Lecture Tutorial: Properties of Gas Giant Planets

Total Page:16

File Type:pdf, Size:1020Kb

Lecture Tutorial: Properties of Gas Giant Planets Lecture Tutorial: Properties of gas giant planets In this class, we've talked often about scale models, which give us a sense of the relative sizes and distances of objects in the solar system. The Sun, Jupiter, and the Earth have the following approximate diameters: The Sun: 1,400,000 km Jupiter: 140,000 km Earth: 13,000 km 1. About how many times bigger is the Sun's diameter than Jupiter's diameter? (a) 2 (b) 5 (c) 10 (d) 100 2. About how many times bigger is the Sun's diameter than Earth's diameter? (a) 2 (b) 5 (c) 10 (d) 100 The last page of this tutorial shows the sizes of the Sun, Jupiter and the Earth, to scale. 3. Suppose you had been provided with this diagram, but not been provided with the actual sizes of the Sun, Jupiter and Earth's diameters. Could you still have answered questions (1) and (2)? If so, how? If not, why not? 4. What three objects would make a good scale model of the Sun, Jupiter and the Earth (in that order)? (a) a basketball, a soccer ball and a baseball (b) a melon, a cherry, and a peppercorn (c) a basketball, a golf ball, and a ping-pong ball (d) an apple, an orange, and a cherry The following figure shows the size of the sun in the sky as seen from each of the planets, plus Pluto. 1 5. Suppose John is floating out in space near Jupiter, and Maria is floating out in space near Venus. Who will feel colder and why? 6. Suppose John is floating out in space near Jupiter, and Carla is floating out in space near Pluto. Who will feel colder and why? 7. The diagram below shows the temperature and pressure in Jupiter's atmosphere. Suppose Juan is flying a spacecraft near the top of Jupiter's atmosphere, where the pressure is 1 atm (1 atm is the same as the pressure on the surface of the Earth). He realizes he forgot a cup of water on top of the spacecraft a few hours ago. When he goes to get it, will the cup contain liquid, or ice? Explain your reasoning. Jupiter orbits the sun on a nearly circular orbit with a radius of 5 Astronomical Units (AU). Saturn orbits the sun on a nearly circular orbit with a radius of 10 AU. 8. In the space below, draw the orbits of Jupiter and Saturn around the Earth, making sure their sizes are to scale. 2 9. On the orbits you just drew, draw two dots to represent Jupiter and Saturn at a time in their orbits when they are closest to each other. At this time, what is the distance between Jupiter and Saturn? 10. At this time, what is the distance between Jupiter and the Sun, in Astronomical Units? Use the diagram you drew and your knowledge about Jupiter and Saturn to complete the following sentences: 11. During Jupiter's orbit around the sun, it is (a) Always about the same distance between the Sun and Saturn (b) Almost always farther from Saturn than from the Sun (c) Almost always closer to Saturn than to the Sun 12. For an observer in a spacecraft orbiting right near Jupiter (a) the Sun and Saturn will be about the same size in the sky (b) the Sun will almost always look larger than Saturn (c) the Sun will almost always look smaller than Saturn Jupiter and Saturn are composed mostly of Hydrogen and Helium gas. 13. What do you think would happen if you tried to land a spacecraft on Jupiter or Saturn? 14. The density of gas on the surface of the Earth is about 1 kg/m3. Although Jupiter is also made of gas, the average density of Jupiter is much higher | about 1000 kg/m3. Why do you think this is? 3 Jupiter Earth The Sun 4.
