DOCSLIB.ORG

Talks Antofagasta, March 1-4, 2016 1

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Talks Antofagasta, March 1-4, 2016 1 XIII Annual Meeting of the Chilean Astronomical Society Book of abstracts - Talks Antofagasta, March 1-4, 2016 1 Claudia Agliozzo Universidad Nacional Andrés Bello A tale of the mass-loss of the magellanic LBV R127 During their lifetime, Luminous Blue Variable stars (LBVs) must rapidlyexpel their H envelope, with the highest mass-loss rates (> 10^(-5) M_sun/yr), in order to evolve into Wolf-Rayet stars.However, the physical mechanism underlying the mass-loss is not yet understood.I present our extraordinary multi- wavelength dataset of R127, a famousLBV in the Large Magellanic Cloud, widely observed in the past at visiblewavelengths. Our dataset comprises high-resolution centimetre ATCA and submillimetre ALMA data, in addition to new high-spectral resolution optical data acquired with the instrument MIKE at Magellan II telescope.As shown by the different spectral features detected, the mass-loss ishighly complex, with signatures of different episodes, such as have beenseen in previous spectroscopic observations and in the galactic prototypeLBV AG Carinae. We newly discover that from theinner to the outer regions, the stellar wind changes geometry.With all our data together, the picture seems much clearer: theasymmetric morphology of the wind and of the circumstellar nebula aremore likely due to external factors than intrinsic asymmetriesof the mass-loss. I will discuss different scenarios.We don't know yet how common this behaviour is in galactic and magellanic LBVs. However, noticeably, the geometry of the nebula resembles that of Eta Carinae and of the blue-supergiant progenitor of Supernova 1987A. 2 Gustavo Aguayo Universidad de Concepción Optical study of the Be star Mu Centauri We present an optical study of the Be star Mu Centauri, this study was developed using spectroscopic data taken with CHIRON and CORALIE spectrograph, there were measured important parameters of some lines located at the optical range as equivalent width and peak separation, also correlations between equivalent widths of some lines were found and are presented here. The peak separation was used to constrain the extension of the line forming regions and this work is also presented in this poster. Also we present in this poster visual photometry of this star covering the same lapse that the spectra, the result of the correlation between equivalent width of H alpha and magnitude is shown below. 3 Claudia Aguilera Pontificia Universidad Católica Lithium enrichment in red giant branch stars Lithium (Li) is easily destroyed inside low mass. During the red giant branch phase the surface Li abundance decreases even further by dilution, but a small number of giants is known to be Li-rich. This is unexpected and it cannot be accounted for by canonical stellar evolution. One of the possible explanations for these atypical giants is the engulfment of a planet or brown dwarf by the star. In this work, we model the evolution of lithium abundance post first dredge up including the accretion of a sub-stellar mass companion. We consider a wide range of stellar and companion masses and initial lithium abundances, stellar metallicities and time of engulfment, including the most optimistic choices that would produce the highest superficial Li abundances. We find that even with the best possible conditions, i.e., a companion with supermeteoritic Li abundance that produces a maximum signature of A(Li) ∼ 2.7, the accretion of a sub-stellar mass companion alone cannot explain all the observed lithium rich giants andthus it seems necessary to include internal production of the light element plus additional non-canonical physics, such as an extra-mixing process. 4 Alba Aller Universidad de Valparaiso Search for binary central stars of planetary nebulae: exploding archival data With the new binary central stars (CSs) identified in the last years, binary interactions have become the main proposed mechanism to explain the complex morphologies seen in planetary nebulae (PNe). There are around 50 binary CSs detected so far. However, this number remains very small as compared to the more than 3000 known PNe in the Milky Way. In this context, we are involved in a project to study how binary interaction processes influence the shape of PNe. Archival data offer a great opportunity to search for new candidates of binary CSs since surveys like, e.g., Catalina, ASAS and OMC provide light curves of a large number of objects in a long timespan. We are exploding these surveys to search for new candidates that will be subsequently followed-up by means of multi-epoch photometric and spectroscopic observations. In this talk, we will summarize the goals of this project and show the first results. 