Turbulent compressible convection with rotation penetration below a convection zone

Details Turbulent compressible convection with rotation penetration below a convection zone Turbulent compressible convection with rotation penetration below a convection zone

Feb 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007ap%26ss.307..399p&link_type=abstract

Astrophysics and Space Science, Volume 307, Issue 4, pp.399-407

Astronomy and Astrophysics

Astrophysics

4

Convection&Mdash, Stars, Interior&Mdash, Sun, Interior&Mdash, Rotation

Scientific paper

We examine the behaviour of penetrative turbulent compressible convection under the influence of rotation by means of three dimensional numerical simulations. We estimate the extent of penetration below a stellar-type rotating convection zone in an f-plane configuration. Several models have been computed with a stable-unstable-stable configuration by varying the rotation rate (Ω), the inclination of the rotation vector and the stability of the lower stable layer. The spatial and temporal average of kinetic energy flux (Fk) is computed for several turnover times after the fluid has thermally relaxed and is used to estimate the amount of penetration below the convectively unstable layer. Our numerical experiments show that with the increase in rotational velocity, the downward penetration decreases. A similar behaviour is observed when the stability of the lower stable layer is increased in a rotating configuration. Furthermore, the relative stability parameter S shows an S -1/4 dependence on the penetration distance implying the existence of a thermal adjustment region in the lower stable layer rather than a nearly adiabatic penetration region.

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