Recommended publications
  • The Jovian Planets (Gas Giants) Discoveries
    The Jovian Planets (Gas Giants) Discoveries Saturn Jupiter Jupiter and Saturn known to ancient astronomers. Uranus discovered in 1781 by Sir William Herschel (England). Neptune discovered in 1845 by Johann Galle (Germany). Predicted to exist by John Adams and Urbain Leverrier because of irregularities in Uranus' orbit. Almost discovered by Galileo in 1613 Uranus Neptune (roughly to scale) Remember that compared to Terrestrial planets, Jovian planets: Orbital Properties: Distance from Sun Orbital Period are massive (AU) (years) are less dense (0.7 – 1.3 g/cm3) Jupiter 5.2 11.9 are mostly gas (and liquid) Saturn 9.5 29.4 rotate fast (9 - 17 hours rotation periods) Uranus 19.2 84 have rings and many moons Neptune 30.1 164 Known Moons Mass (MEarth) Radius (REarth) Major Missions: Launch Planets visited Jupiter 318 11 63 Voyager 1 1977 Jupiter, Saturn (0.001 MSun) Saturn 95 9.5 50 Voyager 2 1979 Jupiter, Saturn, Uranus, Neptune Uranus 15 4 27 Galileo 1989 Jupiter Neptune 17 3.9 13 Cassini 1997 Jupiter, Saturn Jupiter's Atmosphere Composition: mostly H, some He, traces of other elements (true for all Jovians). Gravity strong enough to retain even light elements. Mostly molecular. Altitude 0 km defined as top of troposphere (cloud layer) Ammonia (NH3) ice gives white colors. Ammonium hydrosulfide Optical – colors dictated Infrared - traces heat in (NH4SH) ice should form by how molecules atmosphere. here, somehow giving red, reflect sunlight yellow, brown colors. Water ice layer not seen due to higher layers. So white colors from cooler, higher clouds, brown and red from warmer, lower clouds.
    [Show full text]
  • 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.
    [Show full text]
  • The Inner Solar System Is the Name of the Terrestrial Planets and Asteroid
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
    [Show full text]
  • Heavy Element Enrichment of the Gas Giant Planets By
    Heavy Element Enrichment of the Gas Giant Planets by Jaime Lee Coffey Hon.B.Sc., The University of Toronto, 2006 A THESIS SUBMITTED IN PARTIAL FULFILMENT OF THE REQUIREMENTS FOR THE DEGREE OF Master of Science in The Faculty of Graduate Studies (Astronomy) The University Of British Columbia Vancouver, Canada August 2008 © Jaime Lee Coffey 2008 Abstract According to both spectroscopic measurements and interior models, Jupiter, Saturn, Uranus and Neptune possess gaseous envelopes that are enriched in heavy elements compared to the Sun. Straightforward application of the dominant theories of gas giant formation - core accretion and gravitational instability - fail to provide the observed enrichment, suggesting that the surplus heavy elements were somehow dumped onto the planets after the envelopes were already in existence. Previous work has shown that if giant planets rapidly reached their cur rent configuration and radii, they do not accrete the remaining planetesimals efficiently enough to explain their observed heavy-element surplus. We ex plore the likely scenario that the effective accretion cross-sections of the giants were enhanced by the presence of the massive circumplanetary disks out of which their regular satellite systems formed. Perhaps surprisingly, we find that a simple model with protosatellite disks around Jupiter and Saturn can meet known constraints without tuning any parameters. Fur thermore, we show that the heavy-element budgets in Jupiter and Saturn can be matched slightly better if Saturn’s envelope (and disk) are formed roughly 0.1 — 10 Myr after that of Jupiter. We also show that giant planets forming in an initially-compact con figuration can acquire the observed enrichments if they are surrounded by similar protosatellite disks.
