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*N66 33437 ' Le-P
NEW YOZK UNIVERSITY School of Engineering and Science Research Division Department of Meteorology and Oceanography Grant No. NsG-499 Project HIA LM Informal Report Covering the Period December 1965 - May 1966 THE ATMOSPHERE OF MERCURY Wayne E. McGovern The completion of the investigation mentioned in pr evious reports on the atmosphere of Mercury, in conjunction with Drs. S. I. Rasool and S. H. Gross, resulted in the following conclusions: 1. An atmosphere of pure argon cannot be stable against gravita- tional escape since argon with its poor radiative transfer characteristics will produce prohibitively high exospheric tempteratures, (Tex > 10, OO06K). 2. If Moroz's observations are correct and C02 is present in the atmosphere of Mercury, then the production of CO by photodissociation in the upper atmosphere will produce a cooling mechanism of sufficient strength that exospheric temperatures will result which are stable against thermal escape. The calculated exospheric temperatures were between 800°K. and 1800°K. Thc large tolcrancc is mainly duc to the uncertainty in the value of the solar ultraviolet flux, cfficicncy factor for thc transfer of energy in the atmosphere, thc scale height at which CO emission becomes dominant and the levcl of maximum absorption of ionization energy. It is intcrcsting to note that if the cxospheric tcmperaturc is near our lower limit, thcn the on Mcrcury may bc of primordial origin; CO2 while an exospheric temperature near IBCGOK. would indicate that the ob- served CO conccntration was due to equilibrium between outgassing from 2 - the-interior and gravitational cscape from th top of the atmosphcre. *N66 33437 ' le-P > / - . -
Instrumental Methods for Professional and Amateur
Instrumental Methods for Professional and Amateur Collaborations in Planetary Astronomy Olivier Mousis, Ricardo Hueso, Jean-Philippe Beaulieu, Sylvain Bouley, Benoît Carry, Francois Colas, Alain Klotz, Christophe Pellier, Jean-Marc Petit, Philippe Rousselot, et al. To cite this version: Olivier Mousis, Ricardo Hueso, Jean-Philippe Beaulieu, Sylvain Bouley, Benoît Carry, et al.. Instru- mental Methods for Professional and Amateur Collaborations in Planetary Astronomy. Experimental Astronomy, Springer Link, 2014, 38 (1-2), pp.91-191. 10.1007/s10686-014-9379-0. hal-00833466 HAL Id: hal-00833466 https://hal.archives-ouvertes.fr/hal-00833466 Submitted on 3 Jun 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Instrumental Methods for Professional and Amateur Collaborations in Planetary Astronomy O. Mousis, R. Hueso, J.-P. Beaulieu, S. Bouley, B. Carry, F. Colas, A. Klotz, C. Pellier, J.-M. Petit, P. Rousselot, M. Ali-Dib, W. Beisker, M. Birlan, C. Buil, A. Delsanti, E. Frappa, H. B. Hammel, A.-C. Levasseur-Regourd, G. S. Orton, A. Sanchez-Lavega,´ A. Santerne, P. Tanga, J. Vaubaillon, B. Zanda, D. Baratoux, T. Bohm,¨ V. Boudon, A. Bouquet, L. Buzzi, J.-L. Dauvergne, A. -
Mercury Friday, February 23
ASTRONOMY 161 Introduction to Solar System Astronomy Class 18 Mercury Friday, February 23 Mercury: Basic characteristics Mass = 3.302×1023 kg (0.055 Earth) Radius = 2,440 km (0.383 Earth) Density = 5,427 kg/m³ Sidereal rotation period = 58.6462 d Albedo = 0.11 (Earth = 0.39) Average distance from Sun = 0.387 A.U. Mercury: Key Concepts (1) Mercury has a 3-to-2 spin-orbit coupling (not synchronous rotation). (2) Mercury has no permanent atmosphere because it is too hot. (3) Like the Moon, Mercury has cratered highlands and smooth plains. (4) Mercury has an extremely large iron-rich core. (1) Mercury has a 3-to-2 spin-orbit coupling (not synchronous rotation). Mercury is hard to observe from the Earth (because it is so close to the Sun). Its rotation speed can be found from Doppler shift of radar signals. Mercury’s unusual orbit Orbital period = 87.969 days Rotation period = 58.646 days = (2/3) x 87.969 days Mercury is NOT in synchronous rotation (1 rotation per orbit). Instead, it has 3-to-2 spin-orbit coupling (3 rotations for 2 orbits). Synchronous rotation (WRONG!) 3-to-2 spin-orbit coupling (RIGHT!) Time between one noon and the next is 176 days. Sun is above the horizon for 88 days at the time. Daytime temperatures reach as high as: 700 Kelvin (800 degrees F). Nighttime temperatures drops as low as: 100 Kelvin (-270 degrees F). (2) Mercury has no permanent atmosphere because it is too hot (and has low escape speed). Temperature is a measure of the 3kT v = random speed of m atoms (or v typical speed of atom molecules). -
