1
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Fletcher LN, Cavalié T, Grassi D, Hueso R, Lara LM, Kaspi Y, Galanti E, Greathouse TK, Molyneux PM, Galand M, Vallat C, Witasse O, Lorente R, Hartogh P, Poulet F, Langevin Y, Palumbo P, Gladstone GR, Retherford KD, Dougherty MK, Wahlund JE, Barabash S, Iess L, Bruzzone L, Hussmann H, Gurvits LI, Santolik O, Kolmasova I, Fischer G, Müller-Wodarg I, Piccioni G, Fouchet T, Gérard JC, Sánchez-Lavega A, Irwin PGJ, Grodent D, Altieri F, Mura A, Drossart P, Kammer J, Giles R, Cazaux S, Jones G, Smirnova M, Lellouch E, Medvedev AS, Moreno R, Rezac L, Coustenis A, Costa M. Jupiter Science Enabled by ESA's Jupiter Icy Moons Explorer. SPACE SCIENCE REVIEWS 2023; 219:53. [PMID: 37744214 PMCID: PMC10511624 DOI: 10.1007/s11214-023-00996-6] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 04/21/2023] [Accepted: 08/10/2023] [Indexed: 09/26/2023]
Abstract
ESA's Jupiter Icy Moons Explorer (JUICE) will provide a detailed investigation of the Jovian system in the 2030s, combining a suite of state-of-the-art instruments with an orbital tour tailored to maximise observing opportunities. We review the Jupiter science enabled by the JUICE mission, building on the legacy of discoveries from the Galileo, Cassini, and Juno missions, alongside ground- and space-based observatories. We focus on remote sensing of the climate, meteorology, and chemistry of the atmosphere and auroras from the cloud-forming weather layer, through the upper troposphere, into the stratosphere and ionosphere. The Jupiter orbital tour provides a wealth of opportunities for atmospheric and auroral science: global perspectives with its near-equatorial and inclined phases, sampling all phase angles from dayside to nightside, and investigating phenomena evolving on timescales from minutes to months. The remote sensing payload spans far-UV spectroscopy (50-210 nm), visible imaging (340-1080 nm), visible/near-infrared spectroscopy (0.49-5.56 μm), and sub-millimetre sounding (near 530-625 GHz and 1067-1275 GHz). This is coupled to radio, stellar, and solar occultation opportunities to explore the atmosphere at high vertical resolution; and radio and plasma wave measurements of electric discharges in the Jovian atmosphere and auroras. Cross-disciplinary scientific investigations enable JUICE to explore coupling processes in giant planet atmospheres, to show how the atmosphere is connected to (i) the deep circulation and composition of the hydrogen-dominated interior; and (ii) to the currents and charged particle environments of the external magnetosphere. JUICE will provide a comprehensive characterisation of the atmosphere and auroras of this archetypal giant planet.
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Affiliation(s)
- Leigh N. Fletcher
- School of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH UK
| | - Thibault Cavalié
- Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, 33615 Pessac, France
- LESIA, Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CNRS, 5 place Jules Janssen, 92195 Meudon, France
| | - Davide Grassi
- Istituto di Astrofisica e Planetologia Spaziali - Istituto Nazionale di Astrofisica, Via del Fosso del Cavaliere, 100, I-00133 Roma, Italy
| | - Ricardo Hueso
- Física Aplicada, Escuela de Ingeniería de Bilbao Universidad del País Vasco UPV/EHU, Plaza Ingeniero Torres Quevedo, 1, 48013 Bilbao, Spain
| | - Luisa M. Lara
- Instituto de Astrofísica de Andalucía-CSIC, c/Glorieta de la Astronomía 3, 18008 Granada, Spain
| | - Yohai Kaspi
- Dept. of Earth and Planetray Science, Weizmann Institute of Science, Rehovot, Israel 76100
| | - Eli Galanti
- Dept. of Earth and Planetray Science, Weizmann Institute of Science, Rehovot, Israel 76100
| | | | | | - Marina Galand
- Department of Physics, Imperial College London, Prince Consort Road, London, SW7 2AZ UK
| | - Claire Vallat
- European Space Agency (ESA), ESAC Camino Bajo del Castillo s/n Villafranca del Castillo, 28692 Villanueva de la Cañada (Madrid), Spain
| | - Olivier Witasse
- European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Noordwijk, Netherlands
| | - Rosario Lorente
- European Space Agency (ESA), ESAC Camino Bajo del Castillo s/n Villafranca del Castillo, 28692 Villanueva de la Cañada (Madrid), Spain
| | - Paul Hartogh
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - François Poulet
- Institut d’Astrophysique Spatiale, CNRS/Université Paris-Sud, 91405 Orsay Cedex, France
| | - Yves Langevin
- Institut d’Astrophysique Spatiale, CNRS/Université Paris-Sud, 91405 Orsay Cedex, France
| | - Pasquale Palumbo
- Istituto di Astrofisica e Planetologia Spaziali - Istituto Nazionale di Astrofisica, Via del Fosso del Cavaliere, 100, I-00133 Roma, Italy
| | - G. Randall Gladstone
- Southwest Research Institute, San Antonio, TX 78228 United States
- University of Texas at San Antonio, San Antonio, TX United States
| | - Kurt D. Retherford
- Southwest Research Institute, San Antonio, TX 78228 United States
- University of Texas at San Antonio, San Antonio, TX United States
| | | | | | - Stas Barabash
- Swedish Institute of Space Physics (IRF), Kiruna, Sweden
| | - Luciano Iess
- Dipartimento di ingegneria meccanica e aerospaziale, Universit á La Sapienza, Roma, Italy
| | - Lorenzo Bruzzone
- Department of Information Engineering and Computer Science, Remote Sensing Laboratory, University of Trento, Via Sommarive 14, Trento, I-38123 Italy
| | - Hauke Hussmann
- Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - Leonid I. Gurvits
- Joint Institute for VLBI ERIC, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands
