DOCSLIB.ORG

02. Solar System (2001) 9/4/01 12:28 PM Page 2

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

01. Solar System Cover 9/4/01 12:18 PM Page 1 National Aeronautics and Educational Product Space Administration Educators Grades K–12 LS-2001-08-002-HQ Solar System Lithograph Set for Space Science This set contains the following lithographs: • Our Solar System • Moon • Saturn • Our Star—The Sun • Mars • Uranus • Mercury • Asteroids • Neptune • Venus • Jupiter • Pluto and Charon • Earth • Moons of Jupiter • Comets 01. Solar System Cover 9/4/01 12:18 PM Page 2 NASA’s Central Operation of Resources for Educators Regional Educator Resource Centers offer more educators access (CORE) was established for the national and international distribution of to NASA educational materials. NASA has formed partnerships with universities, NASA-produced educational materials in audiovisual format. Educators can museums, and other educational institutions to serve as regional ERCs in many obtain a catalog and an order form by one of the following methods: States. A complete list of regional ERCs is available through CORE, or electroni- cally via NASA Spacelink at http://spacelink.nasa.gov/ercn NASA CORE Lorain County Joint Vocational School NASA’s Education Home Page serves as a cyber-gateway to informa- 15181 Route 58 South tion regarding educational programs and services offered by NASA for the Oberlin, OH 44074-9799 American education community. This high-level directory of information provides Toll-free Ordering Line: 1-866-776-CORE specific details and points of contact for all of NASA’s educational efforts, Field Toll-free FAX Line: 1-866-775-1460 Center offices, and points of presence within each State. Visit this resource at the E-mail: [email protected] following address: http://education.nasa.gov Home Page: http://core.nasa.gov NASA Spacelink is one of NASA’s electronic resources specifically devel- Educator Resource Center Network (ERCN) oped for the educational community. Spacelink serves as an electronic library to To make additional information available to the education community, NASA has NASA’s educational and scientific resources, with hundreds of subject areas created the NASA Educator Resource Center (ERC) network. Educators may pre- arranged in a manner familiar to educators. Using Spacelink Search, educators view, copy, or receive NASA materials at these sites. Phone calls are welcome if you and students can easily find information among NASA’s thousands of Internet are unable to visit the ERC that serves your geographic area. The ERCs and the resources. Special events, missions, and intriguing NASA Web sites are featured in regions they serve include the following: Spacelink’s “Hot Topics” and “Cool Picks” areas. Spacelink may be accessed at http://spacelink.nasa.gov AK, Northern CA, HI, ID, MT, AL, AR, IA, LA, MO, TN NV, OR, UT, WA, WY U.S. Space and Rocket Center NASA Educator Resource Center NASA Educator Resource Center for NASA Ames Research Center NASA Marshall Space Flight Center NASA Spacelink is the official home of electronic versions of NASA’s Educational Mail Stop 253-2 One Tranquility Base Products. A complete listing of NASA Educational Products can be found at the fol- Moffett Field, CA 94035-1000 Huntsville, AL 35758 Phone: (650) 604-3574 Phone: (256) 544-5812 lowing address: http://spacelink.nasa.gov/products IL, IN, MI, MN, OH, WI MS NASA Educator Resource Center NASA Educator Resource Center NASA Television (NTV) NASA Glenn Research Center NASA Stennis Space Center features Space Station and Shuttle mission cover- Mail Stop 8-1 Building 1200 age, live special events, interactive educational live shows, electronic field trips, 21000 Brookpark Road Stennis Space Center, MS 39529-6000 Cleveland, OH 44135 Phone: (228) 688-3338 aviation and space news, and historical NASA footage. Programming has a three- Phone: (216) 433-2017 hour block—Video (News) File, NASA Gallery, and Education File—beginning at CA CT, DE, DC, ME, MD, MA, NH, NASA Educator Resource Center for noon Eastern and repeated at 3 p.m., 6 p.m., 9 p.m., and midnight, Monday NJ, NY, PA, RI, VT NASA Jet Propulsion Laboratory NASA Educator Resource Laboratory Village at Indian Hill through Friday. Live feeds preempt regularly scheduled programming. NASA Goddard Space Flight Center 1460 East Holt Avenue, Suite 20 Mail Code 130.3 Pomona, CA 91767 Greenbelt, MD 20771-0001 Phone: (909) 397-4420 Check the Internet for programs listings at: Phone: (301) 286-8570 AZ and Southern CA http://www.nasa.gov/ntv CO, KS, NE, NM, ND, OK, SD, TX NASA Educator Resource Center for Space Center Houston NASA Dryden Flight Research Center NASA Educator Resource Center for 45108 N. 3rd Street East For more information on NTV, contact: NASA Johnson Space Center Lancaster, CA 93535 1601 NASA Road One Phone: (661) 948-7347 NASA TV, NASA