5 Simón Ángel Pontificia Universidad Católica Characterisation of stellar populations in the CFHTLS Deep fields Combining the information of the CFHTLS (Gwyn 2011) and WIRDS (Bielby et al. 2012) surveys, I constructed multiwavelength catalogues for the four Deep CFHTLS fields. Using the selection tool presented in Muñoz et al. (2014), I produced a clean and deep (limiting magnitude in r ~ 26) subset of stars. Colour, magnitude, metallicity, and distance distributions have been studied, using for the latter, the methods presented in the Milky Way Tomography series of papers (Jurić et al. 2008, Ivezić et al. 2008, Bond et al. 2010) and in Sesar et al. (2011). In this talk, I will present the dataset and the distributions aforementioned, along with comparisons with the Besançon model of stellar population synthesis of the Galaxy (Robin et al. 2003). 6 Rodolfo Angeloni Gemini Observatory The Sanduleak's star in the Large Magellanic Cloud Sanduleak's star is a variable emission-line object in the Large Magellanic Cloud. It was discovered in 1977 and, already in the early 80's, a similarity with eta Carinae and SN 1987A was proposed on the basis on IUE observations which indicated episodic mass outflow, extreme departures from normal cosmic values of nitrogen relative to carbon and oxygen, and an electron temperature which is hard to reconcile with pure photo-ionization models. Sanduleak's star came abruptly back on stage in 2011, when we discovered that it powers a giant, highly-collimated bipolar jet extending over almost 15 pc: to our knowledge, it is the largest stellar jet discovered so far, and the first one clearly resolved beyond the Milky Way. In this contribution we present our follow-up observations of Sanduleak's star obtained over the last few years. In particular: HST-WFC3 narrow-band images, that allow us to resolve the spectacular inner nebula; Magellan-FIRE and MMIRS near-infrared spectra, which give insight on the symbiotic character of the central binary; Magellan-MIKE high-resolution optical spectra, that further constraint the kinematics, chemistry and energetics of the overall system. We thus discuss the nature of Sanduleak's star and place it in the general context of the late stages of stellar evolution, by also highlighting some tentative links with the Intermediate-Luminosity Optical Transients. 7 Javier Arenas Pontificia Universidad Católica de Valparaiso Can pulsar glitches be explained by "starquakes"? Pulsars are the best clocks known in universe, with very precisely periodic pulses due to the rotation of a neutron star with a strong dipolar magnetic field. The pulses slow down progressively, due to the release of rotational energy. In addition, there are timing irregularities, the most prominent of which are "glitches", sudden spin-up events, in which about 1 % of the spin-down is "recovered".There are two main mechanisms discussed in the scientific literature to explain this kind of events. The first is the sudden transfer of angular momentum from the superfluid (or part of it) to the solid crust of the star. The second is a "starquake", a sudden breaking of the solid crust due to stress accumulated by the spin-down of the star. Our object of study is the second of these mechanisms, which was previously studied by Baym & Pines (1969). They showed that, for known values of Crab pulsar, starquakes due to spin down cannot explain the relatively short recurrence times (of few years), instead requiring hundreds of years between glitches. For Vela the scenario was much worse, exceeding thousands (even millions) of years the time between glitches. However, the size distribution of glitches is bimodal, so one might still try to explain the smaller glitches through this mechanism. In this investigation, using theory of elasticity to demonstrate how the star is deformed by rotation, we study the plausibility of the model in two scenarios. First in a completely solid star, which could store the maximum stress and the second is a more realistic star with fluid core and solid crust. We use observations of pulsars with only small glitches, as the Crab pulsar, and pulsars with bimodal distribution, as the Vela, to test the models. 8 Maria Argudo-Fernandez Universidad de Antofagasta Evolution of Spiral Isolated Galaxies with MaNGA From models, it is predicted that disks grow from inner to outer parts of galaxies, the so–called inside– out model of galaxy formation. As a consequence, we expect to observe gradients in stellar age and metallicity as a function of galactic radius. Thankfully, new integral field spectroscopy of nearby galaxies now provide us with data at sufficient resolution to study the star formation history (SFH) over the disk of a galaxy. But separating the effect secular evolution on the physical properties of galaxies from that of the environment (nature versus nurture) is also a necessary and challenging question to address. Here we report our efforts to constraint the SFH of isolated galaxies that have been already observed by MaNGA. Our preliminary results are in favour of the scenario where spiral disks grow inside-out. 9 Francisco Aros Pontificia Universidad Católica Axisymmetric dynamical models of dwarf spheroidal galaxies The dynamical analysis of dark matter dominated galaxies is expected to contribute significantly in the understanding of the nature of dark matter.
