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Convection and its Stability in the Equatorial Regions of the Convection Zone

Published online by Cambridge University Press:  08 February 2017

A.V. Klyachkin
A.V. Klyachkin*
Affiliation:
Ioffe Physical- Technical Institute Academy of Sciences Ul. Politechnicheskaya 26 194021, Leningrad, USSR

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The problem of the existence, evolution, and stability of spatial structures in convection is of considerable importance to astrophysics as well as to geophysical hydrodynamics. The Boussinesq approximation will be used because the considered motions in stars are sufficiently slow. The system of hydrodynamic equations describing convection in a rotating inhomogeneous medium has the form: Here Dt is the total time derivative, U the velocity, P, T, and C the deviations of the pressure, temperature, and helium abundance (by mass) from the basic equilibrium values, ρm, νm, χm, and Dm the values averaged over the considered layer of the density, viscosity, thermal and helium diffusivities, βT and βc the averaged coefficients of the thermal and helium expansions, g and Ω the gravitational acceleration and angular velocity, ∇Tb, and ∇Cb the values of the basic equilibrium temperature and helium gradients, and ñTad the adiabatic temperature gradient.

Type
V. Large-scale Structure and Dynamics
Information
Symposium - International Astronomical Union , Volume 138: Solar Photosphere: Structure, Convection and Magnetic Fields , 1990 , pp. 325 - 328
Copyright
Copyright © Kluwer 1990 

References

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