Deep Space Chronicle Deep Space Chronicle: a Chronology of Deep Space and Planetary Probes, 1958–2000 | Asifa
dsc_cover (Converted)-1 8/6/02 10:33 AM Page 1 Deep Space Chronicle Deep Space Chronicle: A Chronology ofDeep Space and Planetary Probes, 1958–2000 |Asif A.Siddiqi National Aeronautics and Space Administration NASA SP-2002-4524 A Chronology of Deep Space and Planetary Probes 1958–2000 Asif A. Siddiqi NASA SP-2002-4524 Monographs in Aerospace History Number 24 dsc_cover (Converted)-1 8/6/02 10:33 AM Page 2 Cover photo: A montage of planetary images taken by Mariner 10, the Mars Global Surveyor Orbiter, Voyager 1, and Voyager 2, all managed by the Jet Propulsion Laboratory in Pasadena, California. Included (from top to bottom) are images of Mercury, Venus, Earth (and Moon), Mars, Jupiter, Saturn, Uranus, and Neptune. The inner planets (Mercury, Venus, Earth and its Moon, and Mars) and the outer planets (Jupiter, Saturn, Uranus, and Neptune) are roughly to scale to each other. NASA SP-2002-4524 Deep Space Chronicle A Chronology of Deep Space and Planetary Probes 1958–2000 ASIF A. SIDDIQI Monographs in Aerospace History Number 24 June 2002 National Aeronautics and Space Administration Office of External Relations NASA History Office Washington, DC 20546-0001 Library of Congress Cataloging-in-Publication Data Siddiqi, Asif A., 1966 Deep space chronicle: a chronology of deep space and planetary probes, 1958-2000 / by Asif A. Siddiqi. p.cm. – (Monographs in aerospace history; no. 24) (NASA SP; 2002-4524) Includes bibliographical references and index. 1. Space flight—History—20th century. I. Title. II. Series. III. NASA SP; 4524 TL 790.S53 2002 629.4’1’0904—dc21 2001044012 Table of Contents Foreword by Roger D. -
Morphology and Dynamics of the Venus Atmosphere at the Cloud Top Level As Observed by the Venus Monitoring Camera
Morphology and dynamics of the Venus atmosphere at the cloud top level as observed by the Venus Monitoring Camera Von der Fakultät für Elektrotechnik, Informationstechnik, Physik der Technischen Universität Carolo-Wilhelmina zu Braunschweig zur Erlangung des Grades eines Doktors der Naturwissenschaften (Dr.rer.nat.) genehmigte Dissertation von Richard Moissl aus Grünstadt Bibliografische Information Der Deutschen Bibliothek Die Deutsche Bibliothek verzeichnet diese Publikation in der Deutschen Nationalbibliografie; detaillierte bibliografische Daten sind im Internet über http://dnb.ddb.de abrufbar. 1. Referentin oder Referent: Prof. Dr. Jürgen Blum 2. Referentin oder Referent: Dr. Horst-Uwe Keller eingereicht am: 24. April 2008 mündliche Prüfung (Disputation) am: 9. Juli 2008 ISBN 978-3-936586-86-2 Copernicus Publications, Katlenburg-Lindau Druck: Schaltungsdienst Lange, Berlin Printed in Germany Contents Summary 7 1 Introduction 9 1.1 Historical observations of Venus . .9 1.2 The atmosphere and climate of Venus . .9 1.2.1 Basic composition and structure of the Venus atmosphere . .9 1.2.2 The clouds of Venus . 11 1.2.3 Atmospheric dynamics at the cloud level . 12 1.3 Venus Express . 16 1.4 Goals and structure of the thesis . 19 2 The Venus Monitoring Camera experiment 21 2.1 Scientific objectives of the VMC in the context of this thesis . 21 2.1.1 UV Channel . 21 2.1.1.1 Morphology of the unknown UV absorber . 21 2.1.1.2 Atmospheric dynamics of the cloud tops . 21 2.1.2 The two IR channels . 22 2.1.2.1 Water vapor abundance and cloud opacity . 22 2.1.2.2 Surface and lower atmosphere . -
