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Mariner to Mercury, Venus and Mars
NASA Facts National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, CA 91109 Mariner to Mercury, Venus and Mars Between 1962 and late 1973, NASA’s Jet carry a host of scientific instruments. Some of the Propulsion Laboratory designed and built 10 space- instruments, such as cameras, would need to be point- craft named Mariner to explore the inner solar system ed at the target body it was studying. Other instru- -- visiting the planets Venus, Mars and Mercury for ments were non-directional and studied phenomena the first time, and returning to Venus and Mars for such as magnetic fields and charged particles. JPL additional close observations. The final mission in the engineers proposed to make the Mariners “three-axis- series, Mariner 10, flew past Venus before going on to stabilized,” meaning that unlike other space probes encounter Mercury, after which it returned to Mercury they would not spin. for a total of three flybys. The next-to-last, Mariner Each of the Mariner projects was designed to have 9, became the first ever to orbit another planet when two spacecraft launched on separate rockets, in case it rached Mars for about a year of mapping and mea- of difficulties with the nearly untried launch vehicles. surement. Mariner 1, Mariner 3, and Mariner 8 were in fact lost The Mariners were all relatively small robotic during launch, but their backups were successful. No explorers, each launched on an Atlas rocket with Mariners were lost in later flight to their destination either an Agena or Centaur upper-stage booster, and planets or before completing their scientific missions. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Impact Melt Emplacement on Mercury
Western University Scholarship@Western Electronic Thesis and Dissertation Repository 7-24-2018 2:00 PM Impact Melt Emplacement on Mercury Jeffrey Daniels The University of Western Ontario Supervisor Neish, Catherine D. The University of Western Ontario Graduate Program in Geology A thesis submitted in partial fulfillment of the equirr ements for the degree in Master of Science © Jeffrey Daniels 2018 Follow this and additional works at: https://ir.lib.uwo.ca/etd Part of the Geology Commons, Physical Processes Commons, and the The Sun and the Solar System Commons Recommended Citation Daniels, Jeffrey, "Impact Melt Emplacement on Mercury" (2018). Electronic Thesis and Dissertation Repository. 5657. https://ir.lib.uwo.ca/etd/5657 This Dissertation/Thesis is brought to you for free and open access by Scholarship@Western. It has been accepted for inclusion in Electronic Thesis and Dissertation Repository by an authorized administrator of Scholarship@Western. For more information, please contact [email protected]. Abstract Impact cratering is an abrupt, spectacular process that occurs on any world with a solid surface. On Earth, these craters are easily eroded or destroyed through endogenic processes. The Moon and Mercury, however, lack a significant atmosphere, meaning craters on these worlds remain intact longer, geologically. In this thesis, remote-sensing techniques were used to investigate impact melt emplacement about Mercury’s fresh, complex craters. For complex lunar craters, impact melt is preferentially ejected from the lowest rim elevation, implying topographic control. On Venus, impact melt is preferentially ejected downrange from the impact site, implying impactor-direction control. Mercury, despite its heavily-cratered surface, trends more like Venus than like the Moon. -
N€WS 'RELEASE NATIONAL AERONAUTICS and SPACE Admln ISTRATION 400 MARYLAND AVENUE, SW, WASHINGTON 25, D.C
https://ntrs.nasa.gov/search.jsp?R=19630002483 2020-03-11T16:50:02+00:00Z b " N€WS 'RELEASE NATIONAL AERONAUTICS AND SPACE ADMlN ISTRATION 400 MARYLAND AVENUE, SW, WASHINGTON 25, D.C. TELEPHONES WORTH 2-4155-WORTH. 3-1110 RELEASE NO. 62-182 MARINER SPACECRAFT Mariner 2, the second of a series of spacecraft designed for planetary exploration,- will be launched within a few days (no earlier than August 17) from the Atlantic Missile Range, Cape Canaveral, Florida, by the National Aeronautics and Space Administration. Mariner 1, launched at 4:21 a.m. (EST) on July 22, 1962 from AMR, was destroyed by the Range Safety Officer after about 290 seconds of flight because of a deviation from the planned flight path. Measures have been taken to correct the difficulties experienced in the Mariner 1 launch. These measures include a more rigorous checkout of the Atlas rate beacon and revision of the data editing equation. The data editing equation Is designed as a guard against acceptance of faulty databy the ground guidance equipment. The Mariner 2 spacecraft and its mission are identical to the first Mariner. Mariner 2 will carry six experiments. Two of these instruments, infrared and microwave radiometers, will make measurements at close range as Mariner 2 flys by Venus and communicate this in€ormation over an interplanetary distance of 36 million miles, Four other experiments on the spacecraft -- a magnetometer, ion chamber and particle flux detector, cosmic dust detector and solar plasma spectrometer -- will gather Information on interplantetary phenomena during the trip to Venus and in the vicinity of the planet. -
Evolution and Geochemistry of the Martian Crust: Integrating Mission Datasets
