Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977stin...7733012m&link_type=abstract
Unknown
Astronomy and Astrophysics
Astrophysics
Boundary Value Problems, Equations Of State, Stellar Atmospheres, Astrophysics, Boundary Conditions, Harmonic Analysis, Rotation
Scientific paper
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.
Miketinac M. J.
Parter S. V.
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