Headquarters-Code P-2, Washington, DC 20546-0001 Houston, TX 77058 Phone: (202) 358-3572 Phone: (281) 244-2129 VA and MD’s Eastern Shore NASA Educator Resource Center FL, GA, PR, VI GSFC/Wallops Flight Facility NASA Educator Resource Center Visitor Center Building J-17 How to Access Information on NASA’s Education Program, NASA Kennedy Space Center Wallops Island, VA 23337 Materials, and Services Mail Code ERC Phone: (757) 824-2298 Kennedy Space Center, FL 32899 This brochure serves as a guide to accessing a variety of NASA materials and serv- Phone: (321) 867-4090 ices for educators. Copies are available through the ERC network or electronical- KY, NC, SC, VA, WV ly via NASA Spacelink. Virginia Air & Space Center Educator Resource Center for NASA Langley Research Center 600 Settlers Landing Road Solar System Lithograph Set for Space Science is available in Hampton, VA 23669-4033 electronic format through NASA Spacelink. The most up-to-date lithographs and Phone: (757) 727-0900 x 757 links to the individual images can be downloaded from NASA Spacelink at http://spacelink.nasa.gov/products/Solar.System.Lithograph.Set 02. Solar System (2001) 9/4/01 12:28 PM Page 2 National Aeronautics and Space Administration Our Solar System 02. Solar System (2001) 9/4/01 12:28 PM Page 1 National Aeronautics and Space Administration Our Solar System From our small world we have gazed upon the cosmic ocean for There are at least 91 natural satellites (also called moons) around the Activities thousands of years. Ancient astronomers observed points of light that various planets in our solar system, ranging from bodies larger than our appeared to move among the stars. They called these objects planets, own Moon down to small pieces of debris. Many of these were discov- How big is our solar system? To give you a rough idea, consider that it meaning wanderers, and named them after Roman deities—Jupiter, ered by planetary spacecraft. Some of these have atmospheres (Saturn’s took the Voyager 2 spacecraft, traveling in a sweeping arc at an aver- king of the gods; Mars, the god of war; Mercury, messenger of the Titan); some even have magnetic fields (Jupiter’s Ganymede). Jupiter’s age of 65,000 kilometers per hour, 12 years to reach Neptune! How gods; Venus, the goddess of love and beauty; and Saturn, father of moon Io is the most volcanically active body in the solar system. An fast is that in meters per second? In feet per second? If you could trav- Jupiter and god of agriculture. The stargazers also observed comets ocean may lie beneath the frozen crust of Jupiter’s moon Europa, while el that fast, how long would it take you to reach the next town? To get with sparkling tails, and meteors or shooting stars apparently falling images of Jupiter’s moon Ganymede show historical motion of icy to the Moon? from the sky. crustal plates. Some planetary moons, such as Phoebe at Saturn, may be asteroids that were captured by a planet’s gravity. Can you build a scale model of the solar system? If you use Earth’s Since the invention of the telescope, three more planets have been dis- diameter as a unit of measure (Earth diameter = 1), figure out how big covered in our solar system: Uranus (1781), Neptune (1846), and From 1610 to 1977, Saturn was thought to be the only planet with the other planets are compared to Earth. Hint: divide each planet’s Pluto (1930). In addition, there are thousands of small bodies such as rings. We now know that Jupiter, Uranus, and Neptune also have ring diameter by Earth’s diameter. What objects might you use to depict the asteroids and comets. Most of the asteroids orbit in a region between systems, although Saturn’s is by far the largest. Particles in these ring sizes of the Sun and planets? How far away would the planets be from the orbits of Mars and Jupiter, while the home of comets lies far beyond systems range in size from dust to boulders to house-sized, and they each other? Map out a scale model of the solar system in your town. the orbit of Pluto, in the Oort Cloud. may be rocky and/or icy. Actual Mean Distance Number The four planets closest to the Sun—Mercury, Venus, Earth, and Most of the planets also have magnetic fields, which extend into space Diameter (km) from sun (km) of Moons Mars—are called the terrestrial planets because they have solid and form a “magnetosphere” around each planet. These magnetos- Sun 1,391,900 0 – rocky surfaces. The four large planets beyond the orbit of Mars— pheres rotate with the planet, sweeping charged particles with them. Mercury 4,878 57,910,000 0 Jupiter, Saturn, Uranus, and Neptune—are called gas giants. Tiny, dis- The Sun has a magnetic field, the heliosphere, which envelops our Venus 12,104 108,200,0000 0 tant Pluto has a solid but icier surface than the terrestrial planets.
Recommended publications
  • Curiosity's Candidate Field Site in Gale Crater, Mars

