Structures of Rapidly Rotating Baroclinic Stars - Part One - a Numerical Method for the Angular Velocity Distribution

Astronomy and Astrophysics – Astronomy

Scientific paper

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Hydrodynamics - Methods: Numerical - Celestial Mechanics, Stellar Dynainics - Stars: Rotation

Scientific paper

We succeed in developing a new numerical code to obtain structures and angular momentum distributions of significantly deformed axisymmetric baroclinic stars, which are assumed to be meridional-circulation-free and inviscid. In our method, although all basic equations except for the Poisson equation are handled as differential equations, the gravitational potential is expressed in the integral form by using the Green function for the Laplacian. These equations are discretized and solved using the Newton-Raphson iteration method in the surface-fitted coordinates. Since the numerical scheme is straightforward, we can easily generalize the present scheme to include a meridional circulation, inhomogeneity of the chemical composition, and/or viscosity of the fluid.

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