Enceladus geysers mask the length of Saturn’s day
Saturn's little moon Enceladus is 'weighing down' Saturn’s magnetic field so much that the field is rotating slower than the planet. This phenomenon makes it nearly impossible to measure the length of the Saturnian day with techniques used for the other giant planets.
"No one could have predicted that the little moon Enceladus would have such an influence on the radio technique that has been used for years to determine the length of the Saturn day," said Dr Don Gurnett of the University of Iowa, Iowa City, USA. Gurnett is the principal investigator on the Radio and Plasma Wave Science (RPWS) experiment on board NASA's Cassini spacecraft. The radio technique measures the rotation of the planet by taking its radio pulse rate - the rhythm of natural radio signals from the planet.
A new study of Cassini data, reported this week in the online version of the journal Science, determined that Saturn’s magnetic field lines - invisible lines originating from the interior of a magnetised planet - are being forced to slip relative to the rotation of the planet by the weight of electrically charged particles originating from geysers spewing water vapour and ice from Enceladus. These results are based on joint observations by two Cassini instruments - the RPWS and the magnetometer (MAG).
The neutral gas particles ejected from the geysers on Enceladus form a donut-like torus around Saturn. As these particles become electrically charged, they are captured by Saturn’s magnetic field, forming a disc of ionised gas, or plasma, which surrounds the planet near the equator.
The particles weigh down the magnetic field so much that the rate of rotation of the plasma disc slows down slightly. This slippage causes the radio period, controlled by the plasma disc rotation, to be longer than the planet's actual rotation period.
Scientists conclude the period Cassini has been measuring from radio emission is not the length of the Saturn day, but rather the rotation period of the plasma disc. At present, because of Saturn’s cloud motion, no technique is known that can accurately measure the planet's actual internal rotation.
Finding out the length of Saturn’s day has been a challenge because the gaseous planet has no surface or fixed point to clock its rotation rate. Initially, the approach was to use periodic regular radio signals, as has been done for Jupiter, Uranus and Neptune. However, Saturn’s radio period has turned out to be troubling in two ways.
It seems to be a pulsed signal rather than a rotating, lighthouse-like beam. Secondly, the period seems to be slowly changing over months to years. The day measured by Cassini is some six minutes longer than the day recorded by NASA’s Voyager spacecraft in the early 1980s, a change of nearly one percent.
"We have linked the pulsing radio signal to a rotating magnetic signal. Once each rotation of Saturn's magnetic field, an asymmetry in the field triggers a burst of radio waves," said Prof. David Southwood, co-author, Imperial College, University of London, and ESA's Director of Science. "We have then linked both signals to material that has come from Enceladus."
Based on the new observations, scientists now think there are two possible reasons for the change in radio period. The first theory is that the geysers on Enceladus could be more active now than in Voyagers’ time. The second is that there may be seasonal variations as Saturn orbits the sun once every 29 years.
"One would predict that when the geysers are very active, the particles load down the magnetic field and increase the slippage of the plasma disc, thereby increasing the radio emission period even more. If the geysers are less active, there would be less of a load on the magnetic field, and therefore less slippage of the plasma disc, and a shorter period,” said Gurnett.
"The direct link between radio, magnetic field and deep planetary rotation has been taken for granted up to now. Saturn is showing we need to think further," said Michele Dougherty, principal investigator on MAG, Imperial College London.
Note for editors
The Cassini-Huygens mission is a cooperative project of NASA, ESA and ASI, the Italian space agency. The Cassini orbiter was designed, developed and assembled at JPL. The magnetometer (MAG) team is based at Imperial College, University of London (UK). The Radio and Plasma Wave Science experiment (RPWS) team is based at the University of Iowa, Iowa City (US).
For more information
Prof. David Southwood, ESA Director of Science
Email: david.southwood @ esa.int
Jean-Pierre Lebreton,
ESA Huygens Project Scientist
Email : jean-pierre.lebreton @ esa.int
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