- Aerospace Faculty, Delft University of Technology, Kluyverweg 1, 2629 HS Delft, The Netherlands
| | - Ondřej Santolik
- Department of Space Physics, Institute of Atmospheric Physics of the Czech Academy of Sciences, Prague, Czechia
- Faculty of Mathematics and Physics, Charles University, Prague, Czechia
| | - Ivana Kolmasova
- Department of Space Physics, Institute of Atmospheric Physics of the Czech Academy of Sciences, Prague, Czechia
- Faculty of Mathematics and Physics, Charles University, Prague, Czechia
| | - Georg Fischer
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | | | - Giuseppe Piccioni
- Istituto di Astrofisica e Planetologia Spaziali - Istituto Nazionale di Astrofisica, Via del Fosso del Cavaliere, 100, I-00133 Roma, Italy
| | - Thierry Fouchet
- LESIA, Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CNRS, 5 place Jules Janssen, 92195 Meudon, France
| | | | - Agustin Sánchez-Lavega
- Física Aplicada, Escuela de Ingeniería de Bilbao Universidad del País Vasco UPV/EHU, Plaza Ingeniero Torres Quevedo, 1, 48013 Bilbao, Spain
| | - Patrick G. J. Irwin
- Atmospheric, Oceanic and Planetary Physics, Department of Physics, University of Oxford, Parks Rd, Oxford, OX1 3PU UK
| | - Denis Grodent
- LPAP, STAR Institute, Université de Liège, Liège, Belgium
| | - Francesca Altieri
- Istituto di Astrofisica e Planetologia Spaziali - Istituto Nazionale di Astrofisica, Via del Fosso del Cavaliere, 100, I-00133 Roma, Italy
| | - Alessandro Mura
- Istituto di Astrofisica e Planetologia Spaziali - Istituto Nazionale di Astrofisica, Via del Fosso del Cavaliere, 100, I-00133 Roma, Italy
| | - Pierre Drossart
- LESIA, Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CNRS, 5 place Jules Janssen, 92195 Meudon, France
- Institut d’Astrophysique de Paris, CNRS, Sorbonne Université, 98bis Boulevard Arago, 75014 Paris, France
| | - Josh Kammer
- Southwest Research Institute, San Antonio, TX 78228 United States
| | - Rohini Giles
- Southwest Research Institute, San Antonio, TX 78228 United States
| | - Stéphanie Cazaux
- Faculty of Aerospace Engineering, Delft University of Technology, Delft, The Netherlands
| | - Geraint Jones
- UCL Mullard Space Science Laboratory, Hombury St. Mary, Dorking, RH5 6NT UK
- The Centre for Planetary Sciences at UCL/Birkbeck, London, WC1E 6BT UK
| | - Maria Smirnova
- Dept. of Earth and Planetray Science, Weizmann Institute of Science, Rehovot, Israel 76100
| | - Emmanuel Lellouch
- LESIA, Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CNRS, 5 place Jules Janssen, 92195 Meudon, France
| | | | - Raphael Moreno
- LESIA, Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CNRS, 5 place Jules Janssen, 92195 Meudon, France
| | - Ladislav Rezac
- Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany
| | - Athena Coustenis
- LESIA, Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CNRS, 5 place Jules Janssen, 92195 Meudon, France
| | - Marc Costa
- Rhea Group, for European Space Agency, ESAC, Madrid, Spain
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2
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White TG, Dai J, Riley D. Dynamic and transient processes in warm dense matter. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2023; 381:20220223. [PMID: 37393937 PMCID: PMC10315215 DOI: 10.1098/rsta.2022.0223] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/05/2023] [Accepted: 05/22/2023] [Indexed: 07/04/2023]
Abstract
In this paper, we discuss some of the key challenges in the study of time-dependent processes and non-equilibrium behaviour in warm dense matter. We outline some of the basic physics concepts that have underpinned the definition of warm dense matter as a subject area in its own right and then cover, in a selective, non-comprehensive manner, some of the current challenges, pointing along the way to topics covered by the papers presented in this volume. This article is part of the theme issue 'Dynamic and transient processes in warm dense matter'.
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Affiliation(s)
- Thomas G. White
- Department of Physics, University of Nevada, Reno, NV 89557, USA
| | - Jiayu Dai
- College of Science, National University of Defense Technology, Changsha 410073, People’s Republic of China
| | - David Riley
- School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK
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3
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Liang JH, Hu TX, Wu D, Sheng ZM. Kinetic studies of exchange-correlation effect on the collective excitations of warm dense plasmas. Phys Rev E 2022; 105:045206. [PMID: 35590614 DOI: 10.1103/physreve.105.045206] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/02/2021] [Accepted: 03/25/2022] [Indexed: 06/15/2023]
Abstract
The exchange-correlation of electrons, as a fundamental effect in quantum mechanics, plays an important role in the collective motions of electrons in warm dense matter. We derive the quantum kinetic equations based on the time-dependent Kohn-Sham equation. By using a temperature-dependent functional for the exchange correlation, the excitations of electrostatic waves are analyzed under the adiabatic local density approximation (ALDA). We find that the influences of the exchange-correlation effect on the group velocity of electrostatic waves can be as high as 10% when both the density and temperature are low. Moreover, we also compare the results obtained by using ALDA-based kinetic theory, exchange kinetic theory, and quantum hydrodynamics, and discuss the differences among them.
