Unlike Earth, Saturn has no solid surface; it is a gaseous planet, consisting mostly of hydrogen and helium that move around fluidly.
Strong winds, known as jet streams, form the appearance of stripes on Saturn’s exterior – similar but less stark than those on Jupiter.
Study co-author, Dr Navid Constantinou from The Australian National University (ANU), said the recent space mission Cassini offered a glimpse of what goes on below Saturn’s cloud tops.
“At the end of its mission, Cassini dived into Saturn and made detailed measurements of Saturn’s gravitational field,” he said.
“The measurements revealed that these jet streams continue about 8,500 km inside Saturn, which is roughly 15 per cent of the distance towards the planet’s centre.”
Dr Constantinou said the study may help solve the mystery of why Saturn’s jet streams stop at a certain depth.
“Deep into Saturn, where the pressure is high, the gas becomes a liquid that conducts electricity and is more strongly influenced by the planet’s magnetic field,” he said.
“An electrically conducting, flowing liquid will bend or distort a magnetic field. We showed that the distortion of the magnetic field makes the fluid more viscous, like honey.”
The team’s theoretical model indicates this viscous effect from the magnetic field could be the reason why the jet streams terminate at depths beyond 8,500 km.
“The mysteries of what goes on inside Saturn and the other gas giants in our Solar System are now slowly starting to be unveiled,” Dr Constantinou said.
“Our findings provide a promising way for interpreting the data from planetary missions and offer a better understanding of the planets in our Solar System and beyond.”
Dr Constantinou from the ANU Research School of Earth Sciences and Dr Jeffrey Parker from Lawrence Livermore National Laboratory in the United States conducted the study.
The results are published in the Physical Review Fluids journal.
Citation information: Jeffrey B. Parker and Navid C. Constantinou, Magnetic eddy viscosity of mean shear flows in two-dimensional magnetohydrodynamics, Phys. Rev. Fluids, 4, 083701 (2019)
Dr Navid Constantinou
Research School of Earth Sciences
ANU College of Science
T: +61 2 6125 9123
For media assistance, contact Will Wright on +61 2 6100 3486, the ANU media hotline on +612 6125 7979 or at email@example.com