1
|
Roberts JH, McKinnon WB, Elder CM, Tobie G, Biersteker JB, Young D, Park RS, Steinbrügge G, Nimmo F, Howell SM, Castillo-Rogez JC, Cable ML, Abrahams JN, Bland MT, Chivers C, Cochrane CJ, Dombard AJ, Ernst C, Genova A, Gerekos C, Glein C, Harris CD, Hay HCFC, Hayne PO, Hedman M, Hussmann H, Jia X, Khurana K, Kiefer WS, Kirk R, Kivelson M, Lawrence J, Leonard EJ, Lunine JI, Mazarico E, McCord TB, McEwen A, Paty C, Quick LC, Raymond CA, Retherford KD, Roth L, Rymer A, Saur J, Scanlan K, Schroeder DM, Senske DA, Shao W, Soderlund K, Spiers E, Styczinski MJ, Tortora P, Vance SD, Villarreal MN, Weiss BP, Westlake JH, Withers P, Wolfenbarger N, Buratti B, Korth H, Pappalardo RT. Exploring the Interior of Europa with the Europa Clipper. SPACE SCIENCE REVIEWS 2023; 219:46. [PMID: 37636325 PMCID: PMC10457249 DOI: 10.1007/s11214-023-00990-y] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 12/24/2022] [Accepted: 07/20/2023] [Indexed: 08/29/2023]
Abstract
The Galileo mission to Jupiter revealed that Europa is an ocean world. The Galileo magnetometer experiment in particular provided strong evidence for a salty subsurface ocean beneath the ice shell, likely in contact with the rocky core. Within the ice shell and ocean, a number of tectonic and geodynamic processes may operate today or have operated at some point in the past, including solid ice convection, diapirism, subsumption, and interstitial lake formation. The science objectives of the Europa Clipper mission include the characterization of Europa's interior; confirmation of the presence of a subsurface ocean; identification of constraints on the depth to this ocean, and on its salinity and thickness; and determination of processes of material exchange between the surface, ice shell, and ocean. Three broad categories of investigation are planned to interrogate different aspects of the subsurface structure and properties of the ice shell and ocean: magnetic induction, subsurface radar sounding, and tidal deformation. These investigations are supplemented by several auxiliary measurements. Alone, each of these investigations will reveal unique information. Together, the synergy between these investigations will expose the secrets of the Europan interior in unprecedented detail, an essential step in evaluating the habitability of this ocean world.
Collapse
Affiliation(s)
| | | | - Catherine M Elder
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | | | | | | | - Ryan S Park
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Gregor Steinbrügge
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Francis Nimmo
- University of California, Santa Cruz, Santa Cruz, CA, USA
| | - Samuel M Howell
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | | | - Morgan L Cable
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | | | | | | | - Corey J Cochrane
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | | | - Carolyn Ernst
- Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA
| | | | | | | | | | - Hamish C F C Hay
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Paul O Hayne
- University of Colorado Boulder, Boulder, CO, USA
| | | | - Hauke Hussmann
- German Aerospace Center Institute of Planetary Research, Berlin, Germany
| | | | | | - Walter S Kiefer
- Lunar and Planetary Institute, University Space Research Association, Houston, TX, USA
| | | | | | | | - Erin J Leonard
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | | | | | | | | | | | | | - Carol A Raymond
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Kurt D Retherford
- Sapienza University of Rome, Rome, Italy
- University of Texas at San Antonio, San Antonio, TX, USA
| | - Lorenz Roth
- KTH Royal Institute of Technology, Stockholm, Sweden
| | - Abigail Rymer
- Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA
| | | | | | | | - David A Senske
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Wencheng Shao
- University of California, Santa Cruz, Santa Cruz, CA, USA
| | | | | | - Marshall J Styczinski
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
- University of Washington, Seattle, WA, USA
| | - Paolo Tortora
- Alma Mater Studiorum - Università di Bologna, Bologna, Italy
| | - Steven D Vance
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | | | | | | | | | | | - Bonnie Buratti
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Haje Korth
- Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA
| | - Robert T Pappalardo
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| |
Collapse
|
2
|
Kolmašová I, Santolík O, Imai M, Kurth WS, Hospodarsky GB, Connerney JEP, Bolton SJ, Lán R. Lightning at Jupiter pulsates with a similar rhythm as in-cloud lightning at Earth. Nat Commun 2023; 14:2707. [PMID: 37221170 DOI: 10.1038/s41467-023-38351-6] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/29/2022] [Accepted: 04/24/2023] [Indexed: 05/25/2023] Open
Abstract
Our knowledge about the fine structure of lightning processes at Jupiter was substantially limited by the time resolution of previous measurements. Recent observations of the Juno mission revealed electromagnetic signals of Jovian rapid whistlers at a cadence of a few lightning discharges per second, comparable to observations of return strokes at Earth. The duration of these discharges was below a few milliseconds and below one millisecond in the case of Jovian dispersed pulses, which were also discovered by Juno. However, it was still uncertain if Jovian lightning processes have the fine structure of steps corresponding to phenomena known from thunderstorms at Earth. Here we show results collected by the Juno Waves instrument during 5 years of measurements at 125-microsecond resolution. We identify radio pulses with typical time separations of one millisecond, which suggest step-like extensions of lightning channels and indicate that Jovian lightning initiation processes are similar to the initiation of intracloud lightning at Earth.
