Table 2.
Comparison between the observed periods of GD 278 and the theoretical periods of the adopted asteroseismological model characterized by M⋆ = 0.186 M⊙, Teff = 9335 K, and log(g) = 6.618 [CGS].
| k | ℓ | ΠO [s] | ΠT [s] | |ΔΠ|/Π |
|---|---|---|---|---|
| 25 | 1 | 2367.4 | 2332.6513 | 0.0147 |
| 29 | 1 | 2658.51 | 2681.3868 | 0.0086 |
| 35 | 1 | 3226.1 | 3212.6071 | 0.0042 |
| 44 | 1 | 4028.83 | 4017.2143 | 0.0029 |
| 52 | 1 | 4756.5 | 4735.2063 | 0.0045 |
| 94 | 2 | 4959.6 | 4940.8258 | 0.0038 |
| 99 | 2 | 5198.3 | 5203.3066 | 0.0010 |
| 100 | 2 | 5253.2 | 5255.5214 | 0.0004 |
Notes. This stellar model has undergone CNO flashes during its early-cooling phase (Althaus et al. 2013). Columns indicate the radial order and harmonic degree, the observed and theoretical periods, and the relative difference between the last two quantities, respectively.
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