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Paper: Comparing Two Mode Identification Techniques for a DB White Dwarf
Volume: 479, Progress in Physics of the Sun and Stars
Page: 245
Authors: Nitta, A.; Koester, D.; Chu, D.; Thompson, S. E.; Kepler, S. O.; Kleinman, S. J.; Winget, D. E.; Provencal, J. L.; Castanheira, B. G.
Abstract: Mode identification is one of the most important steps in the asteroseismological analysis of pulsating stars. For pulsating white dwarf stars, the method using pulsation periods has proven to be quite powerful. But there is another method, using the amplitude of the pulsation modes. The advantage of this method is that it can work on pulsators with small numbers of pulsation modes. Since the majority of white dwarf pulsators show a small number of pulsation modes, they are difficult to analyze using their pulsation periods alone. We have applied the mode identification method using pulsation amplitudes to GD 358, a pulsating white dwarf star previously studied successfully using pulsation periods. Both methods agree.
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