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Multi-Periodic Photospheric Pulsations and Connected Wind Structures in HD 64760
A&A 447, 325–341 (2006) Astronomy DOI: 10.1051/0004-6361:20053847 & c ESO 2006 Astrophysics Multi-periodic photospheric pulsations and connected wind structures in HD 64760 A. Kaufer1,O.Stahl2,R.K.Prinja3, and D. Witherick3, 1 European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Santiago 19, Chile e-mail: [email protected] 2 Landessternwarte Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany 3 Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK Received 18 July 2005 / Accepted 17 October 2005 ABSTRACT We report on the results of an extended optical spectroscopic monitoring campaign on the early-type B supergiant HD 64760 (B0.5 Ib) designed to probe the deep-seated origin of spatial wind structure in massive stars. This new study is based on high-resolution echelle spectra obtained with the Feros instrument at ESO La Silla. 279 spectra were collected over 10 nights between February 14 and 24, 2003. From the period analysis of the line-profile variability of the photospheric lines we identify three closely spaced periods around 4.810 h and a splitting of ±3%. The velocity – phase diagrams of the line-profile variations for the distinct periods reveal characteristic prograde non-radial pulsation patterns of high order corresponding to pulsation modes with l and m in the range 6−10. A detailed modeling of the multi-periodic non-radial pulsations with the Bruce and Kylie pulsation-model codes (Townsend 1997b, MNRAS, 284, 839) favors either three modes with l = −m and l = 8, 6, 8 or m = −6andl = 8, 6, 10 with the second case maintaining the closely spaced periods in the co-rotating frame. -
Binocular Universe: You're My Hero! December 2010
Binocular Universe: You're My Hero! December 2010 Phil Harrington on't you just love a happy ending? I know I do. Picture this. Princess Andromeda, a helpless damsel in distress, chained to a rock as a ferocious D sea monster loomed nearby. Just when all appeared lost, our hero -- Perseus! -- plunges out of the sky, kills the monster, and sweeps up our maiden in his arms. Together, they fly off into the sunset on his winged horse to live happily ever after. Such is the stuff of myths and legends. That story, the legend of Perseus and Andromeda, was recounted in last month's column when we visited some binocular targets within the constellation Cassiopeia. In mythology, Queen Cassiopeia was Andromeda's mother, and the cause for her peril in the first place. Left: Autumn star map from Star Watch by Phil Harrington Above: Finder chart for this month's Binocular Universe. Chart adapted from Touring the Universe through Binoculars Atlas (TUBA), www.philharrington.net/tuba.htm This month, we return to the scene of the rescue, to our hero, Perseus. He stands in our sky to the east of Cassiopeia and Andromeda, should the Queen's bragging get her daughter into hot water again. The constellation's brightest star, Mirfak (Alpha [α] Persei), lies about two-thirds of the way along a line that stretches from Pegasus to the bright star Capella in Auriga. Shining at magnitude +1.8, Mirfak is classified as a class F5 white supergiant. It radiates some 5,000 times the energy of our Sun and has a diameter 62 times larger. -
2005 SSM Poster Session
17th Annual SSM Poster Session — 2005 Abstracts by Number 1 Ichthyoplankton Distribution Patterns Across the Continental Shelf off Charleston, SC Ryan Yaden and Gorka Sancho, Department of Biology To compare the seasonal and spatial distribution of ichthyolplankton across the continental shelf off the coast of Charleston a transect was made across the continental shelf. The collection plankton samples took place on a 5 day cruise November 19 and 2004. Seven samples were analyzed by removing ichthyoplankton from other zooplankton. Ichthyoplankton taxa Leptocephalus, Scombridae, Ophidiidae, Pleurinectiformes, and Syngnathidae were identified picked and counted. Larval fishes that could not be classified were put into the "unknown" category. Data were compared with similar collections from May 2004. The abundance of larval fish in November was greater than the abundance in May. The greater abundance in November 2004 could be related to the spawning seasons of fishes over the continental self and Gulf Stream. 2 Lifespan of philometrid larvae (Margolisianum bulbosum) and their infectivity in the copepod Oithona colcarva under different abiotic conditions Lam C. Tsoi1, Vincent A. Conners2, and Isaure deBuron1 1Department of Biology, College of Charleston 2Department of Biology, University of South Carolina-Upstatet Margolisianum bulbosum is a philometrid nematode whose large and viviparous females are found in the buccal and gill cavities of the Southern flounder, Paralichthys lethostigma. As part of a study of the biology of this worm we determined the optimal abiotic (salinity and temperature) conditions for larval survival and infectivity in the hypothesized copepod intermediate host. Experimental infections of copepods collected in the Charleston Harbor showed that the cyclopoid Oithona colcarva was the only species to become infected. -
