1 Introduction . 22 2.2 Historical background . 22 2.3 RR rate coefficients for H-like ions . 25 2.3.1 Photoionization cross sections . 25 2.3.2 Radiative recombination data . 26 2.4 RR rate coefficients for He-like to Na-like ions. 26 2.5 Fitting strategy . -
Observational Cosmology - 30H Course 218.163.109.230 Et Al
Observational cosmology - 30h course 218.163.109.230 et al. (2004–2014) PDF generated using the open source mwlib toolkit. See http://code.pediapress.com/ for more information. PDF generated at: Thu, 31 Oct 2013 03:42:03 UTC Contents Articles Observational cosmology 1 Observations: expansion, nucleosynthesis, CMB 5 Redshift 5 Hubble's law 19 Metric expansion of space 29 Big Bang nucleosynthesis 41 Cosmic microwave background 47 Hot big bang model 58 Friedmann equations 58 Friedmann–Lemaître–Robertson–Walker metric 62 Distance measures (cosmology) 68 Observations: up to 10 Gpc/h 71 Observable universe 71 Structure formation 82 Galaxy formation and evolution 88 Quasar 93 Active galactic nucleus 99 Galaxy filament 106 Phenomenological model: LambdaCDM + MOND 111 Lambda-CDM model 111 Inflation (cosmology) 116 Modified Newtonian dynamics 129 Towards a physical model 137 Shape of the universe 137 Inhomogeneous cosmology 143 Back-reaction 144 References Article Sources and Contributors 145 Image Sources, Licenses and Contributors 148 Article Licenses License 150 Observational cosmology 1 Observational cosmology Observational cosmology is the study of the structure, the evolution and the origin of the universe through observation, using instruments such as telescopes and cosmic ray detectors. Early observations The science of physical cosmology as it is practiced today had its subject material defined in the years following the Shapley-Curtis debate when it was determined that the universe had a larger scale than the Milky Way galaxy. This was precipitated by observations that established the size and the dynamics of the cosmos that could be explained by Einstein's General Theory of Relativity. -
The 13Th HEAD Program Book
13th Meeting of the High Energy Astrophysics Division Program Book Monterey CA 7-11 April 2013 13th Meeting of the American Astronomical Society’s High Energy Astrophysics Division (HEAD) 7-11 April 2013 Monterey, California Scientific sessions will be held at the: Portola Hotel and Spa 2 Portola Plaza ATTENDEE Monterey, CA 93940 SERVICES.......... 4 HEAD Paper Sorters SCHEDULE......... 6 Keith Arnaud Joshua Bloom MONDAY............ 12 Joel Bregman Paolo Coppi Rosanne Di Stefano POSTERS........... 17 Daryl Haggard Chryssa Kouveliotou TUESDAY........... 43 Henric Krawczynski Stephen Reynolds WEDNESDAY...... 48 Randall Smith Jan Vrtilek THURSDAY......... 52 Nicholas White AUTHOR INDEX.. 56 Session Numbering Key 100’s Monday and posters NASA PCOS X-RAY SAG 200’s Tuesday 300’s Wednesday HEAD DISSERTATIONS 400’s Thursday Please Note: All posters are displayed Monday-Thursday. Current HEAD Officers Current HEAD Committee Joel Bregman Chair Daryl Haggard 2013-2016 Nicholas White Vice-Chair Henric Krawczynski 2013-2016 Randall Smith Secretary Rosanne DiStefano 2011-2014 Keith Arnaud Treasurer Stephen Reynolds 2011-2014 Megan Watzke Press Officer Jan Vrtilek 2011-2014 Chryssa Kouveliotou Past Chair Joshua Bloom 2012-2015 Paolo Coppi 2012-2015 1 2 Peter B’s Entrance Cottonwood Plaza Jacks Restaurant Brew Pub s p o h S Cottonwood Bonsai III e Lower Atrium Bonsai II ung Restrooms o e nc cks L Ironwood Redwood Bonsai I a a J Entr Elevators Elevators a l o rt o P Restrooms s De Anza De Anza p Ballroom II-III Ballroom I o De Anza Sh Foyer Upper Atrium Entrance OOMS R Entrance BONZAI Entrance De ANZA BALLROOM FA ELEVATORS TO BONZAI ROOMS Y B OB L TEL O General eANZA D A H O Z T Session ANCE R OLA PLA T ENT R PO FA FA STORAGE A UP F ENTRANCE TO 3 De ANZA FOYER ATTENDEE SERVICES Registration De Anza Foyer Sunday: 1:00pm-7:00pm Monday-Wednesday: 7:30am-6:00pm Thursday: 8:00am-5:00pm Poster Viewing Monday-Wednesday: 7:30am-6:45pm Thursday: 7:30am-5:00pm Please do not leave personal items unattended. -
Orders of Magnitude (Length) - Wikipedia
03/08/2018 Orders of magnitude (length) - Wikipedia Orders of magnitude (length) The following are examples of orders of magnitude for different lengths. Contents Overview Detailed list Subatomic Atomic to cellular Cellular to human scale Human to astronomical scale Astronomical less than 10 yoctometres 10 yoctometres 100 yoctometres 1 zeptometre 10 zeptometres 100 zeptometres 1 attometre 10 attometres 100 attometres 1 femtometre 10 femtometres 100 femtometres 1 picometre 10 picometres 100 picometres 1 nanometre 10 nanometres 100 nanometres 1 micrometre 10 micrometres 100 micrometres 1 millimetre 1 centimetre 1 decimetre Conversions Wavelengths Human-defined scales and structures Nature Astronomical 1 metre Conversions https://en.wikipedia.org/wiki/Orders_of_magnitude_(length) 1/44 03/08/2018 Orders of magnitude (length) - Wikipedia Human-defined scales and structures Sports Nature Astronomical 1 decametre Conversions Human-defined scales and structures Sports Nature Astronomical 1 hectometre Conversions Human-defined scales and structures Sports Nature Astronomical 1 kilometre Conversions Human-defined scales and structures Geographical Astronomical 10 kilometres Conversions Sports Human-defined scales and structures Geographical Astronomical 100 kilometres Conversions Human-defined scales and structures Geographical Astronomical 1 megametre Conversions Human-defined scales and structures Sports Geographical Astronomical 10 megametres Conversions Human-defined scales and structures Geographical Astronomical 100 megametres 1 gigametre -
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