Esa Sere Aeronautics and Européen Space Agency Space ^•Pr Européen Space Administration O M?2-~ Esa SP-281 June 1988 (Volume 1)

Total Page:16

File Type:pdf, Size:1020Kb

Esa Sere Aeronautics and Européen Space Agency Space ^•Pr Européen Space Administration O M?2-~ Esa SP-281 June 1988 (Volume 1) e , fâ&oÀ ï}^f*Wo'à>r<r' SP-281 Volume 1 91},M7<L Proceedings of a Celebratory Symposium held at Goddard Space Flight Center, Greenbelt, Maryland, USA 12-15 April 1988 NASA National tf|esa sere Aeronautics and européen space agency Space ^•pr européen space Administration o M?2-~ esa SP-281 June 1988 (Volume 1) ftoUé C7> \J\j UU/<$<*<: A DECADE OF UV ASTRONOMY WITH THE IUE SATELLITE. v jaov,! Proceedings of a Celebratory Symposium > hold at Goddard Space night Center, Greenbelt, Maryland, USA, 12-15 April 1988 . <\ Sponsored by: -National Aeronautics and Space Administration (NASA) -European Space Agency (ESA) -UK Science and Engineering Research Council (SERC) Co-sponsored by: - American Astronomical Society (AAS) european space agency / agence spatiale européenne 8-10, rue Mario-Nikis, 75738 PARIS CEDEX 15, France Scientific Organising Committee Y. Kondo, Chairman W. Wamsteker, Co-Chairman R. Wilson, Co-Chairman M. A'Hearn M. Maraschi A. Dupree F. Praderie R. Green B. Savage M. Grewing M.-H. Ulrich E. Jenkins A. Willis C. Jordan L. Willson J. Linsky Local Organising Commmittee J. Mead, Co-chairman A. Michalitsianos, Co-chairman P. Boyce D. West D. DeVorkin N. Longdon, Editor S. Maran E.J. Rolfe, Editor J. Nichols-Bohlin Session Chairmen R. Green, M. Grewing, E.B. Jenkins, Y Kondo, J.L. Linsky, J. Mead, A. Michalitsianos, D. Stickland and W. Wamsteker Scientific Coordinators Y Kondo, W. Wamsteker & R. Wilson Proceedings published and ESA Publications Division distributed by ESTEC, Noordwijk, The Netherlands Edited by E.J. Rolfe Price code 140 Dutch Guilders ISSN 0379 6566 Copyright © 1988 European Space Agency "/v Editorial Note These Proceedings are published in two volumes, containing invited and poster papers on the topics indicated below. Some poster papers were selected for oral presentation and these are indicated as 'Contributed Papers'. For convenient reference each volume contains the full list of participants. Volume 1 Solar System Science Supernovae and their Remnants X-ray and Cataclysmic Binary Systems Binary Stars, Circumstellar Matter and Mass Transfer White Dwarf Stars Stellar Activity Stellar Atmospheres and Variable Stars Volume 2 Star Formation, Pre-Main Sequence Stars and Stellar Winds Planetary Nebulae and their Nuclei and Nebulous Stars Star Clusters The Interstellar Medium Quasars and Active Galactic Nuclei Missions, Techniques and Databases Panel Discussion - How to Use IUE Creatively Contents Foreword y. Kondo Welcoming Address J. Sahade Invited Papers Observing SN 1987A with lUE R.P. Kirshner Cataclysmic variables A. Cassatella & P.L Selvelli White dwarfs V. Weidemann 17 lUE observations of pulsating stars: atmospheric structure, shock waves and stellar winds LA Willson 29 lUE observations of planetary atmospheres T. Encrenaz 41 Comets M.F. A'Heam 47 Some recent results from the study of cool stars A.K. Dupree 59 lUE observations and physical processes of interacting binary stars S.N. Shore 67 Solar System Science lo: lUE observations of its atmosphere and the plasma torus (Contributed paper) G.E. Ballester et al. 79 On the abundance of micron-sized particles in Saturn's A and B rings ft Wagener & J. Caldwell 85 Jovian equatorial H2 emission from 1978-1987 M.A. McGrath et al. 89 Large-time-scale variation in hydrogen emission from Jupiter and Saturn D.E. Shemansky, D.T. Hall & J.B. Holberg 93 Phenomenological analysis of Jovian north auroral H2 Lyman band emissions T.A. Livengood, H.W. Moos & G.E Ballester 97 Supernovae and their Remnants Observations of SN 1987a: the narrow emission lines (Contributed paper) N. Panagia 103 The progenitor of SN 1987A (Contributed paper) G. Sonneborn 107 The complete visual light curve of SN 1987A: Thirteen months of FES observations G. Sonneborn 111 Spectral evolution of SN 1987A in the IUE long wavelength range L. Sanz Fernandez de Cordoba et al. 115 IUE observations of oxygen-rich supernova remnants W.P. Blair et al. 117 Ejecta in SN 1006: the knotty issue R.A. Fesen & A.J.S. Hamilton 121 X-ray and Cataclysmic Binary Systems Far UV observations of black hole candidates: The case of LMC X-3 (Contributed paper) A. Treves et al. 127 IUE spectrophotometry of the accretion disk of HZ Her/Her X-1 S.J. Boyle & I.D. Howarth 133 Simultaneous IUE, Exosat and optical observations of the unusual AM Her type variable H0538+608 C.R. Schrader et al. 137 A 0535+26/HDE 245770 - a typical Be/X-ray transient system: 12 years of coordinated multiwavelength monitoring F Giovannelli et al. 141 IUE and optical observations of X-ray sources in the LMC L Bianchi & M. Pakull 145 The analysis of spectra of novae taken near maximum L.L. Stryker et al. 149 CONTENTS Physical parameters of Nova Muscae 1983 during its nebular stage J. Krautter, R.E. Williams & H. Ogelman The 1981 outburst of the old nova GK Persei C.-C. Wu et al. Observations of classical novae in outburst S Starrfield et al. Observations and simulations of Nova Vul 1984 #2: a nova with éjecta rich in oxygen neon and magnesium S. Starrfield et al. Observations and simulations of recurrent novae: U Sco and V394 CrA S Starrfield et al. Optical and UV observations of Nova Vul 1987 S. Starrfield et al. UV observations of the LMC nova 1988 S. Starrfield et al. SS Cygni in quiescence A.V. Holm & R.S. Polidan UV and optical line emission from the shell of the old nova GK Persei M.F. Bode et al. IUE observations of the 1987 superoutburst of the dwarf nova Z Cha E. Harlaftis et al. Binary Stars, Circumstellar Matter and Mass Transfer Observations of galactic WC + 0 binary systems: HD 97152 and HD 152270 L.H. Auer, C. Colomé & G. Koenigsberger Atmospheric eclipse effects in Wolf-Rayet binaries in the small Magellanic cloud G. Koenigsberger, A.F.J. Moffat & L.H. Auer Mass flow in the interacting binary TX Ursae Majoris G.E. McCluskey Jr., C.RS. McCluskey & Y. Kondo A new study of the interacting binary star V356 Sgr R.S. Polidan Matter streams in semi-detached binary systems D. Wonnacott The November 1987 eclipse of the Zeta Aurigae system HR 2554 T.B. Ake III & SB. Parsons Asymmetry in Zeta Aurigae chromospheres I.A. Ahmad VUl CONTENTS Super-ionized plasmas in Algol binaries M.J. Plavec 221 HD 207739 and other F + Be variables S.8. Parsons, R.C. Dempsey & B.W. Bopp 225 Searching for the white dwarf in WZ Sagittae A.V. Holm 229 Model chromosphere and transition region for 56 Peg (KOIIp + wd): a preliminary study M.G. Munday 233 Cepheid binaries with large mass ratios (M,/M2) N.R. Evans 237 The orbit of the cepheid AW Per N.R. Evans & D.L. Welch 241 Companions to peculiar red giants: HR 363 and HR 1105 IB. Ake, H.R. Johnson & B.F. Peery 245 Direct UV observations of the circumstellar envelope of a Orionis R.E. Stencel et al. 249 Multi-wavelength observations of the peculiar red giant HR 3126 J.E. Pesce era/. 