Computer Science – Numerical Analysis
Scientific paper
Oct 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...249..746c&link_type=abstract
Astrophysical Journal, Part 1, vol. 249, Oct. 15, 1981, p. 746-760. Research supported by the Natural Sciences and Engineering
Computer Science
Numerical Analysis
26
Angular Velocity, Dynamic Characteristics, Equations Of Motion, Stellar Models, Stellar Oscillations, Stellar Rotation, Computer Techniques, Eigenvectors, Numerical Analysis, Poisson Equation, Supermassive Stars, Variable Stars
Scientific paper
Some normal modes of rotating stars can be computed numerically without having to assume a slow angular velocity. This can be done by solving directly on a two-dimensional grid the linearized dynamical equations governing adiabatic oscillations. In this paper, the effects of rigid rotation on four axisymmetric modes are found for several equilibrium systems including polytropes and a 15 solar-mass stellar model. It is shown that even a small rotation changes significantly the space dependence of the eigenfunctions.
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