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Cornell University Ithaca, New York 14650 JOSE - JUPITER ORBITING SPACECRAFT
N T Z 33854 C *?** IS81 1? JOSE - JUPITER ORBITING SPACECRAFT: A SYSTEMS STUDY Volume I '>•*,' T COLLEGE OF ENGINEERING Cornell University Ithaca, New York 14650 JOSE - JUPITER ORBITING SPACECRAFT: A SYSTEMS STUDY Volume I Prepared Under Contract No. NGR 33-010-071 NATIONAL AERONAUTICS AND SPACE ADMINISTRATION by NASA-Cornell Doctoral Design Trainee Group (196T-TO) October 1971 College of Engineering Cornell University Ithaca, New York Table of Contents Volume I Preface Chapter I: The Planet Jupiter: A Brief Summary B 1-2 r. Mechanical Properties of the Planet Jupiter. P . T-fi r> 1-10 F T-lfi F T-lfi 0 1-29 H, 1-32 T 1-39 References ... p. I-k2 Chapter II: The Spacecraft Design and Mission Definition A. Introduction p. II-l B. Organizational Structure and the JOSE Mission p. II-l C. JOSE Components p. II-1* D. Proposed Configuration p. II-5 Bibliography and References p. 11-10 Chapter III: Mission Trajectories A. Interplanetary Trajectory Analysis .... p. III-l B. Jupiter Orbital Considerations p. III-6 Bibliography and References. p. 111-38 Chapter IV: Attitude Control A. Introduction and Summary . p. IV-1 B. Expected Disturbance Moments M in Interplanetary Space . p. IV-3 C. Radiation-Produced Impulse Results p. IV-12 D. Meteoroid-Produced Impulse Results p. IV-13 E. Inertia Wheel Analysis p. IV-15 F. Attitude System Tradeoff Analysis p. IV-19 G. Conclusion P. IV-21 References and Bibliography p. TV-26 Chapter V: Propulsion Subsystem A. Mission Requirements p. V-l B. Orbit Insertion Analysis p. -
An Impacting Descent Probe for Europa and the Other Galilean Moons of Jupiter
An Impacting Descent Probe for Europa and the other Galilean Moons of Jupiter P. Wurz1,*, D. Lasi1, N. Thomas1, D. Piazza1, A. Galli1, M. Jutzi1, S. Barabash2, M. Wieser2, W. Magnes3, H. Lammer3, U. Auster4, L.I. Gurvits5,6, and W. Hajdas7 1) Physikalisches Institut, University of Bern, Bern, Switzerland, 2) Swedish Institute of Space Physics, Kiruna, Sweden, 3) Space Research Institute, Austrian Academy of Sciences, Graz, Austria, 4) Institut f. Geophysik u. Extraterrestrische Physik, Technische Universität, Braunschweig, Germany, 5) Joint Institute for VLBI ERIC, Dwingelo, The Netherlands, 6) Department of Astrodynamics and Space Missions, Delft University of Technology, The Netherlands 7) Paul Scherrer Institute, Villigen, Switzerland. *) Corresponding author, [email protected], Tel.: +41 31 631 44 26, FAX: +41 31 631 44 05 1 Abstract We present a study of an impacting descent probe that increases the science return of spacecraft orbiting or passing an atmosphere-less planetary bodies of the solar system, such as the Galilean moons of Jupiter. The descent probe is a carry-on small spacecraft (< 100 kg), to be deployed by the mother spacecraft, that brings itself onto a collisional trajectory with the targeted planetary body in a simple manner. A possible science payload includes instruments for surface imaging, characterisation of the neutral exosphere, and magnetic field and plasma measurement near the target body down to very low-altitudes (~1 km), during the probe’s fast (~km/s) descent to the surface until impact. The science goals and the concept of operation are discussed with particular reference to Europa, including options for flying through water plumes and after-impact retrieval of very-low altitude science data. -
Adaptive Multibody Gravity Assist Tours Design in Jovian System for the Ganymede Landing
TO THE ADAPTIVE MULTIBODY GRAVITY ASSIST TOURS DESIGN IN JOVIAN SYSTEM FOR THE GANYMEDE LANDING Grushevskii A.V.(1), Golubev Yu.F.(2), Koryanov V.V.(3), and Tuchin A.G.(4) (1)KIAM (Keldysh Institute of Applied Mathematics), Miusskaya sq., 4, Moscow, 125047, Russia, +7 495 333 8067, E-mail: [email protected] (2)KIAM, Miusskaya sq., 4, Moscow, 125047, Russia, E-mail: [email protected] (3)KIAM, Miusskaya sq., 4, Moscow, 125047, Russia, E-mail: [email protected] (4)KIAM, Miusskaya sq., 4, Moscow, 125047, Russia, E-mail: [email protected] Keywords: gravity assist, adaptive mission design, trajectory design, TID, phase beam Introduction Modern space missions inside Jovian system are not possible without multiple gravity assists (as well as in Saturnian system, etc.). The orbit design for real upcoming very complicated missions by NASA, ESA, RSA should be adaptive to mission parameters, such as: the time of Jovian system arrival, incomplete information about ephemeris of Galilean Moons and their gravitational fields, errors of flybys implementation, instrumentation