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

Abstract

A monomodal model for stellar and planetary convection is derived for the magnitude of the rms velocity, degree of superadiabaticity, and characteristic length scale as a function of rotation rate as well as with thermal and viscous diffusivities. The convection model is used as a boundary condition for a linearization of the equations of motion in the transition region between convectively unstable and stably-stratified regions, yielding the depth to which convection penetrates into the stable region and establishing a relationship between that depth and the local convective Rossby number, diffusivity, and pressure scale height of those flows. Upward and downward penetrative convection have a similar scaling with rotation rate and diffusivities, but they depend differently upon the pressure scale height due to the differing energetic processes occurring in convective cores of early-type stars versus convective envelopes of late-type stars.

21 pages, 6 figures, Accepted in ApJ

References in corpus (21)

• Simulations of dynamo action in fully convective stars
• Asteroseismic measurement of surface-to-core rotation in a main sequence A star, KIC 11145123
• Simulations of core convection in rotating A-type stars: Magnetic dynamo action
• Asteroseismic measurement of slow, nearly-uniform surface-to-core rotation in the main sequence F star KIC 9244992
• Comparison between two and three dimensional Rayleigh-Bénard convection
• On differential rotation and overshooting in solar-like stars
• Angular Momentum Transport via Internal Gravity Waves in Evolving Stars
• Stochastic excitation of nonradial modes II. Are solar asymptotic gravity modes detectable?
• The interior angular momentum of core hydrogen burning stars from gravity-mode oscillations
• Theoretical seismology in 3D : nonlinear simulations of internal gravity waves in solar-like stars
• Numerical Simulations of Penetration and Overshoot in the Sun
• Angular momentum redistribution by mixed modes in evolved low-mass stars. II. Spin-down of the core of red giants induced by mixed modes
• Theory and simulations of rotating convection
• Lithium depletion in solar-like stars: effect of overshooting based on realistic multi-dimensional simulations
• Angular momentum redistribution by mixed modes in evolved low-mass stars. I. Theoretical formalism
• Impact of rotation on stochastic excitation of gravity and gravito-inertial waves in stars
• Extreme value statistics for two-dimensional convective penetration in a pre-Main Sequence star
• Angular momentum transport by internal gravity waves III - Wave excitation by core convection and the Coriolis effect
• Dynamics of Mixed Convective--Stably-Stratified Fluids
• Angular momentum transport by stochastically excited oscillations in rapidly rotating massive stars
• Turbulent Compressible Convection with Rotation - Penetration above a Convection Zone

Cited by in corpus (3)

• Variability of OB stars from TESS southern Sectors 1-13 and high-resolution IACOB and OWN spectroscopy
• Photometric detection of internal gravity waves in upper main-sequence stars. II. Combined TESS photometry and high-resolution spectroscopy
• Angular momentum transport, layering, and zonal jet formation by the GSF instability: nonlinear simulations at a general latitude