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List of Poster Papers
List of poster papers Downloaded from https://www.cambridge.org/core. IP address: 170.106.202.8, on 29 Sep 2021 at 04:56:15, subject to the Cambridge Core terms of use, available at https://www.cambridge.org/core/terms. https://doi.org/10.1017/S0074180900083601 LIST OF POSTER PAPERS Ρ 1: Christian Doppler (1803- 1853): an Austrian scientist M. Firneis Ρ 2: Austrian astronomy today: a research initiative in stellar astrophysics M. Breger, E. A. Dorß, J. Hron, K. G. Strassmeier, W. W. Weiss, if. Oberhummer, A. Hanslmeier, G. Lustig, if. J. Schober Ρ 3: The Kuffner public observatory in Vienna P. Habison, E. Krebs Ρ 4: Inclination dependence of the mean spectral line shapes of RS CVn stars as evidence for polar spots A. P. Hatzes, S. S. Vbgt, T. F. Ramseyer, A. MiscA Ρ 5: Maximum Entropy spot mapping with simultaneous geometrical and orbital parameter fitting for contact binaries P. D. Hendry Ρ 6: Doppler imaging by the Mean Information Principle S. V. Berdyugina Ρ 7: Prospects of stellar tomographic imaging S. Jsinkov Ρ 8: A new tool for measuring stellar magnetic fields J. Babei, D. Queloz, P. North, M. Mayor Ρ 9: Fourier analysis of time-variable line profiles as a tool to evaluate latitudinal differential rotation A. F. Lanza, M. Rodonö Ρ 10: The interpretation of two-dimensional Fourier analysis of line-profile series Jinxin Hao Ρ 11: On the stability of starspot modelling. I. Zs. Kövari Ρ 12: On the stability of starspot modelling. II. Counteractions between spot parameter determination and inclination Zs. -
Does GD356 Have a Terrestrial Planetary Companion
Mon. Not. R. Astron. Soc. 404, 1984–1991 (2010) doi:10.1111/j.1365-2966.2010.16417.x Does GD 356 have a terrestrial planetary companion? Dayal T. Wickramasinghe,1 Jay Farihi,2 Christopher A. Tout,1,3,4 Lilia Ferrario1 and Richard J. Stancliffe4 1Mathematical Sciences Institute, The Australian National University, ACT 0200, Australia 2Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH 3Institute of Astronomy, The Observatories, Madingley Road, Cambridge CB3 0HA 4Centre for Stellar and Planetary Astrophysics, Monash University, PO Box 28M, VIC 3800, Australia Accepted 2010 January 25. Received 2010 January 20; in original form 2009 November 2 Downloaded from ABSTRACT GD 356 is unique among magnetic white dwarfs because it shows Zeeman-split Balmer lines in pure emission. The lines originate from a region of nearly uniform field strength (δB/B ≈ 0.1) that covers 10 per cent of the stellar surface in which there is a temperature inversion. The energy source that heats the photosphere remains a mystery but it is likely to be associated with http://mnras.oxfordjournals.org/ the presence of a companion. Based on current models, we use archival Spitzer Infrared Array Camera (IRAC) observations to place a new and stringent upper limit of 12 MJ for the mass of such a companion. In the light of this result and the recent discovery of a 115-min photometric period for GD 356, we exclude previous models that invoke accretion and revisit the unipolar inductor model that has been proposed for this system. In this model, a highly conducting planet with a metallic core orbits the magnetic white dwarf and, as it cuts through field lines, a current is set flowing between the two bodies. -
![Arxiv:1108.0403V1 [Astro-Ph.CO] 1 Aug 2011 Esitps Hleg Oglx Omto Oesadthe and Models Formation Galaxy at to Tion](https://docslib.b-cdn.net/cover/5126/arxiv-1108-0403v1-astro-ph-co-1-aug-2011-esitps-hleg-oglx-omto-oesadthe-and-models-formation-galaxy-at-to-tion-515126.webp)
Arxiv:1108.0403V1 [Astro-Ph.CO] 1 Aug 2011 Esitps Hleg Oglx Omto Oesadthe and Models Formation Galaxy at to Tion
