2018/11/11 by Kyle Augustson, Augustson, Kyle, S. Mathis +1 · 1 citation
Engineering · Physics and Astronomy · #FOS: Physical sciences #Fluid Dynamics and Turbulent Flows #Phase Equilibria and Thermodynamics #Solar and Stellar Astrophysics (astro-ph.SR) #Stellar, planetary, and galactic studies
paper · pdf · doi:10.48550/arxiv.1811.04413
openalex publication_date 2018/11/11 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
A simplified model for stellar and planetary convection is derived for the magnitude of the rms velocity, degree of superadiabaticity, and characteristic length scale with Rossby number as well as with thermal and viscous diffusivities. Integrating the convection model into a linearization of the dynamics in the transition region between convectively unstable and stably-stratified region yields a Rossby number, diffusivity, and pressure scale height dependent convective penetration depth into the stable region. This may have important consequences for mixing along the evolution of rotating stars.