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.
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • From Massive Stars to Supernovae
    ISSN 1783-3426 THE MASSIVE STAR NEWSLETTER formerly known as the hot star newsletter * No. 151 2016 January-February Editors: Philippe Eenens (University of Guanajuato) [email protected] Raphael Hirschi (Keele University) http://www.astroscu.unam.mx/massive_stars CONTENTS OF THIS NEWSLETTER: News Obituaries Paul Kunasz and David Hummer Fizeau exchange visitors program Abstracts of 18 accepted papers Classical Oe Stars in the Field of the Small Magellanic Cloud An Apparent Precessing Helical Outflow from a Massive Evolved Star: Evidence for Binary Interaction A Comprehensive Comparative Test of Seven Widely-Used Spectral Synthesis Models Against Multi- Band Photometry of Young Massive Star Clusters Modeling X-ray emission line profiles from massive star winds – A review Long-Wavelength, Free-Free Spectral Energy Distributions from Porous Stellar Winds The Runaways and Isolated O-Type Star Spectroscopic Survey of the SMC (RIOTS4) Eta Carinae's Thermal X-ray Tail Measured with XMM-Newton and NuSTAR Stellar modelling of Spica, a high-mass spectroscopic binary with a beta Cep variable primary component Observational signatures of past mass-exchange episodes in massive binaries: The case of HD149404 The Galactic O-Star Spectroscopic Survey (GOSSS). III. 142 additional O-type systems Probing the Dragonfish star-forming complex: the ionizing population of the young massive cluster Mercer 30 Short-term variability and mass loss in Be stars I. BRITE satellite photometry of eta and mu Centauri Luminous blue variables: An imaging perspective on their binarity and near environment OB stars at the lowest Local Group metallicity. GTC-OSIRIS observations of Sextans A Herschel observations of the nebula M1-67 around the Wolf-Rayet star WR 124 The Massive Stellar Population of W49: A Spectroscopic Survey Line-driven ablation of circumstellar disks: I.
