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

In close two-body astrophysical systems, such as binary stars or Hot Jupitersystems, tidal interactions often drive dynamical evolution on seculartimescales. Many host stars and presumably giant gaseous planets feature aconvective envelope. Tidal flows generated therein by the tidal potential ofthe companion can be dissipated through viscous friction, leading to theredistribution and exchange of angular momentum within the convective shell andwith the companion, respectively. In the tightest systems, nonlinear effectsare likely to have a significant impact on the tidal dissipation and triggerdifferential rotation in the form of zonal flows, as has been shown in previousstudies. In this context, we investigate how the addition of nonlinearitiesaffect the tidal flow properties, and energy and angular momentum balances,using 3D nonlinear simulations of an adiabatic and incompressible convectiveshell. In our study, we have chosen a body forcing where the equilibrium tide(the quasi-hydrostatic tidal flow component) acts via an effective forcing toexcite tidal inertial waves in a spherical shell. Within this set-up, we shownew results for the amplitude of the energy stored in zonal flows, angularmomentum evolution, and its consequences on tidal dissipation in the envelopesof low-mass stars and giant gaseous planets.

Nonlinear simulations of tides in the convective envelopes of low-mass stars and giant gaseous planets