Structures of rapidly rotating baroclinic stars - II. an extended numerical method for realistic stellar models

Details Structures of rapidly rotating baroclinic stars - II. an extended numerical method for realistic stellar models Structures of rapidly rotating baroclinic stars - II. an extended numerical method for realistic stellar models

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.277.1411u&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 277, Issue 4, pp. 1411-1429.

Astronomy and Astrophysics

Astronomy

13

Methods: Numerical, Stars: Rotation

Scientific paper

We have succeeded in developing a numerical code to obtain structures and angular velocity distributions of significantly deformed axisymmetric baroclinic stars with both convective and radiative regions. Stars are assumed to be meridonal-circulation-free, chemically homogeneous and inviscid. In our new method, the energy equation and Poisson's equation are expressed in integral forms by using the Green's function for the Laplacian, although other basic equations are treated as differential equations as they are. In this new scheme, the boundary conditions can be easily included in the integral representation. These equations are discretized and solved by the Newton-Raphson iteration scheme in the surface-fitted coordinates. By applying this new scheme we have solved structures and rotation laws for three types of baroclinic stars which mimic stars consisting of a wholly radiative region, of a convective core and a radiative envelope, and of a radiative core and a convective envelope.

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