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Affiliation(s)
- Jiong-Hang Liang
- Institute for Fusion Theory and Simulation, Department of Physics, Zhejiang University, 310027 Hangzhou, People's Republic of China
| | - Tian-Xing Hu
- Institute for Fusion Theory and Simulation, Department of Physics, Zhejiang University, 310027 Hangzhou, People's Republic of China
| | - D Wu
- Key Laboratory for Laser Plasmas, School of Physics and Astronomy, and Collaborative Innovation Center of IFSA (CICIFSA), Shanghai Jiao Tong University, 200240 Shanghai, People's Republic of China
| | - Zheng-Mao Sheng
- Institute for Fusion Theory and Simulation, Department of Physics, Zhejiang University, 310027 Hangzhou, People's Republic of China
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Bolton SJ, Levin SM, Guillot T, Li C, Kaspi Y, Orton G, Wong MH, Oyafuso F, Allison M, Arballo J, Atreya S, Becker HN, Bloxham J, Brown ST, Fletcher LN, Galanti E, Gulkis S, Janssen M, Ingersoll A, Lunine JL, Misra S, Steffes P, Stevenson D, Waite JH, Yadav RK, Zhang Z. Microwave observations reveal the deep extent and structure of Jupiter's atmospheric vortices. Science 2021; 374:968-972. [PMID: 34709937 DOI: 10.1126/science.abf1015] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
[Figure: see text].
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Affiliation(s)
- S J Bolton
- Southwest Research Institute, San Antonio, TX, USA
| | - S M Levin
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - T Guillot
- Université Côte d'Azur, Observatoire de la Côte d'Azur, Centre National de la Recherche Scientifique, Laboratoire Lagrange, Nice, France
| | - C Li
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI, USA
| | - Y Kaspi
- Weizmann Institute of Science, Rehovot, 76100, Israel
| | - G Orton
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - M H Wong
- Carl Sagan Center for Research, SETI Institute, Mountain View, CA, USA
| | - F Oyafuso
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - M Allison
- Goddard Institute for Space Studies, New York, NY, USA.,Department of Astronomy, Columbia University, New York, NY 10027, USA
| | - J Arballo
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - S Atreya
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI, USA
| | - H N Becker
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - J Bloxham
- Department of Earth and Planetary Sciences, Harvard University, Cambridge, MA 02138, USA
| | - S T Brown
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - L N Fletcher
- School of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UK
| | - E Galanti
- Weizmann Institute of Science, Rehovot, 76100, Israel
| | - S Gulkis
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - M Janssen
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - A Ingersoll
- Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - J L Lunine
- Department of Astronomy, Cornell University, Ithaca, NY, USA
| | - S Misra
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - P Steffes
- Department of Electrical and Computer Engineering, Georgia Institute of Technology, Atlanta, GA, USA
| | - D Stevenson
- Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - J H Waite
- Southwest Research Institute, San Antonio, TX, USA
| | - R K Yadav
- Department of Earth and Planetary Sciences, Harvard University, Cambridge, MA 02138, USA
| | - Z Zhang
- Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
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5
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Dornheim T, Vorberger J. Finite-size effects in the reconstruction of dynamic properties from ab initio path integral Monte Carlo simulations. Phys Rev E 2020; 102:063301. [PMID: 33466040 DOI: 10.1103/physreve.102.063301] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/20/2020] [Accepted: 11/15/2020] [Indexed: 06/12/2023]
Abstract
We systematically investigate finite-size effects in the dynamic structure factor S(q,ω) of the uniform electron gas obtained via the analytic continuation of ab initio path integral Monte Carlo data for the imaginary-time density-density correlation function F(q,τ). Using the recent scheme by Dornheim et al. [Phys. Rev. Lett. 121, 255001 (2018)PRLTAO0031-900710.1103/PhysRevLett.121.255001], we find that the reconstructed spectra are not afflicted with any finite-size effects for as few as N=14 electrons both at warm dense matter (WDM) conditions and at the margins of the strongly correlated electron liquid regime. Our results further corroborate the high quality of our current description of the dynamic density response of correlated electrons, which is of high importance for many applications in WDM theory and beyond.
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Affiliation(s)
- Tobias Dornheim
- Center for Advanced Systems Understanding (CASUS), D-02826 Görlitz, Germany
| | - Jan Vorberger
- Helmholtz-Zentrum Dresden-Rossendorf (HZDR), D-01328 Dresden, Germany
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6
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Yadav RK, Heimpel M, Bloxham J. Deep convection-driven vortex formation on Jupiter and Saturn. SCIENCE ADVANCES 2020; 6:6/46/eabb9298. [PMID: 33188017 PMCID: PMC7673750 DOI: 10.1126/sciadv.abb9298] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 03/27/2020] [Accepted: 10/02/2020] [Indexed: 06/11/2023]
Abstract
The surfaces of Jupiter and Saturn have magnificent vortical storms that help shape the dynamic nature of their atmospheres. Land- and space-based observational campaigns have established several properties of these vortices, with some being similar between the two planets, while others are different. Shallow-water hydrodynamics, where the vortices are treated as shallow weather-layer phenomenon, is commonly evoked for explaining their formation and properties. Here, we report novel formation mechanisms for vortices where the primary driving mechanism is the deep planetary convection occurring in these planets. Using three-dimensional simulations of turbulent convection in rotating spherical shells, we propose two ideas: (i) Rotating turbulent convection generates deep axially aligned cyclones and anticyclones; (ii) a deep planetary dynamo acts to promote additional anticyclones, some as large as Jupiter's Great Red Spot, in an overlying atmospheric layer. We use these ideas to interpret several observational properties of vortices on Jupiter and Saturn.
