July Newsletter.Pub
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
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. -
Fy10 Budget by Program
AURA/NOAO FISCAL YEAR ANNUAL REPORT FY 2010 Revised Submitted to the National Science Foundation March 16, 2011 This image, aimed toward the southern celestial pole atop the CTIO Blanco 4-m telescope, shows the Large and Small Magellanic Clouds, the Milky Way (Carinae Region) and the Coal Sack (dark area, close to the Southern Crux). The 33 “written” on the Schmidt Telescope dome using a green laser pointer during the two-minute exposure commemorates the rescue effort of 33 miners trapped for 69 days almost 700 m underground in the San Jose mine in northern Chile. The image was taken while the rescue was in progress on 13 October 2010, at 3:30 am Chilean Daylight Saving time. Image Credit: Arturo Gomez/CTIO/NOAO/AURA/NSF National Optical Astronomy Observatory Fiscal Year Annual Report for FY 2010 Revised (October 1, 2009 – September 30, 2010) Submitted to the National Science Foundation Pursuant to Cooperative Support Agreement No. AST-0950945 March 16, 2011 Table of Contents MISSION SYNOPSIS ............................................................................................................ IV 1 EXECUTIVE SUMMARY ................................................................................................ 1 2 NOAO ACCOMPLISHMENTS ....................................................................................... 2 2.1 Achievements ..................................................................................................... 2 2.2 Status of Vision and Goals ................................................................................ -
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). -
Instrumental Methods for Professional and Amateur
Instrumental Methods for Professional and Amateur Collaborations in Planetary Astronomy Olivier Mousis, Ricardo Hueso, Jean-Philippe Beaulieu, Sylvain Bouley, Benoît Carry, Francois Colas, Alain Klotz, Christophe Pellier, Jean-Marc Petit, Philippe Rousselot, et al. To cite this version: Olivier Mousis, Ricardo Hueso, Jean-Philippe Beaulieu, Sylvain Bouley, Benoît Carry, et al.. Instru- mental Methods for Professional and Amateur Collaborations in Planetary Astronomy. Experimental Astronomy, Springer Link, 2014, 38 (1-2), pp.91-191. 10.1007/s10686-014-9379-0. hal-00833466 HAL Id: hal-00833466 https://hal.archives-ouvertes.fr/hal-00833466 Submitted on 3 Jun 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Instrumental Methods for Professional and Amateur Collaborations in Planetary Astronomy O. Mousis, R. Hueso, J.-P. Beaulieu, S. Bouley, B. Carry, F. Colas, A. Klotz, C. Pellier, J.-M. Petit, P. Rousselot, M. Ali-Dib, W. Beisker, M. Birlan, C. Buil, A. Delsanti, E. Frappa, H. B. Hammel, A.-C. Levasseur-Regourd, G. S. Orton, A. Sanchez-Lavega,´ A. Santerne, P. Tanga, J. Vaubaillon, B. Zanda, D. Baratoux, T. Bohm,¨ V. Boudon, A. Bouquet, L. Buzzi, J.-L. Dauvergne, A. -
Variable Star Classification and Light Curves Manual
Variable Star Classification and Light Curves An AAVSO course for the Carolyn Hurless Online Institute for Continuing Education in Astronomy (CHOICE) This is copyrighted material meant only for official enrollees in this online course. Do not share this document with others. Please do not quote from it without prior permission from the AAVSO. Table of Contents Course Description and Requirements for Completion Chapter One- 1. Introduction . What are variable stars? . The first known variable stars 2. Variable Star Names . Constellation names . Greek letters (Bayer letters) . GCVS naming scheme . Other naming conventions . Naming variable star types 3. The Main Types of variability Extrinsic . Eclipsing . Rotating . Microlensing Intrinsic . Pulsating . Eruptive . Cataclysmic . X-Ray 4. The Variability Tree Chapter Two- 1. Rotating Variables . The Sun . BY Dra stars . RS CVn stars . Rotating ellipsoidal variables 2. Eclipsing Variables . EA . EB . EW . EP . Roche Lobes 1 Chapter Three- 1. Pulsating Variables . Classical Cepheids . Type II Cepheids . RV Tau stars . Delta Sct stars . RR Lyr stars . Miras . Semi-regular stars 2. Eruptive Variables . Young Stellar Objects . T Tau stars . FUOrs . EXOrs . UXOrs . UV Cet stars . Gamma Cas stars . S Dor stars . R CrB stars Chapter Four- 1. Cataclysmic Variables . Dwarf Novae . Novae . Recurrent Novae . Magnetic CVs . Symbiotic Variables . Supernovae 2. Other Variables . Gamma-Ray Bursters . Active Galactic Nuclei 2 Course Description and Requirements for Completion This course is an overview of the types of variable stars most commonly observed by AAVSO observers. We discuss the physical processes behind what makes each type variable and how this is demonstrated in their light curves. Variable star names and nomenclature are placed in a historical context to aid in understanding today’s classification scheme. -
Publications Et Communications De Florentin Millour (Février 2016) H-Index 21, Total : 130 Publications Dont 53 À Comité De Lecture
Publications et communications de Florentin Millour (Février 2016) h-index 21, total : 130 publications dont 53 à comité de lecture. Articles dans des revues à comité de lecture, thèse 2015 1. Mourard, D., ..., Millour, F. ; et al., . (2015, A&A, 577, 51) Spectral and spatial imaging of the Be+sdO binary Phi Persei 2014 2. Chesneau, O. ; Millour, F. ; de Marco, O. et al., . (2014, A&A, 569, 3) V838 Monocerotis : the central star and its environment a decade after outburst 3. Chesneau, O. ; Millour, F. ; de Marco, O. et al., . (2014, A&A, 569, 4) The RCB star V854 Centauri is surrounded by a hot dusty shell 4. Chesneau, O. ; Meilland, A. ; Chapellier, E. ; Millour, F. ; et al., . (2014, A&A, 563, A71) The yellow hypergiant HR 5171 A : Resolving a massive interacting binary in the common envelope phase. 5. Domiciano de Souza, A. ; Kervella, P. ; Moser Faes, D. et al. (2014, A&A, 569, 10) The environment of the fast rotating star Achernar. III. Photospheric parameters revealed by the VLTI 6. Hadjara, M. ; Domiciano de Souza, A. ; Vakili, F. et al. (2014, A&A, 569, 45) Beyond the diraction limit of optical/IR interferometers. II. Stellar parameters of rotating stars from dierential phases 7. Schutz, A. ; Vannier, M. ; Mary, D. et al. (2014, A&A, 565, 88) Statistical characterisation of polychromatic absolute and dierential squared visibilities obtained from AMBER/VLTI instrument 2013 8. Millour, F. ; Meilland, A. ; Stee, P. & Chesneau, O. (2013, LNP, 857, 149) Interactions in Massive Binary Stars as Seen by Interferometry 9. Stee, P. ; Meilland, A. -
Antike Beobachtungen Farbiger Sterne
Abhandlungen der Königlich Bayerischen Akademie der Wissenschaften Philosophisch - philologische und historische Klasse XXX. Band, 1. Abhandlung Antike Beobachtungen farbiger Sterne von Franz Boll Mit einem Beitrag von Carl Bezold , Vorgelegt am 1. Juli 1916 München 1916 Verlag der Königlich Bayerischen Akademie der Wissenschaften in Kommission des G. Franz'schen Verlags (J. Roth) ,. j / Einleitung. Die Geschichte der antiken Astronomie beruhte bis gegen den Ausgang des vorigen Jahrhunderts auf einer Anzahl von griechischen und einigen römischen Schriftstellern, unter denen Claudius Ptolemäus mit seiner "GroElen Syntaxis" als der letzten und um- fassendsten Kodifizierung des antiken Wissens vom Sternhimmel den ersten Platz einnimmt. Auf dem Almagest fuElten einst Delambre und fast drei Menschenalter später Tannery bei ihren Gesamtdarstellungen 1). Es ist klar, daEl mit diesen Quellen auch eine ganz bestimmte Auswahl und Abgrenzung des Stoffes notwendig gegeben war. Nur neues Material konnte aus diesem Bann herausführen. Das hat sich in den letzten zwei Jahrzehnten aus zwei verschiedenen Quellen unerwartet reich eingestellt. Die babylonischen 'rafein, so sporadisch sie immer noch geblieben sind, und so schwierig oft ihre Verwertung ist, geben gute Hoffnung, einmal zu einer von vorgefaElter Meinung nach beiden Seiten unabhängigen Vorstellung von den sachlichen Unterlagen des ionischen Weltbildes im 6. und 5. Jahr- hundert zu gelangen; und die Erforschung der griechischen astrologischen Handschriften, deren überwiegender Teil zum Glück vor -