deflections. Limited dynamic capabilities, taking place in case of maneuvering around Jupiter's moons, demand multiple encounters (about 15-30 times) for these purposes. Flexible algorithm of current mission scenarios synthesis (specially selected) and their operative transformation is required. Mission design is complicated due to requirements of the Ganymede Orbit Insertion (GOI) ("JUICE" ESA) and also Ganymede Landing implementation ("Laplas-P" RSA [1]) comparing to the ordinary early ―velocity gain" missions since ―Pioneers‖ and "Voyagers‖. Thus such scenario splits in two parts. Part 1(P1), as usually, would be used to reduce the spacecraft’s orbital energy with respect to Jupiter and set up the conditions for more frequent flybys. -
Our Planetary System (Chapter 7) Based on Chapter 7
Our Planetary System (Chapter 7) Based on Chapter 7 • This material will be useful for understanding Chapters 8, 9, 10, 11, and 12 on “Formation of the solar system”, “Planetary geology”, “Planetary atmospheres”, “Jovian planet systems”, and “Remnants of ice and rock” • Chapters 3 and 6 on “The orbits of the planets” and “Telescopes” will be useful for understanding this chapter Goals for Learning • How do planets rotate on their axes and orbit the Sun? • What are the planets made of? • What other classes of objects are there in the solar system? Orbits mostly lie in the same flat plane All planets go around the Sun in the same direction Most orbits are close to circular Not coincidences! Most planets rotate in the same “sense” as they orbit the Sun Coincidence? Planetary equators mostly lie in the same plane as their orbits Coincidence? • Interactive Figure: Orbital and Rotational Properties of the Planets Rotation and Orbits of Moons • Most moons (especially the larger ones) orbit in near-circular orbits in the same plane as the equator of their parent planet • Most moons rotate so that their equator is in the plane of their orbit • Most moons rotate in the same “sense” as their orbit around the parent planet • Everything is rotating/orbiting in the same direction A Brief Tour • Distance from Sun •Size •Mass • Composition • Temperature • Rings/Moons Sun 695000 km = 108 RE 333000 MEarth 98% Hydrogen and helium 99.9% total mass of solar system Surface = 5800K Much hotter inside Giant ball of gas Gravity => orbits Heat/light => weather -
Jupiter Mass
CESAR Science Case Jupiter Mass Calculating a planet’s mass from the motion of its moons Student’s Guide Mass of Jupiter 2 CESAR Science Case Table of Contents The Mass of Jupiter ........................................................................... ¡Error! Marcador no definido. Kepler’s Three Laws ...................................................................................................................................... 4 Activity 1: Properties of the Galilean Moons ................................................................................................. 6 Activity 2: Calculate the period of your favourite moon ................................................................................. 9 Activity 3: Calculate the orbital radius of your favourite moon .................................................................... 12 Activity 4: Calculate the Mass of Jupiter ..................................................................................................... 15 Additional Activity: Predict a Transit ............................................................................................................ 16 To know more… .......................................................................................................................... 19 Links ............................................................................................................................................ 19 Mass of Jupiter 3 CESAR Science Case Background Kepler’s Three Laws The three Kepler’s Laws, published between -
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. -
Tidal Detachment and Evaporation Following an Exoplanet-Star Collision
