Table 4
Comparison of the power-spectral structure of the δ Scuti stars studied, showing the increase of the mean density of peaks with higher rotation rate.
| Modela | KIC 5892969 | CID 546 | CID 8669 | ||
|
|
|||||
| Ω/Ωk | (%) | 59 | 14 ± 7 | 31 ± 3 | 70 ± 7 |
| νc | (μHz) | − b | 400 ± 10 | 310 ± 7 | |
|
( ) |
0.32 ± 0.03 | 2.27 ± 0.25 | 5 ± 1 | |
| nmean { 0 } | (peaks/μHz) | 0.16 ± 0.03 | 0.89 ± 0.19 | 1.38 ± 1.00 | |
| Nenv | (peaks) | 34 | 24 ± 1c | 17 ± 6 | 29 ± 3 |
| Ngrass { 0 } | (peaks) | 270 ± 8 | 13 ± 6b | 282 ± 64 | 320 ± 250 |
Notes.
Expected modes in the characteristic frequency range for a computed model of a star with moderate rotation rate (Lignières & Georgeot 2009).
Since the cut off frequency is not visible, the high frequency limit to calculate the initial number of modes Ngrass { 0 } is the Nyquist frequency (see text).
This mean value of Nenv does not take into account the measurement at Δt = 1470 d. This duration of the light curve is long enough to observe sidelobes caused by RMC (see Barceló Forteza et al. 2015).
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