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. -
Culmination of a Constellation
Culmination of a Constellation Over any night, stars and constellations in the sky will appear to move from east to west due to the Earth’s rotation on its axis. A constellation will culminate (reach its highest point in the sky for your location) when it centres on the meridian - an imaginary line that runs across the sky from north to south and also passes through the zenith (the point high in the sky directly above your head). For example: When to Observe Constellations The taBle shows the approximate time (AEST) constellations will culminate around the middle (15th day) of each month. Constellations will culminate 2 hours earlier for each successive month. Note: add an hour to the given time when daylight saving time is in effect. The time “12” is midnight. Sunrise/sunset times are rounded off to the nearest half an hour. Sun- Jan Feb Mar Apr May Jun Jul Aug Sep Oct Nov Dec Rise 5am 5:30 6am 6am 7am 7am 7am 6:30 6am 5am 4:30 4:30 Set 7pm 6:30 6pm 5:30 5pm 5pm 5pm 5:30 6pm 6pm 6:30 7pm And 5am 3am 1am 11pm 9pm Aqr 5am 3am 1am 11pm 9pm Aql 4am 2am 12 10pm 8pm Ara 4am 2am 12 10pm 8pm Ari 5am 3am 1am 11pm 9pm Aur 10pm 8pm 4am 2am 12 Boo 3am 1am 11pm 9pm 7pm Cnc 1am 11pm 9pm 7pm 3am CVn 3am 1am 11pm 9pm 7pm CMa 11pm 9pm 7pm 3am 1am Cap 5am 3am 1am 11pm 9pm 7pm Car 2am 12 10pm 8pm 6pm Cen 4am 2am 12 10pm 8pm 6pm Cet 4am 2am 12 10pm 8pm Cha 3am 1am 11pm 9pm 7pm Col 10pm 8pm 4am 2am 12 Com 3am 1am 11pm 9pm 7pm CrA 3am 1am 11pm 9pm 7pm CrB 4am 2am 12 10pm 8pm Crv 3am 1am 11pm 9pm 7pm Cru 3am 1am 11pm 9pm 7pm Cyg 5am 3am 1am 11pm 9pm 7pm Del -
Pulsating Components in Binary and Multiple Stellar Systems---A
Research in Astron. & Astrophys. Vol.15 (2015) No.?, 000–000 (Last modified: — December 6, 2014; 10:26 ) Research in Astronomy and Astrophysics Pulsating Components in Binary and Multiple Stellar Systems — A Catalog of Oscillating Binaries ∗ A.-Y. Zhou National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; [email protected] Abstract We present an up-to-date catalog of pulsating binaries, i.e. the binary and multiple stellar systems containing pulsating components, along with a statistics on them. Compared to the earlier compilation by Soydugan et al.(2006a) of 25 δ Scuti-type ‘oscillating Algol-type eclipsing binaries’ (oEA), the recent col- lection of 74 oEA by Liakos et al.(2012), and the collection of Cepheids in binaries by Szabados (2003a), the numbers and types of pulsating variables in binaries are now extended. The total numbers of pulsating binary/multiple stellar systems have increased to be 515 as of 2014 October 26, among which 262+ are oscillating eclipsing binaries and the oEA containing δ Scuti componentsare updated to be 96. The catalog is intended to be a collection of various pulsating binary stars across the Hertzsprung-Russell diagram. We reviewed the open questions, advances and prospects connecting pulsation/oscillation and binarity. The observational implication of binary systems with pulsating components, to stellar evolution theories is also addressed. In addition, we have searched the Simbad database for candidate pulsating binaries. As a result, 322 candidates were extracted. Furthermore, a brief statistics on Algol-type eclipsing binaries (EA) based on the existing catalogs is given. We got 5315 EA, of which there are 904 EA with spectral types A and F. -
