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High- and Low-Degree Modes in Delta Scuti Stars: 1- and 2-D Fourier Analyses Of τ Peg

  • Edward J. Kennelly (a1), Jaymie M. Matthews (a1) (a2) and Gordon A.H. Walker (a1)

Extract

Stellar seismology of δ Scuti stars offers the best prospect for determining the interior properties of normal non-magnetic A-F stars on or near the main sequence. The discovery of rich eigenfrequency spectra in the light variations of several δ Scuti stars (e.g., θ 2 Tau: Breger et al. 1989; GX Peg: Michel et al. 1990) should make this possible for low-degree modes (l ≤ 4). However, due to cancellation effects, modes of higher l cannot be studied through photometry or radial velocity measurements.

The detection of rapid line-profile variations among rapidly rotating δ Scuti stars (e.g., Walker et al. 1987; Kennelly et al. 1992) has extended our sensitivity to much higher modes. These variations are consistent with moderate- to high-degree modes, where |m| ~ l. (In the simplest case, they could be pure sectorial modes with |m| = l and pulsation amplitudes strongly confined to the stellar equator.) To use these data effectively, we need an objective way to identify the modes and their time evolution.

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References

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Breger, M. 1991, Communications in Asteroseismology 29, 1
Breger, M., Garrido, R., Huang, Lin, et al. 1989, Astron. Astrophys. 214, 209
Kennelly, E.J., Yang, S., Walker, G.A.H., and Hubeny, I. 1992, PASP 104, 15
Michel, E., Belmonte, J.A., Alvarez, M., et al. 1990, In Confrontation Between Stellar Pulsation and Evolution, eds. Cacciari, C. and Clementini, G. (ASP Conf. Series 11), p. 332.
Walker, G.A.H., Yang, S. and Fahlman, G.G. 1987, Ap.J. 320, L139

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