MNRAS 000, 000–000 (0000) Preprint 24 June 2019 Compiled using MNRAS LATEX style file v3.0 Orphaned Exomoons: Tidal Detachment and Evaporation Following an Exoplanet-Star Collision Miguel Martinez1, Nicholas C. Stone1;2;3, Brian D. Metzger1 1Department of Physics and Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA 2Racah Institute of Physics, The Hebrew University, Jerusalem, 91904, Israel 3Department of Astronomy, University of Maryland, College Park, MD 20742, USA 24 June 2019 ABSTRACT Gravitational perturbations on an exoplanet from a massive outer body, such as the Kozai- Lidov mechanism, can pump the exoplanet’s eccentricity up to values that will destroy it via a collision or strong interaction with its parent star. During the final stages of this process, any exomoons orbiting the exoplanet will be detached by the star’s tidal force and placed into orbit around the star. Using ensembles of three and four-body simulations, we demonstrate that while most of these detached bodies either collide with their star or are ejected from the system, a substantial fraction, ∼ 10%, of such "orphaned" exomoons (with initial properties similar to those of the Galilean satellites in our own solar system) will outlive their parent exoplanet. The detached exomoons generally orbit inside the ice line, so that strong radiative heating will evaporate any volatile-rich layers, producing a strong outgassing of gas and dust, analogous to a comet’s perihelion passage. Small dust grains ejected from the exomoon may help generate an opaque cloud surrounding the orbiting body but are quickly removed by radiation blow-out. -
PHYS133 – Lab 4 the Revolution of the Moons of Jupiter
PHYS133 – Lab 4 The Revolution of the Moons of Jupiter Goals: Use a simulated remotely controlled telescope to observe Jupiter and the position of its four largest moons. Plot their positions relative to the planet vs. time and fit a curve to them to determine their orbit characteristics (i.e., period and semi‐major axis). Employ Newton’s form of Kepler’s third law to determine the mass of Jupiter. What You Turn In: Graphs of your orbital data for each moon. Calculations of the mass of Jupiter for each moon’s orbit. Calculate the time required to go to Mars from Earth using the lowest possible energy. Background Reading: Background reading for this lab can be found in your text book (specifically, Chapters 3 and 4 and especially section 4.4) and the notes for the course. Equipment provided by the lab: Computer with Internet Connection • Project CLEA program “The Revolutions of the Moons of Jupiter” Equipment provided by the student: Pen Calculator Background: Astronomers cannot directly measure many of the things they study, such as the masses and distances of the planets and their moons. Nevertheless, we can deduce some properties of celestial bodies from their motions despite the fact that we cannot directly measure them. In 1543, Nicolaus Copernicus hypothesized that the planets revolve in circular orbits around the sun. Tycho Brahe (1546‐1601) carefully observed the locations of the planets and 777 stars over a period of 20 years using a sextant and compass. These observations were used by Johannes Kepler, to deduce three empirical mathematical laws governing the orbit of one object around another. -
Jupitor's Great Red Spot
GREAT RED SPOT appears somewhat orange in this remarkably ly ranged from '.'full gray" and "pinkish" to "brick red" and "car· detailed photograph made at the Lunar and Planetary Laboratory mine." The photograph was made on December 23, 1966, by Alika of the University of Arizona. During the century or so that Jupiter's Herring and John Fountain, who used a 61·inch reflecting tele· great red spot bas been closely observed its color has reported. scope. The exposure was one second on High Speed Ektachrome. © 1968 SCIENTIFIC AMERICAN, INC JUPITER'S GREAT RED SPOT There is evidence to suggest that this peculiar Inarking is the top of a "Taylor cohunn": a stagnant region above a bll111p 01' depression at the botton1 of a circulating fluid by Haymond Hide he surface markings of the plan To explain the fluctuations in the red tals suspended in an atmosphere that is Tets have always had a special fas spot's period of rotation one must assume mainly hydrogen admixed with water cination, and no single marking that there are forces acting on the solid and perhaps methane and helium. Other has been more fascinating and puzzling planet capable of causing an equivalent lines of evidence, particularly the fact than the great red spot of Jupiter. Un change in its rotation period. In other that Jupiter's density is only 1.3 times like the elusive "canals" of Mars, the red words, the fluctuations in the rotation the density of water, suggest that the spot unmistakably exists. Although it has period of the red spot are to be regarded main constituents of the planet are hy been known to fade and change color, it as a true reflection of the rotation period drogen and helium. -
Arxiv:1209.5996V1 [Astro-Ph.EP] 26 Sep 2012 1.1
