STRUCTURES OF RAPIDLY ROTATING BAROCLINIC STARS .2. AN EXTENDED NUMERICAL-METHOD FOR REALISTIC STELLAR MODELS

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