    [Show full text]
  • COMMISSION 27 of the I.A.U. INFORMATION BULLETIN on VARIABLE STARS Nos. 3001
    COMMISSION 27 OF THE I.A.U. INFORMATION BULLETIN ON VARIABLE STARS Nos. 3001 - 3100 1987 March - 1987 October EDITORS: L. SZABADOS and B. SZEIDL KONKOLY OBSERVATORY H-1525 BUDAPEST P.O. Box 67, HUNGARY HU ISSN 0374 - 0676 CONTENTS 3001 PHOTOELECTRIC ELEMENTS AND REVISED SPECTRAL TYPES OF XX Cas R.K. Srivastava 18 March 1987 3002 HR 2554 - A POSSIBLE NEW Zeta Aur SYSTEM Thomas B. Ake, S.B. Parsons 19 March 1987 3003 53 PISCIUM - LARGER AMPLITUDE Marek Wolf 23 March 1987 3004 OBSERVATIONS AND A TIME OF MINIMUM OF TV Cet Daniel B. Caton, R. Lee Hawkins 25 March 1987 3005 ON THE PRIMARY MINIMUM OF ECLIPSING BINARY AY Cam J.B. Srivastava, C.D. Kandpal 30 March 1987 3006 AN UNEXPECTEDLY EARLY FADING OF V644 Cen (CPD -60d3278) J.K. Davies, A. Evans, M.F. Bode, D.C.B Whittet 3 April 1987 3007 PHOTOELECTRIC OBSERVATIONS OF TT ARIETIS ON 1/2 OCTOBER 1986 S. Rossiger 6 April 1987 3008 DELTA Cap: A POSSIBLE RS CVn BINARY R.K. Srivastava 9 April 1987 3009 ON THE CONSTANCY OF SOME STARS IN NGC 2287 = MESSIER 41 Brian A. Skiff 13 April 1987 3010 AN IMPROVEMENT OF THE ROTATIONAL PERIOD OF CQ UMa Zdenek Mikulasek 16 April 1987 3011 CORRECT PERIOD OF THE ECLIPSING STAR MN AURIGAE H. Gessner 16 April 1987 3012 JHK LIGHT CURVES OF CG CYGNI J.K. Davies, D.K. Bedford, J.J. Fuensalida, M.J. Arevalo 17 April 1987 3013 OPTICAL BEHAVIOUR OF THE X-RAY BINARY V1727 CYGNI = 4U 2129+47 IN 1986 W.
    [Show full text]
  • Effects of Rotation Arund the Axis on the Stars, Galaxy and Rotation of Universe* Weitter Duckss1
    Effects of Rotation Arund the Axis on the Stars, Galaxy and Rotation of Universe* Weitter Duckss1 1Independent Researcher, Zadar, Croatia *Project: https://www.svemir-ipaksevrti.com/Universe-and-rotation.html; (https://www.svemir-ipaksevrti.com/) Abstract: The article analyzes the blueshift of the objects, through realized measurements of galaxies, mergers and collisions of galaxies and clusters of galaxies and measurements of different galactic speeds, where the closer galaxies move faster than the significantly more distant ones. The clusters of galaxies are analyzed through their non-zero value rotations and gravitational connection of objects inside a cluster, supercluster or a group of galaxies. The constant growth of objects and systems is visible through the constant influx of space material to Earth and other objects inside our system, through percussive craters, scattered around the system, collisions and mergers of objects, galaxies and clusters of galaxies. Atom and its formation, joining into pairs, growth and disintegration are analyzed through atoms of the same values of structure, different aggregate states and contiguous atoms of different aggregate states. The disintegration of complex atoms is followed with the temperature increase above the boiling point of atoms and compounds. The effects of rotation around an axis are analyzed from the small objects through stars, galaxies, superclusters and to the rotation of Universe. The objects' speeds of rotation and their effects are analyzed through the formation and appearance of a system (the formation of orbits, the asteroid belt, gas disk, the appearance of galaxies), its influence on temperature, surface gravity, the force of a magnetic field, the size of a radius.
