1999-2000 Annual Report
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NIR High-Resolution Imaging and Radiative Transfer Modeling of the Frosty Leo Nebula
Planetary Nebulae in our Galaxy and Beyond Proceedings IAU Symposium No. 234, 2006 c 2006 International Astronomical Union M. J. Barlow & R. H. M´endez, eds. doi:10.1017/S1743921306003802 NIR high-resolution imaging and radiative transfer modeling of the Frosty Leo nebula K. Murakawa1, K. Ohnaka1, T. Driebe1, K.-H. Hofmann1, D. Schertl1,S.Oya2, and G. Weigelt1 1Max-Planck-Institut f¨ur Radioastronomie, Auf dem H¨ugel 69, D-53121 Bonn, Germany email: [email protected] 2Subaru telescope, 650 North A’ohoku Place, Hilo, HI 96720, USA Abstract. We present a K-band speckle image and HK-band polarimetric images of the proto- planetary nebula Frosty Leo obtained using the 6 m SAO telescope and the 8 m Subaru telescope, respectively. Our speckle image revealed clumpy structures in the hourglass-like bipolar nebula. The polarimetric data, for the first time, detected an elongated region with small polarizations and polarization vector alignment on the east side of the central star. We have performed radiative transfer calculations to model the dust shell of Frosty Leo. We found that micron-size grains in the equatorial dense region and small grains in the bipolar lobes are required to explain the total intensity images, the polarization images, and the spectral energy distribution. Keywords. speckle imaging, polarimetry, radiative transfer modeling, Frosty Leo, PPN 1. Introduction Frosty Leo is a well-studied oxygen-rich proto-planetary nebula (PPN). The deep wa- ter ice absorption feature at 3.1 µm(τ3.1µm∼3.3) was detected in the L-band spectrum (Rouan et al. -
The Evolutionary Status of the Frosty Leo Nebula
Asymmetrical Planetary Nebulae II: From Origins to Microstructures ASP Conference Series, Vol. 199, 2000 J.H. Kastner, N. Soker, & S. Rappaport, eds. The evolutionary status of The Frosty Leo Nebula Tyler Bourke1, A. R. Hyland2, Garry Robinson3, & Kevin Luhman1 1Harvard-Smithsonian Center for Astrophysics, Cambridge MA, USA 2Southern Cross University, Lismore NSW, Australia 3University College, UNSW-ADFA, Canberra ACT, Australia Abstract. We present new observational data for IRAS 09371+1212, the Frosty Leo Nebula, in the form of infrared spectra from 2.2–2.5µm which reveal photospheric bands of CO. The 12CO/13CO band ratio deter- mined is similar to those exhibited by evolved K giant stars, and supports the proposal that the object is highly evolved. The equivalent width of the CO bands implies, however, that the spectral type lies in the range G5III to K0III, somewhat earlier than K7III, as derived from colours and optical spectra. The smaller equivalent widths of the CO bands may re- flect a low metal abundance which could fit well with the considerable height of the source above the galactic plane (>0.9kpc). 1. Introduction The Frosty Leo Nebula, IRAS 09371+1212, remains unique with its extremely deep 3.1µm absorption feature, almost two decades in depth, its twin far-infrared emission features at 44 and 62µm, and its abnormal location, >0.9kpc from the plane of the Galaxy. Forveille et al. (1987; hereafter FMOL) concluded, primarily on the basis of its 2.6mm CO emission spectrum, that it is a post-AGB star with a bipolar circumstellar envelope, and suggested water ice mantles around the grains as the source of the excess emission in the 60µm IRAS band. -
Title a Self-Consistent Photoionization-Dust