Collapse
Affiliation(s)
- Ivana Kolmašová
- 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.
| | - Ondřej Santolík
- 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
| | - Masafumi Imai
- Department of Electrical Engineering and Information Science, National Institute of Technology (KOSEN), Niihama College, Niihama, Ehime, Japan
| | - William S Kurth
- Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa, USA
| | | | | | - Scott J Bolton
- Space Science Department, Southwest Research Institute, San Antonio, Texas, USA
| | - Radek Lán
- Department of Space Physics, Institute of Atmospheric Physics of the Czech Academy of Sciences, Prague, Czechia
| |
Collapse
|
3
|
Civiš S, Pastorek A, Ferus M, Yurchenko SN, Boudjema NI. Infrared Spectra of Small Radicals for Exoplanetary Spectroscopy: OH, NH, CN and CH: The State of Current Knowledge. Molecules 2023; 28:molecules28083362. [PMID: 37110598 PMCID: PMC10143568 DOI: 10.3390/molecules28083362] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/09/2023] [Revised: 03/29/2023] [Accepted: 03/30/2023] [Indexed: 04/29/2023] Open
Abstract
In this study, we present a current state-of-the-art review of middle-to-near IR emission spectra of four simple astrophysically relevant molecular radicals-OH, NH, CN and CH. The spectra of these radicals were measured by means of time-resolved Fourier transform infrared spectroscopy in the 700-7500 cm-1 spectral range and with 0.07-0.02 cm-1 spectral resolution. The radicals were generated in a glow discharge of gaseous mixtures in a specially designed discharge cell. The spectra of short-lived radicals published here are of great importance, especially for the detailed knowledge and study of the composition of exoplanetary atmospheres in selected new planets. Today, with the help of the James Webb telescope and upcoming studies with the help of Plato and Ariel satellites, when the investigated spectral area is extended into the infrared spectral range, it means that detailed knowledge of the infrared spectra of not only stable molecules but also the spectra of short-lived radicals or ions, is indispensable. This paper follows a simple structure. Each radical is described in a separate chapter, starting with historical and actual theoretical background, continued by our experimental results and concluded by spectral line lists with assigned notation.