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Affiliation(s)
- Rakesh Kumar Yadav
- Department of Earth and Planetary Sciences, Harvard University, Cambridge, MA 02138, USA.
| | - Moritz Heimpel
- Department of Physics, University of Alberta, T6G 2J1 Edmonton, Canada
| | - Jeremy Bloxham
- Department of Earth and Planetary Sciences, Harvard University, Cambridge, MA 02138, USA
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7
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Ingersoll AP. Cassini Exploration of the Planet Saturn: A Comprehensive Review. SPACE SCIENCE REVIEWS 2020; 216:122. [PMID: 35027776 PMCID: PMC8753610 DOI: 10.1007/s11214-020-00751-1] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 10/10/2019] [Accepted: 10/10/2020] [Indexed: 06/14/2023]
Abstract
Before Cassini, scientists viewed Saturn's unique features only from Earth and from three spacecraft flying by. During more than a decade orbiting the gas giant, Cassini studied the planet from its interior to the top of the atmosphere. It observed the changing seasons, provided up-close observations of Saturn's exotic storms and jet streams, and heard Saturn's lightning, which cannot be detected from Earth. During the Grand Finale orbits, it dove through the gap between the planet and its rings and gathered valuable data on Saturn's interior structure and rotation. Key discoveries and events include: watching the eruption of a planet-encircling storm, which is a 20- or 30-year event, detection of gravity perturbations from winds 9000 km below the tops of the clouds, demonstration that eddies are supplying energy to the zonal jets, which are remarkably steady over the 25-year interval since the Voyager encounters, re-discovery of the north polar hexagon after 25 years, determination of elemental abundance ratios He/H, C/H, N/H, P/H, and As/H, which are clues to planet formation and evolution, characterization of the semiannual oscillation of the equatorial stratosphere, documentation of the mysteriously high temperatures of the thermosphere outside the auroral zone, and seeing the strange intermittency of lightning, which typically ceases to exist on the planet between outbursts every 1-2 years. These results and results from the Jupiter flyby are all discussed in this review.
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Affiliation(s)
- Andrew P Ingersoll
- Division of Geological and Planetary Sciences, California Institute of Technology, 1200 East California Blvd, Pasadena, CA 91125, USA
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8
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Vidal J, Cébron D. Acoustic and inertial modes in planetary-like rotating ellipsoids. Proc Math Phys Eng Sci 2020; 476:20200131. [PMID: 32831610 DOI: 10.1098/rspa.2020.0131] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/11/2020] [Accepted: 06/05/2020] [Indexed: 11/12/2022] Open
Abstract
The bounded oscillations of rotating fluid-filled ellipsoids can provide physical insight into the flow dynamics of deformed planetary interiors. The inertial modes, sustained by the Coriolis force, are ubiquitous in rapidly rotating fluids and Vantieghem (2014, Proc. R. Soc. A, 470, 20140093. doi:10.1098/rspa.2014.0093) pioneered a method to compute them in incompressible fluid ellipsoids. Yet, taking density (and pressure) variations into account is required for accurate planetary applications, which has hitherto been largely overlooked in ellipsoidal models. To go beyond the incompressible theory, we present a Galerkin method in rigid coreless ellipsoids, based on a global polynomial description. We apply the method to investigate the normal modes of fully compressible, rotating and diffusionless fluids. We consider an idealized model, which fairly reproduces the density variations in the Earth's liquid core and Jupiter-like gaseous planets. We successfully benchmark the results against standard finite-element computations. Notably, we find that the quasi-geostrophic inertial modes can be significantly modified by compressibility, even in moderately compressible interiors. Finally, we discuss the use of the normal modes to build reduced dynamical models of planetary flows.
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Affiliation(s)
- Jérémie Vidal
- Department of Applied Mathematics, University of Leeds, Leeds LS2 9JT, UK
| | - David Cébron
- Université Grenoble Alpes, CNRS, ISTerre, Grenoble, France
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9
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Dornheim T, Vorberger J, Bonitz M. Nonlinear Electronic Density Response in Warm Dense Matter. PHYSICAL REVIEW LETTERS 2020; 125:085001. [PMID: 32909774 DOI: 10.1103/physrevlett.125.085001] [Citation(s) in RCA: 14] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/09/2020] [Accepted: 07/20/2020] [Indexed: 06/11/2023]
Abstract
Warm dense matter (WDM)-an extreme state with high temperatures and densities that occurs, e.g., in astrophysical objects-constitutes one of the most active fields in plasma physics and materials science. These conditions can be realized in the lab by shock compression or laser excitation, and the most accurate experimental diagnostics is achieved with lasers and free electron lasers which is theoretically modeled using linear response theory. Here, we present first ab initio path integral Monte Carlo results for the nonlinear density response of correlated electrons in WDM and show that for many situations of experimental relevance nonlinear effects cannot be neglected.