Noname manuscript No. (will be inserted by the editor) Production of dust by massive stars at high redshift C. Gall · J. Hjorth · A. C. Andersen To be published in A&A Review Abstract The large amounts of dust detected in sub-millimeter galaxies and quasars at high redshift pose a challenge to galaxy formation models and theories of cosmic dust forma- tion. At z > 6 only stars of relatively high mass (> 3 M⊙) are sufficiently short-lived to be potential stellar sources of dust. This review is devoted to identifying and quantifying the most important stellar channels of rapid dust formation. We ascertain the dust production ef- ficiency of stars in the mass range 3–40 M⊙ using both observed and theoretical dust yields of evolved massive stars and supernovae (SNe) and provide analytical expressions for the dust production efficiencies in various scenarios. We also address the strong sensitivity of the total dust productivity to the initial mass function. From simple considerations, we find that, in the early Universe, high-mass (> 3 M⊙) asymptotic giant branch stars can only be −3 dominant dust producers if SNe generate . 3 × 10 M⊙ of dust whereas SNe prevail if they are more efficient. We address the challenges in inferring dust masses and star-formation rates from observations of high-redshift galaxies. We conclude that significant SN dust pro- duction at high redshift is likely required to reproduce current dust mass estimates, possibly coupled with rapid dust grain growth in the interstellar medium. C. Gall Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark Tel.: +45 353 20 519 Fax: +45 353 20 573 E-mail: [email protected] J. -
Galactic Parameters Derived from Open-Cluster Data T
Astronomy Reports, Vol. 48, No. 2, 2004, pp. 103–107. Translated from Astronomicheski˘ı Zhurnal, Vol. 81, No. 2, 2004, pp. 124–128. Original Russian Text Copyright c 2004 by Gerasimenko. Galactic Parameters Derived from Open-Cluster Data T. P. Gerasimenko Astronomical Observatory, Ural State University, Yekaterinburg, Russia Received September 20, 2001; in final form, July 26, 2003 Abstract—The components U0 and V0 of the solar motion and the Oort constant A0 are determined using the data of a homogeneous open-cluster catalog with corrected distance moduli. The results are based on a sample of 146 open clusters with known radial velocities located in the Galactic plane (b<7◦)within 4 kpc of the Sun. The solar Galactocentric distance R0 is determined usingtwo kinematic methods. The followingresults are obtained: A0 =17.0 ± 0.9 km/s kpc, U0 =10.5 ± 1.0 km/s, V0 =11.5 ± 1.1 km/s, R0 =8.3 ± 0.3 pc. c 2004 MAIK “Nauka/Interperiodica”. 1. INTRODUCTION distance-modulus estimates from the Uniform Cata- logand those determined usingHipparcos trigono- One of the traditional areas of kinematic studies metric parallaxes [12]; the distance scale changed is the determination of the main Galactic parameters by −0.153m, independent of the cluster age. The required to construct theoretical equilibrium models: clusters span a fairly wide age interval. Clusters the gradient of the angular velocity (the Oort constant in different age groups are known to have different AO), the Oort constant B0, and the principal scale motions. Analysis of the rotation of the open-cluster parameter—the distance of the Sun from the Galactic subsystem revealed a small group among the young center, RO. -
Information Bulletin on Variable Stars
COMMISSIONS AND OF THE I A U INFORMATION BULLETIN ON VARIABLE STARS Nos November July EDITORS L SZABADOS K OLAH TECHNICAL EDITOR A HOLL TYPESETTING K ORI ADMINISTRATION Zs KOVARI EDITORIAL BOARD L A BALONA M BREGER E BUDDING M deGROOT E GUINAN D S HALL P HARMANEC M JERZYKIEWICZ K C LEUNG M RODONO N N SAMUS J SMAK C STERKEN Chair H BUDAPEST XI I Box HUNGARY URL httpwwwkonkolyhuIBVSIBVShtml HU ISSN COPYRIGHT NOTICE IBVS is published on b ehalf of the th and nd Commissions of the IAU by the Konkoly Observatory Budap est Hungary Individual issues could b e downloaded for scientic and educational purp oses free of charge Bibliographic information of the recent issues could b e entered to indexing sys tems No IBVS issues may b e stored in a public retrieval system in any form or by any means electronic or otherwise without the prior written p ermission of the publishers Prior written p ermission of the publishers is required for entering IBVS issues to an electronic indexing or bibliographic system to o CONTENTS C STERKEN A JONES B VOS I ZEGELAAR AM van GENDEREN M de GROOT On the Cyclicity of the S Dor Phases in AG Carinae ::::::::::::::::::::::::::::::::::::::::::::::::::: : J BOROVICKA L SAROUNOVA The Period and Lightcurve of NSV ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::: W LILLER AF JONES A New Very Long Period Variable Star in Norma ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::::: EA KARITSKAYA VP GORANSKIJ Unusual Fading of V Cygni Cyg X in Early November ::::::::::::::::::::::::::::::::::::::: -
