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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Tidal interactions in close star-planet or binary star systems may exciteinertial waves (their restoring force is the Coriolis force) in the convectiveregion of the stars. The dissipation of these waves plays a prominent role inthe long-term orbital and rotational evolution of the bodies involved. If theprimary star rotates as a solid body, inertial waves have a Doppler-shiftedfrequency restricted to the range $[-2\Omega, 2\Omega]$ ($\Omega$ being theangular velocity of the star), and they can propagate in the entire convectiveregion. However, turbulent convection can sustain differential rotation with anequatorial acceleration (as in the Sun) or deceleration that modifies thefrequency range and propagation domain of inertial waves and allows corotationresonances for non-axisymmetric oscillations. In this work, we performnumerical simulations of tidally excited inertial waves in a differentiallyrotating convective envelope with a conical (or latitudinal) rotation profile.The tidal forcing that we adopt contains spherical harmonics that correspond tothe case of a circular and coplanar orbit. We study the viscous dissipation ofthe waves as a function of tidal frequency for various stellar masses anddifferential rotation parameters, as well as its dependence on the turbulentviscosity coefficient. We compare our results with previous studies assumingsolid-body rotation and point out the potential key role of corotationresonances in the dynamical evolution of close-in star-planet or binarysystems.

Tidal dissipation by inertial waves in differentially rotating convective envelopes of low-mass stars