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Spiral Arms in Disks: Planets Or Gravitational Instability?
Spiral Arms in Disks: Planets or Gravitational Instability? Item Type Article Authors Dong, Ruobing; Najita, Joan R.; Brittain, Sean Citation Ruobing Dong et al 2018 ApJ 862 103 DOI 10.3847/1538-4357/aaccfc Publisher IOP PUBLISHING LTD Journal ASTROPHYSICAL JOURNAL Rights © 2018. The American Astronomical Society. Download date 27/09/2021 14:50:30 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/631109 The Astrophysical Journal, 862:103 (19pp), 2018 August 1 https://doi.org/10.3847/1538-4357/aaccfc © 2018. The American Astronomical Society. Spiral Arms in Disks: Planets or Gravitational Instability? Ruobing Dong (董若冰)1,2 , Joan R. Najita3, and Sean Brittain3,4 1 Department of Physics & Astronomy, University of Victoria, Victoria BC V8P 1A1, Canada 2 Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA; [email protected] 3 National Optical Astronomical Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA; [email protected] 4 Department of Physics & Astronomy, 118 Kinard Laboratory, Clemson University, Clemson, SC 29634-0978, USA; [email protected] Received 2018 May 8; revised 2018 June 2; accepted 2018 June 13; published 2018 July 27 Abstract Spiral arm structures seen in scattered-light observations of protoplanetary disks can potentially serve as signposts of planetary companions. They can also lend unique insights into disk masses, which are critical in setting the mass budget for planet formation but are difficult to determine directly. A surprisingly high fraction of disks that have been well studied in scattered light have spiral arms of some kind (8/29), as do a high fraction (6/11) of well- studied Herbig intermediate-mass stars (i.e., Herbig stars >1.5 Me). -
7 Planetary Rings Matthew S
7 Planetary Rings Matthew S. Tiscareno Center for Radiophysics and Space Research, Cornell University, Ithaca, NY, USA 1Introduction..................................................... 311 1.1 Orbital Elements ..................................................... 312 1.2 Roche Limits, Roche Lobes, and Roche Critical Densities .................... 313 1.3 Optical Depth ....................................................... 316 2 Rings by Planetary System .......................................... 317 2.1 The Rings of Jupiter ................................................... 317 2.2 The Rings of Saturn ................................................... 319 2.3 The Rings of Uranus .................................................. 320 2.4 The Rings of Neptune ................................................. 323 2.5 Unconfirmed Ring Systems ............................................. 324 2.5.1 Mars ............................................................... 324 2.5.2 Pluto ............................................................... 325 2.5.3 Rhea and Other Moons ................................................ 325 2.5.4 Exoplanets ........................................................... 327 3RingsbyType.................................................... 328 3.1 Dense Broad Disks ................................................... 328 3.1.1 Spiral Waves ......................................................... 329 3.1.2 Gap Edges and Moonlet Wakes .......................................... 333 3.1.3 Radial Structure ..................................................... -
The Future of Spaceimaging
(NASA-CR-198818) THE FUTURE OF N95-31364 SPACE IMAGING. REPORT OF A COMMUNITY-BASED STUDY OF AN ADVANCED CAMERA FOR THE HUBBLE Unclas SPACE TELESCOPE Final Technical Report (Space Telescope Science Inst.) 150 p G3/89 0055789 TheFuture of SpaceImaging hen Lyman Spitzer first proposed a great, earth-orbiting telescope in I946, the nudear energy source of stars had been known for just six years. Knowledge of galaxies beyond our own and the understanding that our universe is expanding were only about twenty years of age in the human consciousness. The planet Pluto was seventeen. Quasars, black holes, gravitational lenses, and detection of the Big Bang were still in the future--together with much of what constitutes our current un- derstanding of the solar system and the cosmos beyond