Diffusion in stars: the case of gravity waves, rigid rotation and stable stratification

Details Diffusion in stars: the case of gravity waves, rigid rotation and stable stratification Diffusion in stars: the case of gravity waves, rigid rotation and stable stratification

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mnras.337..713c&link_type=abstract

Monthly Notice of the Royal Astronomical Society, Volume 337, Issue 2, pp. 713-719.

Astronomy and Astrophysics

Astronomy

5

Turbulence, Stars: Abundances, Stars: Interiors

Scientific paper

We study mixing in the tachocline in the presence of a source (gravity waves of power Π) and two sinks (rigid rotation Ω and stable stratification of strength ∇ad-∇ > 0). The Reynolds stresses Rij are found to be proportional to ΠΩ-1rij, where the dimensionless tensor rij may increase, decrease or saturate with Ω depending on the component (ij). The heat fluxes are found to be proportional to Πhi, where the dimensionless hr,θ first decrease with Ω and then saturate while hθ always decreases with Ω. Numerical values of the momentum and heat diffusivities are derived and discussed. Future studies will include differential rotation, the μ-barrier and meridional currents.

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