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Wong MH, Rowe-Gurney N, Markham S, Sayanagi KM. Multiple Probe Measurements at Uranus Motivated by Spatial Variability. SPACE SCIENCE REVIEWS 2024; 220:15. [PMID: 38343766 PMCID: PMC10858001 DOI: 10.1007/s11214-024-01050-9] [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: 09/26/2023] [Accepted: 01/18/2024] [Indexed: 02/22/2024]
Abstract
A major motivation for multiple atmospheric probe measurements at Uranus is the understanding of dynamic processes that create and maintain spatial variation in thermal structure, composition, and horizontal winds. But origin questions-regarding the planet's formation and evolution, and conditions in the protoplanetary disk-are also major science drivers for multiprobe exploration. Spatial variation in thermal structure reveals how the atmosphere transports heat from the interior, and measuring compositional variability in the atmosphere is key to ultimately gaining an understanding of the bulk abundances of several heavy elements. We review the current knowledge of spatial variability in Uranus' atmosphere, and we outline how multiple probe exploration would advance our understanding of this variability. The other giant planets are discussed, both to connect multiprobe exploration of those atmospheres to open questions at Uranus, and to demonstrate how multiprobe exploration of Uranus itself is motivated by lessons learned about the spatial variation at Jupiter, Saturn, and Neptune. We outline the measurements of highest value from miniature secondary probes (which would complement more detailed investigation by a larger flagship probe), and present the path toward overcoming current challenges and uncertainties in areas including mission design, cost, trajectory, instrument maturity, power, and timeline.
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Affiliation(s)
- Michael H. Wong
- Center for Integrative Planetary Science, University of California, Berkeley, CA 94720-3411 USA
- Carl Sagan Center for Science, SETI Institute, Mountain View, CA 94043-5232 USA
| | - Naomi Rowe-Gurney
- NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA
- University of Maryland, College Park, MD 20742 USA
- The Center for Research and Exploration in Space Science & Technology (CRESST II), Greenbelt, MD 20771 USA
- The Royal Astronomical Society, Piccadilly, London, W1J 0BD UK
| | - Stephen Markham
- Observatoire de la Côte d’Azur, 06300 Nice, France
- Department of Astronomy, New Mexico State University, Las Cruces, NM 88003 USA
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2
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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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3
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Tsai SM, Lee EKH, Powell D, Gao P, Zhang X, Moses J, Hébrard E, Venot O, Parmentier V, Jordan S, Hu R, Alam MK, Alderson L, Batalha NM, Bean JL, Benneke B, Bierson CJ, Brady RP, Carone L, Carter AL, Chubb KL, Inglis J, Leconte J, Line M, López-Morales M, Miguel Y, Molaverdikhani K, Rustamkulov Z, Sing DK, Stevenson KB, Wakeford HR, Yang J, Aggarwal K, Baeyens R, Barat S, de Val-Borro M, Daylan T, Fortney JJ, France K, Goyal JM, Grant D, Kirk J, Kreidberg L, Louca A, Moran SE, Mukherjee S, Nasedkin E, Ohno K, Rackham BV, Redfield S, Taylor J, Tremblin P, Visscher C, Wallack NL, Welbanks L, Youngblood A, Ahrer EM, Batalha NE, Behr P, Berta-Thompson ZK, Blecic J, Casewell SL, Crossfield IJM, Crouzet N, Cubillos PE, Decin L, Désert JM, Feinstein AD, Gibson NP, Harrington J, Heng K, Henning T, Kempton EMR, Krick J, Lagage PO, Lendl M, Lothringer JD, Mansfield M, Mayne NJ, Mikal-Evans T, Palle E, Schlawin E, Shorttle O, Wheatley PJ, Yurchenko SN. Photochemically produced SO 2 in the atmosphere of WASP-39b. Nature 2023; 617:483-487. [PMID: 37100917 PMCID: PMC10191860 DOI: 10.1038/s41586-023-05902-2] [Citation(s) in RCA: 12] [Impact Index Per Article: 12.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/11/2022] [Accepted: 02/28/2023] [Indexed: 04/28/2023]
Abstract
Photochemistry is a fundamental process of planetary atmospheres that regulates the atmospheric composition and stability1. However, no unambiguous photochemical products have been detected in exoplanet atmospheres so far. Recent observations from the JWST Transiting Exoplanet Community Early Release Science Program2,3 found a spectral absorption feature at 4.05 μm arising from sulfur dioxide (SO2) in the atmosphere of WASP-39b. WASP-39b is a 1.27-Jupiter-radii, Saturn-mass (0.28 MJ) gas giant exoplanet orbiting a Sun-like star with an equilibrium temperature of around 1,100 K (ref. 4). The most plausible way of generating SO2 in such an atmosphere is through photochemical processes5,6. Here we show that the SO2 distribution computed by a suite of photochemical models robustly explains the 4.05-μm spectral feature identified by JWST transmission observations7 with NIRSpec PRISM (2.7σ)8 and G395H (4.5σ)9. SO2 is produced by successive oxidation of sulfur radicals freed when hydrogen sulfide (H2S) is destroyed. The sensitivity of the SO2 feature to the enrichment of the atmosphere by heavy elements (metallicity) suggests that it can be used as a tracer of atmospheric properties, with WASP-39b exhibiting an inferred metallicity of about 10× solar. We further point out that SO2 also shows observable features at ultraviolet and thermal infrared wavelengths not available from the existing observations.