253 Recurrent shell infall events in a B0.5e star: HD 58978 1979-1988 C.A. Grady et al. 257 White Dwarf Stars IUE observations of a hot DAO white dwarf: Implications for diffusion theory and photospheric stratification IB. Holberg et al. 263 Temperature determinations of hot DA white dwarfs using IUE continuum flares D. Finley, G. Basri & S. Bowyer 267 The UV emission of accreting magnetic white dwarfs J-M. Bonnet-Bidaud & M. Mouchet 271 Stellar Activity IUE observations of rapidly rotating K dwarfs in the Pleiades T. Simon 279 On the flux-period anc1 flux-flux correlations in late-type stars B. Montesinos & C. Jordan 283 UV emission from the Sun and stars: a comparison of IUE and Skylab data A. Cappelli et al. 287 Spectral images of HD 199178 J.E. Neff, 0. Vilhu & FM. Walter 291 Doppler imaging of AR Lacertae at three epochs FM. Walter et al. 295 Rotational modulation study of hydrogen Lyman-alpha flux from 44i Bootis 0. Vilhu, J.E. Neff & T. Rahunen 299 Mapping of surface activity on the W UMa-type system VW Cephei D.H. Bradstreet & E.F. Guinan 303 UV flares on II Peg JIG. Doyle & P.B. Byrne 307 Chromospheric mass motions during a flare on UV Ceti K.J.H. Phillips et al. 311 The energy input mechanism into the lower transition regions between stellar chromospheres and coronae E. Bohm-Vitense 315 Transition regions of dM stars P.B. Byrne & J.G. Doyle 319 Transition region fluxes in A-F dwarfs: basal fluxes and dynamo activity FM. Walter, C.J. Schrijver & W. Boyd 323 Line formation in cool carbon star chromospheres D.G. Luttermoser, H.B. Johnson & E.H. Avrett 327 Lithium and chromospherically active single giants F.C. Fekel 331 Mg II flux and profile variability of hybrid-chromosphere stars A. Veale & A. Brown 335 The discovery of a co-rotating magnetosphere in a helium weak star: HD 5737 = a Scl S.N. Shore, D.N. Brown & G. Sonneborn 339 Observations of UV variability in RV Tauri stars E.W. Brugel & J.A. Cardelli 343 Stellar Atmospheres and Variable Stars Fluorescence processec and line identifications in the UV spectra of cool stars (Contributed paper) K.G. Carpenter & S. Johansson 349 Fell level population in luminous variable stars R. Viottietal. 357 Identification of new fluorescence processes in the UV spectra of cool stars from new energy levels of Fell and Crll S Johansson & K.G. Carpenter 361 Periodic modulation of the atmosphere of Alpha Orionis A.K. Dupree et al. 365 Mgll line profiles of the Mira S Carinae E.W.
Recommended publications
  • Download This Article in PDF Format
    A&A 619, A61 (2018) Astronomy https://doi.org/10.1051/0004-6361/201833747 & c ESO 2018 Astrophysics Dramatic change in the boundary layer in the symbiotic recurrent nova T Coronae Borealis G. J. M. Luna1,2,3 , K. Mukai4,5, J. L. Sokoloski6, T. Nelson7, P. Kuin8, A. Segreto9, G. Cusumano9, M. Jaque Arancibia10,11, and N. E. Nuñez11 1 CONICET-Universidad de Buenos Aires, Instituto de Astronomía y Física del Espacio (IAFE), Av. Inte. Güiraldes 2620, C1428ZAA Buenos Aires, Argentina e-mail: [email protected] 2 Universidad de Buenos Aires, Facultad de Ciencias Exactas y Naturales, Buenos Aires, Argentina 3 Universidad Nacional Arturo Jauretche, Av. Calchaquí 6200, F. Varela, Buenos Aires, Argentina 4 CRESST and X-ray Astrophysics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 5 Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA 6 Columbia Astrophysics Lab 550 W 120th St., 1027 Pupin Hall, MC 5247 Columbia University, New York, NY 10027, USA 7 Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA 8 University College London, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking RH5 6NT, UK 9 INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, Via U. La Malfa 153, 90146 Palermo, Italy 10 Departamento de Física y Astronomía, Universidad de La Serena, Av. Cisternas 1200, La Serena, Chile 11 Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE-CONICET), Av. España Sur 1512, J5402DSP San Juan, Argentina Received 29 June 2018 / Accepted 23 August 2018 ABSTRACT A sudden increase in the rate at which material reaches the most internal part of an accretion disk, i.e., the boundary layer, can change its structure dramatically.
