Table 3.
Rotational stability of selected Kepler stars for which Ω0 and Ω2 were measured using asteroseismology (Benomar et al. 2018).
| KIC # | Ω0/2π | Ω2/Ω0 ± σ | Ω2/Ω0 + 2/7 |
|---|---|---|---|
| (nHz) | |||
| 5184732 | 785 ± 276 | −1.43 ± 1.87 | −0.6 σ |
| 6225718 | 1725 ± 348 | −1.58 ± 0.77 | −2.1 σ( * ) |
| 7510397 | 2754 ± 469 | −2.11 ± 0.92 | −2.0 σ( * ) |
| 8006161 | 722 ± 137 | −1.08 ± 0.67 | −1.2 σ( * ) |
| 8379927 | 1550 ± 230 | −1.17 ± 0.74 | −1.2 σ( * ) |
| 8694723 | 2276 ± 324 | −1.23 ± 0.61 | −1.5 σ( * ) |
| 9025370 | 1015 ± 460 | −2.63 ± 3.00 | −0.8 σ |
| 9139151 | 1693 ± 426 | −2.10 ± 1.51 | −1.2 σ( * ) |
| 9955598 | 584 ± 243 | −1.72 ± 2.11 | −0.7 σ |
| 9965715 | 2321 ± 338 | −0.73 ± 0.64 | −0.7 σ |
| 10068307 | 1072 ± 313 | −0.92 ± 1.09 | −0.6 σ |
| 10963065 | 1140 ± 219 | −0.5 ± 0.6 | −0.4 σ |
| 12258514 | 1087 ± 432 | −1.3 ± 1.4 | −0.7 σ |
Notes. The asterisk denotes stars that are unstable by more than one standard deviation (σ) according to the criterion of Watson (1981). Benomar et al. (2018) measured the first two coefficients in the expansion 
for a selection of Kepler stars. Keeping these two terms only, we have Ω = Ω0 + Ω2cos2θ with Ω0 = α0 − 3α2/2 and Ω2 = 15α2/2.
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