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Affiliation(s)
- Shang-Min Tsai
- Atmospheric, Oceanic and Planetary Physics, Department of Physics, University of Oxford, Oxford, UK.
- Department of Earth Sciences, University of California, Riverside, Riverside, CA, USA.
| | - Elspeth K H Lee
- Center for Space and Habitability, University of Bern, Bern, Switzerland
| | - Diana Powell
- Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA, USA
| | - Peter Gao
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA
| | - Xi Zhang
- Department of Earth and Planetary Sciences, University of California, Santa Cruz, Santa Cruz, CA, USA
| | | | | | - Olivia Venot
- Université de Paris Cité and Univ. Paris Est Creteil, CNRS, LISA, Paris, France
| | - Vivien Parmentier
- Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France
| | - Sean Jordan
- Institute of Astronomy, University of Cambridge, Cambridge, UK
| | - Renyu Hu
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - Munazza K Alam
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA
| | - Lili Alderson
- School of Physics, University of Bristol, Bristol, UK
| | - Natalie M Batalha
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | - Jacob L Bean
- Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA
| | - Björn Benneke
- Department of Physics and Institute for Research on Exoplanets, Université de Montréal, Montreal, Quebec, Canada
| | - Carver J Bierson
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | - Ryan P Brady
- Department of Physics and Astronomy, University College London, London, UK
| | - Ludmila Carone
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - Aarynn L Carter
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | - Katy L Chubb
- Centre for Exoplanet Science, University of St Andrews, St Andrews, UK
| | - Julie Inglis
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
- Department of Physics & Astronomy, Johns Hopkins University, Baltimore, MD, USA
| | - Jérémy Leconte
- Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, Pessac, France
| | - Michael Line
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | | | - Yamila Miguel
- Leiden Observatory, University of Leiden, Leiden, the Netherlands
- SRON Netherlands Institute for Space Research, Leiden, the Netherlands
| | - Karan Molaverdikhani
- Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Munich, Germany
- Exzellenzcluster Origins, Munich, Germany
| | - Zafar Rustamkulov
- Department of Earth & Planetary Sciences, Johns Hopkins University, Baltimore, MD, USA
| | - David K Sing
- Department of Physics & Astronomy, Johns Hopkins University, Baltimore, MD, USA
- Department of Earth & Planetary Sciences, Johns Hopkins University, Baltimore, MD, USA
| | | | | | - Jeehyun Yang
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | | | - Robin Baeyens
- Anton Pannekoek Institute for Astronomy, University of Amsterdam, Amsterdam, the Netherlands
| | - Saugata Barat
- Anton Pannekoek Institute for Astronomy, University of Amsterdam, Amsterdam, the Netherlands
| | | | - Tansu Daylan
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA
| | - Jonathan J Fortney
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | - Kevin France
- Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Boulder, CO, USA
| | - Jayesh M Goyal
- School of Earth and Planetary Sciences (SEPS), National Institute of Science Education and Research (NISER), Homi Bhabha National Institute (HBNI), Odisha, India
| | - David Grant
- School of Physics, University of Bristol, Bristol, UK
| | - James Kirk
- Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA, USA
- Department of Physics, Imperial College London, London, UK
| | | | - Amy Louca
- Leiden Observatory, University of Leiden, Leiden, the Netherlands
| | - Sarah E Moran
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - Sagnick Mukherjee
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | | | - Kazumasa Ohno
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | - Benjamin V Rackham
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
- Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Seth Redfield
- Astronomy Department and Van Vleck Observatory, Wesleyan University, Middletown, CT, USA
| | - Jake Taylor
- Atmospheric, Oceanic and Planetary Physics, Department of Physics, University of Oxford, Oxford, UK
- Department of Physics and Institute for Research on Exoplanets, Université de Montréal, Montreal, Quebec, Canada