    [Show full text]
  • DISCOVERY of XO-6B: a HOT JUPITER TRANSITING a FAST ROTATING F5 STAR on an OBLIQUE ORBIT N Crouzet 1, P
    Draft version November 18, 2016 Preprint typeset using LATEX style emulateapj v. 01/23/15 DISCOVERY OF XO-6b: A HOT JUPITER TRANSITING A FAST ROTATING F5 STAR ON AN OBLIQUE ORBIT N Crouzet 1, P. R. McCullough 2, D. Long 3, P. Montanes Rodriguez 4, A. Lecavelier des Etangs 5, I. Ribas 6, V. Bourrier 7, G. Hebrard´ 5, F. Vilardell 8, M. Deleuil 9, E. Herrero 6,8, E. Garcia-Melendo 10,11, L. Akhenak 5, J. Foote 12, B. Gary 13, P. Benni 14, T. Guillot 15, M. Conjat 15, D. Mekarnia´ 15, J. Garlitz 16, C. J. Burke 17, B. Courcol 9, and O. Demangeon 9 1 Dunlap Institute for Astronomy & Astrophysics, University of Toronto, 50 St. George Street, Toronto, Ontario, Canada M5S 3H4 2 Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA 3 Space Telescope Science Institute, 3700 San Martin Dr, Baltimore, MD 21218, USA 4 Instituto de Astrof´ısicade Canarias, C/V´ıaL´acteas/n, E-38200 La Laguna, Spain 5 Institut d'Astrophysique de Paris, UMR7095 CNRS, Universit´ePierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France 6 Institut de Ci`enciesde l'Espai (CSIC-IEEC), Campus UAB, Carrer de Can Magrans s/n, 08193 Bellaterra, Spain 7 Observatoire de l'Universit´ede Gen`eve, 51 chemin des Maillettes, 1290 Sauverny, Switzerland 8 Observatori del Montsec (OAdM), Institut d'Estudis Espacials de Catalunya (IEEC), Gran Capit`a,2-4, Edif. Nexus, 08034 Barcelona, Spain 9 Aix Marseille Universit´e,CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388 Marseille, France 10 Departamento de F´ısicaAplicada I, Escuela T´ecnica Superior de Ingenier´ıa,Universidad del Pa´ısVasco UPV/EHU, Alameda Urquijo s/n, 48013 Bilbao, Spain 11 Fundacio Observatori Esteve Duran, Avda.
    [Show full text]
  • Terrestrial Planets in High-Mass Disks Without Gas Giants
    A&A 557, A42 (2013) Astronomy DOI: 10.1051/0004-6361/201321304 & c ESO 2013 Astrophysics Terrestrial planets in high-mass disks without gas giants G. C. de Elía, O. M. Guilera, and A. Brunini Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata and Instituto de Astrofísica de La Plata, CCT La Plata-CONICET-UNLP, Paseo del Bosque S/N, 1900 La Plata, Argentina e-mail: [email protected] Received 15 February 2013 / Accepted 24 May 2013 ABSTRACT Context. Observational and theoretical studies suggest that planetary systems consisting only of rocky planets are probably the most common in the Universe. Aims. We study the potential habitability of planets formed in high-mass disks without gas giants around solar-type stars. These systems are interesting because they are likely to harbor super-Earths or Neptune-mass planets on wide orbits, which one should be able to detect with the microlensing technique. Methods. First, a semi-analytical model was used to define the mass of the protoplanetary disks that produce Earth-like planets, super- Earths, or mini-Neptunes, but not gas giants. Using mean values for the parameters that describe a disk and its evolution, we infer that disks with masses lower than 0.15 M are unable to form gas giants. Then, that semi-analytical model was used to describe the evolution of embryos and planetesimals during the gaseous phase for a given disk. Thus, initial conditions were obtained to perform N-body simulations of planetary accretion. We studied disks of 0.1, 0.125, and 0.15 M.
    [Show full text]
  • The Nature of the Giant Exomoon Candidate Kepler-1625 B-I René Heller
    A&A 610, A39 (2018) https://doi.org/10.1051/0004-6361/201731760 Astronomy & © ESO 2018 Astrophysics The nature of the giant exomoon candidate Kepler-1625 b-i René Heller Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany e-mail: [email protected] Received 11 August 2017 / Accepted 21 November 2017 ABSTRACT The recent announcement of a Neptune-sized exomoon candidate around the transiting Jupiter-sized object Kepler-1625 b could indi- cate the presence of a hitherto unknown kind of gas giant moon, if confirmed. Three transits of Kepler-1625 b have been observed, allowing estimates of the radii of both objects. Mass estimates, however, have not been backed up by radial velocity measurements of the host star. Here we investigate possible mass regimes of the transiting system that could produce the observed signatures and study them in the context of moon formation in the solar system, i.e., via impacts, capture, or in-situ accretion. The radius of Kepler-1625 b suggests it could be anything from a gas giant planet somewhat more massive than Saturn (0:4 MJup) to a brown dwarf (BD; up to 75 MJup) or even a very-low-mass star (VLMS; 112 MJup ≈ 0:11 M ). The proposed companion would certainly have a planetary mass. Possible extreme scenarios range from a highly inflated Earth-mass gas satellite to an atmosphere-free water–rock companion of about +19:2 180 M⊕. Furthermore, the planet–moon dynamics during the transits suggest a total system mass of 17:6−12:6 MJup.