PDF Version in Chronological Order (Updated May 17, 2013)
Complete Bibliography for Ritter Observatory May 17, 2013 The following papers are based in whole or in part on observations made at Ritter Observatory. External collaborators are listed in parentheses unless the research was done while they were University of Toledo students. Refereed or invited: 1. A. H. Delsemme and J. L. Moreau 1973, Astrophys. Lett., 14, 181–185, “Brightness Profiles in the Neutral Coma of Comet Bennett (1970 II)” 2. B. W. Bopp and F. Fekel Jr. 1976, A. J., 81, 771–773, “HR 1099: A New Bright RS CVn Variable” 3. A. H. Delsemme and M. R. Combi 1976, Ap. J. (Letters), 209, L149–L151, “The Production Rate and Possible Origin of O(1D) in Comet Bennett 1970 II” 4. A. H. Delsemme and M. R. Combi 1976, Ap. J. (Letters), 209, L153–L156, “Production + Rate and Origin of H2O in Comet Bennett 1970 II” 5. D. W. Willmarth 1976, Pub. A. S. P., 88, 86–87, “The Orbit of 71 Draconis” 6. W. F. Rush and R. W. Thompson 1977, Ap. J., 211, 184–188, “Rapid Variations of Emission-Line Profiles in Nova Cygni 1975” 7. S. E. Smith and B. W. Bopp 1980, Pub. A. S. P., 92, 225–232, “A Microcomputer-Based System for the Automated Reduction of Astronomical Spectra” 8. B. W. Bopp and P. V. Noah 1980, Pub. A. S. P., 92, 333–337, “Spectroscopic Observations of the Surface-Activity Binary II Pegasi (HD 224085)” 9. M. R. Combi and A. H. Delsemme 1980, Ap. J., 237, 641–645, “Neutral Cometary Atmospheres. II. -
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, -
Prof. Dr. L. Woltjer EUROPEAN SOUTHERN
EUROPEAN SOUTHERN OBSERVATORY COVER PICTURE PHOTOGRAPHIE DE UMSCHLAGSFOTO COUVERTURE False colour image of the jet of the Crab Sur cette image en fausses couleurs, prise Diese Falschfarbenabbildung, die mit Nebula taken with EFOSC at the 3.6 m avec EFOSC au telescope de 3,6 m, on EFOSC am 3,6-m-Teleskop aufgenorw telescope by S. D'Odorico. voit le «jet» de la nebuleuse du Crabe. men wurde, zeigt den "Jet" des Krebs" Observateur: S. D'Odorico. Nebels. Beobachter: S. D'Odorico Annual Report / Rapport annuel / Jahresbericht 1985 presented to the Council by the Director General presente au Conseil par le Directeur general dem Rat vorgelegt vom Generaldirektor Prof. Dr. L. Woltjer EUROPEAN SOUTHERN OBSERVATORY Organisation Europeenne pour des Recherches Astronomiques dans I'Hemisphere Austral Europäische Organisation für astronomische Forschung in der südlichen Hemisphäre Table Table des Inhalts ., of Contents matleres verzeichnis INTRODUCTION . 5 INTRODUCTION . 5 EINLEITUNG 5 RESEARCH 9 RECHERCHES , 9 FORSCHUNG 9 Joint Research Recherches communes Gemeinsame Forschung mit with Chilean Institutes 22 avec les instituts chiliens ... 22 chilenischen Instituten .... 22 Conferences and Workshops .. 23 Conferences et colloques ., .. , 23 Konferenzen und Workshops .. 23 Sky Survey 23 Carte du ciel 23 Himmelsatlas 23 Image Processing 24 Traitement des images 24 Bildauswertung 24 The European Coordinating Le Centre Europeen de Coor- Die Europäische Koordinie- Facility for the Space dination pour le Telescope rungsstelle für das Weltraum- Telescope (ST-ECF) 26 Spatial (ST-ECF) .. , ..... , 26 Teleskop (ST-ECF) 26 FACILITIES INSTALLATIONS EINRICHTUNGEN TeIescopes 31 Teiescopes 31 Teleskope 31 Instrumentation 38 Instrumentation 38 Instrumentierung 38 Buildings 43 Batiments 38 Gebäude " 43 FINANCIAL AND ORGA- FINANCES ET FINANZEN UND NIZATIONAL MATTERS 45 ORGANISATION 45 ORGANISATION 45 APPENDIXES ANNEXES ANHANG Appendix 1- Annexe I- Anhang 1- Use of Telescopes ....... -
Vibrations of Be Stars O