Gum 48D: an Evolved HII Region with Ongoing Star Formation
Gum 48d: an evolved HII region with ongoing star formation J.L. Karr Academia Sinica Institute of Astronomy and Astrophysics, Taipei, Taiwan, ROC P. Manoj Department of Physics and Astronomy, University of Rochester, NY N. Ohashi Academia Sinica Institute of Astronomy and Astrophysics, Taipei, Taiwan, ROC ABSTRACT High mass star formation and the evolution of HII regions have a substantial impact on the morphology and star formation history of molecular clouds. The HII region Gum 48d, located in the Centaurus Arm at a distance of 3.5 kpc, is an old, well evolved HII region whose ionizing stars have moved off the main sequence. As such, it represents a phase in the evolution of HII regions that is less well studied than the earlier, more energetic, main sequence phase. In this paper we use multi-wavelength archive data from a variety of sources to perform a detailed study of this interesting region. Morphologically, Gum 48d displays a ring-like faint HII region associated with diffuse emission from the associated PDR, and is formed from part of a large, massive molecular cloud complex. There is extensive ongoing star formation in the region, at scales ranging from low to high mass, which is consistent with triggered star formation scenarios. We investigate the dynamical history and evolution of this region, and conclude that arXiv:0903.0934v1 [astro-ph.GA] 5 Mar 2009 the original HII region was once larger and more energetic than the faint region currently seen. The proposed history of this molecular cloud complex is one of multiple, linked generations of star formation, over a period of 10 Myr. -
Southern Stars the JOURNAL of the ROYAL ASTRONOMICAL SOCIETY of NEW ZEALAND P
Southern Stars THE JOURNAL OF THE ROYAL ASTRONOMICAL SOCIETY OF NEW ZEALAND P VolumeVolume 55, No 2 2016 JuneJune ISSN Page0049-1640 1 Royal Astronomical Society Southern Stars of New Zealand (Inc.) Journal of the RASNZ Founded in 1920 as the New Zealand Astronomical Volume 55, Number 2 Society and assumed its present title on receiving the 2016 June Royal Charter in 1946. In 1967 it became a member body of the R oyal Society of New Zealand. CONTENTS P O Box 3181, Wellington 6140, New Zealand Quasars - The Brightest Objects in the Universe [email protected] http://www.rasnz.org.nz Anushka Kharbanda ................................................ 3 Subscriptions (NZ$) for 2016: Norman Dickie ........................................................... 5 Ordinary member: $40.00 Student member: $20.00 Astronomy and Me! Affi liated society: $3.75 per member. Joshua Daglish ........................................................ 6 Minimum $75.00, Maximum $375.00 Corporate member: $200.00 SN 2015lh: Printed copies of Southern Stars (NZ$): The Most Luminous Supernova Discovered $35.00 (NZ) Brent Nicholls .......................................................... 7 $45.00 (Australia & South Pacifi c) $50.00 (Rest of World) The 2015 June 29 Occultation by Pluto Brian Loader .......................................................... 10 Council & Offi cers 2016 to 2018 President: Murray Geddes Prize - Dave Cochrane ................. 17 John Drummond P O Box 113, Patutahi 4045. [email protected] Jennie McCormick - FRASNZ, MNZM .................... 18 Immediate Past President: John Hearnshaw Dep’t Physics & Astronomy, Book Review University of Canterbury, John Drummond ..................................................... 22 Private Bag 4800, Christchurch 8140. [email protected] Vice President: Nicholas Rattenbury The Department of Physics, FRONT COVER The University of Auckland, Brian Loader’s light curve of the Pluto occultation of a th th 38 Princes St, Auckland.