Collapse
Affiliation(s)
- Svatopluk Civiš
- J. Heyrovsky Institute of Physical Chemistry, Czech Academy of Sciences, Dolejškova 2155/3, 18200 Prague 8, Czech Republic
| | - Adam Pastorek
- Department of Chemistry and Biochemistry, Old Dominion University, Norfolk, VA 23529, USA
| | - Martin Ferus
- J. Heyrovsky Institute of Physical Chemistry, Czech Academy of Sciences, Dolejškova 2155/3, 18200 Prague 8, Czech Republic
| | - Sergei N Yurchenko
- Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK
| | - Noor-Ines Boudjema
- Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK
| |
Collapse
|
4
|
Giant Planet Atmospheres: Dynamics and Variability from UV to Near-IR Hubble and Adaptive Optics Imaging. REMOTE SENSING 2022. [DOI: 10.3390/rs14061518] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/10/2022]
Abstract
Each of the giant planets, Jupiter, Saturn, Uranus, and Neptune, has been observed by at least one robotic spacecraft mission. However, these missions are infrequent; Uranus and Neptune have only had a single flyby by Voyager 2. The Hubble Space Telescope, particularly the Wide Field Camera 3 (WFC3) and Advanced Camera for Surveys (ACS) instruments, and large ground-based telescopes with adaptive optics systems have enabled high-spatial-resolution imaging at a higher cadence, and over a longer time, than can be achieved with targeted missions to these worlds. These facilities offer a powerful combination of high spatial resolution, often <0.05”, and broad wavelength coverage, from the ultraviolet through the near infrared, resulting in compelling studies of the clouds, winds, and atmospheric vertical structure. This coverage allows comparisons of atmospheric properties between the planets, as well as in different regions across each planet. Temporal variations in winds, cloud structure, and color over timescales of days to years have been measured for all four planets. With several decades of data already obtained, we can now begin to investigate seasonal influences on dynamics and aerosol properties, despite orbital periods ranging from 12 to 165 years. Future facilities will enable even greater spatial resolution and, combined with our existing long record of data, will continue to advance our understanding of atmospheric evolution on the giant planets.
Collapse
|
5
|
Bland MT, Weller LA, Archinal BA, Smith E, Wheeler BH. Improving the Usability of Galileo and Voyager Images of Jupiter's Moon Europa. EARTH AND SPACE SCIENCE (HOBOKEN, N.J.) 2021; 8:e2021EA001935. [PMID: 35864914 PMCID: PMC9286035 DOI: 10.1029/2021ea001935] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 07/29/2021] [Revised: 09/29/2021] [Accepted: 10/14/2021] [Indexed: 06/15/2023]
Abstract
NASA's Voyager 1, Voyager 2, and Galileo spacecraft acquired hundreds of images of Jupiter's moon Europa. These images provide the only moderate- to high-resolution views of the moon's surface and are therefore a critical resource for scientific analysis and future mission planning. Unfortunately, uncertain knowledge of the spacecraft's position and pointing during image acquisition resulted in significant errors in the location of the images on the surface. The result is that adjacent images are poorly aligned, with some images displaced by more than 100 km from their correct location. These errors severely degrade the usability of the Voyager and Galileo imaging data sets. To improve the usability of these data sets, we used the U.S. Geological Survey Integrated Software for Imagers and Spectrometers to build a nearly global image tie-point network with more than 50,000 tie points and 135,000 image measurements on 481 Galileo and 221 Voyager images. A global least-squares bundle adjustment of our final Europa tie-point network calculated latitude, longitude, and radius values for each point by minimizing residuals globally, and resulted in root mean square (RMS) uncertainties of 246.6 m, 307.0 m, and 70.5 m in latitude, longitude, and radius, respectively. The total RMS uncertainty was 0.32 pixels. This work enables direct use of nearly the entire Galileo and Voyager image data sets for Europa. We are providing the community with updated NASA Navigation and Ancillary Information Facility Spacecraft, Planet, Instrument, C-matrix (pointing), and Events kernels, mosaics of Galileo images acquired during each observation sequence, and individual processed and projected level 2 images.
