Table 3.
Average frequency shifts of the dipole modes caused by different internal magnetic field configurations for three stellar models.
M*/M⊙ | Zinit | νmax/μHz | Bcrit, cen/MG | Bcrit, H/MG |
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---|---|---|---|---|---|---|---|
1 | 0.02 | 127.03 | 8.78 | 0.39 | 1.33 (2.65) | 1.40 (2.80) | 2.09 (4.18) |
1 | 0.005 | 129.53 | 8.87 | 0.47 | 1.36 (2.72) | 1.40 (2.81) | 2.38 (4.75) |
1.3 | 0.02 | 127.99 | 8.90 | 0.35 | 1.34 (2.69) | 1.36 (2.71) | 2.06 (4.13) |
Notes. The models were selected from each evolutionary track to mimic the observed value of νmax of KIC 6975038 (e.g., Deheuvels et al. 2023). The magnetic field strengths have been chosen such that the suppression of the multipole modes behaves as shown in Fig. 7. The average frequency shifts have been determined using the first-order perturbation approach of Li et al. (2022). Note that the application of this method to magnetic field strengths close to the critical field strength is expected to lead to an underestimation of the frequency shifts (Rui et al. 2024). The quantity (δω0/2π)PG, H corresponds to the frequency shift induced by a Prendergast field that is contained by the region at and within the hydrogen-burning shell, while (δω0/2π)PG, core corresponds to a Prendergast field that extends over the entire radiative core. (δω0/2π)pla corresponds to the frequency shift induced by the improvised field with a plateau within the hydrogen-burning shell introduced in Sect. 3.3. The value of the average frequency shifts without brackets (in brackets) corresponds to the azimuthal order m = 0 (m = ±1).
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