Table 3
Derived parameters and abundances for HD 47887 (second column) and HD 47777 (third column).
| HD 47887 | HD 47777 | Sun | ||
|
|
||||
| Teff [K] | 24 000 ± 1000 | 22 000 ± 1000 | 5777 | |
| log g | 4.1 ± 0.1 | 4.2 ± 0.1 | 4.438 | |
| υmic [km s-1] | 5 ± 1 | 4 ± 1 | 0.875 | |
| υr [km s-1] | 22.9 ± 1.5(7) | 24.9 ± 1.3(11) | − | |
| υsini [km s-1] | 45 | 60 | 1.2 | |
| Rot. period [d] | 1.947807 | 2.640426 | 24.47 | |
| υeq [km s-1] | 116 | 67 | 2.067 | |
| i [°] | 23 | 64 | − | |
| log L/L⊙ | 3.80 ± 0.15 | 3.42 ± 0.15 | 0.0 | |
| ageevol [log t] | 7.00 |
6.92 |
9.66 | |
| Mevol [M⊙] | 9.4 |
7.6 |
1.0 | |
| Revol [R⊙] | 4.4 |
3.6 |
1.0 | |
| RSED [R⊙] | 4.45 ± 0.50 | 3.50 ± 0.50 | 1.0 | |
| ⟨ Bz ⟩ [G] | 373 ± 48 | 469 ± 87 | − | |
|
|
||||
| LTE | non-LTE | |||
| He [dex] | −1.04 ± 0.10 | −1.74 ± 0.10 | −1.04 | −1.11 |
| C [dex] | −4.35 ± 0.10 | −4.15 ± 0.13 | −3.49 | −3.61 |
| N [dex] | −4.36 ± 0.10 | −4.36 ± 0.13 | −4.07 | −4.21 |
| O [dex] | −3.28 ± 0.10 | −3.48 ± 0.10 | −3.17 | −3.35 |
| Ne* [dex] | −3.62 ± 0.08(2) | −3.89 ± 0.05(2) | −3.96 | −4.11 |
| Mg [dex] | −5.01 ± 0.15 | −4.81 ± 0.19 | −4.46 | −4.44 |
| Al* [dex] | −6.26 ± 0.08(3) | −6.18 ± 0.10(4) | −5.57 | −5.59 |
| Si [dex] | −4.83 ± 0.10 | −4.83 ± 0.20 | −4.49 | −4.53 |
| P* [dex] | −5.93(1) | −6.59 | −6.63 | |
| S* [dex] | −5.05(1) | −5.38 ± 0.11(6) | −4.71 | −4.92 |
| Ar* [dex] | −5.39(1) | −5.30(1) | −5.52 | −5.64 |
| Fe* [dex] | −4.52 ± 0.32(14) | −4.82 ± 0.11(7) | −4.54 | −4.54 |
Notes. The listed radial velocity υr is the average value obtained from all spectra analysed in this work, and the number in parenthesis indicates the number of spectra for which we determined a υr value. The angle i, in degrees, corresponds to the inclination angle of the star’s rotational axis to the line of sight. Revol and RSED indicate the stellar radius obtained from the comparison to the evolutionary tracks (see Sect. 4) and from the fitting of the synthetic fluxes to the observed photometry converted to physical units (see Sect. 3.4). For comparison, the LTE and non-LTE solar abundance values obtained by Grevesse et al. (1996) and Asplund et al. (2009), respectively, are given in the fourth and fifth columns. The abundances, listed in the second half of the table, are given in log (N ! Ntot) and the number in parenthesis indicates the number of lines used to determine the element abundance. The abundance of the elements marked with an asterisk was determined assuming LTE on the basis of the final fastwind models, as described in Sect. 3.2.
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