| | - Pascal Tremblin
- Maison de la Simulation, CEA, CNRS, Univ. Paris-Sud, UVSQ, Université Paris-Saclay, Gif-sur-Yvette, France
| | - Channon Visscher
- Space Science Institute, Boulder, CO, USA
- Chemistry and Planetary Sciences, Dordt University, Sioux Center, IA, USA
| | - Nicole L Wallack
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - Luis Welbanks
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | | | - Eva-Maria Ahrer
- Centre for Exoplanets and Habitability, University of Warwick, Coventry, UK
- Department of Physics, University of Warwick, Coventry, UK
| | | | - Patrick Behr
- Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Boulder, CO, USA
| | - Zachory K Berta-Thompson
- Department of Astrophysical and Planetary Sciences, University of Colorado Boulder, Boulder, CO, USA
| | - Jasmina Blecic
- Department of Physics, New York University Abu Dhabi, Abu Dhabi, United Arab Emirates
- Center for Astro, Particle, and Planetary Physics (CAP3), New York University Abu Dhabi, Abu Dhabi, United Arab Emirates
| | - S L Casewell
- School of Physics and Astronomy, University of Leicester, Leicester, UK
| | - Ian J M Crossfield
- Department of Physics & Astronomy, University of Kansas, Lawrence, KS, USA
| | - Nicolas Crouzet
- Leiden Observatory, University of Leiden, Leiden, the Netherlands
| | - Patricio E Cubillos
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
- INAF - Turin Astrophysical Observatory, Pino Torinese, Italy
| | - Leen Decin
- Institute of Astronomy, Department of Physics and Astronomy, KU Leuven, Leuven, Belgium
| | - Jean-Michel Désert
- Anton Pannekoek Institute for Astronomy, University of Amsterdam, Amsterdam, the Netherlands
| | - Adina D Feinstein
- Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA
| | - Neale P Gibson
- School of Physics, Trinity College Dublin, Dublin, Ireland
| | - Joseph Harrington
- Planetary Sciences Group, Department of Physics and Florida Space Institute, University of Central Florida, Orlando, FL, USA
| | - Kevin Heng
- Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Munich, Germany
- Department of Physics, University of Warwick, Coventry, UK
| | | | - Eliza M-R Kempton
- Department of Astronomy, University of Maryland, College Park, MD, USA
| | - Jessica Krick
- Infrared Processing and Analysis Center (IPAC), California Institute of Technology, Pasadena, CA, USA
| | - Pierre-Olivier Lagage
- Maison de la Simulation, CEA, CNRS, Univ. Paris-Sud, UVSQ, Université Paris-Saclay, Gif-sur-Yvette, France
| | - Monika Lendl
- Département d'Astronomie, Université de Genève, Sauverny, Switzerland
| | | | | | - N J Mayne
- Department of Physics and Astronomy, Faculty of Environment, Science and Economy, University of Exeter, Exeter, UK
| | | | - Enric Palle
- Instituto de Astrofísica de Canarias (IAC), Tenerife, Spain
| | | | - Oliver Shorttle
- Institute of Astronomy, University of Cambridge, Cambridge, UK
| | - Peter J Wheatley
- Centre for Exoplanets and Habitability, University of Warwick, Coventry, UK
- Department of Physics, University of Warwick, Coventry, UK
| | - Sergei N Yurchenko
- Department of Physics and Astronomy, University College London, London, UK
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4
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Paul GC, Barman MC, Rahman H. An effective method in investigating structures of polytropic protoplanets formed via gravitational instability. Heliyon 2022; 8:e10394. [PMID: 36119897 PMCID: PMC9475278 DOI: 10.1016/j.heliyon.2022.e10394] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/09/2021] [Revised: 11/02/2021] [Accepted: 08/15/2022] [Indexed: 10/31/2022] Open
Abstract
In this article, we have reinvestigated the initial distribution of thermodynamic variables inside the protoplanets formed via gravitational instability having mass range 0.3 - 10 M J ( 1 M J = 1.8986 × 10 30 gm ) by an embedded RKACeM(4,4) method assuming that the polytropic gas law holds in the protoplanets. The findings attained by our numerical experiments are recognized to be consistent with the results acquired through other notable investigations in this regard. Furthermore, the model is easily computable. The used method is found to be efficient in investing the structures of polytropic protoplanets in their initial stages in terms of accuracy, stability, computational cost, and solving endpoint constraints.