0.00 0.10 ANNOUNCEMENT OF AN ESO WORKSHOP ON Int. Li I >..6707.8 + 0.20 "THE VIRGO CLUSTER 10 OF GALAXIES" o + to be held in GARCHING, September 1984 A large amount of observational and theoretical work has been done on this cluster. The workshop is intended to bring together people with a wide range of experience in an attempt to resolve some of the important controversies such o as the membership definition, distance estimates, or the density contrast to the local environment, etc. 0.9 Both review papers and short contributions will be given, and there could be two panel discussions (if there is enough interest) on (a) dependence of conclusions on membership assignment to individual galaxies, and (b) differences be tween Virgo cluster galaxies and "field" galaxies: signs of different evolution or different formation? For further information, write to: G.-G. Richter B. Binggelli M. Tarenghi Astronomisches Institut European Southern Obser Venusstraße 7 0.8 vatory CH-4102 Binningen Karl-Schwarzschild-Straße 2 Switzerland 0-8046 Garehing bei München o Federal Republic of Germany 0.1 Ä Fig. 2: The observed spectrum ofßHyi and theoretical Li line profiles the whole, our run was a very convincing demonstration of the (dots) for three isotope ratios. The (VI ?) line at A 6707.43 in the violet quality and efficiency of this new facility, and Oaniel Enard and wing of the Li fine was not included in the theoretical profiles. his colleagues are to be cordially congratulated on this achievement. We trust that our readers will, in the end, share of the last observation while integrating on the next star, and our preference for the kind of excitement derived from new, trying occasionally to remind ourselves what a disgusting place interesting results rather than from ever so picturesque disas the smelly interior of a darkroom used to be in the old days. -
Stars, Galaxies, and Beyond, 2012
Stars, Galaxies, and Beyond Summary of notes and materials related to University of Washington astronomy courses: ASTR 322 The Contents of Our Galaxy (Winter 2012, Professor Paula Szkody=PXS) & ASTR 323 Extragalactic Astronomy And Cosmology (Spring 2012, Professor Željko Ivezić=ZXI). Summary by Michael C. McGoodwin=MCM. Content last updated 6/29/2012 Rotated image of the Whirlpool Galaxy M51 (NGC 5194)1 from Hubble Space Telescope HST, with Companion Galaxy NGC 5195 (upper left), located in constellation Canes Venatici, January 2005. Galaxy is at 9.6 Megaparsec (Mpc)= 31.3x106 ly, width 9.6 arcmin, area ~27 square kiloparsecs (kpc2) 1 NGC = New General Catalog, http://en.wikipedia.org/wiki/New_General_Catalogue 2 http://hubblesite.org/newscenter/archive/releases/2005/12/image/a/ Page 1 of 249 Astrophysics_ASTR322_323_MCM_2012.docx 29 Jun 2012 Table of Contents Introduction ..................................................................................................................................................................... 3 Useful Symbols, Abbreviations and Web Links .................................................................................................................. 4 Basic Physical Quantities for the Sun and the Earth ........................................................................................................ 6 Basic Astronomical Terms, Concepts, and Tools (Chapter 1) ............................................................................................. 9 Distance Measures ...................................................................................................................................................... -
The Messenger
THE MESSENGER No. 34 - December 1983 The Very Large Telescope Project D. Enard, Head of the VL T Project Group, and J. -Po Swings, Chairman of the VL T Astronomy Advisory Committee Artist's view ofan early ESO VL T concept, representing a array offour 8 metre lelescopes, of which Iwo are shown 10 be Iinked for interferometric capabilities. 11 now seems preferable 10 do interferometry byadding 10 Ihe large dishes a few smaller size (2-3 metre) lelescopes thai would be movable. (Drawing by J.-M. Leclercqz.) As emphasized unanimously at the time of the Cargese - Spectroscopy in the IR of quasars and active galaxies to workshop" a Very Large Telescope (VLT) project is of vital determine the internal absorption and to study the kinema importance to the future vigour of European astronomy. The tics of the absorbed region; table given below shows indeed that "competing" projects exist - High spectral resolution observations of quasar narrow in the US, UK, USSR, all of which are to be completed within absorption lines and the consequent mapping of the distribu about 10 years. The Space Telescope is indicated in the same tion of intergalactic matter in the universe; table for comparison, in order to stress its high cost and its size - Spectroscopic observations of very distant galaxies to study of "only" 2.4 metres. It is also very important to keep in mind their evolution, and from this to gain further information on that the Space Telescope and future large ground-based the expansion of the universe. telescopes are to be considered as complementary, not as High resolution imaging is perhaps one of the most fascinat competitors. -
NSO Scientific Papers 1985-1999