    Curiosity's Candidate Field Site in Gale Crater, Mars

    Curiosity’s Candidate Field Site in Gale Crater, Mars K. S. Edgett – 27 September 2010 Simulated view from Curiosity rover in landing ellipse looking toward the field area in Gale; made using MRO CTX stereopair images; no vertical exaggeration. The mound is ~15 km away 4th MSL Landing Site Workshop, 27–29 September 2010 in this view. Note that one would see Gale’s SW wall in the distant background if this were Edgett, 1 actually taken by the Mastcams on Mars. Gale Presents Perhaps the Thickest and Most Diverse Exposed Stratigraphic Section on Mars • Gale’s Mound appears to present the thickest and most diverse exposed stratigraphic section on Mars that we can hope access in this decade. • Mound has ~5 km of stratified rock. (That’s 3 miles!) • There is no evidence that volcanism ever occurred in Gale. • Mound materials were deposited as sediment. • Diverse materials are present. • Diverse events are recorded. – Episodes of sedimentation and lithification and diagenesis. – Episodes of erosion, transport, and re-deposition of mound materials. 4th MSL Landing Site Workshop, 27–29 September 2010 Edgett, 2 Gale is at ~5°S on the “north-south dichotomy boundary” in the Aeolis and Nepenthes Mensae Region base map made by MSSS for National Geographic (February 2001); from MOC wide angle images and MOLA topography 4th MSL Landing Site Workshop, 27–29 September 2010 Edgett, 3 Proposed MSL Field Site In Gale Crater Landing ellipse - very low elevation (–4.5 km) - shown here as 25 x 20 km - alluvium from crater walls - drive to mound Anderson & Bell
  • JUICE Red Book

