The above diagram illustrates the method used by the Cassini Radio and Plasma Wave Science (RPWS) instrument to study the rotation rate of Saturn. Since giant gas planets such as Saturn have no surface and are shrouded by clouds it is not possible to obtain an accurate rotation rate from visual observations. The rotation rate most commonly quoted is obtained by analyzing the periodic rotational modulation of radio emissions. These radio emissions are generated by charged particles whose motions are controlled by the planetary magnetic field. Since the magnetic field is linked to the deep interior of the planet this technique is believed to give the best indication of the average rotation rate of the planet. At Saturn the radio emission that is used to determine the radio rotation rate occurs in the frequency range from about 50 to 500 kHz and is called Saturn Kilometric Radiation (SKR). The color frequency-time spectrogram in the diagram shows the SKR intensity detected over a five day interval, from June 2 to June 7, 2004. The audio sounds of these radio emissions have been generated by shifting the radio frequency range from 100 to 300 kHz down to the frequency range from 0 to 3 kHz and speeding up the recording so that 1 second corresponds to one rotation. The average rotation period obtained over an approximate one year interval, from April 29, 2003, to June 10, 2004, during the Cassini approach to Saturn, is 10 hr 45 min 45 ± 36 sec. This period differs significantly from the rotation period obtained during the 1980-81 Voyager flybys of Saturn which was 10 hr 39 min 24 ± 7 sec [see Desch and Kaiser, Geophys. Res. Lett., 8, 253-256, 1981]. The Cassini observations confirm a result first reported by Lecacheux [Radio Emissions IV, ed. by H. O. Rucker, S. J. Bauer, and A. Lecacheux, Austrian Academy of Sciences Press, Vienna, pp. 313-325, 1977; also see Galopeau and Lecacheux, Geophys. Res. Lett., 105, 13,089-13,101, 2000] using the Ulysses spacecraft that Saturn's radio period often deviates substantially from the Voyager value. A comparison of the power spectrums for the Voyager and Cassini measurements is shown in the Figure below. The reason for the long term variations in Saturn's radio rotation period is poorly understood and will require further study.Don Gurnett
RPWS Principal Investigator
|Measured period of SKR radio signals by Voyagers 1 & 2 (23 years ago) and Cassini (today).|
|Another Java animation is available which shows a larger version of the RPWS spectrogram with a cursor synchronized with the audio.|
Scientists Find that Saturn's Rotation Period is a Puzzle - UIowa press release
Return to "Space Audio" page
© The University of Iowa
2004. All rights reserved.
Contact information. Send questions or comments to the site custodian.
The Radio and Plasma Wave Group, Department of Physics & Astronomy, College of Liberal Arts & Sciences.