English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Tidally distorted rotating stars and gaseous planets are subject to awell-known linear fluid instability -- the elliptical instability. It has beenproposed that this instability might drive enough energy dissipation to solvethe long-standing problem of the origin of tidal dissipation in stars andplanets. But the nonlinear outcome of the elliptical instability has yet to beinvestigated in the parameter regime of interest, and the resulting turbulentenergy dissipation has not yet been quantified. We do so by performing threedimensional hydrodynamical simulations of a small patch of a tidally deformedfluid planet or star subject to the elliptical instability. We show that whenthe tidal deformation is weak, the nonlinear outcome of the instability leadsto the formation of long-lived columnar vortices aligned with the axis ofrotation. These vortices shut off the elliptical instability, and the netresult is insufficient energy dissipation to account for tidal dissipation.However, further work is required to account for effects neglected here,including magnetic fields, turbulent convection, and realistic boundaryconditions.

Nonlinear evolution of the tidal elliptical instability in gaseous planets and stars