    JUICE Red Book

    ESA/SRE(2014)1 September 2014 JUICE JUpiter ICy moons Explorer Exploring the emergence of habitable worlds around gas giants Definition Study Report European Space Agency 1 This page left intentionally blank 2 Mission Description Jupiter Icy Moons Explorer Key science goals The emergence of habitable worlds around gas giants Characterise Ganymede, Europa and Callisto as planetary objects and potential habitats Explore the Jupiter system as an archetype for gas giants Payload Ten instruments Laser Altimeter Radio Science Experiment Ice Penetrating Radar Visible-Infrared Hyperspectral Imaging Spectrometer Ultraviolet Imaging Spectrograph Imaging System Magnetometer Particle Package Submillimetre Wave Instrument Radio and Plasma Wave Instrument Overall mission profile 06/2022 - Launch by Ariane-5 ECA + EVEE Cruise 01/2030 - Jupiter orbit insertion Jupiter tour Transfer to Callisto (11 months) Europa phase: 2 Europa and 3 Callisto flybys (1 month) Jupiter High Latitude Phase: 9 Callisto flybys (9 months) Transfer to Ganymede (11 months) 09/2032 – Ganymede orbit insertion Ganymede tour Elliptical and high altitude circular phases (5 months) Low altitude (500 km) circular orbit (4 months) 06/2033 – End of nominal mission Spacecraft 3-axis stabilised Power: solar panels: ~900 W HGA: ~3 m, body fixed X and Ka bands Downlink ≥ 1.4 Gbit/day High Δv capability (2700 m/s) Radiation tolerance: 50 krad at equipment level Dry mass: ~1800 kg Ground TM stations ESTRAC network Key mission drivers Radiation tolerance and technology Power budget and solar arrays challenges Mass budget Responsibilities ESA: manufacturing, launch, operations of the spacecraft and data archiving PI Teams: science payload provision, operations, and data analysis 3 Foreword The JUICE (JUpiter ICy moon Explorer) mission, selected by ESA in May 2012 to be the first large mission within the Cosmic Vision Program 2015–2025, will provide the most comprehensive exploration to date of the Jovian system in all its complexity, with particular emphasis on Ganymede as a planetary body and potential habitat.
  • Terrestrial Impact Structures Provide the Only Ground Truth Against Which Computational and Experimental Results Can Be Com­ Pared

    Terrestrial Impact Structures Provide the Only Ground Truth Against Which Computational and Experimental Results Can Be Com­ Pared

    Ann. Rev. Earth Planet. Sci. 1987. 15:245-70 Copyright([;; /987 by Annual Reviews Inc. All rights reserved TERRESTRIAL IMI!ACT STRUCTURES ··- Richard A. F. Grieve Geophysics Division, Geological Survey of Canada, Ottawa, Ontario KIA OY3, Canada INTRODUCTION Impact structures are the dominant landform on planets that have retained portions of their earliest crust. The present surface of the Earth, however, has comparatively few recognized impact structures. This is due to its relative youthfulness and the dynamic nature of the terrestrial geosphere, both of which serve to obscure and remove the impact record. Although not generally viewed as an important terrestrial (as opposed to planetary) geologic process, the role of impact in Earth evolution is now receiving mounting consideration. For example, large-scale impact events may hav~~ been responsible for such phenomena as the formation of the Earth's moon and certain mass extinctions in the biologic record. The importance of the terrestrial impact record is greater than the relatively small number of known structures would indicate. Impact is a highly transient, high-energy event. It is inherently difficult to study through experimentation because of the problem of scale. In addition, sophisticated finite-element code calculations of impact cratering are gen­ erally limited to relatively early-time phenomena as a result of high com­ putational costs. Terrestrial impact structures provide the only ground truth against which computational and experimental results can be com­ pared. These structures provide information on aspects of the third dimen­ sion, the pre- and postimpact distribution of target lithologies, and the nature of the lithologic and mineralogic changes produced by the passage of a shock wave.
  • Transit Timing Analysis of the Hot Jupiters WASP-43B and WASP-46B and the Super Earth Gj1214b

    Transit Timing Analysis of the Hot Jupiters WASP-43B and WASP-46B and the Super Earth Gj1214b

    Transit timing analysis of the hot Jupiters WASP-43b and WASP-46b and the super Earth GJ1214b Mathias Polfliet Promotors: Michaël Gillon, Maarten Baes 1 Abstract Transit timing analysis is proving to be a promising method to detect new planetary partners in systems which already have known transiting planets, particularly in the orbital resonances of the system. In these resonances we might be able to detect Earth-mass objects well below the current detection and even theoretical (due to stellar variability) thresholds of the radial velocity method. We present four new transits for WASP-46b, four new transits for WASP-43b and eight new transits for GJ1214b observed with the robotic telescope TRAPPIST located at ESO La Silla Observatory, Chile. Modelling the data was done using several Markov Chain Monte Carlo (MCMC) simulations of the new transits with old data and a collection of transit timings for GJ1214b from published papers. For the hot Jupiters this lead to a general increase in accuracy for the physical parameters of the system (for the mass and period we found: 2.034±0.052 MJup and 0.81347460±0.00000048 days and 2.03±0.13 MJup and 1.4303723±0.0000011 days for WASP-43b and WASP-46b respectively). For GJ1214b this was not the case given the limited photometric precision of TRAPPIST. The additional timings however allowed us to constrain the period to 1.580404695±0.000000084 days and the RMS of the TTVs to 16 seconds. We investigated given systems for Transit Timing Variations (TTVs) and variations in the other transit parameters and found no significant (3sv) deviations.
  • Apollo Program 1 Apollo Program