    [Show full text]
  • The Radio Light Curve of the Gamma-Ray Nova in V407 Cyg: Thermal Emission from the Ionized Symbiotic Envelope, Devoured from Within by the Nova Blast
    The Astrophysical Journal, 761:173 (19pp), 2012 December 20 doi:10.1088/0004-637X/761/2/173 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE RADIO LIGHT CURVE OF THE GAMMA-RAY NOVA IN V407 CYG: THERMAL EMISSION FROM THE IONIZED SYMBIOTIC ENVELOPE, DEVOURED FROM WITHIN BY THE NOVA BLAST Laura Chomiuk1,2,3, Miriam I. Krauss1, Michael P. Rupen1, Thomas Nelson4, Nirupam Roy1, Jennifer L. Sokoloski5, Koji Mukai6,7, Ulisse Munari8, Amy Mioduszewski1, Jennifer Weston5, Tim J. O’Brien9, Stewart P. S. Eyres10, and Michael F. Bode11 1 National Radio Astronomy Observatory, P.O. Box O, Socorro, NM 87801, USA; [email protected] 2 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 3 Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA 4 School of Physics and Astronomy, University of Minnesota, 116 Church Street SE, Minneapolis, MN 55455, USA 5 Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA 6 CRESST and X-ray Astrophysics Laboratory, NASA/GSFC, Greenbelt, MD 20771, USA 7 Center for Space Science and Technology, University of Maryland Baltimore County, Baltimore, MD 21250, USA 8 INAF Astronomical Observatory of Padova, I-36012 Asiago (VI), Italy 9 Jodrell Bank Centre for Astrophysics, University of Manchester, Manchester M13 9PL, UK 10 Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK 11 Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD, UK Received 2012 June 23; accepted 2012 October 26; published 2012 December 5 ABSTRACT We present multi-frequency radio observations of the 2010 nova event in the symbiotic binary V407 Cygni, obtained with the Karl G.
    [Show full text]
  • An Atlas of Far-Ultraviolet Spectra of the Zeta Aurigae Binary 31 Cygni with Line Identifications
    The Astrophysical Journal Supplement Series, 211:27 (14pp), 2014 April doi:10.1088/0067-0049/211/2/27 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. AN ATLAS OF FAR-ULTRAVIOLET SPECTRA OF THE ZETA AURIGAE BINARY 31 CYGNI WITH LINE IDENTIFICATIONS Wendy Hagen Bauer1 and Philip D. Bennett2,3 1 Whitin Observatory, Wellesley College, 106 Central Street, Wellesley, MA 02481, USA; [email protected] 2 Department of Astronomy & Physics, Saint Mary’s University, Halifax, NS B3H 3C3, Canada 3 Eureka Scientific, Inc., 2452 Delmer Street, Suite 100, Oakland, CA 94602-3017, USA Received 2013 March 29; accepted 2013 October 26; published 2014 April 2 ABSTRACT The ζ Aurigae system 31 Cygni (K4 Ib + B4 V) was observed by the FUSE satellite during total eclipse and at three phases during chromospheric eclipse. We present the coadded, calibrated spectra and atlases with line identifications. During total eclipse, emission from high ionization states (e.g., Fe iii and Cr iii) shows asymmetric profiles redshifted from the systemic velocity, while emission from lower ionization states (e.g., Fe ii and O i) appears more symmetric and is centered closer to the systemic velocity. Absorption from neutral and singly ionized elements is detected during chromospheric eclipse. Late in chromospheric eclipse, absorption from the K star wind is detected at a terminal velocity of ∼80 km s−1. These atlases will be useful for interpreting the far-UV spectra of other ζ Aur systems, as the observed FUSE spectra of 32 Cyg, KQ Pup, and VV Cep during chromospheric eclipse resemble that of 31 Cyg.
