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A formidable unsolved problem in general relativity is how to calculate the nonaxisymmetric pulsational modes of rotating stars. Even in Newtonian gravity, the mode equations for rotating stars have only recently been solved numerically by Ipser and Lindblom (1989, 1990). In this paper, their Newtonian calculations are straightforwardly extended to post-Newtonian order.
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Curt Cutler (1991) studied this question.
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