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Affiliation(s)
- Tobias Dornheim
- Center for Advanced Systems Understanding (CASUS), D-028262 Görlitz, Germany
| | - Jan Vorberger
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstraße 400, D-01328 Dresden, Germany
| | - Michael Bonitz
- Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel, Leibnizstraße 15, D-24098 Kiel, Germany
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10
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Lemasquerier D, Facchini G, Favier B, Le Bars M. Remote determination of the shape of Jupiter's vortices from laboratory experiments. NATURE PHYSICS 2020; 16:695-700. [PMID: 32514283 PMCID: PMC7279954 DOI: 10.1038/s41567-020-0833-9] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 06/07/2019] [Accepted: 02/10/2020] [Indexed: 06/11/2023]
Abstract
Jupiter's dynamics shapes its cloud patterns but remains largely unknown below this natural observational barrier. Unraveling the underlying three-dimensional flows is thus a primary goal for NASA's ongoing Juno mission that was launched in 2011. Here, we address the dynamics of large Jovian vortices using laboratory experiments complemented by theoretical and numerical analyses. We determine the generic force balance responsible for their three-dimensional pancake-like shape. From this, we define scaling laws for their horizontal and vertical aspect ratios as a function of the ambient rotation, stratification and zonal wind velocity. For the Great Red Spot in particular, our predicted horizontal dimensions agree well with measurements at the cloud level since the Voyager mission in 1979. We additionally predict the Great Red Spot's thickness, inaccessible to direct observation: it has surprisingly remained constant despite the observed horizontal shrinking. Our results now await comparison with upcoming Juno observations.
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Affiliation(s)
- Daphné Lemasquerier
- Aix-Marseille Univ, CNRS, Centrale Marseille, Institut de Recherche
sur les Phénomènes Hors Équilibre, UMR 7342, 49 rue F. Joliot
Curie, 13013 Marseille, France
| | - Giulio Facchini
- Aix-Marseille Univ, CNRS, Centrale Marseille, Institut de Recherche
sur les Phénomènes Hors Équilibre, UMR 7342, 49 rue F. Joliot
Curie, 13013 Marseille, France
| | - Benjamin Favier
- Aix-Marseille Univ, CNRS, Centrale Marseille, Institut de Recherche
sur les Phénomènes Hors Équilibre, UMR 7342, 49 rue F. Joliot
Curie, 13013 Marseille, France
| | - Michael Le Bars
- Aix-Marseille Univ, CNRS, Centrale Marseille, Institut de Recherche
sur les Phénomènes Hors Équilibre, UMR 7342, 49 rue F. Joliot
Curie, 13013 Marseille, France
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11
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Frydrych S, Vorberger J, Hartley NJ, Schuster AK, Ramakrishna K, Saunders AM, van Driel T, Falcone RW, Fletcher LB, Galtier E, Gamboa EJ, Glenzer SH, Granados E, MacDonald MJ, MacKinnon AJ, McBride EE, Nam I, Neumayer P, Pak A, Voigt K, Roth M, Sun P, Gericke DO, Döppner T, Kraus D. Demonstration of X-ray Thomson scattering as diagnostics for miscibility in warm dense matter. Nat Commun 2020; 11:2620. [PMID: 32457297 PMCID: PMC7251136 DOI: 10.1038/s41467-020-16426-y] [Citation(s) in RCA: 10] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/22/2019] [Accepted: 04/29/2020] [Indexed: 11/12/2022] Open
Abstract
The gas and ice giants in our solar system can be seen as a natural laboratory for the physics of highly compressed matter at temperatures up to thousands of kelvins. In turn, our understanding of their structure and evolution depends critically on our ability to model such matter. One key aspect is the miscibility of the elements in their interiors. Here, we demonstrate the feasibility of X-ray Thomson scattering to quantify the degree of species separation in a 1:1 carbon-hydrogen mixture at a pressure of ~150 GPa and a temperature of ~5000 K. Our measurements provide absolute values of the structure factor that encodes the microscopic arrangement of the particles. From these data, we find a lower limit of [Formula: see text]% of the carbon atoms forming isolated carbon clusters. In principle, this procedure can be employed for investigating the miscibility behaviour of any binary mixture at the high-pressure environment of planetary interiors, in particular, for non-crystalline samples where it is difficult to obtain conclusive results from X-ray diffraction. Moreover, this method will enable unprecedented measurements of mixing/demixing kinetics in dense plasma environments, e.g., induced by chemistry or hydrodynamic instabilities.