, 1{28 Is the Solar System stable ? Jacques Laskar ASD, IMCCE-CNRS UMR8028, Observatoire de Paris, UPMC, 77 avenue Denfert-Rochereau, 75014 Paris, France [email protected] R´esum´e. Since the formulation of the problem by Newton, and during three centuries, astrono- mers and mathematicians have sought to demonstrate the stability of the Solar System. Thanks to the numerical experiments of the last two decades, we know now that the motion of the pla- nets in the Solar System is chaotic, which prohibits any accurate prediction of their trajectories beyond a few tens of millions of years. The recent simulations even show that planetary colli- sions or ejections are possible on a period of less than 5 billion years, before the end of the life of the Sun. 1. Historical introduction 1 Despite the fundamental results of Henri Poincar´eabout the non-integrability of the three-body problem in the late 19th century, the discovery of the non-regularity of the Solar System's motion is very recent. It indeed required the possibility of calculating the trajectories of the planets with a realistic model of the Solar System over very long periods of time, corresponding to the age of the Solar System. This was only made possible in the past few years. Until then, and this for three centuries, the efforts of astronomers and mathematicians were devoted to demonstrate the stability of the Solar System. arXiv:1209.5996v1 [astro-ph.EP] 26 Sep 2012 1.1. Solar System stability The problem of the Solar System stability dates back to Newton's statement concerning the law of gravitation. -
Cold Plasma Diagnostics in the Jovian System
341 COLD PLASMA DIAGNOSTICS IN THE JOVIAN SYSTEM: BRIEF SCIENTIFIC CASE AND INSTRUMENTATION OVERVIEW J.-E. Wahlund(1), L. G. Blomberg(2), M. Morooka(1), M. André(1), A.I. Eriksson(1), J.A. Cumnock(2,3), G.T. Marklund(2), P.-A. Lindqvist(2) (1)Swedish Institute of Space Physics, SE-751 21 Uppsala, Sweden, E-mail: [email protected], [email protected], mats.andré@irfu.se, [email protected] (2)Alfvén Laboratory, Royal Institute of Technology, SE-100 44 Stockholm, Sweden, E-mail: [email protected], [email protected], [email protected], per- [email protected] (3)also at Center for Space Sciences, University of Texas at Dallas, U.S.A. ABSTRACT times for their atmospheres are of the order of a few The Jovian magnetosphere equatorial region is filled days at most. These atmospheres can therefore rightly with cold dense plasma that in a broad sense co-rotate with its magnetic field. The volcanic moon Io, which be termed exospheres, and their corresponding ionized expels sodium, sulphur and oxygen containing species, parts can be termed exo-ionospheres. dominates as a source for this cold plasma. The three Observations indicate that the exospheres of the three icy Galilean moons (Callisto, Ganymede, and Europa) icy Galilean moons (Europa, Ganymede and Callisto) also contribute with water group and oxygen ions. are oxygen rich [1, 2]. Several authors have also All the Galilean moons have thin atmospheres with modelled these exospheres [3, 4, 5], and the oxygen was residence times of a few days at most. -
SPITZER SPACE TELESCOPE MID-IR LIGHT CURVES of NEPTUNE John Stauffer1, Mark S
The Astronomical Journal, 152:142 (8pp), 2016 November doi:10.3847/0004-6256/152/5/142 © 2016. The American Astronomical Society. All rights reserved. SPITZER SPACE TELESCOPE MID-IR LIGHT CURVES OF NEPTUNE John Stauffer1, Mark S. Marley2, John E. Gizis3, Luisa Rebull1,4, Sean J. Carey1, Jessica Krick1, James G. Ingalls1, Patrick Lowrance1, William Glaccum1, J. Davy Kirkpatrick5, Amy A. Simon6, and Michael H. Wong7 1 Spitzer Science Center (SSC), California Institute of Technology, Pasadena, CA 91125, USA 2 NASA Ames Research Center, Space Sciences and Astrobiology Division, MS245-3, Moffett Field, CA 94035, USA 3 Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, USA 4 Infrared Science Archive (IRSA), 1200 E. California Boulevard, MS 314-6, California Institute of Technology, Pasadena, CA 91125, USA 5 Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology, Pasadena, CA 91125, USA 6 NASA Goddard Space Flight Center, Solar System Exploration Division (690.0), 8800 Greenbelt Road, Greenbelt, MD 20771, USA 7 University of California, Department of Astronomy, Berkeley CA 94720-3411, USA Received 2016 July 13; revised 2016 August 12; accepted 2016 August 15; published 2016 October 27 ABSTRACT We have used the Spitzer Space Telescope in 2016 February to obtain high cadence, high signal-to-noise, 17 hr duration light curves of Neptune at 3.6 and 4.5 μm. The light curve duration was chosen to correspond to the rotation period of Neptune. Both light curves are slowly varying with time, with full amplitudes of 1.1 mag at 3.6 μm and 0.6 mag at 4.5 μm.