    [Show full text]
  • THE 1979 ECLIPSE of ZETA AURIGAE Robert D. Chapman
    THE 1979 ECLIPSE OF ZETA AURIGAE Robert D. Chapman Laboratory forAstronomy and Solar Physics Goddard Space Flight Center Greenbelt, ND 20771 ABSTRACT Observations of the system ; Aurigae made around primary eclipse are described, and their significance is discussed in a preliminary fashion. THE OBSERVATIONS High-dispersion, long- and short-wavelength spectra of the atmospheric eclipsing binary star system ; Aurigae (K2II + B8V) have been obtained during a total of ten observing sessions between September 15, 1979 and March 31, 1980. Dates of observations, corresponding to numbered positions in Figure I are: (I) Sept. 15, (2) Nov. i, (3) Nov. 13, (4) Nov. 15, (S) Nov. 18, (6) Nov. 22, (7) Dec. 16, [8) Jan. 29, (9) Feb. 29, (10) Mar. 31. The spectrum obtained on Sept. 15 resembles the spectrum of a single late B-star [e.g. the B6V star o Eri). Atmospheric effects are present and increasing in strength between Nov. i and Nov. 18. To a first approximation, the spectrum changes appear to be an increase in strength and number of absorption lines with changes in the undisturbed continuum being small. This point requires further study, however. On Nov. 22, the B star had passed second contact, and the spectrum of the system was a pure emission line spectrum. At mid-eclipse, on Dec. 16 the spectrum had changed but little from its appearance on Nov. 22. The egress spectra obtained in 1980 are not significantly different in appearance from the ingress spectra. A study of differences in detail is being undertaken now. Figure 2 shows the behavior of the Fe II resonance lines in three spectra.
    [Show full text]
  • 136, June 2008
    British Astronomical Association VARIABLE STAR SECTION CIRCULAR No 136, June 2008 Contents Group Photograph, AAVSO/BAAVSS meeting ........................ inside front cover From the Director ............................................................................................... 1 Eclipsing Binary News ....................................................................................... 4 Experiments in the use of a DSLR camera for V photometry ............................ 5 Joint Meeting of the AAVSO and the BAAVSS ................................................. 8 Coordinated HST and Ground Campaigns on CVs ............................... 8 Eclipsing Binaries - Observational Challenges .................................................. 9 Peer to Peer Astronomy Education .................................................................. 10 AAVSO Acronyms De-mystified in Fifteen Minutes ...................................... 11 New Results on SW Sextantis Stars and Proposed Observing Campaign ........ 12 A Week in the Life of a Remote Observer ........................................................ 13 Finding Eclipsing Binaries in NSVS Data ......................................................... 13 British Variable Star Associations 1848-1908 .................................................. 14 “Chasing Rainbows” (The European Amateur Spectroscopy Scene) .............. 15 Long Term Monitoring and the Carbon Miras ................................................. 18 Cataclysmic Variables from Large Surveys: A Silent Revolution
    [Show full text]
  • On the Progenitor System of V392 Persei M
    Draft version September 26, 2018 Typeset using LATEX RNAAS style in AASTeX62 On the progenitor system of V392 Persei M. J. Darnley1 and S. Starrfield2 1Astrophysics Research Institute, Liverpool John Moores University, IC2 Liverpool Science Park, Liverpool, L3 5RF, UK 2School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287-1504, USA (Received 2018 May 2; Revised 2018 May 6; Accepted 2018 May 2; Published TBC) Keywords: novae, cataclysmic variables | stars: individual (V392 Per) On 2018 April 29.474 UT Nakamura(2018) reported the discovery of a new transient, TCP J04432130+4721280, at m = 6:2 within the constellation of Perseus. Follow-up spectroscopy by Leadbeater(2018) and Wagner et al.(2018) independently verified the transient as a nova eruption in the `Fe ii curtain' phase; suggesting that the eruption was discovered before peak. Buczynski(2018) reported that the nova peaked on April 29.904 with m = 5:6. Nakamura (2018) noted that TCP J04432130+4721280 is spatially coincident with the proposed Z Camelopardalis type dwarf nova (DN) V392 Persei (see Downes & Shara 1993). V392 Per is therefore among just a handful of DNe to subsequently undergo a nova eruption (see, e.g., Mr´ozet al. 2016). The AAVSO1 2004{2018 light curve for V392 Per indicates a quiescent system with V ∼ 16−17 mag, punctuated with three of four DN outbursts, the last in 2016. Downes & Shara(1993) recorded a quiescent range of 15 :0 ≤ mpg ≤ 17:5, Zwitter & Munari(1994) reported a magnitude limit of V > 17. These observations suggest an eruption amplitude of . 12 magnitudes, which could indicate the presence of an evolved donor in the system.
