Rotating Convection and Gravito-Inertial Wave Generation in Stellar Interiors. (arXiv:1902.10594v1 [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>
Gravito-inertial waves can be excited at the interface of convective and
radiative regions and by the Reynolds stresses in the bulk of the convection
zone. The magnitude of their energy flux will therefore vary with the
properties of the convection. To assess how convection changes with rotation, a
simplified local monomodal model for rotating convection is presented that
provides the magnitude of the rms velocity, degree of superadiabaticity, and
characteristic length scale as a function of the convective Rossby number as
well as with thermal and viscous diffusivities. In the context of this
convection model, two models for assessing the gravito-inertial wave flux are
considered: an interfacial model and a full treatment of the Reynolds stress
impact on the waves. It is found that there are regimes where the sub-inertial
waves may carry a significant energy flux relative to pure gravity waves that
depend upon the convective Rossby number, the ratio of the buoyancy time-scale
in the stable region to the convective overturning time, and the wave
frequency.
Gravito-inertial waves can be excited at the interface of convective and
radiative regions and by the Reynolds stresses in the bulk of the convection
zone. The magnitude of their energy flux will therefore vary with the
properties of the convection. To assess how convection changes with rotation, a
simplified local monomodal model for rotating convection is presented that
provides the magnitude of the rms velocity, degree of superadiabaticity, and
characteristic length scale as a function of the convective Rossby number as
well as with thermal and viscous diffusivities. In the context of this
convection model, two models for assessing the gravito-inertial wave flux are
considered: an interfacial model and a full treatment of the Reynolds stress
impact on the waves. It is found that there are regimes where the sub-inertial
waves may carry a significant energy flux relative to pure gravity waves that
depend upon the convective Rossby number, the ratio of the buoyancy time-scale
in the stable region to the convective overturning time, and the wave
frequency.
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