Sky & Telescope
Eclipse from the See Sirius B: The Nearest Spot the Other EDGE OF SPACE p. 66 WHITE DWARF p. 30 BLUE PLANETS p. 50 THE ESSENTIAL GUIDE TO ASTRONOMY What Put the Bang in the Big Bang p. 22 Telescope Alignment Made Easy p. 64 Explore the Nearby Milky Way p. 32 How to Draw the Moon p. 54 OCTOBER 2013 Cosmic Gold Rush Racing to fi nd exploding stars p. 16 Visit SkyandTelescope.com Download Our Free SkyWeek App FC Oct2013_J.indd 1 8/2/13 2:47 PM “I can’t say when I’ve ever enjoyed owning anything more than my Tele Vue products.” — R.C, TX Tele Vue-76 Why Are Tele Vue Products So Good? Because We Aim to Please! For over 30-years we’ve created eyepieces and telescopes focusing on a singular target; deliver a cus- tomer experience “...even better than you imagined.” Eyepieces with wider, sharper fields of view so you see more at any power, Rich-field refractors with APO performance so you can enjoy Andromeda as well as Jupiter in all their splendor. Tele Vue products complement each other to pro- vide an observing experience as exquisite in performance as it is enjoyable and effortless. And how do we score with our valued customers? Judging by superlatives like: “in- credible, truly amazing, awesome, fantastic, beautiful, work of art, exceeded expectations by a mile, best quality available, WOW, outstanding, uncom- NP101 f/5.4 APO refractor promised, perfect, gorgeous” etc., BULLSEYE! See these superlatives in with 110° Ethos-SX eye- piece shown on their original warranty card context at TeleVue.com/comments. -
A Tail Structure Associated with Protoplanetary Disk Around SU
Draft version February 28, 2019 A Preprint typeset using LTEX style emulateapj v. 12/16/11 A TAIL STRUCTURE ASSOCIATED WITH PROTOPLANETARY DISK AROUND SU AURIGAE EIJI AKIYAMA1, EDUARD I. VOROBYOV2,3, HAUYU BAOBABU LIU4,5, RUOBING DONG5,6, JEROME de LEON7, SHENG-YUAN LIU5, MOTOHIDE TAMURA7,8,9 1Institute for the Advancement of Higher Education, Hokkaido University, Kita17, Nishi8, Kita-ku, Sapporo, 060-0817, Japan; [email protected] 2Department of Astrophysics, University of Vienna, Vienna 1018, Austria 3Research Institute of Physics, Southern Federal University, Rostov-on-Don, 344090, Russia 4European Southern Observatory, Karl Schwarzschild Str 2, 85748 Garching bei M¨unchen, Germany 5Institute of Astronomy and Astrophysics, Academia Sinica, P.O. Box 23-141, Taipei, 10617, Taiwan 6Department of Astronomy/Steward Observatory, The University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA 7Department of Astronomy, The University of Tokyo, 7-3-1, Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan 8Astrobiology Center of NINS, 2-21-1, Osawa, Mitaka, Tokyo, 181-8588, Japan 9National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo, 181-8588, Japan Draft version February 28, 2019 ABSTRACT We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the CO (J=2– 1) line emission from the protoplanetary disk around T-Tauri star SU Aurigae (hereafter SU Aur). Previous observations in optical and near infrared wavelengths find a unique structure in SU Aur. One of the highlights of the observational results is that an extended tail-like structure is associated with the disk, indicating mass transfer from or into the disk. -
Astrophysical Studies of Extrasolar Planetary Systems Using Infrared Interferometric Techniques Olivier Absil
Astrophysical studies of extrasolar planetary systems using infrared interferometric techniques Olivier Absil To cite this version: Olivier Absil. Astrophysical studies of extrasolar planetary systems using infrared interferometric techniques. Astrophysics [astro-ph]. Université de Liège, 2006. English. tel-00124720 HAL Id: tel-00124720 https://tel.archives-ouvertes.fr/tel-00124720 Submitted on 15 Jan 2007 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. Facult´edes Sciences D´epartement d’Astrophysique, G´eophysique et Oc´eanographie Astrophysical studies of extrasolar planetary systems using infrared interferometric techniques THESE` pr´esent´eepour l’obtention du