    [Show full text]
  • On the Detection of Exomoons in Photometric Time Series
    On the Detection of Exomoons in Photometric Time Series Dissertation zur Erlangung des mathematisch-naturwissenschaftlichen Doktorgrades “Doctor rerum naturalium” der Georg-August-Universität Göttingen im Promotionsprogramm PROPHYS der Georg-August University School of Science (GAUSS) vorgelegt von Kai Oliver Rodenbeck aus Göttingen, Deutschland Göttingen, 2019 Betreuungsausschuss Prof. Dr. Laurent Gizon Max-Planck-Institut für Sonnensystemforschung, Göttingen, Deutschland und Institut für Astrophysik, Georg-August-Universität, Göttingen, Deutschland Prof. Dr. Stefan Dreizler Institut für Astrophysik, Georg-August-Universität, Göttingen, Deutschland Dr. Warrick H. Ball School of Physics and Astronomy, University of Birmingham, UK vormals Institut für Astrophysik, Georg-August-Universität, Göttingen, Deutschland Mitglieder der Prüfungskommision Referent: Prof. Dr. Laurent Gizon Max-Planck-Institut für Sonnensystemforschung, Göttingen, Deutschland und Institut für Astrophysik, Georg-August-Universität, Göttingen, Deutschland Korreferent: Prof. Dr. Stefan Dreizler Institut für Astrophysik, Georg-August-Universität, Göttingen, Deutschland Weitere Mitglieder der Prüfungskommission: Prof. Dr. Ulrich Christensen Max-Planck-Institut für Sonnensystemforschung, Göttingen, Deutschland Dr.ir. Saskia Hekker Max-Planck-Institut für Sonnensystemforschung, Göttingen, Deutschland Dr. René Heller Max-Planck-Institut für Sonnensystemforschung, Göttingen, Deutschland Prof. Dr. Wolfram Kollatschny Institut für Astrophysik, Georg-August-Universität, Göttingen,
    [Show full text]
  • Exploration of the Ice Giant Systems
    Exploration of the Ice Giant Systems A White Paper for NASA's Planetary Science and Astrobiology Decadal Survey 2023-2032 Uranus (left) [1] and Neptune (right) (NASA) Lead Authors: Chloe B. Beddingfield1,2 1The SETI Institute 2NASA Ames Research Center [email protected] (972) 415-7604 Cheng Li3 3University of California, Berkeley [email protected] Primary Co-Authors: Sushil Atreya4 Patricia Beauchamp5 Ian Cohen6 Jonathan Fortney7 Heidi Hammel8 Matthew Hedman9 Mark Hofstadter5 Abigail Rymer6 Paul Schenk10 Mark Showalter1 4University of Michigan, Ann Arbor, 5Jet Propulsion Laboratory, 6Johns Hopkins University Applied Physics Laboratory, 7University of California, Santa Cruz, 8Association of Universities for Research in Astronomy, 9University of Idaho, 10Lunar and Planetary Institute Additional Coauthors and Endorsers: For a full list of the 145 authors and endorsers, see the following link: https://docs.google.com/document/d/158h8ZK0HXp- DSQqVhV7gcGzjHqhUJ_2MzQAsRg3sxXw/edit?usp=sharing Motivation Ice giants are the only unexplored class of planet in our Solar System. Much that we currently know about these systems challenges our understanding of how planets, rings, satellites, and magnetospheres form and evolve. We assert that an ice giant Flagship mission with an atmospheric probe should be a priority for the decade 2023-2032. Investigation of Uranus or Neptune would advance fundamental understanding of many key issues in Solar System formation: 1) how ice giants formed and migrated through the Solar System; 2) what processes control the current conditions of this class of planet, its rings, satellites, and magnetospheres; 3) how the rings and satellites formed and evolved, and how Triton was captured from the Kuiper Belt; 4) whether the large satellites of the ice giants are ocean worlds that may harbor life now or in the past; and 5) the range of possible characteristics for exoplanets.
