A rapidly time-varying equatorial jet in Jupiter’s deep interior

Jeremy Bloxham (), Hao Cao, David J. Stevenson, John E. P. Connerney and Scott J. Bolton
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Jeremy Bloxham: Harvard University
Hao Cao: Harvard University
David J. Stevenson: California Institute of Technology
John E. P. Connerney: Space Research Corporation
Scott J. Bolton: Southwest Research Institute

Nature, 2024, vol. 627, issue 8002, 64-66

Abstract: Abstract Planetary magnetic fields provide a window into the otherwise largely inaccessible dynamics of a planet’s deep interior. In particular, interaction between fluid flow in electrically conducting interior regions and the magnetic field there gives rise to observable secular variation (time dependency) of the externally observed magnetic field. Secular variation of Jupiter’s field has recently been revealed1–3 and been shown to arise, in part, from an axisymmetric, equatorial jet2. Whether this jet is time dependent has not previously been addressed, yet it is of critical importance for understanding the dynamics of the planet’s interior. If steady, it would probably be a manifestation of deep dynamo convective flow (and jets are anticipated as part of that flow4–9) but if time dependent on a timescale much shorter than the convective turnover timescale of several hundred years, it would probably have a different origin. Here we show that the jet has a wavelike fluctuation with a period of roughly 4 years, strongly suggestive of the presence of a torsional oscillation10 (a cylindrically symmetric oscillating flow about the rotation axis) or a localized Alfvén wave in Jupiter’s metallic hydrogen interior. This opens a pathway towards revealing otherwise hidden aspects of the magnetic field within the metallic hydrogen region and hence constraining the dynamo that generates Jupiter’s magnetic field.

Date: 2024
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DOI: 10.1038/s41586-024-07046-3

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