    [Show full text]
  • The Everchanging Pulsating White Dwarf GD358
    Astronomy & Astrophysics manuscript no. gd358 January 23, 2003 (DOI: will be inserted by hand later) The Everchanging Pulsating White Dwarf GD358 S.O. Kepler1, R. Edward Nather2, Don E. Winget2, Atsuko Nitta3, S. J. Kleinman3, Travis Metcalfe2;4, Kazuhiro Sekiguchi5, Jiang Xiaojun6, Denis Sullivan7, Tiri Sullivan7, Rimvydas Janulis8, Edmund Meistas8, Romualdas Kalytis8, Jurek Krzesinski9, Waldemar OgÃloza9, Staszek Zola10, Darragh O’Donoghue11, Encarni Romero-Colmenero11, Peter Martinez11, Stefan Dreizler12, Jochen Deetjen12, Thorsten Nagel12, Sonja L. Schuh12, Gerard Vauclair13, Fu Jian Ning13, Michel Chevreton14, Jan-Erik Solheim15, Jose M. Gonzalez Perez15, Frank Johannessen15, Antonio Kanaan16, Jos´eEduardo Costa1, Alex Fabiano Murillo Costa1, Matt A. Wood17, Nicole Silvestri17, T.J. Ahrens17, Aaron Kyle Jones18;¤, Ansley E. Collins19;¤, Martha Boyer20;¤, J. S. Shaw21, Anjum Mukadam2, Eric W. Klumpe22, Jesse Larrison22, Steve Kawaler23, Reed Riddle23, Ana Ulla24, and Paul Bradley25 1 Instituto de F´ısicada UFRGS, Porto Alegre, RS - Brazil e-mail: [email protected] 2 Department of Astronomy & McDonald Observatory, University of Texas, Austin, TX 78712, USA 3 Sloan Digital Sky Survey, Apache Pt. Observatory, P.O. Box 59, Sunspot, NM 88349, USA 4 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 USA e-mail: [email protected] 5 Subaru National Astronomical Observatory of Japan e-mail: [email protected] 6 Beijing Astronomical Observatory, Academy of Sciences, Beijing 100080, China e-mail: [email protected] 7 University of Victoria, Wellington, New Zealand 8 Institute of Theoretical Physics and Astronomy, Gostauto 12, Vilnius 2600, Lithuania 9 Mt. Suhora Observatory, Cracow Pedagogical University, Ul. Podchorazych 2, 30-084 Cracow, Poland 10 Jagiellonian University, Krakow, Poland e-mail: [email protected] 11 South African Astronomical Observatory 12 Universitat T¨ubingen,Germany 13 Universit´ePaul Sabatier, Observatoire Midi-Pyr´en´ees,CNRS/UMR5572, 14 av.
