Table 3.
Comparison between the observed frequencies, fobs, and the GYRE frequencies of the MESA model resulting in the best description of the CoRoT data of HD 43317, fng,l,m.
| fobs [d−1] | ng | ℓ | m | fng,l,m model [d−1] | fng,l,0 rot. [d−1] | fng,l,0 no rot. [d−1] | fshift rot. [d−1] | fshift 26.1 kG [d−1] | fshift 82.4 kG [d−1] | Sc [G−2] | I | |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| f4 | 0.6916 | −11 | 1 | −1 | 0.6867 | 1.1927 | 0.8187 | 0.3740 | 0.0210 | 0.2092 | 3.7661 × 10−11 | 1.5487 × 107 |
| f5 | 0.7529 | −10 | 1 | −1 | 0.7573 | 1.2595 | 0.8979 | 0.3617 | 0.0159 | 0.1592 | 2.6131 × 10−11 | 1.2925 × 107 |
| f6 | 0.8278 | −9 | 1 | −1 | 0.8381 | 1.3388 | 0.9923 | 0.3465 | 0.0125 | 0.1250 | 1.8565 × 10−11 | 1.1215 × 107 |
| f7 | 0.8752 | −15 | 2 | −1 | 0.8720 | 1.6623 | 1.0462 | 0.6161 | 0.0110 | 0.1101 | 1.5515 × 10−11 | 4.3758 × 107 |
| f8 | 0.9279 | −8 | 1 | −1 | 0.9222 | 1.4236 | 1.0933 | 0.3303 | 0.0104 | 0.1041 | 1.4035 × 10−11 | 1.0293 × 107 |
| f9 | 0.9954 | −7 | 1 | −1 | 1.0037 | 1.5086 | 1.1943 | 0.3143 | 0.0097 | 0.0972 | 1.1994 × 10−11 | 1.0496 × 107 |
| f11 | 1.1004 | −11 | 2 | −1 | 1.1268 | 1.9545 | 1.4108 | 0.5438 | 0.0029 | 0.0288 | 3.0120 × 10−12 | 1.5448 × 107 |
| f13 | 1.1754 | −6 | 1 | −1 | 1.1483 | 1.6594 | 1.3708 | 0.2887 | 0.0086 | 0.0861 | 9.2633 × 10−12 | 1.0679 × 107 |
| f14 | 1.2280 | −10 | 2 | −1 | 1.2198 | 2.0621 | 1.5454 | 0.5167 | 0.0022 | 0.0220 | 2.0968 × 10−12 | 1.2904 × 107 |
| f15 | 1.3424 | −9 | 2 | −1 | 1.3337 | 2.1920 | 1.7058 | 0.4861 | 0.0017 | 0.0173 | 1.4932 × 10−12 | 1.1195 × 107 |
| f16 | 1.3529 | −5 | 1 | −1 | 1.3775 | 1.8992 | 1.6455 | 0.2537 | 0.0063 | 0.0626 | 5.6119 × 10−12 | 9.3225 × 106 |
| f20 | 1.7045 | −4 | 1 | −1 | 1.7358 | 2.2719 | 2.0601 | 0.2118 | 0.0045 | 0.0451 | 3.2246 × 10−12 | 8.3961 × 106 |
| f21 | 1.8156 | −6 | 2 | −1 | 1.8191 | 2.7238 | 2.3408 | 0.3829 | 0.0012 | 0.0121 | 7.5960 × 10−13 | 1.0725 × 107 |
| f29 | 3.4958 | −2 | 1 | −1 | 3.4811 | 4.1058 | 3.9638 | 0.1420 | 0.0022 | 0.0221 | 8.2084 × 10−13 | 7.9125 × 106 |
| f31 | 4.3311 | −6 | 2 | 2 | 4.3408 | 2.7238 | 2.3408 | 0.3829 | 0.0048 | 0.0483 | 3.0384 × 10−12 | 1.0725 × 107 |
| f32 | 5.0047 | −1 | 1 | −1 | 4.9948 | 6.1855 | 6.1084 | 0.0771 | 0.0015 | 0.0150 | 3.6143 × 10−13 | 8.2739 × 106 |
Notes. We compared the frequency shift due to rotation according to the traditional approximation with the frequency shift due to an internal (purely) poloidal magnetic field. For each observed frequency, we provide the best model frequency for the indicated mode geometry, as well as the corresponding zonal pulsation mode frequencies fng,l,0 computed with and without the Coriolis force in the traditional approximation. The frequency shift due to the Lorentz force was computed following the approach of Hasan et al. (2005), for the lower and upper limit of an internal magnetic field at the convective core boundary, by extrapolating the surface field inward. We also included the magnetic splitting coefficient Sc and the quantity I.
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