    [Show full text]
  • Ground Based, Space Based, Infrastructure, Technological Development, and State of the Profession Activities
    Ground Based, Space Based, Infrastructure, Technological Development, and State of the Profession Activities Ground Based, Space Based, Technological Development, and State of the Profession Activities Ground Based, Space Based, and Technological Development Activities Ground Based and Space Based Activities Ground Based, Infrastructure, Technological Development, and State of the Profession Activities Ground Based, Infrastructure, Technological Development, State of the Profession, and Other Activities Ground Based, Infrastructure, and Technological Development Activities Ground Based, Infrastructure, and State of the Profession Activities Ground Based and Infrastructure Activities Ground Based, Technological Development, and State of the Profession Activities Ground Based and Technological Development Activities Ground Based Projects Space Based, Infrastructure, Technological Development, and State of the Profession Activities Space Based, Infrastructure, Technological Development Activities Space Based and Infrastructure Activities Space Based, Technological Development, and State of the Profession Activities Space Based and Technological Development Activities Space Based and State of the Profession Activities Space Based Projects Infrastructure, Technological Development, and State of the Profession Activities Infrastructure, Technological Development, and Other Activities Infrastructure and Technological Development Activities Infrastructure, State of the Profession, and Other Activities Infrastructure and State of the Profession
    [Show full text]
  • Variable Star Section
    No. 21 (C1996) PUBLICATIONS OF THE VARIABLE STAR SECTION ROYAL ASTRONOMICAL SOCIETY OF NEW ZEALAND A GENERAL INDEX by Stars, Subjects and Authors to Publications No. 1-20 Director: Frank M. Bateson P.O. Box 3093 Greerton, tauranga New Zealand ISSN 0111-736X PUBLICATIONS OF THE VARIABLE STAR SECTION ROYAL ASTRONOMICAL SOCIETY OF NEW ZEALAND No. 21 CONTENTS 1. A GENERAL INDEX TO THE PUBLICATIONS OF THE VARIABLE STAR SECTION (R.A.S.N.Z.) NUMBERS 1-20 G.W. Christie, Ranald Mcintosh and O.R. Hull 2. INDIVIDUAL STARS 15. SUBJECT INDEX 24. AUTHOR INDEX 1996 July 20th PubL Variable Star Section, RASNZ ©Astronomical Research Ltd 21:1-28 General Index to the Publications of the Variable Star Section (R.A.S.N.Z.) Numbers 1-20 G.w. CHRISTIE1, RANALD MCINTOSH2 AND O.R. HULL3 'Auckland Observatory, Auckland, New Zealand Electronic matt [email protected] 'Variable Star Section, RASNZ Electronic mail: [email protected] 'Variable Star Section, RASNZ Abstract: A cummulative index to the first twenty issues of the Publications of the Variable Star Section (R. A.S.N.Z.) covering the period 1973 to 1995 is presented. 1. EXPLANATION The following index is divided into three sections. The first part is the index to Individual Stars, the second part is the Subject Index and the third part is the Author Index. In all sections, each entry consists of the title of the paper followed by the list of authors, the Publication number in parentheses, the page number and finally the nominal year of publication, also in parentheses.
    [Show full text]
  • Brightest Stars : Discovering the Universe Through the Sky's Most Brilliant Stars / Fred Schaaf
    ffirs.qxd 3/5/08 6:26 AM Page i THE BRIGHTEST STARS DISCOVERING THE UNIVERSE THROUGH THE SKY’S MOST BRILLIANT STARS Fred Schaaf John Wiley & Sons, Inc. flast.qxd 3/5/08 6:28 AM Page vi ffirs.qxd 3/5/08 6:26 AM Page i THE BRIGHTEST STARS DISCOVERING THE UNIVERSE THROUGH THE SKY’S MOST BRILLIANT STARS Fred Schaaf John Wiley & Sons, Inc. ffirs.qxd 3/5/08 6:26 AM Page ii This book is dedicated to my wife, Mamie, who has been the Sirius of my life. This book is printed on acid-free paper. Copyright © 2008 by Fred Schaaf. All rights reserved Published by John Wiley & Sons, Inc., Hoboken, New Jersey Published simultaneously in Canada Illustration credits appear on page 272. Design and composition by Navta Associates, Inc. No part of this publication may be reproduced, stored in a retrieval system, or transmitted in any form or by any means, electronic, mechanical, photocopying, recording, scanning, or otherwise, except as permitted under Section 107 or 108 of the 1976 United States Copyright Act, without either the prior written permission of the Publisher, or authorization through payment of the appropriate per-copy fee to the Copyright Clearance Center, 222 Rosewood Drive, Danvers, MA 01923, (978) 750-8400, fax (978) 646-8600, or on the web at www.copy- right.com. Requests to the Publisher for permission should be addressed to the Permissions Department, John Wiley & Sons, Inc., 111 River Street, Hoboken, NJ 07030, (201) 748-6011, fax (201) 748-6008, or online at http://www.wiley.com/go/permissions.