Mariner 10 Observations of Field-Aligned Currents at Mercury
Planet. Space Sci., Vol. 45, No. 1, pp. 133-141, 1997 Pergamon #I? 1997 Published bv Elsevier Science Ltd P&ted in Great Brit& All rights reserved 0032-0633/97 $17.00+0.00 PII: S0032-0633(96)00104-3 Mariner 10 observations of field-aligned currents at Mercury J. A. Slavin,’ J. C. J. Owen,’ J. E. P. Connerney’ and S. P. Christon ‘Laboratory for Extraterrestrial Physics, NASA/GSFC, Greenbelt, MD 20771, U.S.A. ‘Astronomy Unit, Queen Mary and Westfield College, London, U.K. 3Department of Physics, University of Maryland, College Park, MD 20742, U.S.A. Received 5 October 1995; revised 11 April 1996; accepted 13 April 1996 magnetic field at Mercury with a dipole moment of about 300nT R& (see review by Connerney and Ness (1988)). This magnetic field is sufficient to stand-off the average solar wind at an altitude of about 1 RM as depicted in Fig. 1 (see review by Russell et al. (1988)). For the purposes of comparison the diameter of the Earth is indicated at the bottom of the figure (i.e. 1 RE = 6380 km ; 1 RM = 2439 km). Whether or not the solar wind is ever able to compress and/or erode the dayside magnetosphere to the point where solar wind ions could directly impact the surface remains a topic of considerable controversy (Siscoe and Christopher, 1975 ; Slavin and Holzer, 1979 ; Hood and Schubert, 1979; Suess and Goldstein, 1979; Goldstein et al., 1981). Overall, the basic morphology of this small mag- netosphere appears quite similar to that of the Earth. -
Dsc Pub Edited
Deep Space Chronicle: Foreword Foreword From the 1950s to the present, to some and asteroids, have been visited. We have Americans, space has represented prestige placed spacecraft in orbit around our Moon and a positive image for the United States on and the planets Venus, Mars, and Jupiter; we the world stage. To others, it has signified have landed on Venus, Mars, and our Moon. the quest for national security. Some view it NASA’s stunning missions to explore the as a place to station telecommunications outer Solar System have yielded a treasure of satellites and little else. To still others, space knowledge about our universe, how it origi- is, or should be, about gaining greater knowl- nated, and how it works. NASA’s exploration edge of the universe. It represents, for them, of Mars—coupled with the efforts of the pure science and the exploration of the Soviet Union/Russia—has powerfully shown unknown. Even so, the history of space sci- the prospect of past life on the Red Planet. ence and technology is one of the largely neg- Missions to Venus (including some that lected aspects in the history of the space landed on it) and Mercury have increased our program. This important monograph by Asif understanding of the inner planets. Lunar A. Siddiqi chronicles the many space probes exploration has exponentially advanced that have been sent from Earth to explore human knowledge about the origins and evo- other bodies of the solar system. It provides lution of the solar system. Most importantly, a chronological discussion of all space we have learned that, like Goldilocks and the probes, both those developed by the United three bears, Earth is a place in which every- States and those developed by the Soviet thing necessary to sustain life is “just right,” Union/Russia and other nations; basic data while all the other planets of our system about them; their findings; and their status seem exceptionally hostile. -
The Science Return from Venus Express the Science Return From