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Affiliation(s)
- Gour Chandra Paul
- Department of Mathematics, University of Rajshahi, Rajshahi 6205, Bangladesh
| | - Mrinal Chandra Barman
- Department of Mathematics, University of Rajshahi, Rajshahi 6205, Bangladesh.,Department of Mathematics, Mawlana Bhashani Science and Technology University, Tangail 1902, Bangladesh
| | - Hafijur Rahman
- Department of Mathematics, University of Rajshahi, Rajshahi 6205, Bangladesh.,Department of Applied Mathematics, Gono University, Dhaka 1344, Bangladesh
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5
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Hellmann R, Harvey AH. First-Principles Diffusivity Ratios for Atmospheric Isotope Fractionation on Mars and Titan. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2021; 126:10.1029/2021je006857. [PMID: 34849323 PMCID: PMC8628554 DOI: 10.1029/2021je006857] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/09/2021] [Accepted: 03/25/2021] [Indexed: 06/13/2023]
Abstract
Recent work used the kinetic theory of molecular gases, along with state-of-the-art intermolecular potentials, to calculate from first principles the diffusivity ratios necessary for modeling kinetic fractionation of water isotopes in air. Here, we extend that work to the Martian atmosphere, employing potential-energy surfaces for the interaction of water with carbon dioxide and with nitrogen. We also derive diffusivity ratios for methane isotopes in the atmosphere of Titan by using a high-quality potential for the methane-nitrogen pair. The Mars calculations cover 100 K to 400 K, while the Titan calculations cover 50 K to 200 K. Surprisingly, the simple hard-sphere theory that is inaccurate for Earth's atmosphere is in good agreement with the rigorous results for the diffusion of water isotopes in the Martian atmosphere. A modest disagreement with the hard-sphere results is observed for the diffusivity ratio of CH3D in the atmosphere of Titan. We present temperature-dependent correlations, as well as estimates of uncertainty, for the diffusivity ratios involving HDO, H2 17O, and H2 18O in the Martian atmosphere, and for CH3D and 13CH4 in the atmosphere of Titan, providing for the first time the necessary data to be able to model kinetic isotope fractionation in these environments.
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Affiliation(s)
- Robert Hellmann
- Institut für Thermodynamik, Helmut-Schmidt-Universität / Universität der Bundeswehr Hamburg, Holstenhofweg 85, 22043 Hamburg, Germany
| | - Allan H. Harvey
- Applied Chemicals and Materials Division, National Institute of Standards and Technology, 325 Broadway, Boulder, Colorado 80305, U.S.A
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6
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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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Brown S, Janssen M, Adumitroaie V, Atreya S, Bolton S, Gulkis S, Ingersoll A, Levin S, Li C, Li L, Lunine J, Misra S, Orton G, Steffes P, Tabataba-Vakili F, Kolmašová I, Imai M, Santolík O, Kurth W, Hospodarsky G, Gurnett D, Connerney J. Prevalent lightning sferics at 600 megahertz near Jupiter's poles. Nature 2018; 558:87-90. [PMID: 29875484 DOI: 10.1038/s41586-018-0156-5] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/21/2017] [Accepted: 03/14/2018] [Indexed: 11/09/2022]
Abstract
Lightning has been detected on Jupiter by all visiting spacecraft through night-side optical imaging and whistler (lightning-generated radio waves) signatures1-6. Jovian lightning is thought to be generated in the mixed-phase (liquid-ice) region of convective water clouds through a charge-separation process between condensed liquid water and water-ice particles, similar to that of terrestrial (cloud-to-cloud) lightning7-9. Unlike terrestrial lightning, which emits broadly over the radio spectrum up to gigahertz frequencies10,11, lightning on Jupiter has been detected only at kilohertz frequencies, despite a search for signals in the megahertz range 12 . Strong ionospheric attenuation or a lightning discharge much slower than that on Earth have been suggested as possible explanations for this discrepancy13,14. Here we report observations of Jovian lightning sferics (broadband electromagnetic impulses) at 600 megahertz from the Microwave Radiometer 15 onboard the Juno spacecraft. These detections imply that Jovian lightning discharges are not distinct from terrestrial lightning, as previously thought. In the first eight orbits of Juno, we detected 377 lightning sferics from pole to pole. We found lightning to be prevalent in the polar regions, absent near the equator, and most frequent in the northern hemisphere, at latitudes higher than 40 degrees north. Because the distribution of lightning is a proxy for moist convective activity, which is thought to be an important source of outward energy transport from the interior of the planet16,17, increased convection towards the poles could indicate an outward internal heat flux that is preferentially weighted towards the poles9,16,18. The distribution of moist convection is important for understanding the composition, general circulation and energy transport on Jupiter.