it. In I993, forty- seven years after it was conceived in a forgotten milieu of thought, the Hubble Space Telescope is a reality. Today, the science of the Hubble attests to the forward momentum of astronomical exploration from ancient times. The qualities of motion and drive for knowledge it exemplifies are not fixed in an epoch or a generation: most of the astronomers using Hubble today were not born when the idea of it was first advanced, and many were in the early stages of their education when the glass for its mirror was cast, The commitments we make today to the future of the Hubble observatory will equip a new genera- tion of young men and women to explore the astro- nomical frontier at the start of the 2I st century. -
The Gemini NICI Planet-Finding Campaign: the Frequency of Giant
The Gemini NICI Planet-Finding Campaign: The Frequency of Giant Planets around Young B and A Stars Eric L. Nielsen,1 Michael C. Liu,1 Zahed Wahhaj,2 Beth A. Biller,3 Thomas L. Hayward,4 Laird M. Close,5 Jared R. Males,6 Andrew J. Skemer,7 Mark Chun,1 Christ Ftaclas,1 Silvia H. P. Alencar,6 Pawel Artymowicz,7 Alan Boss,8 Fraser Clarke,9 Elisabete de Gouveia Dal Pino,10 Jane Gregorio-Hetem,10 Markus Hartung,4 Shigeru Ida,11 Marc Kuchner,12 Douglas N. C. Lin,13 I. Neill Reid,14 Evgenya L. Shkolnik,15 Matthias Tecza,9 Niranjan Thatte,9 Douglas W. Toomey16 ABSTRACT We have carried out high contrast imaging of 70 young, nearby B and A stars to search for brown dwarf and planetary companions as part of the Gemini NICI Planet- Finding Campaign. Our survey represents the largest, deepest survey for planets around high-mass stars (≈1.5–2.5 M⊙) conducted to date and includes the planet hosts β Pic and Fomalhaut. We obtained follow-up astrometry of all candidate companions within 400 AU projected separation for stars in uncrowded fields and identified new low-mass 1Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu HI 96822, USA 2European Southern Observatory, Alonso de C´ordova 3107, Vitacura, Santiago, Chile 3Max-Planck-Institut f¨ur Astronomie, K¨onigstuhl 17, 69117 Heidelberg, Germany 4Gemini Observatory, Southern Operations Center, c/o AURA, Casilla 603, La Serena, Chile 5Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA 6Departamento de Fisica - ICEx - Universidade Federal de Minas Gerais, Av. -
Planetary Ring Systems Edited by Matthew S
Cambridge University Press 978-1-107-11382-4 — Planetary Ring Systems Edited by Matthew S. Tiscareno , Carl D. Murray Frontmatter More Information Planetary Ring Systems Properties, Structure, and Evolution Planetary rings are among the most intriguing structures of our solar system and have fas- cinated generations of astronomers. Collating emerging knowledge in the field, this volume reviews our current understanding of ring systems with reference to the rings of Saturn, Uranus, Neptune, and more. Written by leading experts, the history of ring research and the basics of ring-particle orbits is followed by a review of the known planetary ring sys- tems. All aspects of ring system science are described in detail, including specific dynamical processes, types of structures, thermal properties, their origins, and investigations using com- puter simulations and laboratory experiments. The concluding chapters discuss the prospects of future missions to planetary rings, the ways in which ring science informs and is informed by the study of other astrophysical disks, and a perspective on the field’s future. Researchers of all levels benefit from this thorough and engaging presentation. MATTHEW S. TISCARENO is a Senior Research Scientist at the SETI Institute, California. He is a Participating Scientist and an Imaging Team Associate with the Cassini- Huygens mission. His research output includes solar system dynamics and space-based observations of the outer solar system. CARL D. MURRAYis Professor of Mathematics and Astronomy at Queen Mary Univer- sity of London. He has contributed to numerous ring and moon discoveries as an original member of the Imaging Team with the Cassini-Huygens mission and he is co-author of the textbook Solar System Dynamics (1999). -
Science with MATISSE
