Table 2.
Parameters of the 20 best models based on the identification of 16 out of the 28 detected frequencies of HD 43317, ordered by the resulting χ 2 value.
| χ2 | M⋆ [M⊙] | Xc | fov | R⋆ [R⊙] | ΔΠ [s] | Age [Myr] | Teff [K] | log g [dex] | qc |
|---|---|---|---|---|---|---|---|---|---|
| 7.23 | 5.8 | 0.54 | 0.004 | 3.39 | 12645 | 28.4 | 17822 | 4.14 | 0.229 |
| 7.76 | 5.8 | 0.53 | 0.004 | 3.43 | 12619 | 29.8 | 17782 | 4.13 | 0.226 |
| 8.46 | 5.7 | 0.54 | 0.010 | 3.39 | 12550 | 31.9 | 17652 | 4.13 | 0.231 |
| 8.82 | 5.8 | 0.54 | 0.006 | 3.41 | 12668 | 29.2 | 17826 | 4.14 | 0.230 |
| 8.89 | 5.7 | 0.53 | 0.010 | 3.43 | 12532 | 33.3 | 17617 | 4.12 | 0.229 |
| 9.31 | 5.8 | 0.53 | 0.002 | 3.42 | 12590 | 29.2 | 17772 | 4.13 | 0.225 |
| 9.40 | 5.8 | 0.54 | 0.002 | 3.39 | 12618 | 27.8 | 17812 | 4.14 | 0.227 |
| 9.44 | 5.8 | 0.53 | 0.006 | 3.44 | 12645 | 30.6 | 17788 | 4.13 | 0.227 |
| 10.00 | 5.7 | 0.53 | 0.008 | 3.42 | 12504 | 32.7 | 17605 | 4.13 | 0.227 |
| 10.15 | 5.7 | 0.54 | 0.008 | 3.38 | 12526 | 31.1 | 17646 | 4.14 | 0.230 |
| 10.21 | 5.7 | 0.54 | 0.012 | 3.40 | 12575 | 32.6 | 17663 | 4.13 | 0.232 |
| 10.87 | 5.8 | 0.55 | 0.004 | 3.36 | 12668 | 27.0 | 17859 | 4.15 | 0.231 |
| 11.58 | 5.6 | 0.54 | 0.016 | 3.38 | 12454 | 35.3 | 17489 | 4.13 | 0.233 |
| 11.61 | 5.7 | 0.53 | 0.012 | 3.44 | 12558 | 34.2 | 17624 | 4.12 | 0.230 |
| 11.72 | 5.7 | 0.55 | 0.010 | 3.35 | 12567 | 30.3 | 17690 | 4.14 | 0.234 |
| 12.05 | 5.8 | 0.55 | 0.006 | 3.37 | 12691 | 27.6 | 17868 | 4.15 | 0.233 |
| 12.11 | 5.8 | 0.52 | 0.004 | 3.47 | 12591 | 31.2 | 17742 | 4.12 | 0.223 |
| 12.37 | 5.7 | 0.55 | 0.012 | 3.36 | 12590 | 30.9 | 17701 | 4.14 | 0.235 |
| 12.41 | 5.6 | 0.53 | 0.016 | 3.43 | 12441 | 37.1 | 17449 | 4.12 | 0.231 |
| 13.00 | 5.6 | 0.53 | 0.014 | 3.42 | 12415 | 36.3 | 17440 | 4.12 | 0.230 |
Notes. For each MESA model, the stellar mass, M⋆, central hydrogen mass fraction, Xc, convective core overshooting parameter, fov, stellar radius, R⋆, asymptotic period spacing, ΔΠ, age, effective temperature, Teff, surface gravity, log g, and fractional mass of the convective core, qc, are given. Degeneracies among the stellar parameters occur when only considering the value for the asymptotic period spacing.
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