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Affiliation(s)
- Shannon Brown
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA.
| | - Michael Janssen
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Virgil Adumitroaie
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Sushil Atreya
- Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI, USA
| | - Scott Bolton
- Southwest Research Institute, San Antonio, TX, USA
| | - Samuel Gulkis
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | | | - Steven Levin
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Cheng Li
- California Institute of Technology, Pasadena, CA, USA
| | - Liming Li
- Department of Physics, University of Houston, Houston, TX, USA
| | - Jonathan Lunine
- Department of Astronomy, Cornell University, Ithaca, NY, USA
| | - Sidharth Misra
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Glenn Orton
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Paul Steffes
- School of Electrical and Computer Engineering, Georgia Institute of Technology, Atlanta, GA, USA
| | | | - Ivana Kolmašová
- Department of Space Physics, Institute of Atmospheric Physics, The Czech Academy of Sciences, Prague, Czechia.,Faculty of Mathematics and Physics, Charles University, Prague, Czechia
| | - Masafumi Imai
- Department of Physics and Astronomy, University of Iowa, Iowa City, IA, USA
| | - Ondřej Santolík
- Department of Space Physics, Institute of Atmospheric Physics, The Czech Academy of Sciences, Prague, Czechia.,Faculty of Mathematics and Physics, Charles University, Prague, Czechia
| | - William Kurth
- Department of Physics and Astronomy, University of Iowa, Iowa City, IA, USA
| | - George Hospodarsky
- Department of Physics and Astronomy, University of Iowa, Iowa City, IA, USA
| | - Donald Gurnett
- Department of Physics and Astronomy, University of Iowa, Iowa City, IA, USA
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Kreidberg L, Line MR, Bean JL, Stevenson KB, Désert JM, Madhusudhan N, Fortney JJ, Barstow JK, Henry GW, Williamson MH, Showman AP. A DETECTION OF WATER IN THE TRANSMISSION SPECTRUM OF THE HOT JUPITER WASP-12b AND IMPLICATIONS FOR ITS ATMOSPHERIC COMPOSITION. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/814/1/66] [Citation(s) in RCA: 186] [Impact Index Per Article: 20.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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Young PA, Desch SJ, Anbar AD, Barnes R, Hinkel NR, Kopparapu R, Madhusudhan N, Monga N, Pagano MD, Riner MA, Scannapieco E, Shim SH, Truitt A. Astrobiological stoichiometry. ASTROBIOLOGY 2014; 14:603-626. [PMID: 25014611 DOI: 10.1089/ast.2014.1143] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/03/2023]
Abstract
Chemical composition affects virtually all aspects of astrobiology, from stellar astrophysics to molecular biology. We present a synopsis of the research results presented at the "Stellar Stoichiometry" Workshop Without Walls hosted at Arizona State University April 11-12, 2013, under the auspices of the NASA Astrobiology Institute. The results focus on the measurement of chemical abundances and the effects of composition on processes from stellar to planetary scales. Of particular interest were the scientific connections between processes in these normally disparate fields. Measuring the abundances of elements in stars and giant and terrestrial planets poses substantial difficulties in technique and interpretation. One of the motivations for this conference was the fact that determinations of the abundance of a given element in a single star by different groups can differ by more than their quoted errors. The problems affecting the reliability of abundance estimations and their inherent limitations are discussed. When these problems are taken into consideration, self-consistent surveys of stellar abundances show that there is still substantial variation (factors of ∼ 2) in the ratios of common elements (e.g., C, O, Na, Al, Mg, Si, Ca) important in rock-forming minerals, atmospheres, and biology. We consider how abundance variations arise through injection of supernova nucleosynthesis products into star-forming material and through photoevaporation of protoplanetary disks. The effects of composition on stellar evolution are substantial, and coupled with planetary atmosphere models can result in predicted habitable zone extents that vary by many tens of percent. Variations in the bulk composition of planets can affect rates of radiogenic heating and substantially change the mineralogy of planetary interiors, affecting properties such as convection and energy transport.