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Affiliation(s)
- S Frydrych
- Lawrence Livermore National Laboratory, Livermore, CA, 94550, USA
- Institut für Kernphysik, Technische Universität Darmstadt, Schlossgartenstraße 9, Darmstadt, 64289, Germany
| | - J Vorberger
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstraße 400, Dresden, 01328, Germany
| | - N J Hartley
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstraße 400, Dresden, 01328, Germany
- SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA, 94025, USA
| | - A K Schuster
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstraße 400, Dresden, 01328, Germany
- Institute of Solid State and Materials Physics, Technische Universität Dresden, Dresden, 01069, Germany
| | - K Ramakrishna
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstraße 400, Dresden, 01328, Germany
- Institute of Solid State and Materials Physics, Technische Universität Dresden, Dresden, 01069, Germany
| | - A M Saunders
- Department of Physics, University of California, Berkeley, CA, 94720, USA
| | - T van Driel
- SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA, 94025, USA
| | - R W Falcone
- Department of Physics, University of California, Berkeley, CA, 94720, USA
- Lawrence Berkeley National Laboratory, Berkeley, CA, 94720, USA
| | - L B Fletcher
- SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA, 94025, USA
| | - E Galtier
- SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA, 94025, USA
| | - E J Gamboa
- SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA, 94025, USA
| | - S H Glenzer
- SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA, 94025, USA
| | - E Granados
- SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA, 94025, USA
| | - M J MacDonald
- SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA, 94025, USA
- University of Michigan, Ann Arbor, MI, 48109, USA
| | - A J MacKinnon
- Lawrence Livermore National Laboratory, Livermore, CA, 94550, USA
- SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA, 94025, USA
| | - E E McBride
- SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA, 94025, USA
- European XFEL GmbH, Holzkoppel 4, Schenefeld, 22869, Germany
| | - I Nam
- SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA, 94025, USA
| | - P Neumayer
- GSI Helmholtzzentrum für Schwerionenforschung, Planckstraße 1, Darmstadt, 64291, Germany
| | - A Pak
- Lawrence Livermore National Laboratory, Livermore, CA, 94550, USA
| | - K Voigt
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstraße 400, Dresden, 01328, Germany
- Institute of Solid State and Materials Physics, Technische Universität Dresden, Dresden, 01069, Germany
| | - M Roth
- Institut für Kernphysik, Technische Universität Darmstadt, Schlossgartenstraße 9, Darmstadt, 64289, Germany
| | - P Sun
- SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA, 94025, USA
| | - D O Gericke
- Centre for Fusion, Space and Astrophysics, Department of Physics, University of Warwick, Coventry, CV4 7AL, United Kingdom
| | - T Döppner
- Lawrence Livermore National Laboratory, Livermore, CA, 94550, USA
| | - D Kraus
- Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstraße 400, Dresden, 01328, Germany.
- Institute of Solid State and Materials Physics, Technische Universität Dresden, Dresden, 01069, Germany.
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12
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Allers KN, Vos JM, Biller BA, Williams PKG. A measurement of the wind speed on a brown dwarf. Science 2020; 368:169-172. [PMID: 32273464 DOI: 10.1126/science.aaz2856] [Citation(s) in RCA: 21] [Impact Index Per Article: 5.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/26/2019] [Accepted: 03/12/2020] [Indexed: 11/02/2022]
Abstract
Zonal (latitudinal) winds dominate the bulk flow of planetary atmospheres. For gas giant planets such as Jupiter, the motion of clouds can be compared with radio emissions from the magnetosphere, which is connected to the planet's interior, to determine the wind speed. In principle, this technique can be applied to brown dwarfs and/or directly imaged exoplanets if periods can be determined for both the infrared and radio emissions. We apply this method to measure the wind speeds on the brown dwarf 2MASS J10475385+2124234. The difference between the radio period of 1.751 to 1.765 hours and infrared period of 1.741 ± 0.007 hours implies a strong wind (+650 ± 310 meters per second) proceeding eastward. This could be due to atmospheric jet streams and/or low frictional drag at the bottom of the atmosphere.
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Affiliation(s)
- Katelyn N Allers
- Department of Physics and Astronomy, Bucknell University, Lewisburg, PA 17837-2029, USA.
| | - Johanna M Vos
- Department of Astrophysics, American Museum of Natural History, New York, NY 10024-5102, USA
| | - Beth A Biller
- Scottish Universities Physics Alliance, Institute for Astronomy, University of Edinburgh, Edinburgh EH9 3HJ, UK.,Centre for Exoplanet Science, University of Edinburgh, Edinburgh EH9 3FD, UK
| | - Peter K G Williams
- Center for Astrophysics, Harvard Smithsonian, Cambridge, MA 02138-1516, USA.,American Astronomical Society, Washington, DC 20006-1681, USA
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13
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Abstract
The Cassini-Huygens mission to Saturn provided a close-up study of the gas giant planet, as well as its rings, moons, and magnetosphere. The Cassini spacecraft arrived at Saturn in 2004, dropped the Huygens probe to study the atmosphere and surface of Saturn's planet-sized moon Titan, and orbited Saturn for the next 13 years. In 2017, when it was running low on fuel, Cassini was intentionally vaporized in Saturn's atmosphere to protect the ocean moons, Enceladus and Titan, where it had discovered habitats potentially suitable for life. Mission findings include Enceladus' south polar geysers, the source of Saturn's E ring; Titan's methane cycle, including rain that creates hydrocarbon lakes; dynamic rings containing ice, silicates, and organics; and Saturn's differential rotation. This Review discusses highlights of Cassini's investigations, including the mission's final year.
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Affiliation(s)
- Linda Spilker
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
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14
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Guillot T, Fletcher LN. Revealing giant planet interiors beneath the cloudy veil. Nat Commun 2020; 11:1555. [PMID: 32214104 PMCID: PMC7096516 DOI: 10.1038/s41467-020-15431-5] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/14/2020] [Accepted: 02/28/2020] [Indexed: 11/16/2022] Open
Abstract
Observations from the Juno and Cassini missions provide essential constraints on the internal structures and compositions of Jupiter and Saturn, resulting in profound revisions of our understanding of the interior and atmospheres of Gas Giant planets. The next step to understand planetary origins in our Solar System requires a mission to their Ice Giant siblings, Uranus and Neptune.