The Science Return from Venus Express Venus Express Science Håkan Svedhem & Olivier Witasse Research and Scientific Support Department, ESA Directorate of Scientific Programmes, ESTEC, Noordwijk, The Netherlands Dmitri V. Titov Max Planck Institute for Solar System Studies, Katlenburg-Lindau, Germany (on leave from IKI, Moscow) ince the beginning of the space era, Venus has been an attractive target for Splanetary scientists. Our nearest planetary neighbour and, in size at least, the Earth’s twin sister, Venus was expected to be very similar to our planet. However, the first phase of Venus spacecraft exploration (1962-1985) discovered an entirely different, exotic world hidden behind a curtain of dense cloud. The earlier exploration of Venus included a set of Soviet orbiters and descent probes, the Veneras 4 to14, the US Pioneer Venus mission, the Soviet Vega balloons and the Venera 15, 16 and Magellan radar-mapping orbiters, the Galileo and Cassini flybys, and a variety of ground-based observations. But despite all of this exploration by more than 20 spacecraft, the so-called ‘morning star’ remains a mysterious world! Introduction All of these earlier studies of Venus have given us a basic knowledge of the conditions prevailing on the planet, but have generated many more questions than they have answered concerning its atmospheric composition, chemistry, structure, dynamics, surface-atmosphere interactions, atmospheric and geological evolution, and plasma environment. It is now high time that we proceed from the discovery phase to a thorough -
The Ultimate Guide to the Solar System
FOCUS MAGAZINE Collection VOL.12 THE ULTIMATE GUIDE TO THE SOLAR SYSTEM How the Solar System The most mysterious How humans will began and how it will end objects in space colonise Mars Mission into the Sun Back to the Moon Dodging an asteroid The ice volcanoes The new gold rush: Searching for life in of Saturn’s moon Titan mining Mercury Europa’s oceans a big impact in any room Spectacular wall art from astro photographer Chris Baker. See the exciting new pricing and images! Available as frameless acrylic or framed and backlit up to 1.2 metres wide. All limited editions. www.galaxyonglass.com | [email protected] Or call Chris now on 07814 181647 EDITORIAL Editor Daniel Bennett Neighbourhood watch Managing editor Alice Lipscombe-Southwell Production editor Jheni Osman Commissioning editor Jason Goodyer How well do you know your neighbours? They Staff writer James Lloyd might only be next door, a little further down the Editorial assistant Helen Glenny street or just around the corner; you might see Additional editing Rob Banino Additional editing Iain Todd them passing by most days, you may even pop in for a cuppa and a chat now and then. But however ART & PICTURES familiar your neighbours may be, there’s probably Art editor Joe Eden Deputy art editor Steve Boswell still a lot you don’t know about them – enough Designer Jenny Price that they can still surprise you from time to time. Additional design Dean Purnell Picture editor James Cutmore The same can be said for our celestial neighbours spinning around the Solar System. -
1 the Lifecycle of Hollows on Mercury
The Lifecycle of Hollows on Mercury: An Evaluation of Candidate Volatile Phases and a Novel Model of Formation. 1 1 2 3 M. S. Phillips , J. E. Moersch , C. E. Viviano , J. P. Emery 1Department of Earth and Planetary Sciences, University of Tennessee, Knoxville 2Planetary Exploration Group, Johns Hopkins University Applied Physics Laboratory 3Department of Astronomy and Planetary Sciences, Northern Arizona University Corresponding author: Michael Phillips ([email protected]) Keywords: Mercury, hollows, thermal model, fumarole. Abstract On Mercury, high-reflectance, flat-floored depressions called hollows are observed nearly globally within low-reflectance material, one of Mercury’s major color units. Hollows are thought to be young, or even currently active, features that form via sublimation, or a “sublimation-like” process. The apparent abundance of sulfides within LRM combined with spectral detections of sulfides associated with hollows suggests that sulfides may be the phase responsible for hollow formation. Despite the association of sulfides with hollows, it is still not clear whether sulfides are the hollow-forming phase. To better understand which phase(s) might be responsible for hollow formation, we calculated sublimation rates for 57 candidate hollow-forming volatile phases from the surface of Mercury and as a function of depth beneath regolith lag deposits of various thicknesses. We found that stearic acid (C18H36O2), fullerenes (C60, C70), and elemental sulfur (S) have the appropriate thermophysical properties to explain hollow formation. Stearic acid and fullerenes are implausible hollow-forming phases because they are unlikely to have been delivered to or generated on Mercury in high enough volume to account for hollows. -
