On the existence of a surface boundary layer in a slowly rotating, early-type star

Details On the existence of a surface boundary layer in a slowly rotating, early-type star On the existence of a surface boundary layer in a slowly rotating, early-type star

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...427..388t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 427, no. 1, p. 388-393

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Applications

1

Applications Of Mathematics, Astronomical Models, Differential Equations, Early Stars, Hydrodynamics, Meridional Flow, Stars, Thermal Boundary Layer, Angular Velocity, Eddy Viscosity, Entropy, Legendre Functions, Poloidal Flux

Scientific paper

This paper deals with the thermally driven meridional currents and concomitant differential rotation that exist in a slowly rotating, nonmagnetic, early-type star. Neglecting the viscous force acting on the meridional flow, one can obtain a nonsingular solution that satisfies all the boundary conditions; unfortunately, this solution does not satisfy all the basic equations -- one component of the Navier-Stokes equations remaining necessarily unfulfilled. On the contrary, by making allowance for viscous friction acting on the circulatory currents, one can obtain a solution that satisfies all the surface boundary conditions and all the basic equations. To be specific, there exists a thin thermoviscous boundary layer in which turbulent friction prevents the formation of unwanted singularities in the meridional flow -- the circulation velocities thus remaining uniformly small everywhere in the radiative envelope. This free boundary layer bears no relation whatsoever to those encountered in geophysics and in hydrodynamics.

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