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

Motivated by the recent discovery of subsurface oceans on planetary moons andthe interest they have generated, we explore convective flows in shallowspherical shells of dimensionless gap width $\varepsilon^2\ll 1$ in the rapidrotation limit $\mathrm{E}\ll1$, where $\mathrm{E}$ is the Ekman number. Weemploy direct numerical simulations (DNS) of the Boussinesq equations tocompute the local heat flux $\mathrm{Nu}(\lambda)$ as a function of thelatitude $\lambda$ and use the results to characterize the trapping ofconvection at low latitudes, around the equator. We show that these results arequantitatively reproduced by an asymptotically exact nonhydrostatic equatorial$\beta$-plane convection model at a much more modest computational cost thanDNS. We identify the trapping parameter $\beta=\varepsilon \mathrm{E}^{-1}$ asthe key parameter that controls the vigor and latitudinal extent of convectionfor moderate thermal forcing when $\mathrm{E}\sim\varepsilon$ and$\varepsilon\downarrow 0$. This model provides a new theoretical paradigm fornonlinear investigations.

Equatorially Trapped Convection in a Rapidly Rotating Shallow Shell