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Affiliation(s)
- Tristan Guillot
- Université Côte d'Azur, OCA, Lagrange CNRS, 06304, Nice, France.
| | - Leigh N Fletcher
- School of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH, UK
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15
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Fletcher LN, Kaspi Y, Guillot T, Showman AP. How Well Do We Understand the Belt/Zone Circulation of Giant Planet Atmospheres? SPACE SCIENCE REVIEWS 2020; 216:30. [PMID: 32214508 PMCID: PMC7067733 DOI: 10.1007/s11214-019-0631-9] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/08/2019] [Accepted: 12/24/2019] [Indexed: 05/20/2023]
Abstract
The atmospheres of the four giant planets of our Solar System share a common and well-observed characteristic: they each display patterns of planetary banding, with regions of different temperatures, composition, aerosol properties and dynamics separated by strong meridional and vertical gradients in the zonal (i.e., east-west) winds. Remote sensing observations, from both visiting spacecraft and Earth-based astronomical facilities, have revealed the significant variation in environmental conditions from one band to the next. On Jupiter, the reflective white bands of low temperatures, elevated aerosol opacities, and enhancements of quasi-conserved chemical tracers are referred to as 'zones.' Conversely, the darker bands of warmer temperatures, depleted aerosols, and reductions of chemical tracers are known as 'belts.' On Saturn, we define cyclonic belts and anticyclonic zones via their temperature and wind characteristics, although their relation to Saturn's albedo is not as clear as on Jupiter. On distant Uranus and Neptune, the exact relationships between the banded albedo contrasts and the environmental properties is a topic of active study. This review is an attempt to reconcile the observed properties of belts and zones with (i) the meridional overturning inferred from the convergence of eddy angular momentum into the eastward zonal jets at the cloud level on Jupiter and Saturn and the prevalence of moist convective activity in belts; and (ii) the opposing meridional motions inferred from the upper tropospheric temperature structure, which implies decay and dissipation of the zonal jets with altitude above the clouds. These two scenarios suggest meridional circulations in opposing directions, the former suggesting upwelling in belts, the latter suggesting upwelling in zones. Numerical simulations successfully reproduce the former, whereas there is a wealth of observational evidence in support of the latter. This presents an unresolved paradox for our current understanding of the banded structure of giant planet atmospheres, that could be addressed via a multi-tiered vertical structure of "stacked circulation cells," with a natural transition from zonal jet pumping to dissipation as we move from the convectively-unstable mid-troposphere into the stably-stratified upper troposphere.
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Affiliation(s)
- Leigh N. Fletcher
- School of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH UK
| | - Yohai Kaspi
- Department of Earth and Planetary Sciences, Weizmann Institute of Science, Rehovot, 76100 Israel
| | - Tristan Guillot
- Université Côte d’Azur, OCA, Lagrange CNRS, 06304 Nice, France
| | - Adam P. Showman
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721-0092 USA
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16
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Saturn’s Probable Interior: An Exploration of Saturn’s Potential Interior Density Structures. ACTA ACUST UNITED AC 2020. [DOI: 10.3847/1538-4357/ab71ff] [Citation(s) in RCA: 17] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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17
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18
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Iess L, Militzer B, Kaspi Y, Nicholson P, Durante D, Racioppa P, Anabtawi A, Galanti E, Hubbard W, Mariani MJ, Tortora P, Wahl S, Zannoni M. Measurement and implications of Saturn’s gravity field and ring mass. Science 2019; 364:science.aat2965. [DOI: 10.1126/science.aat2965] [Citation(s) in RCA: 104] [Impact Index Per Article: 20.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/12/2018] [Accepted: 12/19/2018] [Indexed: 11/03/2022]
Abstract
The interior structure of Saturn, the depth of its winds, and the mass and age of its rings constrain its formation and evolution. In the final phase of the Cassini mission, the spacecraft dived between the planet and its innermost ring, at altitudes of 2600 to 3900 kilometers above the cloud tops. During six of these crossings, a radio link with Earth was monitored to determine the gravitational field of the planet and the mass of its rings. We find that Saturn’s gravity deviates from theoretical expectations and requires differential rotation of the atmosphere extending to a depth of at least 9000 kilometers. The total mass of the rings is (1.54 ± 0.49) × 1019 kilograms (0.41 ± 0.13 times that of the moon Mimas), indicating that the rings may have formed 107 to 108 years ago.