A self-consistent photoionization-dust continuum-molecular line Title transfer model of NGC 7027 Author(s) Volk, K; Kwok, S Citation The Astrophysical Journal, 1997, v. 477 n. 2 pt. 1, p. 722-731 Issued Date 1997 URL http://hdl.handle.net/10722/179686 Rights Creative Commons: Attribution 3.0 Hong Kong License THE ASTROPHYSICAL JOURNAL, 477:722È731, 1997 March 10 ( 1997. The American Astronomical Society. All rights reserved. Printed in U.S.A. A SELF-CONSISTENT PHOTOIONIZATIONÈDUST CONTINUUMÈMOLECULAR LINE TRANSFER MODEL OF NGC 7027 KEVIN VOLK AND SUN KWOK Department of Physics and Astronomy, University of Calgary, Calgary, Alberta, Canada T2N 1N4 Received 1996 June 20; accepted 1996 September 23 ABSTRACT A model to simulate the entire spectrum (1000Ó to 1 cm) of the high-excitation young planetary nebula NGC 7027 is presented. The ionized, dust, and molecular components of the object are modeled using geometric parameters obtained from visible, radio, infrared, and CO data. The physical processes considered include recombination lines of H and He, collisional excited lines of metals, bf and † contin- uum radiations, two-photon radiation, dust continuum radiation, and molecular rotational and vibra- tional transitions. The dust component is assumed to be heated by a combination of direct starlight and the line and continuum radiation from the ionized nebula. The molecular component of the nebula is coupled to the dust component through the stimulated absorption of the dust continuum radiation. Spe- ciÐcally, we compare the predicted Ñuxes of the CO rotational lines and the 179.5 km water rotational line to those observed by the Infrared Space Observatory satellite. -
A Massive Bipolar Outflow and a Dusty Torus with Large Grains in the Preplanetary Nebula Iras 22036+5306 R
The Astrophysical Journal, 653:1241Y1252, 2006 December 20 # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. A MASSIVE BIPOLAR OUTFLOW AND A DUSTY TORUS WITH LARGE GRAINS IN THE PREPLANETARY NEBULA IRAS 22036+5306 R. Sahai,1 K. Young,2 N. A. Patel,2 C. Sa´nchez Contreras,3 and M. Morris4 Received 2006 June 19; accepted 2006 August 10 ABSTRACT We report high angular resolution (100)COJ ¼ 3Y2 interferometric mapping using the Submillimeter Array (SMA) of IRAS 22036+5306 (I22036), a bipolar preplanetary nebula (PPN) with knotty jets discovered in our HST snapshot survey of young PPNs. In addition, we have obtained supporting lower resolution (1000) CO and 13CO J ¼ 1Y0 observations with the Owens Valley Radio Observatory (OVRO) interferometer, as well as optical long-slit echelle spectra at the Palomar Observatory. The CO J ¼ 3Y2 observations show the presence of a very fast (220 km sÀ1), 39 À1 highly collimated, massive (0.03 M ) bipolar outflow with a very large scalar momentum (about 10 gcms ), and the characteristic spatiokinematic structure of bow shocks at the tips of this outflow. The H line shows an absorption feature blueshifted from the systemic velocity by 100 km sÀ1, which most likely arises in neutral interface material between the fast outflow and the dense walls of the bipolar lobes at low latitudes. The fast outflow in I22036, as in most PPNs, cannot be driven by radiation pressure. We find an unresolved source of submillimeter (and millimeter- wave) continuum emission in I22036, implying a very substantial mass (0.02Y0.04 M ) of large (radius k1 mm), cold (P50 K) dust grains associated with I22036’s toroidal waist. -
The Chemical Composition of Solar-Type Stars and Its Impact on the Presence of Planets