    [Show full text]
  • Abstracts Connecting to the Boston University Network
    20th Cambridge Workshop: Cool Stars, Stellar Systems, and the Sun July 29 - Aug 3, 2018 Boston / Cambridge, USA Abstracts Connecting to the Boston University Network 1. Select network ”BU Guest (unencrypted)” 2. Once connected, open a web browser and try to navigate to a website. You should be redirected to https://safeconnect.bu.edu:9443 for registration. If the page does not automatically redirect, go to bu.edu to be brought to the login page. 3. Enter the login information: Guest Username: CoolStars20 Password: CoolStars20 Click to accept the conditions then log in. ii Foreword Our story starts on January 31, 1980 when a small group of about 50 astronomers came to- gether, organized by Andrea Dupree, to discuss the results from the new high-energy satel- lites IUE and Einstein. Called “Cool Stars, Stellar Systems, and the Sun,” the meeting empha- sized the solar stellar connection and focused discussion on “several topics … in which the similarity is manifest: the structures of chromospheres and coronae, stellar activity, and the phenomena of mass loss,” according to the preface of the resulting, “Special Report of the Smithsonian Astrophysical Observatory.” We could easily have chosen the same topics for this meeting. Over the summer of 1980, the group met again in Bonas, France and then back in Cambridge in 1981. Nearly 40 years on, I am comfortable saying these workshops have evolved to be the premier conference series for cool star research. Cool Stars has been held largely biennially, alternating between North America and Europe. Over that time, the field of stellar astro- physics has been upended several times, first by results from Hubble, then ROSAT, then Keck and other large aperture ground-based adaptive optics telescopes.
    [Show full text]
  • VLBI Imaging of the RS Cvn Binary Star System HR 5110
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Accepted to the Astrophysical Journal on 2002 December 12 VLBI imaging of the RS CVn binary star system HR 5110 R. R. Ransom, N. Bartel and M. F. Bietenholz Department of Physics and Astronomy, York University 4700 Keele St., Toronto, Ontario, Canada M3J 1P3 M. I. Ratner, D. E. Lebach and I. I. Shapiro Harvard-Smithsonian Center for Astrophysics 60 Garden St., Cambridge, MA 02138 and J.-F. Lestrade Observatoire de Paris/DEMIRM 77 av. Denfert Rochereau, F-75014 Paris, France ABSTRACT We present VLBI images of the RS CVn binary star HR 5110 (=BH CVn; HD 118216), obtained from observations made at 8.4 GHz on 1994 May 29/30 in support of the NASA/Stanford Gravity Probe B project. Our images show an emission region with a core-halo morphology. The core was 0:39 0:09 mas ± (FWHM) in size, or 66% 20% of the 0:6 0:1 mas diameter of the chromospher- ± ± ically active K subgiant star in the binary system. The halo was 1:95 0:22 mas ± (FWHM) in size, or 1:8 0:2timesthe1:1 0:1 mas separation of the centers of ± ± the K and F stars. (The uncertainties given for the diameter of the K star and its separation from the F star each reflect the level of agreement of the two most recent published determinations.) The core increased significantly in brightness over the course of the observations and seems to have been the site of flare activ- ity that generated an increase in the total flux density of 200% in 12 hours.
    [Show full text]
  • September 2020 BRAS Newsletter
    A Neowise Comet 2020, photo by Ralf Rohner of Skypointer Photography Monthly Meeting September 14th at 7:00 PM, via Jitsi (Monthly meetings are on 2nd Mondays at Highland Road Park Observatory, temporarily during quarantine at meet.jit.si/BRASMeets). GUEST SPEAKER: NASA Michoud Assembly Facility Director, Robert Champion What's In This Issue? President’s Message Secretary's Summary Business Meeting Minutes Outreach Report Asteroid and Comet News Light Pollution Committee Report Globe at Night Member’s Corner –My Quest For A Dark Place, by Chris Carlton Astro-Photos by BRAS Members Messages from the HRPO REMOTE DISCUSSION Solar Viewing Plus Night Mercurian Elongation Spooky Sensation Great Martian Opposition Observing Notes: Aquila – The Eagle Like this newsletter? See PAST ISSUES online back to 2009 Visit us on Facebook – Baton Rouge Astronomical Society Baton Rouge Astronomical Society Newsletter, Night Visions Page 2 of 27 September 2020 President’s Message Welcome to September. You may have noticed that this newsletter is showing up a little bit later than usual, and it’s for good reason: release of the newsletter will now happen after the monthly business meeting so that we can have a chance to keep everybody up to date on the latest information. Sometimes, this will mean the newsletter shows up a couple of days late. But, the upshot is that you’ll now be able to see what we discussed at the recent business meeting and have time to digest it before our general meeting in case you want to give some feedback. Now that we’re on the new format, business meetings (and the oft neglected Light Pollution Committee Meeting), are going to start being open to all members of the club again by simply joining up in the respective chat rooms the Wednesday before the first Monday of the month—which I encourage people to do, especially if you have some ideas you want to see the club put into action.