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Affiliation(s)
- L. Iess
- Department of Mechanical and Aerospace Engineering, Sapienza Università di Roma, Rome 00184, Italy
| | - B. Militzer
- Department of Astronomy, University of California, Berkeley, Berkeley, CA 94720, USA
- Department of Earth and Planetary Science, University of California, Berkeley, Berkeley, CA 94720, USA
| | - Y. Kaspi
- Department of Earth and Planetary Sciences Weizmann Institute of Science, Rehovot 76100, Israel
| | - P. Nicholson
- Department of Astronomy, Cornell University, Ithaca, NY 14853, USA
| | - D. Durante
- Department of Mechanical and Aerospace Engineering, Sapienza Università di Roma, Rome 00184, Italy
| | - P. Racioppa
- Department of Mechanical and Aerospace Engineering, Sapienza Università di Roma, Rome 00184, Italy
| | - A. Anabtawi
- Jet Propulsion Laboratory–Caltech, Pasadena, CA 91109, USA
| | - E. Galanti
- Department of Earth and Planetary Sciences Weizmann Institute of Science, Rehovot 76100, Israel
| | - W. Hubbard
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - M. J. Mariani
- Department of Mechanical and Aerospace Engineering, Sapienza Università di Roma, Rome 00184, Italy
| | - P. Tortora
- Department of Industrial Engineering, Università di Bologna, Forlì 47100, Italy
| | - S. Wahl
- Department of Earth and Planetary Science, University of California, Berkeley, Berkeley, CA 94720, USA
| | - M. Zannoni
- Department of Industrial Engineering, Università di Bologna, Forlì 47100, Italy
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19
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Mitra SP, Sarkar H, Sen P, Bhattacharya AB. Implementation of the system II transit point data for investigating the reduction of the rotational speed of the planet Jupiter. SN APPLIED SCIENCES 2019. [DOI: 10.1007/s42452-018-0105-9] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/27/2022] Open
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20
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Kaspi Y, Galanti E, Hubbard WB, Stevenson DJ, Bolton SJ, Iess L, Guillot T, Bloxham J, Connerney JEP, Cao H, Durante D, Folkner WM, Helled R, Ingersoll AP, Levin SM, Lunine JI, Miguel Y, Militzer B, Parisi M, Wahl SM. Jupiter's atmospheric jet streams extend thousands of kilometres deep. Nature 2018. [PMID: 29516995 DOI: 10.1038/nature25793] [Citation(s) in RCA: 30] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Abstract
The depth to which Jupiter's observed east-west jet streams extend has been a long-standing question. Resolving this puzzle has been a primary goal for the Juno spacecraft, which has been in orbit around the gas giant since July 2016. Juno's gravitational measurements have revealed that Jupiter's gravitational field is north-south asymmetric, which is a signature of the planet's atmospheric and interior flows. Here we report that the measured odd gravitational harmonics J3, J5, J7 and J9 indicate that the observed jet streams, as they appear at the cloud level, extend down to depths of thousands of kilometres beneath the cloud level, probably to the region of magnetic dissipation at a depth of about 3,000 kilometres. By inverting the measured gravity values into a wind field, we calculate the most likely vertical profile of the deep atmospheric and interior flow, and the latitudinal dependence of its depth. Furthermore, the even gravity harmonics J8 and J10 resulting from this flow profile also match the measurements, when taking into account the contribution of the interior structure. These results indicate that the mass of the dynamical atmosphere is about one per cent of Jupiter's total mass.
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Affiliation(s)
- Y Kaspi
- Department of Earth and Planetary Sciences, Weizmann Institute of Science, Rehovot 76100, Israel
| | - E Galanti
- Department of Earth and Planetary Sciences, Weizmann Institute of Science, Rehovot 76100, Israel
| | - W B Hubbard
- Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona 85721, USA
| | - D J Stevenson
- Divison of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA
| | - S J Bolton
- Southwest Research Institute, San Antonio, Texas 78238, USA
| | - L Iess
- Department of Mechanical and Aerospace Engineering, Sapienza Universita di Roma, 00184 Rome, Italy
| | - T Guillot
- Université Côte d'Azur, OCA, Lagrange CNRS, 06304 Nice, France
| | - J Bloxham
- Department of Earth and Planetary Sciences, Harvard University, Cambridge, Massachusetts 02138, USA
| | - J E P Connerney
- Space Research Corporation, Annapolis, Maryland 21403, USA.,NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - H Cao
- Divison of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA.,Department of Earth and Planetary Sciences, Harvard University, Cambridge, Massachusetts 02138, USA
| | - D Durante
- Department of Mechanical and Aerospace Engineering, Sapienza Universita di Roma, 00184 Rome, Italy
| | - W M Folkner
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA
| | - R Helled
- Institute for Computational Science, Center for Theoretical Astrophysics and Cosmology, University of Zurich, 8057 Zurich, Switzerland
| | - A P Ingersoll
- Divison of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA
| | - S M Levin
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA
| | - J I Lunine
- Department of Astronomy, Cornell University, Ithaca, New York 14853, USA
| | - Y Miguel
- Université Côte d'Azur, OCA, Lagrange CNRS, 06304 Nice, France.,Leiden Observatory, University of Leiden, Leiden, The Netherlands
| | - B Militzer
- Department of Earth and Planetray Science, University of California, Berkeley, California 94720, USA
| | - M Parisi
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA
| | - S M Wahl
- Department of Earth and Planetray Science, University of California, Berkeley, California 94720, USA
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21
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Computer simulations of Jupiter's deep internal dynamics help interpret what Juno sees. Proc Natl Acad Sci U S A 2018; 115:6896-6904. [PMID: 29941563 PMCID: PMC6142197 DOI: 10.1073/pnas.1709125115] [Citation(s) in RCA: 10] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
We describe computer simulations of thermal convection and magnetic field generation in Jupiter's deep interior: that is, its convective dynamo. Results from three different simulations highlight the importance of including the dynamics in the very deep interior, although much of the convection and field generation seems to be confined to the upper part of the interior. A long-debated question is to what depth do Jupiter's zonal winds extend below its surface. Our simulations suggest that, if global latitudinally banded patterns in Jupiter's near-surface magnetic and gravity fields were detected by Juno, NASA's orbiting spacecraft at Jupiter [Bolton S, et al. (2017) Science 356:821-825], they would provide evidence for Jupiter's zonal winds extending deep below the surface. One of our simulations has also maintained, for a couple simulated years, a deep axisymmetric inertial wave, with properties at the surface that depend on the size of the model's small rocky core. If such a wave was detected on Jupiter's surface, its latitudes and oscillation frequency would provide evidence for the existence and size of Jupiter's rocky core.
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22
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23
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A deeper look at Jupiter. Nature 2018; 555:168-169. [DOI: 10.1038/d41586-018-02612-y] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
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