Seventh International Conference on Mars 3179.pdf EVOLUTION AND GEOCHEMISTRY OF THE MARTIAN CRUST: INTEGRATING MISSION DATASETS. B. C. Hahn1 and S. M. McLennan1, 1Department of Geosciences, Stony Brook University, Stony Brook, NY, 11794-2100 ([email protected], [email protected]). Introduction: The Martian crust is an important the Odyssey GRS has an inherently low resolving ca- geochemical reservoir. It is the only portion of the pacity with a spatially large footprint and thus cannot planet surveyed by broad-scale remote sensing obser- be used effectively for fine-scale regional analysis. vations (beginning with the Mariner program through Additionally, element abundance maps are subject to the Mars Reconnaissance Orbiter) or by in situ lander considerable smoothing and auto-correlation effects experiments (from the Viking missions through the due to element correction factors, the large footprint Mars Exploration Rovers). Mars experienced a unique and necessary data processing [6, 10]. This too, limits mechanism for crustal emplacement, resurfacing, and GRS analysis to areally-large regional or global stud- recycling [1] – different from the continuous plate tec- ies. For cross-instrument data analysis (e.g., comparing tonic regime of Earth or the episodic, widespread ba- GRS elemental abundances to TES mineralogies or salt flooding of Venus. USGS relative apparent surface ages), higher- Further, it is well-established that crusts of the in- resolution global datasets (e.g., TES mineralogical ner planets and rocky satellites become substantially maps) must be smoothed to GRS’s lower-resolution. enriched in a suite of geochemically important ele- The Mars Exploration Rovers, Spirit and Oppor- ments during early differentiation and further evolu- tunity, have each traveled several kilometers across the tion [2, 3]. -
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 . -
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. -
Lecture 21: Venus
Lecture 21: Venus 1 Venus Terrestrial Planets Animation Venus •The orbit of Venus is almost circular, with eccentricity e = 0.0068 •The average Sun-Venus distance is 0.72 AU (108,491,000 km) •Like Mercury, Venus always appears close to the Sun in the sky Venus 0.72 AU 47o 1 AU Sun Earth 2 Venus •Venus is visible for no more than about three hours •The Earth rotates 360o in 24 hours, or o o 360 = 15 24 hr hr •Since the maximum elongation of Venus is 47o, the maximum time for the Sun to rise after Venus is 47o ∆ t = ≈ 3 hours 15o / hr Venus •The albedo of an object is the fraction of the incident light that is reflected Albedo = 0.1 for Mercury Albedo = 0.1 for Moon Albedo = 0.4 for Earth Albedo = 0.7 for Venus •Venus is the third brightest object in the sky (Sun, Moon, Venus) •It is very bright because it is Close to the Sun Fairly large (about Earth size) Highly reflective (large albedo) Venus •Where in its orbit does Venus appears brightest as viewed from Earth? •There are two competing effects: Venus appears larger when closer The phase of Venus changes along its orbit •Maximum brightness occurs at elongation angle 39o 3 Venus •Since Venus is closer to the Sun than the Earth is, it’s apparent motion can be retrograde •Transits occur when Venus passes in front of the solar disk as viewed from Earth •This happens about once every 100 years (next one is in 2004) Venus (2 hour increments) Orbit of Venus •The semi-major axis of the orbit of Venus is a = 0.72 AU Venus Sun a •Kepler’s third law relates the semi-major axis to the orbital period -
Towards the 2012 Transit of Venus Report on a Talk by Darren Bellingham, Section Director ASV Solar Section
Towards the 2012 Transit of Venus Report on a Talk by Darren Bellingham, Section Director ASV Solar Section A Venus Transit, we call when we can see the planet Venus passing directly in front of the Sun. That is, when the Sun, Venus and Earth are exactly in line. This is similar to when the Moon passes in front of the Sun on a solar eclipse. But unlike the Moon, which covers most of the Sun, Venus does not eclipse the Sun because it is so much further away. It appears only as a small dot, slowly crossing the face of the Sun. A transit (sometime called a passage) can only occur with the inner planets – Mercury and Venus – because they are the only planets that during their orbits can pass between the Earth and Sun. The astronomical term for it is ‘inferior conjunction’. Transits of Venus are amongst the rarest of solar-system alignments, a rare, once in a life time event. Only seven have occurred since Galileo first pointed his telescope towards the heaven. Because the orbit of Venus is tilted 4.3 degrees with respect to the Ecliptic (Earth’s orbit), alignment occurs only when both meet at the nodes (the up and down crossing points) of the two orbits. Usually the alignment lasts for two successive meets at that point, 8 years apart. The current 2004 - 2012 pair occurs at the descending node. The previous Venus transit (pair) occurred at the upward node 129.5 years ago in 1874 and 1882. The next pair will start 113.5 years from now, in 2117 and 2125, again at the ascending node. -
Session 2 Presentations
Mercury: From Mariner to MESSENGER Sean C. Solomon Lamont-Doherty Earth Observatory Columbia University LPI 50th Anniversary Science Symposium 17 March 2018 40th LPSC The Woodlands, Texas 25 March 2009 Mariner 10 (1973–1975) • Mariner 10 – the last in the Mariner series – was the first spacecraft to visit Mercury. • Launched in November 1973, Mariner 10 flew by Mercury three times, in March and September 1974 and March 1975. Mariner 10 backup spacecraft, Udvar-Hazy Center. Mariner 10 and Mercury’s Magnetic Field • Mariner 10’s first flyby detected a magnetic field near Mercury. • Mariner 10’s third flyby (at high latitude on Mercury’s night side) confirmed that the field is internal. • A dipole field could fit the data, but there were large uncertainties. Mariner 10 third flyby observations of Mercury’s magnetic field [Connerney and Ness, 1988]. Mariner 10 and Mercury’s Geology • Mariner 10 imaged about 45% of Mercury’s surface. • Heavily cratered terrain was thought to be comparable in age to the lunar highlands. • Smooth plains were seen to be less cratered and younger, but unlike the lunar maria are not darker than the surrounding highlands. Mariner 10 mosaic of the Caloris basin. LPI Topical Conference (1976) • LPI convened a topical conference on Comparisons of Mercury and the Moon in November 1976. • A number of the papers given at the conference were collected into a special issue of Physics of the Earth and Planetary Interiors (1977). Mercury’s Exosphere • Mariner 10 had detected H and He in Mercury’s exosphere and set an upper bound on O.