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Cassini Plasma Spectrometer Investigation

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Abstract

The Cassini Plasma Spectrometer (CAPS) will make comprehensive three-dimensional mass-resolved measurements of the full variety of plasma phenomena found in Saturn’s magnetosphere. Our fundamental scientific goals are to understand the nature of saturnian plasmas primarily their sources of ionization, and the means by which they are accelerated, transported, and lost. In so doing the CAPS investigation will contribute to understanding Saturn’s magnetosphere and its complex interactions with Titan, the icy satellites and rings, Saturn’s ionosphere and aurora, and the solar wind. Our design approach meets these goals by emphasizing two complementary types of measurements: high-time resolution velocity distributions of electrons and all major ion species; and lower-time resolution, high-mass resolution spectra of all ion species. The CAPS instrument is made up of three sensors: the Electron Spectrometer (ELS), the Ion Beam Spectrometer (IBS), and the Ion Mass Spectrometer (IMS). The ELS measures the velocity distribution of electrons from 0.6 eV to 28,250 keV, a range that permits coverage of thermal electrons found at Titan and near the ring plane as well as more energetic trapped electrons and auroral particles. The IBS measures ion velocity distributions with very high angular and energy resolution from 1 eV to 49,800 keV. It is specially designed to measure sharply defined ion beams expected in the solar wind at 9.5 AU, highly directional rammed ion fluxes encountered in Titan’s ionosphere, and anticipated field-aligned auroral fluxes. The IMS is designed to measure the composition of hot, diffuse magnetospheric plasmas and low-concentration ion species 1 eV to 50,280 eV with an atomic resolution M/ΔM ∼70 and, for certain molecules, (such asN 2 + and CO+), effective resolution as high as ∼2500. The three sensors are mounted on a motor-driven actuator that rotates the entire instrument over approximately one-half of the sky every 3 min.

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Authors and Affiliations

  1. Southwest Research Institute, San Antonio, TX, U.S.A.

    D. T. Young, J. L. Burch, R. Goldstein, D. J. Mccomas, D. Anderson, R. K. Black, T. Booker, R. Bowman, P. Casey, F. J. Crary, G. Dirks, N. Eaker, J. D. Furman, P. Jensen, J. Rudzki, K. Smith, M. Wüest & C. Zinsmeyer

  2. Los Alamos National Laboratory, Los Alamos, NM, U.S.A.

    B. L. Barraclough, D. Delapp, H. Funsten, J. T. Gosling, K. P. Mccabe, J. E. Nordholt & M. F. Thomsen

  3. Centre d’étude des Environnements Terrestre et Planetaires, CNRS, St. Maur, France

    J. J. Berthelier & J. M. Illiano

  4. Observatoire Midi-Pyrenées, Toulouse, France

    M. Blanc & S. Maurice

  5. Mullard Space Science Laboratory, University College London, Surrey, England

    A. J. Coates & D. R. Linder

  6. Jet Propulsion Laboratory, Pasadena, CA, U.S.A.

    S. Bolton & T. E. Wahl

  7. Rutherford Appleton Laboratory, Oxfordshire, England

    M. Grande & A. Preece

  8. Rice University, Houston, TX, U.S.A.

    T. W. Hill

  9. Goddard Space Flight Center, Greenbelt, MD, U.S.A.

    E. C. Sittler, S. Bakshi, M. A. Johnson, A. Ruitberg & T. Vollmer

  10. University of Virginia, Charlottesville, VA, U.S.A.e

    R. E. Johnson & R. A. Baragiola

  11. VTT Information Technology, Espoo, Finland

    V. Kelha, H. Hannula, C. Holmlund, T. Luntama, K. Viherkanto & T. Ylikorpi

  12. Norwegian Defense Research Establishment, Kjeller, Norway

    K. R. Svenes & B. T. Narheim

  13. KFKI Research Institute for Particle and Nuclear Physics, Budapest, Hungary

    K. Szegö & S. Szalai

  14. University of Oulu, Oulu, Finland

    P. Tanskanen, K. Mursula & J. Vilppola

  15. Nokia Corporation, Helsinki, Finland

    H. Huomo

  16. TEKES Technology Development Centre, Helsinki, Finland

    K. Ahola

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Young, D.T., Berthelier, J.J., Blanc, M. et al. Cassini Plasma Spectrometer Investigation. Space Sci Rev 114, 1–112 (2004). https://doi.org/10.1007/s11214-004-1406-4

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