The chemical composition of solar-type stars and its impact on the presence of planets Patrick Baumann Munchen¨ 2013 The chemical composition of solar-type stars and its impact on the presence of planets Patrick Baumann Dissertation der Fakultat¨ fur¨ Physik der Ludwig-Maximilians-Universitat¨ Munchen¨ durchgefuhrt¨ am Max-Planck-Institut fur¨ Astrophysik vorgelegt von Patrick Baumann aus Munchen¨ Munchen,¨ den 31. Januar 2013 Erstgutacher: Prof. Dr. Achim Weiss Zweitgutachter: Prof. Dr. Joachim Puls Tag der mündlichen Prüfung: 8. April 2013 Zusammenfassung Wir untersuchen eine mogliche¨ Verbindung zwischen den relativen Elementhaufig-¨ keiten in Sternatmospharen¨ und der Anwesenheit von Planeten um den jeweili- gen Stern. Um zuverlassige¨ Ergebnisse zu erhalten, untersuchen wir ausschließlich sonnenahnliche¨ Sterne und fuhren¨ unsere spektroskopischen Analysen zur Bestim- mung der grundlegenden Parameter und der chemischen Zusammensetzung streng differenziell und relativ zu den solaren Werten durch. Insgesamt untersuchen wir 200 Sterne unter Zuhilfenahme von Spektren mit herausragender Qualitat,¨ die an den modernsten Teleskopen gewonnen wurden, die uns zur Verfugung¨ stehen. Mithilfe der Daten fur¨ 117 sonnenahnliche¨ Sterne untersuchen wir eine mogliche¨ Verbindung zwischen der Oberflachenh¨ aufigkeit¨ von Lithium in einem Stern, seinem Alter und der Wahrscheinlichkeit, dass sich ein oder mehrere Sterne in einer Um- laufbahn um das Objekt befinden. Fur¨ jeden Stern erhalten wir sehr exakte grundle- gende Parameter unter Benutzung einer sorgfaltig¨ zusammengestellten Liste von Fe i- und Fe ii-absorptionslinien, modernen Modellatmospharen¨ und Routinen zum Erstellen von Modellspektren. Die Massen und das Alter der Objekte werden mithilfe von Isochronen bestimmt, was zu sehr soliden relativen Werten fuhrt.¨ Bei jungen Sternen, fur¨ die die Isochronenmethode recht unzuverlssig¨ ist, vergleichen wir verschiedene alternative Methoden. -
A Guide to Smartphone Astrophotography National Aeronautics and Space Administration
National Aeronautics and Space Administration A Guide to Smartphone Astrophotography National Aeronautics and Space Administration A Guide to Smartphone Astrophotography A Guide to Smartphone Astrophotography Dr. Sten Odenwald NASA Space Science Education Consortium Goddard Space Flight Center Greenbelt, Maryland Cover designs and editing by Abbey Interrante Cover illustrations Front: Aurora (Elizabeth Macdonald), moon (Spencer Collins), star trails (Donald Noor), Orion nebula (Christian Harris), solar eclipse (Christopher Jones), Milky Way (Shun-Chia Yang), satellite streaks (Stanislav Kaniansky),sunspot (Michael Seeboerger-Weichselbaum),sun dogs (Billy Heather). Back: Milky Way (Gabriel Clark) Two front cover designs are provided with this book. To conserve toner, begin document printing with the second cover. This product is supported by NASA under cooperative agreement number NNH15ZDA004C. [1] Table of Contents Introduction.................................................................................................................................................... 5 How to use this book ..................................................................................................................................... 9 1.0 Light Pollution ....................................................................................................................................... 12 2.0 Cameras ................................................................................................................................................ -
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, -
Planetary Nebulas
The History, Observation, and Science of Planetary Nebulas Plus: Mars Exploration Update (at end) Tuesday, February 5, 2013 What is a “Planetary” Nebula? Dark Nebula: We see it because of light it blocks. Emission Nebula: The cloud itself glows. Planetary Nebula Galaxies were once classed as nebulas, too. Supernova Remnant: Reflection Nebula: What’s left after a star goes “boom” Reflects light from a star. “nebula” is latin for mist, fog, or cloud. Tuesday, February 5, 2013 Origin of the Term ‘Planetary Nebula’ William Herschel: Philosophical Transactions of the Royal Society, 1785, Volume 75, Page 263 ff*: Planetary Nebulae “I shall conclude this paper