    [Show full text]
  • Rest of the Solar System” As We Have Covered It in MMM Through the Years
    As The Moon, Mars, and Asteroids each have their own dedicated theme issues, this one is about the “rest of the Solar System” as we have covered it in MMM through the years. Not yet having ventured beyond the Moon, and not yet having begun to develop and use space resources, these articles are speculative, but we trust, well-grounded and eventually feasible. Included are articles about the inner “terrestrial” planets: Mercury and Venus. As the gas giants Jupiter, Saturn, Uranus, and Neptune are not in general human targets in themselves, most articles about destinations in the outer system deal with major satellites: Jupiter’s Io, Europa, Ganymede, and Callisto. Saturn’s Titan and Iapetus, Neptune’s Triton. We also include past articles on “Space Settlements.” Europa with its ice-covered global ocean has fascinated many - will we one day have a base there? Will some of our descendants one day live in space, not on planetary surfaces? Or, above Venus’ clouds? CHRONOLOGICAL INDEX; MMM THEMES: OUR SOLAR SYSTEM MMM # 11 - Space Oases & Lunar Culture: Space Settlement Quiz Space Oases: Part 1 First Locations; Part 2: Internal Bearings Part 3: the Moon, and Diferent Drums MMM #12 Space Oases Pioneers Quiz; Space Oases Part 4: Static Design Traps Space Oases Part 5: A Biodynamic Masterplan: The Triple Helix MMM #13 Space Oases Artificial Gravity Quiz Space Oases Part 6: Baby Steps with Artificial Gravity MMM #37 Should the Sun have a Name? MMM #56 Naming the Seas of Space MMM #57 Space Colonies: Re-dreaming and Redrafting the Vision: Xities in
    [Show full text]
  • Planets Worksheets
    Planets Worksheets Thank you so much for purchasing my work! I hope you enjoy it as much as I enjoyed making it! Make sure to stop by my store again for great specials! You are always a valued customer. If you have any request, I will surely try and see if I can make it happen for you! -Mary Name: ______________________ Date:_____________________ Facts about Mercury • In Roman mythology Mercury is the god of commerce, travel and thievery, the Roman counterpart of the Greek god Hermes, the messenger of the Gods. The planet received this name because it moves so quickly across the sky. • Mercury is a small planet which orbits closer to the sun than any other planet in our solar system. • Mercury has no moons. • Mercury’s surface is very hot, it features a barren, crater covered surface which looks similar to Earth’s moon. • Mercury is so close to the Sun, the daytime temperature is scorching reaching over 400 degrees Celsius. • At night however, without an atmosphere to hold heat in, the temperatures plummet, dropping to -180 degrees Celsius. • Mercury has a very low surface gravity. • Mercury has no atmosphere which means there is no wind or weather to speak of. • Mercury has no water or air on the surface. Mercury’s symbol Name: ______________________ Date:_____________________ Read each question. Then, write your answer. 1. How many moons does Mercury have? 2. Why was the planet Mercury named after the Roman god? 3. Mercury’s surface looks similar to what moon? 4. What is Mercury’s temperature at night? 5.
    [Show full text]
  • Giant Planet Formation, Evolution, and Internal Structure
    Giant Planet Formation, Evolution, and Internal Structure Ravit Helled Tel-Aviv University Peter Bodenheimer University of California, Santa Cruz Morris Podolak Tel-Aviv University Aaron Boley University of Florida & The University of British Columbia Farzana Meru ETH Zurich¨ Sergei Nayakshin University of Leicester Jonathan J. Fortney University of California, Santa Cruz Lucio Mayer University of Zurich¨ Yann Alibert University of Bern Alan P. Boss Carnegie Institution The large number of detected giant exoplanets offers the opportunity to improve our un- derstanding of the formation mechanism, evolution, and interior structure of gas giant planets. The two main models for giant planet formation are core accretion and disk instability. There are substantial differences between these formation models, including formation timescale, favorable formation location, ideal disk properties for planetary formation, early evolution, planetary composition, etc. First, we summarize the two models including their substantial differences, advantages, and disadvantages, and suggest how theoretical models should be connected to available (and future) data. We next summarize current knowledge of the internal structures of solar- and extrasolar- giant planets. Finally, we suggest the next steps to be taken in giant planet exploration. 1. INTRODUCTION conditions of protoplanetary disks in which planets form. Furthermore, the diversity in properties (e.g. mass, radius, Giant planets play a critical role in shaping the architec- semi-major axis, density)
    [Show full text]