diplˆomede Docteur en Sciences par Olivier Absil Soutenue publiquement le 17 mars 2006 devant le Jury compos´ede : Pr´esident: Pr. Jean-Pierre Swings Directeur de th`ese: Pr. Jean Surdej Examinateurs : Dr. Vincent Coude´ du Foresto Dr. Philippe Gondoin Pr. Jacques Henrard Pr. Claude Jamar Dr. Fabien Malbet Institut d’Astrophysique et de G´eophysique de Li`ege Mis en page avec la classe thloria. i Acknowledgments First and foremost, I want to express my deepest gratitude to my advisor, Professor Jean Surdej. I am forever indebted to him for striking my interest in interferometry back in my undergraduate student years; for introducing me to the world of scientific research and fostering so many international collaborations; for helping me put this work in perspective when I needed it most; and for guiding my steps, from the supervision of diploma thesis to the conclusion of my PhD studies. -
Arxiv:2001.10147V1
Magnetic fields in isolated and interacting white dwarfs Lilia Ferrario1 and Dayal Wickramasinghe2 Mathematical Sciences Institute, The Australian National University, Canberra, ACT 2601, Australia Adela Kawka3 International Centre for Radio Astronomy Research, Curtin University, Perth, WA 6102, Australia Abstract The magnetic white dwarfs (MWDs) are found either isolated or in inter- acting binaries. The isolated MWDs divide into two groups: a high field group (105 − 109 G) comprising some 13 ± 4% of all white dwarfs (WDs), and a low field group (B < 105 G) whose incidence is currently under investigation. The situation may be similar in magnetic binaries because the bright accretion discs in low field systems hide the photosphere of their WDs thus preventing the study of their magnetic fields’ strength and structure. Considerable research has been devoted to the vexed question on the origin of magnetic fields. One hypothesis is that WD magnetic fields are of fossil origin, that is, their progenitors are the magnetic main-sequence Ap/Bp stars and magnetic flux is conserved during their evolution. The other hypothesis is that magnetic fields arise from binary interaction, through differential rotation, during common envelope evolution. If the two stars merge the end product is a single high-field MWD. If close binaries survive and the primary develops a strong field, they may later evolve into the arXiv:2001.10147v1 [astro-ph.SR] 28 Jan 2020 magnetic cataclysmic variables (MCVs). The recently discovered population of hot, carbon-rich WDs exhibiting an incidence of magnetism of up to about 70% and a variability from a few minutes to a couple of days may support the [email protected] [email protected] [email protected] Preprint submitted to Journal of LATEX Templates January 29, 2020 merging binary hypothesis. -
Download This Issue (Pdf)
Volume 46 Number 2 JAAVSO 2018 The Journal of the American Association of Variable Star Observers Unmanned Aerial Systems for Variable Star Astronomical Observations The NASA Altair UAV in flight. Also in this issue... • A Study of Pulsation and Fadings in some R CrB Stars • Photometry and Light Curve Modeling of HO Psc and V535 Peg • Singular Spectrum Analysis: S Per and RZ Cas • New Observations, Period and Classification of V552 Cas • Photometry of Fifteen New Variable Sources Discovered by IMSNG Complete table of contents inside... The American Association of Variable Star Observers 49 Bay State Road, Cambridge, MA 02138, USA The Journal of the American Association of Variable Star Observers Editor John R. Percy Laszlo L. Kiss Ulisse Munari Dunlap Institute of Astronomy Konkoly Observatory INAF/Astronomical Observatory and Astrophysics Budapest, Hungary of Padua and University of Toronto Asiago, Italy Toronto, Ontario, Canada Katrien Kolenberg Universities of Antwerp Karen Pollard Associate Editor and of Leuven, Belgium Director, Mt. John Observatory Elizabeth O. Waagen and Harvard-Smithsonian Center University of Canterbury for Astrophysics Christchurch, New Zealand Production Editor Cambridge, Massachusetts Michael Saladyga Nikolaus Vogt Kristine Larsen Universidad de Valparaiso Department of Geological Sciences, Valparaiso, Chile Editorial Board Central Connecticut State Geoffrey C. Clayton University, Louisiana State University New Britain, Connecticut Baton Rouge, Louisiana Vanessa McBride Kosmas Gazeas IAU Office of Astronomy for University of Athens Development; South African Athens, Greece Astronomical Observatory; and University of Cape Town, South Africa The Council of the American Association of Variable Star Observers 2017–2018 Director Stella Kafka President Kristine Larsen Past President Jennifer L. -