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Affiliation(s)
- Patrick A Young
- 1 School of Earth and Space Exploration, Arizona State University , Tempe, Arizona
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Moses JI, Madhusudhan N, Visscher C, Freedman RS. CHEMICAL CONSEQUENCES OF THE C/O RATIO ON HOT JUPITERS: EXAMPLES FROM WASP-12b, COROT-2b, XO-1b, AND HD 189733b. THE ASTROPHYSICAL JOURNAL 2012; 763:25. [PMID: 30842680 PMCID: PMC6398958 DOI: 10.1088/0004-637x/763/1/25] [Citation(s) in RCA: 26] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/15/2023]
Abstract
Motivated by recent spectroscopic evidence for carbon-rich atmospheres on some transiting exo-planets, we investigate the influence of the C/O ratio on the chemistry, composition, and spectra of extrasolar giant planets both from a thermochemical-equilibrium perspective and from consideration of disequilibrium processes like photochemistry and transport-induced quenching. We find that although CO is predicted to be a major atmospheric constituent on hot Jupiters for all C/O ratios, other oxygen-bearing molecules like H2O and CO2 are much more abundant when C/O < 1, whereas CH4, HCN, and C2H2 gain significantly in abundance when C/O > 1. Other notable species like N2 and NH3 that do not contain carbon or oxygen are relatively unaffected by the C/O ratio. Disequilibrium processes tend to enhance the abundance of CH4, NH3, HCN, and C2H2 over a wide range of C/O ratios. We compare the results of our models with secondary-eclipse photometric data from the Spitzer Space Telescope and conclude that (1) disequilibrium models with C/O ~ 1 are consistent with spectra of WASP-12b, XO-1b, and CoRoT-2b, confirming the possible carbon-rich nature of these planets, (2) spectra from HD 189733b are consistent with C/O ≲ 1, but as the assumed metallicity is increased above solar, the required C/O ratio must increase toward 1 to prevent too much H2O absorption, (3) species like HCN can have a significant influence on spectral behavior in the 3.6 and 8.0 μm Spitzer channels, potentially providing even more opacity than CH4 when C/O > 1, and (4) the very high CO2 abundance inferred for HD 189733b from near-infrared observations cannot be explained through equilibrium or disequilibrium chemistry in a hydrogen-dominated atmosphere. We discuss possible formation mechanisms for carbon-rich hot Jupiters, including scenarios in which the accretion of CO-rich, H2O-poor gas dominates the atmospheric envelope, and scenarios in which the planets accrete carbon-rich solids while migrating through disk regions inward of the snow line. The C/O ratio and bulk atmospheric metallicity provide important clues regarding the formation and evolution of the giant planets.
