Three-Dimensional Modeling of the Stratospheres of Gas Giants
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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. -
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. -
The Inner Solar System Is the Name of the Terrestrial Planets and Asteroid
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Lecture 23: Jupiter Solar System Jupiter's Orbit
Lecture 23: Jupiter Solar System Jupiter’s Orbit •The semi-major axis of Jupiter’s orbit is a = 5.2 AU Jupiter Sun a •Kepler’s third law relates the semi-major axis to the orbital period 1 Jupiter’s Orbit •Kepler’s third law relates the semi-major axis a to the orbital period P 2 3 ⎛ P ⎞ = ⎛ a ⎞ ⎜ ⎟ ⎜ ⎟ ⎝ years⎠ ⎝ AU ⎠ •Solving for the period P yields 3/ 2 ⎛ P ⎞ = ⎛ a ⎞ ⎜ ⎟ ⎜ ⎟ ⎝ years ⎠ ⎝ AU ⎠ •Since a = 5.2 AU for Jupiter, we obtain P = 11.9 Earth years •Jupiter’s orbit has eccentricity e = 0.048 Jupiter’s Orbit •The distance from the Sun varies by about 10% during an orbit Dperihelion = 4.95 AU Daphelion = 5.45 AU •Like Mars, Jupiter is easiest to observe during favorable opposition •At this time, the Earth-Jupiter distance is only about 3.95 AU Earth Jupiter Jupiter Sun (perihelion) (aphelion) •Jupiter appears full during favorable opposition Bulk Properties of Jupiter •Jupiter is the largest planet in the solar system •We have for the radius and mass of Jupiter Rjupiter = 71,400 km = 11.2 Rearth 30 Mjupiter = 1.9 x 10 g = 318 Mearth •The volume of Jupiter is therefore given by 4 V = π R 3 jupiter 3 jupiter 30 3 •Hence Vjupiter = 1.5 x 10 cm 2 Bulk Properties of Jupiter •The average density of Jupiter is therefore M × 30 ρ = jupiter = 1.9 10 g jupiter × 30 3 Vjupiter 1.5 10 cm •We obtain ρ = −3 jupiter 1.24 g cm •This is much less than the average density of the Earth •Hence there is little if any iron and no dense core inside Jupiter Bulk Properties of Jupiter •The average density of the Earth is equal to −3 ρ⊕ = 6 g cm •The density -
Thermal Structure and Composition of Jupiter's Great Red Spot from High-Resolution Thermal Imaging
Thermal Structure and Composition of Jupiter’s Great Red Spot from High-Resolution Thermal Imaging Leigh N. Fletchera,b, G. S. Ortona, O. Mousisc,d, P. Yanamandra-Fishera, P. D. Parrishe,a, P. G. J. Irwinb, B. M. Fishera, L. Vanzif, T. Fujiyoshig, T. Fuseg, A.A. Simon-Millerh, E. Edkinsi, T.L. Haywardj, J. De Buizerk aJet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA, 91109, USA bAtmospheric, Oceanic and Planetary Physics, Department of Physics, University of Oxford, Clarendon Laboratory, Parks Road, Oxford, OX1 3PU, UK cInstitut UTINAM, CNRS-UMR 6213, Observatoire de Besan¸con, Universit´ede Franche-Comt´e, Besan¸con, France dLunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA eSchool of GeoScience, University of Edinburgh, Crew Building, King’s Buildings, Edinburgh, EH9 3JN, UK fPontificia Universidad Catolica de Chile, Department of Electrical Engineering, Av. Vicuna Makenna 4860, Santiago, Chile. gSubaru Telescope, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 650 North A’ohoku Place, Hilo, Hawaii 96720, USA hNASA/Goddard Spaceflight Center, Greenbelt, Maryland, 20771, USA iUniversity of California, Santa Barbara, Santa Barbara, CA 93106, USA jGemini Observatory, Southern Operations Center, c/o AURA, Casilla 603, La Serena, Chile. kSOFIA - USRA, NASA Ames Research Center, Moffet Field, CA 94035, USA. Abstract Thermal-IR imaging from space-borne and ground-based observatories was used to investigate the temperature, composition and aerosol structure of Jupiter’s Great Red Spot (GRS) and its temporal variability between 1995-2008. An elliptical warm core, extending over 8◦ of longitude and 3◦ of latitude, was observed within the cold anticyclonic vortex at 21◦S. -
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. -
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. -
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. -
Dynamics of Jupiter's Atmosphere
6 Dynamics of Jupiter's Atmosphere Andrew P. Ingersoll California Institute of Technology Timothy E. Dowling University of Louisville P eter J. Gierasch Cornell University GlennS. Orton J et P ropulsion Laboratory, California Institute of Technology Peter L. Read Oxford. University Agustin Sanchez-Lavega Universidad del P ais Vasco, Spain Adam P. Showman University of A rizona Amy A. Simon-Miller NASA Goddard. Space Flight Center Ashwin R . V asavada J et Propulsion Laboratory, California Institute of Technology 6.1 INTRODUCTION occurs on both planets. On Earth, electrical charge separa tion is associated with falling ice and rain. On Jupiter, t he Giant planet atmospheres provided many of the surprises separation mechanism is still to be determined. and remarkable discoveries of planetary exploration during The winds of Jupiter are only 1/ 3 as strong as t hose t he past few decades. Studying Jupiter's atmosphere and of aturn and Neptune, and yet the other giant planets comparing it with Earth's gives us critical insight and a have less sunlight and less internal heat than Jupiter. Earth broad understanding of how atmospheres work that could probably has the weakest winds of any planet, although its not be obtained by studying Earth alone. absorbed solar power per unit area is largest. All the gi ant planets are banded. Even Uranus, whose rotation axis Jupiter has half a dozen eastward jet streams in each is tipped 98° relative to its orbit axis. exhibits banded hemisphere. On average, Earth has only one in each hemi cloud patterns and east- west (zonal) jets. -
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. -
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, -
The Meteorology of Jupiter the Visible Features of the Giant Planet Reflect the Circulation of Its Atmosphere
The Meteorology of Jupiter The visible features of the giant planet reflect the circulation of its atmosphere. A model reproducing those features should apply to other planetary atmospheres, including the earth's by Andrew P. Ingersoll very feature that is visible in a picture mospheres of the two planets consist chiefly inferred ratio of helium to hydrogen in the of the planet Jupiter is a cloud: the of noncondensable gases: hydrogen and he sun (I 15). It is the abundance ratios, to E : dark belts, the light-colored zones lium on Jupiter, nitrogen and oxygen on the gether with the low density of Jupiter as a and the Great Red Spot. The solid surface, earth; mixed in are small amounts of water whole, that suggest that the planet is very if indeed there is one, lies many thousands vapor and other gases that do condense, much like the sun in its composition. of kilometers below the visible surface. Yet forming clouds. In terms of the temperature The amount of heat Jupiter radiates im most of the atmospheric features of Jupiter changes that would occur on the two plan plies that the interior of the planet is hot. If have an extremely long lifetime and an or ets if the condensable vapors were entirely it were cold, there would not be enough ganized structure that is unknown in atmo converted into liquid or solid form, thus heat in the interior to have lasted until the spheric features of the earth. Those differ releasing all their latent heat, Jupiter's at present time.