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Review of Knowledge Prior to the Cassini-Huygens Mission and Concurrent Research

  • Chapter
Saturn from Cassini-Huygens

Abstract

The scientific achievements of the Cassini-Huygens mission have been based on previous decades of investigations from ground-based observations, an intensive 2-year time span of exploration by three spacecraft (Pioneer Saturn, Voyagers 1 and 2) in 1979–1981, and observations by the Infrared Space Observatory, the International Ultraviolet Explorer, and Hubble Space Telescope. We review both these and research concurrent with the nominal mission which often provided directly supporting results. Saturn's “bulk” composition remains uncertain. Its few discrete cloud features include a hexagon near the sorth pole, and a major episodic storm at the equator. A heterogeneous cloud field at depth was uncovered at 5 μm. Temperatures are enhanced at Saturn's south pole both from seasonal variations of sunlight and from dynamical forcing. Zonal winds peak near Saturn's equator. Saturn possesses a well-defined ionosphere, but with significant structure and variability. The magnetic field is aligned to within a degree of Saturn's rotation axis. An equatorial ring current of ~107 A has been inferred, with inner and outer radii of ~8 and ~16RS. Radiation belts at Saturn are well-established up to the edge of the outer rings, and the higherenergy (>1 meV) proton component is readily absorbed by the inner satellites. The magnetosphere includes both a well-developed plasma sheet and a magneto-tail. Radio emissions and plasma waves exist throughout, and the auroral kilometric radiation (SKR), modulated at 10 h 39.4 min, has been widely adopted as a measure of the internal rotation. The plasma population consists principally of protons, but with a heavier component close to the equatorial plane widely assumed to be nitrogen or oxygen. Saturn's ring system is the most accessible in the solar system and consists of three primary components, the A, B and C rings. The A ring contains a large number of spiral density wages generated by gravitational interactions with Saturn's satellites. Other rings include the tenuous D, E, and G rings, and the narrow F ring. Voyager imaging detected “spokes” in the rings and, through occultation studies, an intricate detailed radial structure. Spectroscopic information on the icy satellites reveals the presence of crystalline water ice, mixed with a non-ice surface component with strong UV absorption. Detailed information on the geology of Saturn's eight largest icy satellites before the Cassini arrival was based entirely on Voyager observations. They were found to be surprisingly heterogeneous, with implied internal activity in Ence-ladus and the dichotomous albedo of Iapetus being two of the biggest mysteries. Among the smaller satellites are those embedded in Saturn's rings and irregular captured satellites outside the orbits of the co-planar satellites.

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Notes

  1. 1.

    We use hereafter this modern reference for all the solar abundances.

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Acknowledgments

The authors would like to thank Aharon Eviatar, John Clarke, Leigh Fletcher, John Spencer, Linda Spilker, and Thomas Stallard for insights and comments on this chapter during its preparation. Portions of the work of this review were carried out at the Jet Propulsion Laboratory, California Institute of Technology, and the Applied Physics Laboratory, Johns Hopkins University, under contract to the National Aeronautics and Space Administration, as well as NASA's Ames Research Center. Funding was also provided by the UK Science and Technology Facilities Council, and the European Commission Framework 6 EuroPlaNet project.

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Authors and Affiliations

  1. MS 169-237, Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, 91109, USA

    Glenn S. Orton & Kevin H. Baines

  2. 245-6, NASA Ames Research Center, Moffet Field, California, 94035, USA

    Dale Cruikshank & Jeffrey N. Cuzzi

  3. Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, Maryland, 20723, USA

    Stamatios M. Krimigis

  4. Academy of Athens, Athens, 28 Panepistimiou Avenue 106 79, Athens, Greece

    Stamatios M. Krimigis

  5. Imperial College London, Gower Street, London, WCIE 6BT, UK

    Steve Miller

  6. Observatoire de Paris, Place Jules Jansen, 92195 Meudon-Cedex, France

    Emmanuel Lellouch

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  1. Glenn S. Orton
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Editors and Affiliations

  1. Imperial College, The Blackett Laboratory, Prince Consort Road, London, SW7 2AZ, United Kingdom

    Michele K. Dougherty

  2. University of Colorado, Boulder, Boulder CO, 80309-0449, USA

    Larry W. Esposito

  3. Applied Physics Lab, Johns Hopkins University, 11100 John Hopkins Rd, Laurel, MD, 20723, USA

    Stamatios M. Krimigis

  4. Center for Space Research and Technology, Academy of Athens, Soranou Efesiou 4, Athens, 11527, Greece

    Stamatios M. Krimigis

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© 2009 Springer Science+Business Media B.V.

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Orton, G.S. et al. (2009). Review of Knowledge Prior to the Cassini-Huygens Mission and Concurrent Research. In: Dougherty, M.K., Esposito, L.W., Krimigis, S.M. (eds) Saturn from Cassini-Huygens. Springer, Dordrecht. https://doi.org/10.1007/978-1-4020-9217-6_2

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