Probing the Close Environment of Young Stellar Objects With
Probing the close environment of young stellar objects with interferometry Fabien Malbet ([email protected]) Laboratoire d’Astrophysique, Observatoire de Grenoble, UMR 5571 CNRS/UJF, Grenoble, France Abstract. The study of Young Stellar Objects (YSOs) is one of the most ex- citing topics that can be undertaken by long baseline optical interferometry. The magnitudes of these objects are at the edge of capabilities of current optical inter- ferometers, limiting the studies to a few dozen, but are well within the capability of coming large aperture interferometers like the VLT Interferometer, the Keck Inter- ferometer, the Large Binocular Telescope or ’OHANA. The milli-arcsecond spatial resolution reached by interferometry probes the very close environment of young stars, down to a tenth of an astronomical unit. In this paper, I review the different aspects of star formation that can be tackled by interferometry: circumstellar disks, multiplicity, jets. I present recent observations performed with operational infrared interferometers, IOTA, PTI and ISI, and I show why in the next future one will extend these studies with large aperture interferometers. Keywords: Interferometry, Optical, Infrared, Star Formation, Young Stellar Ob- jects, Pre-Main Sequence Stars 1. Introduction When trying to understand the origin of our planetary system, one has basically two approaches: (i) looking for other existing planetary systems in the universe to characterize them or (ii) investigate how stellar systems have been forming. By studying young stellar objects (hereafter YSOs) in our Universe, i.e. stars in their early stages of evolution, one focuses our attention to the second approach. So far, these objects have been extensively observed by spectropho- arXiv:astro-ph/0303260v1 12 Mar 2003 tometry with seeing-limited resolution that corresponds at best to a hundred of astronomical units for typical star formation regions, thus many questions are still unresolved 1 because our incapability to disen- tangle the various phenomena at smaller scales. -
An Upper Limit to Coronal X-Rays from Single, Magnetic White Dwarfs
J. Astrophys. Astr. (1993) 14, 141–143 An Upper Limit to Coronal X-rays from Single, Magnetic White Dwarfs 1 1 2 Rob Cavallo , Keith A. Arnaud & Virginia Trimble Astronomy Department, University of Maryland, College Park MD 20742 USA 1 Also Code 666, Goddard Space Flight Center, Greenbelt MD 20771 USA 2 Also Physics Department, University of California, Irvine CA 92717 Received 1993 August 19; accepted 1993 September 28 Abstract. Pointed ROSAT PSPC exposures of 9277 and 6992 sec, directed toward the nearby, single, cool, magnetic white dwarfs GR 290 and EG 250 yielded no counts significantly above the expected background rate. The corresponding flux limits (for an assumed source temperature of l keV) are 1.0 and 1.7 × 10 –14erg cm–2 s–1, within the 0.1–2.5 keV bandpass of the instrument (99% confidence limits). This is more than an order of magnitude below the tentative detection level (for GR 290) and limits (for four other similar stars) obtained from archival Einstein data in 1991. The corresponding limits on coronal electron density are comparable with those implied if cyclotron emission is not responsible for any of the features observed in the optical spectra of magnetic white dwarfs. X-ray data currently provide no evidence for the existence of coronae around these stars. A final long observation (25,000 sec of GD 356) is scheduled for later this year on ROSAT, along with coordinated EUVE observations. Key words: White dwarfs—stellar coronae—X-ray emission 1. Introduction Motivated by theoretical considerations (Zheleznyakov & Litvinchuk 1985; Serber 1990) and by the preponderance of magnetic systems among known cataclysmic variable X-ray sources, Arnaud et al.