    Apollo Program 1 Apollo Program

    Apollo program 1 Apollo program The Apollo program was the third human spaceflight program carried out by the National Aeronautics and Space Administration (NASA), the United States' civilian space agency. First conceived during the Presidency of Dwight D. Eisenhower as a three-man spacecraft to follow the one-man Project Mercury which put the first Americans in space, Apollo was later dedicated to President John F. Kennedy's national goal of "landing a man on the Moon and returning him safely to the Earth" by the end of the 1960s, which he proposed in a May 25, 1961 address to Congress. Project Mercury was followed by the two-man Project Gemini (1962–66). The first manned flight of Apollo was in 1968 and it succeeded in landing the first humans on Earth's Moon from 1969 through 1972. Kennedy's goal was accomplished on the Apollo 11 mission when astronauts Neil Armstrong and Buzz Aldrin landed their Lunar Module (LM) on the Moon on July 20, 1969 and walked on its surface while Michael Collins remained in lunar orbit in the command spacecraft, and all three landed safely on Earth on July 24. Five subsequent Apollo missions also landed astronauts on the Moon, the last in December 1972. In these six spaceflights, 12 men walked on the Moon. Apollo ran from 1961 to 1972, and was supported by the two-man Gemini program which ran concurrently with it from 1962 to 1966. Gemini missions developed some of the space travel techniques that were necessary for the success of the Apollo missions.
  • Martian Crater Morphology

    Martian Crater Morphology

    ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter.
  • Astrometric Positions for 18 Irregular Satellites of Giant Planets from 23

    Astrometric Positions for 18 Irregular Satellites of Giant Planets from 23

    Astronomy & Astrophysics manuscript no. Irregulares c ESO 2018 October 20, 2018 Astrometric positions for 18 irregular satellites of giant planets from 23 years of observations,⋆,⋆⋆,⋆⋆⋆,⋆⋆⋆⋆ A. R. Gomes-Júnior1, M. Assafin1,†, R. Vieira-Martins1, 2, 3,‡, J.-E. Arlot4, J. I. B. Camargo2, 3, F. Braga-Ribas2, 5,D.N. da Silva Neto6, A. H. Andrei1, 2,§, A. Dias-Oliveira2, B. E. Morgado1, G. Benedetti-Rossi2, Y. Duchemin4, 7, J. Desmars4, V. Lainey4, W. Thuillot4 1 Observatório do Valongo/UFRJ, Ladeira Pedro Antônio 43, CEP 20.080-090 Rio de Janeiro - RJ, Brazil e-mail: [email protected] 2 Observatório Nacional/MCT, R. General José Cristino 77, CEP 20921-400 Rio de Janeiro - RJ, Brazil e-mail: [email protected] 3 Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ 20921-400, Brazil 4 Institut de mécanique céleste et de calcul des éphémérides - Observatoire de Paris, UMR 8028 du CNRS, 77 Av. Denfert-Rochereau, 75014 Paris, France e-mail: [email protected] 5 Federal University of Technology - Paraná (UTFPR / DAFIS), Rua Sete de Setembro, 3165, CEP 80230-901, Curitiba, PR, Brazil 6 Centro Universitário Estadual da Zona Oeste, Av. Manual Caldeira de Alvarenga 1203, CEP 23.070-200 Rio de Janeiro RJ, Brazil 7 ESIGELEC-IRSEEM, Technopôle du Madrillet, Avenue Galilée, 76801 Saint-Etienne du Rouvray, France Received: Abr 08, 2015; accepted: May 06, 2015 ABSTRACT Context. The irregular satellites of the giant planets are believed to have been captured during the evolution of the solar system. Knowing their physical parameters, such as size, density, and albedo is important for constraining where they came from and how they were captured.
  • The Minor Planet Bulletin

