A model of rotating convection in stellar and planetary interiors: I – convective penetration. (arXiv:1902.10593v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Augustson_K/0/1/0/all/0/1">Kyle C. Augustson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mathis_S/0/1/0/all/0/1">Stéphane Mathis</a>
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.
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.
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