with an account of a few heavenly bodies, that from their singular appearance leave me almost in doubt where to class them...being all over of an uniform brightness, which it differs from nebulae, it light seems however to be of the starry nature, which suffers not so much as the planetary disks are know to do, when much magnified. The planetary appearance of the first two is so remarkable that we can hardly suppose them to be nebulae; their light is so uniform, as well as vivid, the diameters so small and well defined as to make it almost improbable that they should belong to that species of bodies. On the other hand, the effect of different power seems to be much against their light’s being of a planetary nature, since it preserves its brightness nearly in the same manner as to the stars in similar trials.” He describes five planetaries (Six listed, 5 and 6 appear to be repeats): NGC 7293 (Helix), NGC 7662 (Blue Snowball), NGC 6369 (Little Ghost), NGC 6853 (Dumbbell), NGC 6894 (Diamond Ring) He makes two guesses in 1785 about what they are: Star clusters that can’t be resolved, or Dead or dying stars, possibly multiple stars falling into each other. -
Seeing the Light: the Art and Science of Astronomy
Chapter 1 Seeing the Light: The Art and Science of Astronomy In This Chapter ▶ Understanding the observational nature of astronomy ▶ Focusing on astronomy’s language of light ▶ Weighing in on gravity ▶ Recognizing the movements of objects in space tep outside on a clear night and look at the sky. If you’re a city dweller Sor live in a cramped suburb, you see dozens, maybe hundreds, of twin- kling stars. Depending on the time of the month, you may also see a full Moon and up to five of the eight planets that revolve around the Sun. A shooting star or “meteor” may appear overhead. What you actually see is the flash of light from a tiny piece of comet dust streaking through the upper atmosphere. Another pinpoint of light moves slowly and steadily across the sky. Is it a space satellite, such as the Hubble Space Telescope, or just a high-altitude airliner? If you have a pair of binoculars, you may be able to see the difference. Most air- liners have running lights, and their shapes may be perceptible. If you liveCOPYRIGHTED in the country — on the seashore MATERIAL away from resorts and develop- ments, on the plains, or in the mountains far from any floodlit ski slope — you can see thousands of stars. The Milky Way appears as a beautiful pearly swath across the heavens. What you’re seeing is the cumulative glow from millions of faint stars, individually indistinguishable with the naked eye. At a great observation place, such as Cerro Tololo in the Chilean Andes, you can see even more stars. -
Observational Constraints on Models of Beta Hydri
Observational Constraints on Models of β Hydri João Fernandes Observatório Astronómico da Universidade de Coimbra, Coimbra, Portugal Mário J.P.F.G. Monteiro Departamento de Matemática Aplicada, Faculdade de Ciências da Universidade do Porto, and Centro de Astrofísica da Universidade do Porto, Porto, Portugal 2002 September 25 Abstract. A review of the models for the star β Hydri is done by adjusting the evolutionary sequences to the most recent bolometric, spectroscopic and astrometric data. The dependence of the solution on some of the relevant modelling parameters is analysed and the degeneracy of the solution using the HR Diagram analysis is discussed. We briefly describe how the seismic study of the star can help to clarify some of the degeneracy of the model solutions. Keywords: β Hydri; Stellar Evolution; Oscillations 1. Observations of β Hydri β Hydri (HD 2151, HR 98, HIP 2021) is a G2 IV star, in the neighbourhood of the Sun, belonging to the old disc of the Galaxy. This evolved star is fre- quently seen as the distant future of the Sun (Dravins et al. 1993). Recently, Bedding et al. (2001) and Carrier et al. (2001) confirmed the presence of solar-type oscillations in β Hydri. In Table I we present the available data on β Hydri. Table I. Observational data for β Hydri. Observable Value Source L=L 3:51±0:11 Blackwell et al. (1998);DiBenedetto (1998) Teff (K) 5774±60 DiBenedetto (1998) Z=X 0:019±0:003 Favata et al. (1997);Castro et al. (1999) ∆ν (µHz) 56:2±2:0 Bedding et al. -