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Affiliation(s)
- J I Moses
- Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO, 80301, USA
| | - N Madhusudhan
- Department of Physics and Department of Astronomy, Yale University, New Haven, CT, 06520-8101, USA
| | - C Visscher
- Southwest Research Institute, Boulder, CO, 80302, USA
| | - R S Freedman
- SETI Institute, Mountain View, CA, 94043 and NASA Ames Research Center, Moffett Field, CA, 94035, USA
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11
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Petrova T, Solodov A, Solodov A. Line mixing in the water vapour transitions of the ν1 + ν2 + ν3band perturbed by helium pressure. Mol Phys 2012. [DOI: 10.1080/00268976.2012.701341] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/28/2022]
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12
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Petrova T, Solodov A, Starikov V, Solodov A. Measurements and calculations of He-broadening and -shifting parameters of the water vapor transitions of theν1 + ν2 + ν3band. Mol Phys 2012. [DOI: 10.1080/00268976.2012.663939] [Citation(s) in RCA: 15] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/28/2022]
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13
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Preston TC, Signorell R. The formation and stability of co-crystalline NH3 · C2H2 aerosol particles. Mol Phys 2012. [DOI: 10.1080/00268976.2012.701343] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/28/2022]
Affiliation(s)
- Thomas C. Preston
- a Department of Chemistry , University of British Columbia , 2036 Main Mall, Vancouver , BC, V6T 1Z1 , Canada
| | - Ruth Signorell
- a Department of Chemistry , University of British Columbia , 2036 Main Mall, Vancouver , BC, V6T 1Z1 , Canada
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14
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Sofiev M, Sofieva V, Elperin T, Kleeorin N, Rogachevskii I, Zilitinkevich SS. Turbulent diffusion and turbulent thermal diffusion of aerosols in stratified atmospheric flows. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009jd011765] [Citation(s) in RCA: 23] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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15
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Owen T, Niemann HB. The origin of Titan's atmosphere: some recent advances. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2009; 367:607-615. [PMID: 19019783 DOI: 10.1098/rsta.2008.0247] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/27/2023]
Abstract
It is possible to make a consistent story for the origin of Titan's atmosphere starting with the birth of Titan in the Saturn subnebula. If we use comet nuclei as a model, Titan's nitrogen and methane could have easily been delivered by the ice that makes up approximately 50 per cent of its mass. If Titan's atmospheric hydrogen is derived from that ice, it is possible that Titan and comet nuclei are in fact made of the same protosolar ice. The noble gas abundances are consistent with relative abundances found in the atmospheres of Mars and Earth, the Sun, and the meteorites.
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Affiliation(s)
- Tobias Owen
- Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA.
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16
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Adriani A, Coradini A, Filacchione G, Lunine JI, Bini A, Pasqui C, Calamai L, Colosimo F, Dinelli BM, Grassi D, Magni G, Moriconi ML, Orosei R. JIRAM, the image spectrometer in the near infrared on board the Juno mission to Jupiter. ASTROBIOLOGY 2008; 8:613-622. [PMID: 18680411 DOI: 10.1089/ast.2007.0167] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/26/2023]
Abstract
The Jovian InfraRed Auroral Mapper (JIRAM) has been accepted by NASA for inclusion in the New Frontiers mission "Juno," which will launch in August 2011. JIRAM will explore the dynamics and the chemistry of Jupiter's auroral regions by high-contrast imaging and spectroscopy. It will also analyze jovian hot spots to determine their vertical structure and infer possible mechanisms for their formation. JIRAM will sound the jovian meteorological layer to map moist convection and determine water abundance and other constituents at depths that correspond to several bars pressure. JIRAM is equipped with a single telescope that accommodates both an infrared camera and a spectrometer to facilitate a large observational flexibility in obtaining simultaneous images in the L and M bands with the spectral radiance over the central zone of the images. Moreover, JIRAM will be able to perform spectral imaging of the planet in the 2.0-5.0 microm interval of wavelengths with a spectral resolution better than 10 nm. Instrument design, modes, and observation strategy will be optimized for operations onboard a spinning satellite in polar orbit around Jupiter. The JIRAM heritage comes from Italian-made, visual-infrared imaging spectrometers dedicated to planetary exploration, such as VIMS-V on Cassini, VIRTIS on Rosetta and Venus Express, and VIR-MS on the Dawn mission.
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Affiliation(s)
- Alberto Adriani
- Istituto Nazionale di Astrofisica-Istituto di Fisica dello Spazio Interplanetario (INAF-IFSI), Rome, Italy.
