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

A monomodal model for stellar and planetary convection is derived for themagnitude of the rms velocity, degree of superadiabaticity, and characteristiclength scale as a function of rotation rate as well as with thermal and viscousdiffusivities. The convection model is used as a boundary condition for alinearization of the equations of motion in the transition region betweenconvectively unstable and stably-stratified regions, yielding the depth towhich convection penetrates into the stable region and establishing arelationship between that depth and the local convective Rossby number,diffusivity, and pressure scale height of those flows. Upward and downwardpenetrative convection have a similar scaling with rotation rate anddiffusivities, but they depend differently upon the pressure scale height dueto the differing energetic processes occurring in convective cores ofearly-type stars versus convective envelopes of late-type stars.

A model of rotating convection in stellar and planetary interiors: I - convective penetration