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Paper: Pulsations of an Evolved Self-consistently Distorted Star
Volume: 462, Progress in Solar/Stellar Physics with Helio- and Asteroseismology
Page: 402
Authors: Ouazzani, R.-M.; Dupret, M.-A.; Roxburgh, I. W.; Goupil, M.-J.
Abstract: A new two-dimensional (2D) non-perturbative method to compute accurate oscillation modes of rapidly rotating stars is presented. The 2D calculations fully take into account the centrifugal distortion of the star while the non-perturbative method includes the full influence of the Coriolis acceleration, and are used to compute oscillation modes of rapid rotators — high-order p-modes in δ Scuti stars, as well as low-order p- and g-modes in β Cephei stars. We compare the oscillation spectra obtained for centrifugally distorted polytropes with those of Reese et al. (2006), and give the first results for a realistic 2D model of a rapidly rotating 2 M evolved star computed with the method developed by Roxburgh (2006).
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