Using the Method of Orthogonal Collocation for Certain Three-Dimensional Problems of Stellar Structure.
Abstract
The method is developed for two specific problems: computation of the structure of the primary component (assumed to consist of a polytropic gas) in a synchronous close binary system; and search for non-axisymmetric configurations of differentially rotating polytropes. In both cases the structure equations reduce to a mildly non-linear elliptic partial differential equation in three dimensions with boundary conditions at the center, on a sphere containing the star and involving a 'free' boundary. The present method has several advantages over the 'standard' methods (namely, improvements of Chandrasekhar's perturbation analysis). The most important of these are consistency and easier application to real stars. However, the method becomes computationally inefficient when used for computing the configurations with strong angular dependence. In such cases (related) Galerkin methods offer significant advantages.
Document Details
- Document Type
- Technical Report
- Publication Date
- Jun 01, 1977
- Accession Number
- ADA042728
Entities
People
- M. J. Miketinac
- S. V. Parter
Organizations
- University of Wisconsin–Madison