Collapse
Affiliation(s)
- Michael T. Bland
- Astrogeology Science CenterU. S. Geological SurveyFlagstaffAZUSA
| | - Lynn A. Weller
- Astrogeology Science CenterU. S. Geological SurveyFlagstaffAZUSA
| | | | - Ethan Smith
- Astrogeology Science CenterU. S. Geological SurveyFlagstaffAZUSA
| | | |
Collapse
|
6
|
Fletcher LN, Melin H, Adriani A, Simon AA, Sanchez-Lavega A, Donnelly PT, Antuñano A, Orton GS, Hueso R, Kraaikamp E, Wong MH, Barnett M, Moriconi ML, Altieri F, Sindoni G. Jupiter's Mesoscale Waves Observed at 5 μm by Ground-based Observations and Juno JIRAM. THE ASTRONOMICAL JOURNAL 2018; 156:67. [PMID: 30510303 PMCID: PMC6267995 DOI: 10.3847/1538-3881/aace02] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
We characterize the origin and evolution of a mesoscale wave pattern in Jupiter's North Equatorial Belt (NEB), detected for the first time at 5 μm using a 2016-17 campaign of "lucky imaging" from the VISIR instrument on the Very Large Telescope and the NIRI instrument on the Gemini observatory, coupled with M-band imaging from Juno's JIRAM instrument during the first seven Juno orbits. The wave is compact, with a 1°.1-1°.4 longitude wavelength (wavelength 1300-1600 km, wavenumber 260-330) that is stable over time, with wave crests aligned largely north-south between 14°N and 17°N (planetographic). The waves were initially identified in small (10° longitude) packets immediately west of cyclones in the NEB at 16°N but extended to span wider longitude ranges over time. The waves exhibit a 7-10 K brightness temperature amplitude on top of an ∼210 K background at 5 μm. The thermal structure of the NEB allows for both inertio-gravity waves and gravity waves. Despite detection at 5 μm, this does not necessarily imply a deep location for the waves, and an upper tropospheric aerosol layer near 400-800 mbar could feature a gravity wave pattern modulating the visible-light reflectivity and attenuating the 5-μm radiance originating from deeper levels. Strong rifting activity appears to obliterate the pattern, which can change on timescales of weeks. The NEB underwent a new expansion and contraction episode in 2016-17 with associated cyclone-anticyclone formation, which could explain why the mesoscale wave pattern was more vivid in 2017 than ever before.
Collapse
Affiliation(s)
- Leigh N Fletcher
- Department of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH, UK;
| | - H Melin
- Department of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH, UK;
| | - A Adriani
- INAF-Istituto di Astrofisica e Planetologia Spaziali, Roma, Italy
| | - A A Simon
- NASA Goddard Space Flight Center Solar System Exploration Division (690) Greenbelt, MD 20771, USA
| | - A Sanchez-Lavega
- Departamento de Física Aplicada I, Escuela de Ingeniera de Bilbao, UPV/EHU, Plaza Ingeniero Torres Quevedo, 1, E-48013 Bilbao, Spain
| | - P T Donnelly
- Department of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH, UK;
| | - A Antuñano
- Department of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH, UK;
| | - G S Orton
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - R Hueso
- Departamento de Física Aplicada I, Escuela de Ingeniera de Bilbao, UPV/EHU, Plaza Ingeniero Torres Quevedo, 1, E-48013 Bilbao, Spain
| | - E Kraaikamp
- Jourdanstraat 121/8, B-1060, Sint-Gillis, Belgium
| | - M H Wong
- University of California at Berkeley, Astronomy Department, Berkeley, CA 947200-3411, USA
| | - M Barnett
- University of California at Berkeley, Astronomy Department, Berkeley, CA 947200-3411, USA
| | - M L Moriconi
- CNR-Istituto di Scienze dell Atmosfera e del Clima, Bologna e Roma, Italy
| | - F Altieri
- INAF-Istituto di Astrofisica e Planetologia Spaziali, Roma, Italy
| | - G Sindoni
- INAF-Istituto di Astrofisica e Planetologia Spaziali, Roma, Italy
| |
Collapse
|
7
|
Suer TA, Padovan S, Whitten JL, Potter RW, Shkolyar S, Cable M, Walker C, Szalay J, Parker C, Cumbers J, Gentry D, Harrison T, Naidu S, Trammell HJ, Reimuller J, Budney CJ, Lowes LL. FIRE - Flyby of Io with Repeat Encounter: A conceptual design for a New Frontiers mission to Io. ADVANCES IN SPACE RESEARCH : THE OFFICIAL JOURNAL OF THE COMMITTEE ON SPACE RESEARCH (COSPAR) 2017; 60:1080-1100. [PMID: 33162637 PMCID: PMC7646308 DOI: 10.1016/j.asr.2017.05.019] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/11/2023]
Abstract
A conceptual design is presented for a low complexity, heritage-based flyby mission to Io, Jupiter's innermost Galilean satellite and the most volcanically active body in the Solar System. The design addresses the 2011 Decadal Surveys recommendation for a New Frontiers class mission to Io and is based upon the result of the June 2012 NASA-JPL Planetary Science Summer School. A science payload is proposed to investigate the link between the structure of Io's interior, it's volcanic activity, it's surface composition, and it's tectonics. A study of Io's atmospheric processes and Io's role in the Jovian magnetosphere is also planned. The instrument suite includes a visible/near IR imager, a magnetic field and plasma suite, a dust analyzer and a gimbaled high gain antenna to perform radio science investigations. Payload activity and spacecraft operations would be powered by three Advanced Stirling Radioisotope Generators (ASRG). The primary mission includes 10 flybys with close-encounter altitudes as low as 100 km. The mission risks are mitigated by ensuring that relevant components are radiation tolerant and by using redundancy and flight-proven parts in the design. The spacecraft would be launched on an Atlas V rocket with a delta-v of 1.3 km/s. Three gravity assists (Venus, Earth, Earth) would be used to reach the Jupiter system in a 6-year cruise. The resulting concept demonstrates the rich scientific return of a flyby mission to Io.