Astrophysics
Publications of the Astronomical Institute rais-mf—ii«o of the Czechoslovak Academy of Sciences Publication No. 70 EUROPEAN REGIONAL ASTRONOMY MEETING OF THE IA U Praha, Czechoslovakia August 24-29, 1987 ASTROPHYSICS Edited by PETR HARMANEC Proceedings, Vol. 1987 Publications of the Astronomical Institute of the Czechoslovak Academy of Sciences Publication No. 70 EUROPEAN REGIONAL ASTRONOMY MEETING OF THE I A U 10 Praha, Czechoslovakia August 24-29, 1987 ASTROPHYSICS Edited by PETR HARMANEC Proceedings, Vol. 5 1 987 CHIEF EDITOR OF THE PROCEEDINGS: LUBOS PEREK Astronomical Institute of the Czechoslovak Academy of Sciences 251 65 Ondrejov, Czechoslovakia TABLE OF CONTENTS Preface HI Invited discourse 3.-C. Pecker: Fran Tycho Brahe to Prague 1987: The Ever Changing Universe 3 lorlishdp on rapid variability of single, binary and Multiple stars A. Baglln: Time Scales and Physical Processes Involved (Review Paper) 13 Part 1 : Early-type stars P. Koubsfty: Evidence of Rapid Variability in Early-Type Stars (Review Paper) 25 NSV. Filtertdn, D.B. Gies, C.T. Bolton: The Incidence cf Absorption Line Profile Variability Among 33 the 0 Stars (Contributed Paper) R.K. Prinja, I.D. Howarth: Variability In the Stellar Wind of 68 Cygni - Not "Shells" or "Puffs", 39 but Streams (Contributed Paper) H. Hubert, B. Dagostlnoz, A.M. Hubert, M. Floquet: Short-Time Scale Variability In Some Be Stars 45 (Contributed Paper) G. talker, S. Yang, C. McDowall, G. Fahlman: Analysis of Nonradial Oscillations of Rapidly Rotating 49 Delta Scuti Stars (Contributed Paper) C. Sterken: The Variability of the Runaway Star S3 Arietis (Contributed Paper) S3 C. Blanco, A. -
Arxiv:Astro-Ph/0306160V1 9 Jun 2003
Submitted to Astronomical Journal The Chemical Composition of Two Supergiants in the Dwarf Irregular Galaxy WLM Kim A. Venn Macalester College, Saint Paul, MN, 55105; [email protected] University of Minnesota, 116 Church Street S.E., Minneapolis, MN, 55455 Eline Tolstoy Kapteyn Institute, University of Groningen, PO Box 800, 9700AV Groningen, the Netherlands; [email protected] Andreas Kaufer European Southern Observatory, Alonso de Cordova 3107, Santiago 19, Chile; [email protected] Evan D. Skillman Department of Astronomy, University of Minnesota, 116 Church Street S.E., Minneapolis, MN, 55455; [email protected] Sonya M. Clarkson Macalester College, Saint Paul, MN, 55105 arXiv:astro-ph/0306160v1 9 Jun 2003 Stephen J. Smartt Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK; [email protected] Danny J. Lennon Isaac Newton Group of Telescopes (ING), Santa Cruz de La Palma, Canary Islands, E-38700, Spain; [email protected] and Rolf P. Kudritzki –2– Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, 95822; [email protected] ABSTRACT The chemical composition of two stars in WLM have been determined from high quality UVES data obtained at the VLT UT21. The model atmospheres analysis shows that they have the same metallicity, [Fe/H] = −0.38 ±0.20 (±0.29)2. Reliable magnesium abundances are determined from several lines of two ionization states in both stars resulting in [Mg/Fe] = −0.24 ±0.16 (±0.28). This result suggests that the [α(Mg)/Fe] ratio in WLM may be suppressed rel- ative to solar abundances (also supported by differential abundances relative to similar stars in NGC 6822 and the SMC).