    The Minor Planet Bulletin

    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin.
  • Sky and Telescope

    Sky and Telescope

    SkyandTelescope.com The Lunar 100 By Charles A. Wood Just about every telescope user is familiar with French comet hunter Charles Messier's catalog of fuzzy objects. Messier's 18th-century listing of 109 galaxies, clusters, and nebulae contains some of the largest, brightest, and most visually interesting deep-sky treasures visible from the Northern Hemisphere. Little wonder that observing all the M objects is regarded as a virtual rite of passage for amateur astronomers. But the night sky offers an object that is larger, brighter, and more visually captivating than anything on Messier's list: the Moon. Yet many backyard astronomers never go beyond the astro-tourist stage to acquire the knowledge and understanding necessary to really appreciate what they're looking at, and how magnificent and amazing it truly is. Perhaps this is because after they identify a few of the Moon's most conspicuous features, many amateurs don't know where Many Lunar 100 selections are plainly visible in this image of the full Moon, while others require to look next. a more detailed view, different illumination, or favorable libration. North is up. S&T: Gary The Lunar 100 list is an attempt to provide Moon lovers with Seronik something akin to what deep-sky observers enjoy with the Messier catalog: a selection of telescopic sights to ignite interest and enhance understanding. Presented here is a selection of the Moon's 100 most interesting regions, craters, basins, mountains, rilles, and domes. I challenge observers to find and observe them all and, more important, to consider what each feature tells us about lunar and Earth history.
  • 1 INTRODUCTION 1.1 Document Overview 1.2 Software Overview

    1 INTRODUCTION 1.1 Document Overview 1.2 Software Overview

    625-645-234011, Rev. A TABLE OF CONTENTS 1 INTRODUCTION 1.1 Document Overview 1.2 Software Overview 1.3 System Hardware/Software Requirements 1.3.1 SUN 1.3.2 Windows 3.1 or Macintosh 1.4 Packaging 1.4.1 MIRAGE System Files 1.4.2 MIRAGE Data Files 1.4.3 Sequence Delivery Directories 1.5 Typographical Conventions 2 SETTING UP TO RUN MIRAGE 2.1 Obtaining a Unix Account 2.2 Installing the X terminal Server 2.2.1 MacIntosh 2.2.2 Windows 3.1 2.2.3 What's your IP Address? 2.3 Starting and Exiting MIRAGE 2.3.1 From Donatello 2.3.2 From a MAC 2.3.3 From Windows 2.3.4 From a Sun Workstation (e.g. POINTER) 3 MIRAGE INTERFACE BASICS 3.1 The MIRAGE Display 3.1.1 Command Pane 3.1.2 History Pane 3.1.3 Display Work Area 3.1.4 The Legend 3.2 Configuring MIRAGE 3.2.1 Changing Legends 3.2.2 Zooming and Scaling 625-645-234011, Rev. A 3.2.3 Vertical Ruler 3.3 MIRAGE Commands 3.3.1 Aborting Commands 3.3.2 Command Help 3.3.3 Mouse Command Sets 3.4 The MIRAGE Menus 4 MODELING IN MIRAGE 4.1 Multi Use Buffer 4.1.1 Buffer High and Low Water Marks 4.1.2 Filling the Buffer 4.1.3 Draining the Buffer 4.1.4 Modeling the Effects of Real Time Activities on the MUB 4.1.5 Modeling the Effect of Buffer Dump to Tape on the MUB 4.1.6 Modeling the Effect of Playback on the MUB 4.1.7 Modeling the Effect of Telemetry on the MUB 4.1.8 User Control of the MUB Level 4.2 Priority Buffer 4.3 DMS 4.4 Running the Models 4.5 How Modeling Results are Displayed 4.6 OAPEL-level Resource Conflict Checking 4.7 How OAPEL-level Conflict Checking Results are Displayed 5 USING MIRAGE 5.1 Starting MIRAGE 5.1.1 Miscellaneous (But Useful) Commands 5.1.2 Moving around the screen 5.2 Create OAPEL 5.2.1 Activity ID Usage 5.2.2 Adding PAs to an OAPEL 5.3 Edit OAPEL 5.4 Create PA 5.5 Edit PA 625-645-234011, Rev.
  • The Effect of Jupiter\'S Mass Growth on Satellite Capture