Science with MATISSE Sebastian Wolfa, Bruno Lopezb, Jean-Charles Augereauc, Marco Delbob, Carsten Dominikd, Thomas Henninge, Karl-Heinz Hofmannf, Michiel Hogerheijdeg, Josef Hronh, Walter Jaffeg, Thierry Lanzb, Klaus Meisenheimere, Florentin Millourb, Eric Pantini, Roman Petrovb, Dieter Schertlf, Roy van Boekele, Gerd Weigeltf, Andrea Chiavassab, Attila Juhaszj, Alexis Matterb, Anthony Meillandb, Nicolas Nardettob, and Claudia Paladinik aUniversit¨atzu Kiel, Institut f¨urTheoretische Physik und Astrophysik, Leibnizstr. 15, 24098 Kiel, Germany bLaboratoire Lagrange, UMR7293, Universit´ede Nice Sophia-Antipolis, CNRS, Observatoire de la C^oted'Azur, Nice, France cUJF-Grenoble 1/CNRS-INSU, Institut de Plan´etologie d'Astrophysique de Grenoble (IPAG) UMR 5274, Grenoble, 38041, France dSterrenkundig Instituut "Anton Pannekoek", Science Park 904, 1098 XH, Amsterdam, The Netherlands; Afdeling Sterrenkunde, Radboud Universiteit Nijmegen, Postbus 9010, 6500 GL, Nijmegen, The Netherlands eMax-Planck-Institut f¨urAstronomie, K¨onigstuhl17, 69117 Heidelberg, Germany fMax-Planck-Institut f¨urRadioastronomie, Auf dem H¨ugel69, 53121 Bonn, Germany gSterrewacht Leiden, Universiteit Leiden, Niels-Bohr-Weg 2, 2300 CA, Leiden, The Netherlands hInstitut f¨urAstronomie, Universit¨atWien, T¨urkenschanzstraße 17, 1180 Wien, Austria iCEA/DSM/IRFU/Service d'Astrophysique, CE Saclay, France jInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, United Kingdom kInstitut d'Astronomie et d'Astrophysique, Universite' libre de Bruxelles, Boulevard du Triomphe CP 226, B-1050 Bruxelles, Belgium ABSTRACT We present an overview of the scientific potential of MATISSE, the Multi Aperture mid-Infrared SpectroScopic Experiment for the Very Large Telescope Interferometer. For this purpose we outline selected case studies from various areas, such as star and planet formation, active galactic nuclei, evolved stars, extrasolar planets, and solar system minor bodies and discuss strategies for the planning and analysis of future MATISSE observations. -
Annual Report 2011
ESO European Organisation for Astronomical Research in the Southern Hemisphere Annual Report 2011 ESO European Organisation for Astronomical Research in the Southern Hemisphere Annual Report 2011 presented to the Council by the Director General Prof. Tim de Zeeuw The European Southern Observatory ESO, the European Southern Observa tory, is the foremost intergovernmental astronomy organisation in Europe. It ESO/J. PérezESO/J. is supported by 15 countries: Austria, Belgium, Brazil1, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. Several other countries have expressed an interest in membership. Created in 1962, ESO carries out an ambitious programme focused on the design, construction and operation of powerful groundbased observing facilities enabling astronomers to make important scientific discoveries. ESO also plays a leading role in promoting and organising cooperation in astro nomical research. ESO operates three unique worldclass Star trails over ESO’s La Silla Observatory. observing sites in the Atacama Desert region of Chile: La Silla, Paranal and Chajnantor. ESO’s first site is at La Silla, a 2400metrehigh mountain 600 kilo in visible light, is the flagship facility of images of celestial objects as faint as metres north of Santiago de Chile. It is European astron omy. Paranal is situated magnitude 30 have been obtained in equipped with several optical telescopes about 130 kilo metres south of Antofagasta a onehour exposure. This corresponds with mirror diameters of up to 3.6 metres. in Chile, 12 kilometres inland from the to seeing objects that are four billion Pacific coast in one of the driest areas in times fainter than those seen with the The 3.5metre New Technology Tele the world. -
Weighing Uranus' Moon Cressida with the Η Ring