    [Show full text]
  • Mark Blackford’S Equipment Setup for Imaging the Very Bright Binary Eta Carinae - See Mark’S Article on This New VSS Project on Page 12
    Newsletter 2019-2 April 2019 www.variablestarssouth.org Mark Blackford’s equipment setup for imaging the very bright binary eta Carinae - see Mark’s article on this new VSS project on page 12. Contents From the director - Mark Blackford .............................................................................................................................................................2 Period issues in BS Mus: interim report – Tom Richards, Robert Jenkins ......................................3 An archive of Variable Star Section publications – Mati Morel ..........................................................................7 Photometry of eta Carinae – Mark Blackford...........................................................................................................................12 V777 Sag - a successful campaign – S Walker, M Blackford, EBudding ......................................13 ToMs, insights into Algolism, and the IBVS – E. Budding, D. Blane, M. G. Blackford, P. A. Reed ............................................................................................................................................................................................................................15 Two new pulsating discoveries – Mark Blackford ...........................................................................................................17 What can one do about lightning? – Greg Crawford ....................................................................................................20 Publication
    [Show full text]
  • Stellar Structure and Evolution: Syllabus 3.3 the Virial Theorem and Its Implications (ZG: P5-2; CO: 2.4) Ph
    Page 2 Stellar Structure and Evolution: Syllabus 3.3 The Virial Theorem and its Implications (ZG: P5-2; CO: 2.4) Ph. Podsiadlowski (MT 2006) 3.4 The Energy Equation and Stellar Timescales (CO: 10.3) (DWB 702, (2)73343, [email protected]) (www-astro.physics.ox.ac.uk/˜podsi/lec mm03.html) 3.5 Energy Transport by Radiation (ZG: P5-10, 16-1) and Con- vection (ZG: 16-1; CO: 9.3, 10.4) Primary Textbooks 4. The Equations of Stellar Structure (ZG: 16; CO: 10) ZG: Zeilik & Gregory, “Introductory Astronomy & Astro- • 4.1 The Mathematical Problem (ZG: 16-2; CO: 10.5) physics” (4th edition) 4.1.1 The Vogt-Russell “Theorem” (CO: 10.5) CO: Carroll & Ostlie, “An Introduction to Modern Astro- • 4.1.2 Stellar Evolution physics” (Addison-Wesley) 4.1.3 Convective Regions (ZG: 16-1; CO: 10.4) also: Prialnik, “An Introduction to the Theory of Stellar Struc- • 4.2 The Equation of State ture and Evolution” 4.2.1 Perfect Gas and Radiation Pressure (ZG: 16-1: CO: 1. Observable Properties of Stars (ZG: Chapters 11, 12, 13; CO: 10.2) Chapters 3, 7, 8, 9) 4.2.2 Electron Degeneracy (ZG: 17-1; CO: 15.3) 1.1 Luminosity, Parallax (ZG: 11; CO: 3.1) 4.3 Opacity (ZG: 10-2; CO: 9.2) 1.2 The Magnitude System (ZG: 11; CO: 3.2, 3.6) 5. Nuclear Reactions (ZG: P5-7 to P5-9, P5-12, 16-1D; CO: 10.3) 1.3 Black-Body Temperature (ZG: 8-6; CO: 3.4) 5.1 Nuclear Reaction Rates (ZG: P5-7) 1.4 Spectral Classification, Luminosity Classes (ZG: 13-2/3; CO: 5.2 Hydrogen Burning 5.1, 8.1, 8.3) 5.2.1 The pp Chain (ZG: P5-7, 16-1D) 1.5 Stellar Atmospheres (ZG: 13-1; CO: 9.1, 9.4) 5.2.2 The CN Cycle (ZG: P5-9; 16-1D) 1.6 Stellar Masses (ZG: 12-2/3; CO: 7.2, 7.3) 5.3 Energy Generation from H Burning (CO: 10.3) 1.7 Stellar Radii (ZG: 12-4/5; CO: 7.3) 5.4 Other Reactions Involving Light Elements (Supplementary) 2.
    [Show full text]