NSO Publications, 1985-1999 NSO Publications, 1985-1999 Sorted Alphabetically by Author Abdelatif, T.E. 1985, Umbral Oscillations as a Probe of Sunspot Structure. PhD Thesis (University of Rochester) Abdelatif, T.E., Lites, B.W., and Thomas, J.H. 1984, in Small-Scale Dynamical Processes in Quiet Stellar Atmospheres: Workshop Proceedings, Sunspot, New Mexico, 25-29 Jul. 1983. S.L. Keil, ed., 141-147: Oscillations in a Sunspot and the Surrounding Photosphere Abdelatif, T.E., Lites, B.W., and Thomas, J.H. 1986, Astrophys. J. 311, 1015-1024: The Interaction of Solar P-Modes with a Sunspot. I. Observations Abrams, D., and Kumar, P. 1996, Astrophys. J. 472, 882-890: Asymmetries of Solar p-Mode Line Profiles Abrams, M.C., Davis, S.P., Rao, M.L., and Engleman, R. 1990, Astrophys. J. 363, 326-330: Highly Excited Rotational States of the Meinel System of OH Abrams, M.C., Davis, S.P., Rao, M.L., Engleman, R., and Brault, J.W. 1994, Astrophys. J. Suppl. Ser. 93, 351-395: High-Resolution Fourier Transform Spectroscopy of the Meinel System of OH Acton, D.S. 1989, in High Spatial Resolution Solar Observations: Proceedings of the Tenth Sacramento Peak Summer Symposium, Sunspot, New Mexico, 22-26 August, 1988. O. Von der Luhe, ed., 71-86: Results from the Lockheed Solar Adaptive Optics System Acton, D.S. 1990, Real-Time Solar Imaging with a 19-Segment Active Mirror System: a Study of the Standard Atmospheric Turbulence Model. PhD Thesis (Texas Tech University). Acton, D.S. 1994, in Real-Time and Post-Facto Solar Image Correction. -
Almanacco Astronomico 2002 – Introduzione
Almanacco Astronomico per l’anno 2002 Sergio Alessandrelli C.C.C.D.S. - Hipparcos La Luna – Principali formazioni geologiche Almanacco Astronomico per l’anno 2002 A tutti gli amici astrofili… 1 Almanacco Astronomico 2002 – Introduzione Introduzione all’Almanacco Astronomico 2002 Il presente Almanacco Astronomico è stato realizzato utilizzando comuni programmi di calcolo astronomico facilmente reperibili sul mercato del software, ovvero scaricabili gratuitamente tramite Internet. La precisione nei calcoli è quindi quella tipica per questo tipo di software, ossia sufficiente per gli usi dell’astrofilo medio. Tutti gli eventi sono stati calcolati per le coordinate di Roma (Lat. 41° 52’ 48” N, Long. 12° 30’ 00” E) e gli orari espressi (tranne laddove altrimenti specificato) in tempo universale. 2 Almanacco Astronomico 2002 – Calendario del 2002 Calendario del 2002 January February March Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa 1 2 3 4 5 1 2 1 2 6 7 8 9 10 11 12 3 4 5 6 7 8 9 3 4 5 6 7 8 9 13 14 15 16 17 18 19 10 11 12 13 14 15 16 10 11 12 13 14 15 16 20 21 22 23 24 25 26 17 18 19 20 21 22 23 17 18 19 20 21 22 23 27 28 29 30 31 24 25 26 27 28 24 25 26 27 28 29 30 31 April May June Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa 1 2 3 4 5 6 1 2 3 4 1 7 8 9 10 11 12 13 5 6 7 8 9 10 11 2 3 4 5 6 7 8 14 15 16 17 18 19 20 12 13 14 15 16 17 18 9 10 11 12 13 14 15 21 22 23 24 25 26 27 19 20 21 22 23 24 25 16 17 18 19 20 21 22 28 29 30 26 27 28 29 30 31 23 24 25 26 27 28 29 30 July August September Su Mo Tu We -
A Summary of the Different Classes of Stellar Pulsators
A Summary of the Different Classes of Stellar Pulsators A summary of all the classes of pulsating stars and their main properties as described in Chapter 2 is given in the tables below. This list originated from a combination of observational discoveries, measured stellar properties, and theoretical developments. Observers who found a new type of pulsator either named it after the prototype or gave the class a name according to the ob- served characteristics of the oscillations. Several pulsators, or even groups of pulsators, were afterwards found to originate from the same physical mech- anism and were thus merged into one and the same class. We sort this out here in Tables A.1 and A.2 in order to avoid further confusion on pulsating star nomenclature. The effective temperature and luminosity indicated in Tables A.1 and A.2 should be taken as rough indications only of the borders of instability strips. Often the theory is not sufficiently refined to consider these boundaries as final. Moreover, there is overlap between various classes where so-called hy- brid pulsators, whose oscillations are excited in two different layers and/or by two different mechanisms, occur. Finally, new discoveries are being made frequently, which then drive new theoretical developments possibly leading to new instability regions. The results from the future observing facilities as described in Chapter 8 will surely lead to new classes and/or subclasses with lower amplitudes compared to what is presently achievable. In the tables below, F stands for fundamental radial mode, FO for first radial overtone and S for strange mode oscillations.