The Astronomical Journal, 154:153 (8pp), 2017 October https://doi.org/10.3847/1538-3881/aa880e © 2017. The American Astronomical Society. All rights reserved. Weighing Uranus’ Moon Cressida with the η Ring Robert O. Chancia1 , Matthew M. Hedman1 , and Richard G. French2 1 Department of Physics, University of Idaho, Moscow, ID 83844-0903, USA; [email protected] 2 Astronomy Department, Wellesley College, Wellesley, MA 02481, USA Received 2017 June 19; revised 2017 August 9; accepted 2017 August 21; published 2017 September 20 Abstract The η ring is one of the narrow rings of Uranus, consisting of a dense core that is 1–2 km wide and a diffuse outer sheet spanning about 40 km. Its dense core lies just exterior to the 3:2 Inner Lindblad Resonance of the small moon Cressida. We fit the η ring radius residuals and longitudes from a complete set of both ground-based and Voyager stellar and radio occultations of the Uranian rings spanning 1977–2002. We find variations in the radial position of the η ring that are likely generated by this resonance, and take the form of a 3-lobed structure rotating at an angular rate equal to the mean motion of the moon Cressida. The amplitude of these radial oscillations is 0.667±0.113 km, which is consistent with the expected shape due to the perturbations from Cressida. The magnitude of these variations provides the first measurement of the mass and density of the moon Cressida (m =´()2.5 0.4 1017 kg and r =0.86 0.16 gcm−3) or, indeed, any of Uranus’ small inner moons. -
Arxiv:1509.00872V1 [Astro-Ph.EP] 2 Sep 2015 H Bevblt Fipcso in Xpaes H Oe Matc Impact Comet the Exoplanets
Detectability of Planetesimal Impacts on Giant Exoplanets Laura Flagga,b,∗, Alycia J. Weinbergerb, Keith Matthewsc aDepartment of Physics and Astronomy, Northern Arizona University, Flagstaff, AZ 86011-6010, USA bDepartment of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road NW, Washington, DC 20015, USA cCaltech Optical Observatories, California Institute of Technology, MC 301-17, Pasadena, CA 91125, USA Abstract The detectability of planetesimal impacts on imaged exoplanets can be measured using Jupiter during the 1994 comet Shoemaker-Levy 9 events as a proxy. By integrating the whole planet flux with and without impact spots, the effect of the impacts at wavelengths from 2 - 4 µm is revealed. Jupiter’s reflected light spectrum in the near-infrared is dominated by its methane opacity including a deep band at 2.3 µm. After the impact, sunlight that would have normally been absorbed by the large amount of methane in Jupiter’s atmosphere was instead reflected by the cometary material from the impacts. As a result, at 2.3 µm, where the planet would normally have low reflectivity, it brightened substantially and stayed brighter for at least a month. Keywords: comets, debris disks, extra-solar planets, Jupiter 1. Introduction The frequencies with which giant planets and cold circumstellar debris disks encircle old (i.e. >1 Gyr) Sun-like stars are both ∼20% (Eiroa et al. 2013; Marshall et al. 2014). The debris disks are generated in the collisions and evaporation of planetesimals, analogous to the comets and asteroids of today’s Solar System. That most debris disks contain cold, ∼50 K, dust indicates that the reservoirs of parent bodies are at ∼100 AU from the parent stars, in a region analogous to our Edgeworth-Kuiper Belt. -
Number 28 Space Telescope European Coordinating Facility
January 2001 Number 28 Page 1 Number 28 January 2001 This 140 nm ultraviolet image of Jupiter was taken with the Hubble Space Telescope Imaging Spectrograph (STIS) on 26 November 1998 (Credit: NASA; ESA & John T. Clarke, Univ. of Michigan) when Jupiter was at a distance of 700 million km from Earth. In addition to the main auroral oval, centred on the magnetic north pole, and a pattern of more diffuse emission inside the polar cap, unique features are the ‘magnetic footprints’ of three of Jupiter’s satellites, Io, Ganymede and Europa. Space Telescope ST-ECF Newsletter ST-ECF European Coordinating Facility Page 2 ST–ECF Newsletter European news As the ESA contribution to HST moves away Group and, in September, by the Space Science Advisory from hardware provision, support for another Committee that NGST be selected as the next ‘Flexi-mission’ project has been agreed for the ST-ECF. in ESA’s future plan for implementation between 2008 and Following the successful provision of a 2013. This selection was endorsed by the Science Programme software package for extraction of NICMOS Committee at its meeting in October. grism spectra (NICMOSLook, see ST-ECF Newsletter 24, p. 7, This approval has allowed ESA to follow up the industry 1997), support for the spectroscopic modes of the ACS will studies it funded during 1999 with new investigations also be provided. ACS has both grisms and prisms: the Wide focussed on the specific European contributions to the Field Camera, with a coverage of 3.4' × 3.4', is fitted with a mission. In November, a study of the 1–5µm near-IR multi- grism offering 40Å/pixel resolution (5500–11000Å) over the object spectrograph to be provided by ESA was awarded to a full WFC field; the High resolution Camera (26'' × 29'') consortium headed by Astrium (Munich) and Laboratoire provides 30Å/pix grism spectra and prism spectra with a d’Astronomie Spatiale (Marseille). -