Collapse
Affiliation(s)
- Terry-Ann Suer
- Institut de Mineralogie, de Physique des Materiaux, et de Cosmochimie (IMPMC) Sorbonne Universites - UPMC, Univ Paris 06, France
| | - Sebastiano Padovan
- German Aerospace Center (DLR), Department of Planetary Physics, Rutherfordstraße 2, Berlin 12489, Germany
| | - Jennifer L. Whitten
- Center for Earth and Planetary Studies, Smithsonian Institution, MRC 315, PO Box 37012, Washington, DC 20013-7012, United States
| | - Ross W.K. Potter
- Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI 02912, United States
| | - Svetlana Shkolyar
- Geophysical Laboratory, Carnegie Institution for Science, Jocelyn St NW, Washington, DC 20015, USA
| | - Morgan Cable
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, United Statess
| | - Catherine Walker
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, United Statess
| | - Jamey Szalay
- Southwest Research Institute, San Antonio, TX, United States
| | - Charles Parker
- John Hopkins Applied Physics Lab, Laurel, MD 20723, United States
| | - John Cumbers
- SynBioBeta LLC, Mountain View, CA 94040, United States
| | | | - Tanya Harrison
- School of Earth and Space Exploration, Arizona State University, AR, United States
| | - Shantanu Naidu
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, United Statess
| | | | | | - Charles J. Budney
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, United Statess
| | - Leslie L. Lowes
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, United Statess
| |
Collapse
|
8
|
Trammell HJ, Li L, Jiang X, Pan Y, Smith MA, Bering EA, Hörst SM, Vasavada AR, Ingersoll AP, Janssen MA, West RA, Porco CC, Li C, Simon AA, Baines KH. Vortices in Saturn's Northern Hemisphere (2008-2015) Observed by Cassini ISS. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2016; 121:1814-1826. [PMID: 29629249 PMCID: PMC5886353 DOI: 10.1002/2016je005122] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/08/2023]
Abstract
We use observations from the Imaging Science Subsystem on Cassini to create maps of Saturn's Northern Hemisphere (NH) from 2008 to 2015, a time period including a seasonal transition (i.e., Spring Equinox in 2009) and the 2010 giant storm. The processed maps are used to investigate vortices in the NH during the period of 2008-2015. All recorded vortices have diameters (east-west) smaller than 6000 km except for the largest vortex that developed from the 2010 giant storm. The largest vortex decreased its diameter from ~11000 km in 2011 to ~5000 km in 2015, and its average diameter is ~6500 km during the period of 2011-2015. The largest vortex lasts at least 4 years, which is much longer than the lifetimes of most vortices (less than 1 year). The largest vortex drifts to north, which can be explained by the beta drift effect. The number of vortices displays varying behaviors in the meridional direction, in which the 2010 giant storm significantly affects the generation and development of vortices in the middle latitudes (25-45°N). In the higher latitudes (45-90°N), the number of vortices also displays strong temporal variations. The solar flux and the internal heat do not directly contribute to the vortex activities, leaving the temporal variations of vortices in the higher latitudes (45-90°N) unexplained.