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17
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18
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Temma T, Baines KH, Butler RAH, Brown LR, Sagui L, Kleiner I. Exponential sum absorption coefficients of phosphine from 2750 to 3550 cm−1for application to radiative transfer analyses on Jupiter and Saturn. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002720] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- T. Temma
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - K. H. Baines
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - R. A. H. Butler
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
- Pittsburg State University; Pittsburg Kansas USA
| | - L. R. Brown
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - L. Sagui
- Laboratoire Inter-Universitaire des Systèmes Atmosphériques, CNRS; Université Paris VII and Paris XII; Créteil France
| | - I. Kleiner
- Laboratoire Inter-Universitaire des Systèmes Atmosphériques, CNRS; Université Paris VII and Paris XII; Créteil France
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19
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Carrier W, Zheng W, Osamura Y, Kaiser RI. Infrared spectroscopic identification of digermene, Ge2H4(X1Ag), and of the digermenyl radical, Ge2H3(X2A″), together with their deuterated counterparts in low temperature germane matrices. Chem Phys 2006. [DOI: 10.1016/j.chemphys.2006.08.022] [Citation(s) in RCA: 19] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/30/2022]
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20
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First infrared spectroscopic characterization of digermyl (Ge2H5) and d5-digermyl (Ge2D5) radicals in low temperature germane matrices. Chem Phys 2006. [DOI: 10.1016/j.chemphys.2005.11.046] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/25/2022]
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21
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Owen T, Encrenaz T. Element Abundances and Isotope Ratios in the Giant Planets and Titan. SOLAR SYSTEM HISTORY FROM ISOTOPIC SIGNATURES OF VOLATILE ELEMENTS 2003. [DOI: 10.1007/978-94-010-0145-8_9] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 02/12/2023]
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22
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23
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Affiliation(s)
- Adam P. Showman
- National Research Council (NRC)/NASA Ames Research Center, Mail Stop 245-3, Moffett Field, CA 94035–1000, USA
| | - Timothy E. Dowling
- Comparative Planetology Laboratory, University of Louisville, 211 Sackett Hall, Louisville, KY 40292, USA
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24
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Wang JH, Liu K, Min Z, Su H, Bersohn R, Preses J, Larese JZ. Vacuum ultraviolet photochemistry of CH4 and isotopomers. II. Product channel fields and absorption spectra. J Chem Phys 2000. [DOI: 10.1063/1.1288145] [Citation(s) in RCA: 67] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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25
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Roos-Serote M, Vasavada AR, Kamp L, Drossart P, Irwin P, Nixon C, Carlson RW. Proximate humid and dry regions in Jupiter's atmosphere indicate complex local meteorology. Nature 2000; 405:158-60. [PMID: 10821265 DOI: 10.1038/35012023] [Citation(s) in RCA: 25] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
Abstract
Models of Jupiter's formation and structure predict that its atmosphere is enriched in oxygen, relative to the Sun, and that consequently water clouds should be present globally near the 5-bar pressure level. Past attempts to confirm these predictions have led to contradictory results; in particular, the Galileo probe revealed a very dry atmosphere at the entry site, with no significant clouds at depths exceeding the 2-bar level. Although the entry site was known to be relatively cloud-free, the contrast between the observed local dryness and the expected global wetness was surprising. Here we analyse near-infrared (around 5 microm) observations of Jupiter, a spectral region that can reveal the water vapour abundance and vertical cloud structure in the troposphere. We find that humid and extremely dry regions exist in close proximity, and that some humid regions are spatially correlated with bright convective clouds extending from the deep water clouds to the visible atmosphere.
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Affiliation(s)
- M Roos-Serote
- Observatório Astronómico de Lisboa, Tapada da Ajuda, Lisbon, Portugal.
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26
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Owen T, Mahaffy P, Niemann HB, Atreya S, Donahue T, Bar-Nun A, de Pater I. A low-temperature origin for the planetesimals that formed Jupiter. Nature 1999; 402:269-70. [PMID: 10580497 DOI: 10.1038/46232] [Citation(s) in RCA: 248] [Impact Index Per Article: 9.9] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
Abstract
The four giant planets in the Solar System have abundances of 'metals' (elements heavier than helium), relative to hydrogen, that are much higher than observed in the Sun. In order to explain this, all models for the formation of these planets rely on an influx of solid planetesimals. It is generally assumed that these planetesimals were similar, if not identical, to the comets from the Oort cloud that we see today. Comets that formed in the region of the giant planets should not have contained much neon, argon and nitrogen, because the temperatures were too high for these volatile gases to be trapped effectively in ice. This means that the abundances of those elements on the giant planets should be approximately solar. Here we show that argon, krypton and xenon in Jupiter's atmosphere are enriched to the same extent as the other heavy elements, which suggests that the planetesimals carrying these elements must have formed at temperatures lower than predicted by present models of giant-planet formation.
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Affiliation(s)
- T Owen
- University of Hawaii, Institute for Astronomy, Honolulu 96822, USA.
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