    The Effect of Jupiter\'S Mass Growth on Satellite Capture

    A&A 414, 727–734 (2004) Astronomy DOI: 10.1051/0004-6361:20031645 & c ESO 2004 Astrophysics The effect of Jupiter’s mass growth on satellite capture Retrograde case E. Vieira Neto1;?,O.C.Winter1, and T. Yokoyama2 1 Grupo de Dinˆamica Orbital & Planetologia, UNESP, CP 205 CEP 12.516-410 Guaratinguet´a, SP, Brazil e-mail: [email protected] 2 Universidade Estadual Paulista, IGCE, DEMAC, CP 178 CEP 13.500-970 Rio Claro, SP, Brazil e-mail: [email protected] Received 13 June 2003 / Accepted 12 September 2003 Abstract. Gravitational capture can be used to explain the existence of the irregular satellites of giants planets. However, it is only the first step since the gravitational capture is temporary. Therefore, some kind of non-conservative effect is necessary to to turn the temporary capture into a permanent one. In the present work we study the effects of Jupiter mass growth for the permanent capture of retrograde satellites. An analysis of the zero velocity curves at the Lagrangian point L1 indicates that mass accretion provides an increase of the confinement region (delimited by the zero velocity curve, where particles cannot escape from the planet) favoring permanent captures. Adopting the restricted three-body problem, Sun-Jupiter-Particle, we performed numerical simulations backward in time considering the decrease of M . We considered initial conditions of the particles to be retrograde, at pericenter, in the region 100 R a 400 R and 0 e 0:5. The results give Jupiter’s mass at the X moment when the particle escapes from the planet.
  • The Rings and Inner Moons of Uranus and Neptune: Recent Advances and Open Questions

    The Rings and Inner Moons of Uranus and Neptune: Recent Advances and Open Questions

    Workshop on the Study of the Ice Giant Planets (2014) 2031.pdf THE RINGS AND INNER MOONS OF URANUS AND NEPTUNE: RECENT ADVANCES AND OPEN QUESTIONS. Mark R. Showalter1, 1SETI Institute (189 Bernardo Avenue, Mountain View, CA 94043, mshowal- [email protected]! ). The legacy of the Voyager mission still dominates patterns or “modes” seem to require ongoing perturba- our knowledge of the Uranus and Neptune ring-moon tions. It has long been hypothesized that numerous systems. That legacy includes the first clear images of small, unseen ring-moons are responsible, just as the nine narrow, dense Uranian rings and of the ring- Ophelia and Cordelia “shepherd” ring ε. However, arcs of Neptune. Voyager’s cameras also first revealed none of the missing moons were seen by Voyager, sug- eleven small, inner moons at Uranus and six at Nep- gesting that they must be quite small. Furthermore, the tune. The interplay between these rings and moons absence of moons in most of the gaps of Saturn’s rings, continues to raise fundamental dynamical questions; after a decade-long search by Cassini’s cameras, sug- each moon and each ring contributes a piece of the gests that confinement mechanisms other than shep- story of how these systems formed and evolved. herding might be viable. However, the details of these Nevertheless, Earth-based observations have pro- processes are unknown. vided and continue to provide invaluable new insights The outermost µ ring of Uranus shares its orbit into the behavior of these systems. Our most detailed with the tiny moon Mab. Keck and Hubble images knowledge of the rings’ geometry has come from spanning the visual and near-infrared reveal that this Earth-based stellar occultations; one fortuitous stellar ring is distinctly blue, unlike any other ring in the solar alignment revealed the moon Larissa well before Voy- system except one—Saturn’s E ring.