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The Cassini Radio and Plasma Wave Investigation

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Abstract

The Cassini radio and plasma wave investigation is designed to study radio emissions, plasma waves, thermal plasma, and dust in the vicinity of Saturn. Three nearly orthogonal electric field antennas are used to detect electric fields over a frequency range from 1 Hz to 16 MHz, and three orthogonal search coil magnetic antennas are used to detect magnetic fields over a frequency range from 1 Hz to 12 kHz. A Langmuir probe is used to measure the electron density and temperature. Signals from the electric and magnetic antennas are processed by five receiver systems: a high frequency receiver that covers the frequency range from 3.5 kHz to 16 MHz, a medium frequency receiver that covers the frequency range from 24 Hz to 12 kHz, a low frequency receiver that covers the frequency range from 1 Hz to 26 Hz, a five-channel waveform receiver that covers the frequency range from 1 Hz to 2.5 kHz in two bands, 1 Hz to 26 Hz and 3 Hz to 2.5 kHz, and a wideband receiver that has two frequency bands, 60 Hz to 10.5 kHz and 800 Hz to 75 kHz. In addition, a sounder transmitter can be used to stimulate plasma resonances over a frequency range from 3.6 kHz to 115.2 kHz. Fluxes of micron-sized dust particles can be counted and approximate masses of the dust particles can be determined using the same techniques as Voyager. Compared to Voyagers 1 and 2, which are the only spacecraft that have made radio and plasma wave measurements in the vicinity of Saturn, the Cassini radio and plasma wave instrument has several new capabilities. These include (1) greatly improved sensitivity and dynamic range, (2) the ability to perform direction-finding measurements of remotely generated radio emissions and wave normal measurements of plasma waves, (3) both active and passive measurements of plasma resonances in order to give precise measurements of the local electron density, and (4) Langmuir probe measurements of the local electron density and temperature. With these new capabilities, it will be possible to perform a broad range of studies of radio emissions, wave-particle interactions, thermal plasmas and dust in the vicinity of Saturn.

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Authors and Affiliations

  1. Department of Physics and Astronomy, University of Iowa, Iowa City, IA, 52242, U.S.A.

    D. A. Gurnett, W. S. Kurth, D. L. Kirchner, G. B. Hospodarsky & T. F. Averkamp

  2. Observatoire de Paris, Meudon, France

    P. Zarka, A. Lecacheux & R. Manning

  3. CETP/UVSQ, Velizy, France

    A. Roux, P. Canu, N. Cornilleau-Wehrlin, P. Galopeau & A. Meyer

  4. Swedish Institute of Space Physics, Uppsala, Sweden

    R. Boström, G. Gustafsson, J.-E. Wahlund & L. Åhlen

  5. Austrian Academy of Sciences, Space Research Institute, Graz, Austria

    H. O. Rucker, H. P. Ladreiter & W. Macher

  6. Department of Automatic Control and Systems Engineering, University of Sheffield, Sheffield, U.K.

    L. J. C. Woolliscroft & H. Alleyne

  7. NASA/Goddard Space Flight Center, Greenbelt, MD, 20771, U.S.A.

    M. L. Kaiser, M. D. Desch & W. M. Farrell

  8. CESR/CNRS, Toulouse, France

    C. C. Harvey & P. Louarn

  9. Department of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, U.S.A.

    P. J. Kellogg & K. Goetz

  10. Department of Physics, University of Oslo, Blindern, Oslo, Norway

    A. Pedersen

Authors
  1. D. A. Gurnett
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  2. W. S. Kurth
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  3. D. L. Kirchner
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  13. A. Meyer
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  14. R. Boström
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  15. G. Gustafsson
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  16. J.-E. Wahlund
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  17. L. Åhlen
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  18. H. O. Rucker
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  19. H. P. Ladreiter
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  20. W. Macher
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  21. L. J. C. Woolliscroft
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  22. H. Alleyne
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  23. M. L. Kaiser
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  24. M. D. Desch
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  25. W. M. Farrell
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  26. C. C. Harvey
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  27. P. Louarn
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  28. P. J. Kellogg
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  29. K. Goetz
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  30. A. Pedersen
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Corresponding author

Correspondence to D. A. Gurnett.

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Gurnett, D.A., Kurth, W.S., Kirchner, D.L. et al. The Cassini Radio and Plasma Wave Investigation. Space Sci Rev 114, 395–463 (2004). https://doi.org/10.1007/s11214-004-1434-0

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  • DOI: https://doi.org/10.1007/s11214-004-1434-0

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