Meet the Planets Table of Contents
Teaching Activity Guide Meet the Planets Table of Contents 3 How to Use This Activity Guide 4 What Do Children Already Know? 4 Pre-Reading Questions 5 Thinking It Through & Writing Prompts 5 Comprehension Questions 6 Find in the Art 8 People of History in the Art 11 Vocabulary Game 11 Using the Words 12 Silly Sentence Structure Activity 13 Sequence Sentence Strips 15 Word Search 16 Solar System Cards 21 Rotation or Revolution? 22 Science Journal 24 True or False? 25 Which Planet? 26 Temperatures 27 Scale and Distance 30 Coloring Pages 33 Glossary 39 Answers 51 Appendix A—“What Children Know” Cards 52 Appendix B—Venn Diagram 53 Appendix C—Vocabulary Cards Copyright 2011 © Arbordale Publishing These activities may be copied for personal and non-commercial use in educational settings. www.ArbordalePublishing.com Arbordale Publishing formerly Sylvan Dell Publishing by John McGranaghan Mt. Pleasant, SC 29464 illustrated by Laurie Allen Klein How to Use This Activity Guide There are a wide variety of activities that teach or supplement all curricular areas. The activities are easily adapted up or down depending on the age and abilities of the children involved. And, it is easy to pick and choose what is appropriate for your setting and the time involved. Most activities can be done with an individual child or a group of children. Glossary/Vocabulary words: Words may be written on index cards, a poster board, or on a chalkboard for a “word wall.” If writing on poster board or chalkboard, you might want to sort words into nouns, verbs, etc. -
Space Environment of Mercury at the Time of the First MESSENGER Flyby: Solar Wind and Interplanetary Magnetic Field Modeling of Upstream Conditions Daniel N
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 114, A10101, doi:10.1029/2009JA014287, 2009 Space environment of Mercury at the time of the first MESSENGER flyby: Solar wind and interplanetary magnetic field modeling of upstream conditions Daniel N. Baker,1 Dusan Odstrcil,2,3 Brian J. Anderson,4 C. Nick Arge,5 Mehdi Benna,6 George Gloeckler,7 Jim M. Raines,7 David Schriver,8 James A. Slavin,9 Sean C. Solomon,10 Rosemary M. Killen,11 and Thomas H. Zurbuchen7 Received 23 March 2009; revised 7 July 2009; accepted 20 July 2009; published 2 October 2009. [1] The first flyby of Mercury by the Mercury Surface, Space Environment, Geochemistry and Ranging (MESSENGER) spacecraft occurred on 14 January 2008. In order to provide contextual information about the solar wind (SW) properties and the interplanetary magnetic field near the planet, we have used an empirical modeling technique combined with a numerical physics-based SW model. The Wang-Sheeley-Arge (WSA) method uses solar photospheric magnetic field observations (from Earth-based instruments) in order to estimate inner heliospheric conditions out to 21.5 solar radii from the Sun. This information is then used as input to the global numerical magnetohydrodynamic model, ENLIL, which calculates SW velocity, density, temperature, and magnetic field strength and polarity throughout the inner heliosphere. The present paper shows WSA-ENLIL conditions computed for the several week period encompassing the first flyby. This information is used in conjunction with MESSENGER magnetometer data (and the only limited available MESSENGER SW plasma data) to help understand the Mercury flyby results. The in situ spacecraft data, in turn, can also be used iteratively to improve the model accuracy for inner heliospheric ‘‘space weather’’ purposes.