Collapse
Affiliation(s)
- Harold Justin Trammell
- Department of Earth and Atmospheric Sciences, University of Houston, Houston, Texas, USA
| | - Liming Li
- Department of Physics, University of Houston, Houston, Texas, USA
| | - Xun Jiang
- Department of Earth and Atmospheric Sciences, University of Houston, Houston, Texas, USA
| | - Yefeng Pan
- Department of Physics, University of Houston, Houston, Texas, USA
| | - Mark A Smith
- Department of Chemistry, University of Houston, Houston, Texas, USA
| | - Edgar A Bering
- Department of Physics, University of Houston, Houston, Texas, USA
| | - Sarah M Hörst
- Department of Earth and Planetary Sciences, The Johns Hopkins University, Baltimore, Maryland, USA
| | - Ashwin R Vasavada
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - Andrew P Ingersoll
- Division of Geological and Planetary Sciences, Caltech, Pasadena, California, USA
| | - Michael A Janssen
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - Robert A West
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - Carolyn C Porco
- Space Science and Engineering Center, University of Wisconsin-Madison, Madison, Wisconsin, USA
| | - Cheng Li
- Division of Geological and Planetary Sciences, Caltech, Pasadena, California, USA
| | - Amy A Simon
- NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
| | - Kevin H Baines
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| |
Collapse
|
9
|
Head JW, Coffin MF. Large Igneous Provinces: A Planetary Perspective. ACTA ACUST UNITED AC 2013. [DOI: 10.1029/gm100p0411] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/17/2023]
|
10
|
Schenk PM. Central pit and dome craters: Exposing the interiors of Ganymede and Callisto. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/93je00176] [Citation(s) in RCA: 77] [Impact Index Per Article: 6.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
11
|
Schenk PM. Ganymede and Callisto: Complex crater formation and planetary crusts. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/91je00932] [Citation(s) in RCA: 62] [Impact Index Per Article: 5.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
12
|
|
13
|
|
14
|
Conrath BJ, Flasar FM, Pirraglia JA, Gierasch PJ, Hunt GE. Thermal structure and dynamics of the Jovian atmosphere 2. Visible cloud features. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/ja086ia10p08769] [Citation(s) in RCA: 63] [Impact Index Per Article: 5.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
15
|
|
16
|
|
17
|
|
18
|
|
19
|
Sinton WM. The thermal emission spectrum of Io and a determination of the heat flux from its hot spots. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/jb086ib04p03122] [Citation(s) in RCA: 40] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
20
|
|
21
|
Acuña MH, Neubauer FM, Ness NF. Standing Alfvén wave current system at Io: Voyager 1 observations. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/ja086ia10p08513] [Citation(s) in RCA: 138] [Impact Index Per Article: 11.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
22
|
Hunt GE, Conrath BJ, Pirraglia JA. Visible and infrared observations of Jovian plumes during the Voyager encounter. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/ja086ia10p08777] [Citation(s) in RCA: 27] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
23
|
Flasar FM, Conrath BJ, Pirraglia JA, Clark PC, French RG, Gierasch PJ. Thermal structure and dynamics of the Jovian atmosphere 1. The great red spot. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/ja086ia10p08759] [Citation(s) in RCA: 63] [Impact Index Per Article: 5.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
24
|
Kumar S. Photochemistry of SO2in the atmosphere of Io and implications on atmospheric escape. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/ja087ia03p01677] [Citation(s) in RCA: 43] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
25
|
|
26
|
|
27
|
Johnson TV, Soderblom LA, Mosher JA, Danielson GE, Cook AF, Kupferman P. Global multispectral mosaics of the icy Galilean satellites. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/jb088ib07p05789] [Citation(s) in RCA: 75] [Impact Index Per Article: 6.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
28
|
Mekler Y, Eviatar A. Time analysis of volcanic activity on Io by means of plasma observations. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/ja085ia03p01307] [Citation(s) in RCA: 22] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
29
|
|
30
|
|
31
|
Hall JL, Solomon SC, Head JW. Lunar floor-fractured craters: Evidence for viscous relaxation of crater topography. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/jb086ib10p09537] [Citation(s) in RCA: 47] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
32
|
Hatzes A, Wenkert DD, Ingersoll AP, Danielson GE. Oscillations and velocity structure of a long-lived cyclonic spot. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/ja086ia10p08745] [Citation(s) in RCA: 22] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
33
|
Hartmann WK. Planetary cratering 1. The question of multiple impactor populations: Lunar evidence. ACTA ACUST UNITED AC 2012. [DOI: 10.1111/j.1945-5100.1995.tb01152.x] [Citation(s) in RCA: 37] [Impact Index Per Article: 3.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/27/2022]
|
34
|
|
35
|