    [Show full text]
  • Referierte Publikationen
    14 Publikationslisten Referierte Publikationen Abbott, T.M.C., M. Aguena, A. Alarcon, S. Allam, S. Allen, J. Granot, D. Green, I.A. Grenier, M.-H. Grondin, S. Guiriec, J. Annis, S. Avila, D. Bacon, K. Bechtol, A. Bermeo, G.M. E. Hays, D. Horan, G. Jóhannesson, D. Kocevski, M. Kova- Bernstein, E. Bertin, S. Bhargava, S. Bocquet, D. Brooks, D. cevic, M. Kuss, S. Larsson, L. Latronico, M. Lemoine-Gou- Brout, E. Buckley-Geer, D.L. Burke, A. Carnero Rosell, M. mard, J. Li, I. Liodakis, F. Longo, F. Loparco, M.N. Lovel- Carrasco Kind, J. Carretero, F.J. Castander, R. Cawthon, C. lette, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, Chang, X. Chen, A. Choi, M. Costanzi, M. Crocce, L.N. da G. Martí-Devesa, M.N. Mazziotta, J.E. McEnery, I. Mereu, Costa, T.M. Davis, J. de Vicente, J. de Rose, S. Desai, H.T. M. Meyer, P.F. Michelson, W. Mitthumsiri, T. Mizuno, Diehl, J.P. Dietrich, S. Dodelson, P. Doel, A. Drlica-Wagner, M.E. Monzani, E. Moretti, A. Morselli, I.V. Moskalenko, K. Eckert, T.F. Eifl er, J. Elvin-Poole, J. Estrada, S. Everett, M. Negro, E. Nuss, N. Omodei, M. Orienti, E. Orlando, M. A.E. Evrard, A. Farahi, I. Ferrero, B. Flaugher, P. Fosalba, Palatiello, V.S. Paliya, D. Paneque, Z. Pei, M. Persic, M. J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, D.W. Pesce-Rollins, V. Petrosian, F. Piron, H. Poon, T.A. Porter, Gerdes, T. Giannantonio, P. Giles, S. Grandis, D. Gruen, G. Principe, J.L.
    [Show full text]
  • The HR Diagram
    Name_______________________ Class_______________________ Date_______________________ Assignment #10 – The H-R Diagram A star is a delicately balanced ball of gas, fighting between two impulses: gravity, which wants to squeeze the gas all down to a single point, and radiation pressure, which wants to blast all the gas out to infinity. These two opposite forces balance out in a process called Hydrostatic Equilibrium, and keep the gas at a stable, fairly constant size. The radiation itself is due to the fusion of protons in the star's core – a process that produces huge amounts of energy. In class we've examined the most important properties of stars: their temperatures, colors and brightnesses. Now let's see if we can find some relationships between these stellar properties. We know that hotter stars are brighter, as described by the Stefan-Boltzmann Law, and we know that the hotter stars are also bluer, as described by Wien's Law. The H-R diagram is a way of displaying an important relationship between a star's Absolute Magnitude (or Luminosity), and its Spectral Type (or temperature). Remember, Absolute Magnitude is how bright a star would appear to be, if it were 10 parsecs away. Luminosity is how much total energy a star gives off per second. As we studied in a previous exercise, Spectral Type is a system of classifying stars by temperature, from hottest (type O) to coldest (type M). Each letter in the Spectral Type list (O, B, A, F, G, K, and M) is further subdivided into 10 steps, numbered 0 through 9, to make finer distinctions between stars.
    [Show full text]