Exploring the Origins and Evolution of Ice Giant Planets
Exp Astron DOI 10.1007/s10686-011-9251-4 ORIGINAL ARTICLE Uranus Pathfinder: exploring the origins and evolution of Ice Giant planets Christopher S. Arridge Craig B. Agnor Nicolas André Kevin H. Baines · · · · Leigh N. Fletcher Daniel Gautier Mark D. Hofstadter Geraint H. Jones · · · · Laurent Lamy Yves Langevin Olivier Mousis Nadine Nettelmann · · · · Christopher T. Russell Tom Stallard Matthew S. Tiscareno · · · Gabriel Tobie Andrew Bacon Chris Chaloner Michael Guest · · · · Steve Kemble Lisa Peacocke Nicholas Achilleos Thomas P. Andert · · · · Don Banfield Stas Barabash Mathieu Barthelemy Cesar Bertucci · · · · Pontus Brandt Baptiste Cecconi Supriya Chakrabarti Andy F. Cheng · · · · Ulrich Christensen Apostolos Christou Andrew J. Coates · · · Glyn Collinson John F. Cooper Regis Courtin Michele K. Dougherty · · · · Robert W. Ebert Marta Entradas Andrew N. Fazakerley · · · Jonathan J. Fortney Marina Galand Jaques Gustin Matthew Hedman · · · · Ravit Helled Pierre Henri Sebastien Hess Richard Holme · · · · Özgur Karatekin Norbert Krupp Jared Leisner Javier Martin-Torres · · · · Adam Masters Henrik Melin Steve Miller Ingo Müller-Wodarg · · · · Benoît Noyelles Chris Paranicas Imke de Pater Martin Pätzold · · · · Renée Prangé Eric Quémerais Elias Roussos Abigail M. Rymer · · · · Agustin Sánchez-Lavega Joachim Saur Kunio M. Sayanagi Paul Schenk · · · · Gerald Schubert Nick Sergis Frank Sohl Edward C. Sittler Jr. · · · · Nick A. Teanby Silvia Tellmann Elizabeth P. Turtle Sandrine Vinatier · · · · Jan-Erik Wahlund Philippe Zarka · Received: 26 November 2010 / Accepted: 21 July 2011 ©SpringerScience+BusinessMediaB.V.2011 N. Achilleos Department of Physics and Astronomy, University College London, London, UK C. B. Agnor School of Physics and Astronomy, Queen Mary University of London, London, UK T. P. Andert Universität der Bundeswehr, Munich, Germany N. André Centre d’Etude Spatiale des Rayonnements / CNRS, Toulouse, France C. -
Uranus, Neptune, Pluto, and the Outer Solar System Linda T
Uranus, Neptune, Pluto, and the Outer Solar System Linda T. Elkins-Tanton Uranus, Neptune, Pluto, and the Outer Solar System Copyright © 2006 by Linda T.Elkins-Tanton All rights reserved. No part of this book may be reproduced or utilized in any form or by any means, electronic or mechani- cal, including photocopying, recording, or by any information storage or retrieval systems, without permission in writing from the publisher. For information contact: Chelsea House An imprint of Infobase Publishing 132 West 31st Street New York NY 10001 Library of Congress Cataloging-in-Publication Data Elkins-Tanton, Linda T. Uranus, Neptune, Pluto, and the outer solar system / Linda T.Elkins-Tanton. p. cm. — (The Solar system) Includes bibliographical references and index. ISBN 0-8160-5197-6 (acid-free paper) 1. Uranus (Planet)—Popular works. 2. Neptune (Planet)—Popular works. 3. Pluto (Planet)—Popular works. 4. Solar system—Popular works. I.Title. QB681.E45 2006 523.47—dc22 2005014801 Chelsea House books are available at special discounts when purchased in bulk quantities for businesses, associations, institu- tions, or sales promotions. Please call our Special Sales Department in New York at (212) 967-8800 or (800) 322-8755. You can find Chelsea House on the World Wide Web at http://www.chelseahouse.com Text and cover design by Dorothy M. Preston Illustrations by Richard Garratt Printed in the United States of America VB Hermitage 10 9 8 7 6 5 4 3 2 1 This book is printed on acid-free paper. In memory of my brother Thomas Turner Elkins, who, when I was 10 years old, taught me about the Oort cloud, and together we named our pet mouse Oort.