Broadfoot AL, Belton MJ, Takacs PZ, Sandel BR, Shemansky DE, Holberg JB, Ajello JM, Atreya SK, Donahue TM, Moos HW, Bertaux JL, Blamont JE, Strobel DF, McConnell JC, Dalgarno A, Goody R, McElroy MB. Extreme ultraviolet observations from voyager 1 encounter with jupiter. Science 2010; 204:979-82. [PMID: 17800434 DOI: 10.1126/science.204.4396.979] [Citation(s) in RCA: 430] [Impact Index Per Article: 30.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Observations of the optical extreme ultraviolet spectrum of the Jupiter planetary system during the Voyager 1 encounter have revealed previously undetected physical processes of significant proportions. Bright emission lines of S III, S IV, and O III indicating an electron temperature of 10(5) K have been identified in preliminary analyses of the Io plasma torus spectrum. Strong auroral atomic and molecular hydrogen emissions have been observed in the polar regions of Jupiter near magnetic field lines that map the torus into the atmosphere of Jupiter. The observed resonance scattering of solar hydrogen Lyman alpha by the atmosphere of Jupiter and the solar occultation experiment suggest a hot thermosphere (>/= 1000 K) wvith a large atomic hydrogen abundance. A stellar occultation by Ganymede indicates that its atmosphere is at most an exosphere.
Collapse
|
36
|
Abstract
An overview of the Voyager 2 encounter with Jupiter is presented, including a brief discussion of the trajectory, the major sequence modifications performed because of the Jupiter measurements obtained with Voyager 1, and high-lights of the results that are described in the subsequent reports.
Collapse
|
37
|
Abstract
Despite major differences in the solar and internal energy inputs, the atmospheres of the four Jovian planets all exhibit latitudinal banding and high-speed jet streams. Neptune and Saturn are the windiest planets, Jupiter is the most active, and Uranus is a tipped-over version of the others. Large oval storm systems exhibit complicated time-dependent behavior that can be simulated in numerical models and laboratory experiments. The largest storm system, the Great Red Spot of Jupiter, has survived for more than 300 years in a chaotic shear zone where smaller structures appear and dissipate every few days. Future space missions will add to our understanding of small-scale processes, chemical composition, and vertical structure. Theoretical hypotheses about the interiors provide input for fluid dynamical models that reproduce many observed features of the winds, temperatures, and cloud patterns. In one set of models the winds are confined to the thin layer where clouds form. In other models, the winds extend deep into the planetary fluid interiors. Hypotheses will be tested further as observations and theories become more exact and detailed comparisons are made.
Collapse
|
38
|
Baines KH, Simon-Miller AA, Orton GS, Weaver HA, Lunsford A, Momary TW, Spencer J, Cheng AF, Reuter DC, Jennings DE, Gladstone GR, Moore J, Stern SA, Young LA, Throop H, Yanamandra-Fisher P, Fisher BM, Hora J, Ressler ME. Polar Lightning and Decadal-Scale Cloud Variability on Jupiter. Science 2007; 318:226-9. [DOI: 10.1126/science.1147912] [Citation(s) in RCA: 48] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- Kevin H. Baines
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - Amy A. Simon-Miller
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - Glenn S. Orton
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - Harold A. Weaver
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - Allen Lunsford
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - Thomas W. Momary
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - John Spencer
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - Andrew F. Cheng
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - Dennis C. Reuter
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - Donald E. Jennings
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - G. R. Gladstone
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - Jeffrey Moore
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - S. Alan Stern
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - Leslie A. Young
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - Henry Throop
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - Padma Yanamandra-Fisher
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - Brendan M. Fisher
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - Joseph Hora
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| | - Michael E. Ressler
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
- NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA
- The Johns Hopkins University Applied Physics Laboratory, 1110 Johns Hopkins Road, Laurel, MD 20723, USA
- Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238. USA
| |
Collapse
|
39
|
|
40
|
Porco CC, West RA, McEwen A, Del Genio AD, Ingersoll AP, Thomas P, Squyres S, Dones L, Murray CD, Johnson TV, Burns JA, Brahic A, Neukum G, Veverka J, Barbara JM, Denk T, Evans M, Ferrier JJ, Geissler P, Helfenstein P, Roatsch T, Throop H, Tiscareno M, Vasavada AR. Cassini imaging of Jupiter's atmosphere, satellites, and rings. Science 2003; 299:1541-7. [PMID: 12624258 DOI: 10.1126/science.1079462] [Citation(s) in RCA: 338] [Impact Index Per Article: 16.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Cassini Imaging Science Subsystem acquired about 26,000 images of the Jupiter system as the spacecraft encountered the giant planet en route to Saturn. We report findings on Jupiter's zonal winds, convective storms, low-latitude upper troposphere, polar stratosphere, and northern aurora. We also describe previously unseen emissions arising from Io and Europa in eclipse, a giant volcanic plume over Io's north pole, disk-resolved images of the satellite Himalia, circumstantial evidence for a causal relation between the satellites Metis and Adrastea and the main jovian ring, and information on the nature of the ring particles.
Collapse
Affiliation(s)
- Carolyn C Porco
- Department of Space Sciences, Southwest Research Institute, 1050 Walnut Street, Suite 400, Boulder, CO 80302, USA.
| | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | |
Collapse
|
41
|
|
42
|
Affiliation(s)
- Alfred S McEwen
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA.
| |
Collapse
|
43
|
Abstract
Life as we know it on Earth depends on liquid water, a suite of 'biogenic' elements (most famously carbon) and a useful source of free energy. Here we review Europa's suitability for life from the perspective of these three requirements. It is likely, though not yet certain, that Europa harbors a subsurface ocean of liquid water whose volume is about twice that of Earth's oceans. Little is known about Europa's inventory of carbon, nitrogen, and other biogenic elements, but lower bounds on these can be placed by considering the role of commentary delivery over Europa's history. Sources of free energy are challenging for a world covered with an ice layer kilometers thick, but it is possible that hydrothermal activity and/or organics and oxidants provided by the action of radiation chemistry at Europa's surface and subsequent mixing into Europa's ocean could provide the electron donors and acceptors needed to power a Europan ecosystem. It is not premature to draw lessons from the search for life on Mars with the Viking spacecraft for planning exobiological missions to Europa.
Collapse
Affiliation(s)
- Christopher F Chyba
- Center for the Study of Life in the Universe, SETI Institute, Mountain View, CA, USA
| | | |
Collapse
|
44
|
|
45
|
Prockter LM. Morphology of Europan bands at high resolution: A mid-ocean ridge-type rift mechanism. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2000je001458] [Citation(s) in RCA: 83] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
|
46
|
Keszthelyi L, McEwen AS, Phillips CB, Milazzo M, Geissler P, Turtle EP, Radebaugh J, Williams DA, Simonelli DP, Breneman HH, Klaasen KP, Levanas G, Denk T. Imaging of volcanic activity on Jupiter's moon Io by Galileo during the Galileo Europa Mission and the Galileo Millennium Mission. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000je001383] [Citation(s) in RCA: 88] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
|
47
|
Marchis F, Prangé R, Fusco T. A survey of Io's volcanism by adaptive optics observations in the 3.8-μm thermal band (1996-1999). ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000je001376] [Citation(s) in RCA: 19] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
48
|
Burns JA, Hamilton DP, Showalter MR. Dusty Rings and Circumplanetary Dust: Observations and Simple Physics. ASTRONOMY AND ASTROPHYSICS LIBRARY 2001. [DOI: 10.1007/978-3-642-56428-4_13] [Citation(s) in RCA: 22] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/03/2022]
|
49
|
Phillips CB, McEwen AS, Hoppa GV, Fagents SA, Greeley R, Klemaszewski JE, Pappalardo RT, Klaasen KP, Breneman HH. The search for current geologic activity on Europa. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001139] [Citation(s) in RCA: 45] [Impact Index Per Article: 1.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
50
|
Greeley R, Figueredo PH, Williams DA, Chuang FC, Klemaszewski JE, Kadel SD, Prockter LM, Pappalardo RT, Head JW, Collins GC, Spaun NA, Sullivan RJ, Moore JM, Senske DA, Tufts BR, Johnson TV, Belton MJS, Tanaka KL. Geologic mapping of Europa. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001173] [Citation(s) in RCA: 100] [Impact Index Per Article: 4.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|