Table 3
Newly derived stellar parameters and elemental abundances.
| Parameter | HD 220197 | HD 233832 |
|---|---|---|
| Mass (M⊙)a | 0.91 ± 0.02 | 0.71 ± 0.02 |
| Radius (R⊙)a | 0.98 ± 0.02 | 0.68 ± 0.03 |
| Age (Gyr)b | 10.165 ± 1.367 | 5.417 ± 4.165 |
| Teff (K)c | 5683 ± 15 | 4981 ± 31 |
| log g (cgs)c | 4.42 ± 0.03 | 4.49 ± 0.06 |
| ξ (km s−1)c | 1.01 ± 0.03 | 1.04 ± 0.02 |
| vmacro (km s−1) | 3.1 | 1.8 |
| v sin i (km s−1) | 1.5 ± 0.5 | 0.8 ± 0.5 |
 |
− 4.96 | − 5.01 |
| Prot (d)d | ~19 | ~41 |
| [Fe/H]c | − 0.55 ± 0.02 (+ −0.06) | − 0.66 ± 0.03 (+ −0.10) |
| [C I/H] | − 0.26 ± 0.09 (+ −0.04) | + 0.09 ± 0.08 (+ −0.07) |
| [Na I/H] | − 0.41 ± 0.03 (+ −0.02) | − 0.60 ± 0.04 (+ −0.07) |
| [Mg I/H] | − 0.21 ± 0.04 (+ −0.02) | − 0.42 ± 0.04 (+ −0.04) |
| [Al I/H] | − 0.30 ± 0.17 (+ −0.01) | − 0.46 ± 0.16 (+ −0.05) |
| [Si I/H] | − 0.35 ± 0.09 (+ −0.01) | − 0.55 ± 0.08 (+ −0.03) |
| [S I/H] | − 0.27 ± 0.04 (+ −0.04) | − 0.27 ± 0.09 (+ −0.07) |
| [Ca I/H] | − 0.29 ± 0.06 (+ −0.03) | − 0.51 ± 0.12 (+ −0.09) |
| [Ti I/H] | − 0.22 ± 0.06 (+ −0.03) | − 0.45 ± 0.12 (+ −0.11) |
| [Ti II/H] | − 0.40 ± 0.09 (+ −0.05) | − 0.61 ± 0.09 (+ −0.06) |
| [Cr I/H] | − 0.49 ± 0.06 (+ −0.02) | − 0.65 ± 0.10 (+ −0.08) |
| [Cr II/H] | − 0.57 ± 0.06 (+ −0.05) | − 0.66 ± 0.10 (+ −0.06) |
| [Ni I/H] | − 0.51 ± 0.07 (+ −0.02) | − 0.73 ± 0.09 (+ −0.04) |
| [Zn I/H] | − 0.37 ± 0.04 (+ −0.02) | − 0.61 ± 0.06 (+ −0.04) |
| [Y II/H] | − 0.66 ± 0.06 (+ −0.05) | − 0.88 ± 0.10 (+ −0.06) |
| [Zr II/H] | − 0.51 ± 0.03 (+ −0.06) | − 0.59 ± 0.12 (+ −0.06) |
| [Nd II/H] | − 0.65 ± 0.08 (+ −0.06) | − 0.62 ± 0.18 (+ −0.07) |
| [Cu II/H] | − 0.52 ± 0.12 (+ −0.03) | − 0.73 ± 0.16 (+ −0.05) |
| [Eu II/H] | − 0.44 ± 0.07 (+ −0.05) | − 0.47 ± 0.06 (+ −0.07) |
| [La II/H] | − 0.73 ± 0.10 (+ −0.06) | − 0.82 ± 0.08 (+ −0.07) |
| [Mn I/H] | − 0.76 ± 0.09 (+ −0.03) | − 0.80 ± 0.09 (+ −0.09) |
| [Ba II/H] | − 0.73 ± 0.10 (+ −0.05) | − 0.99 ± 0.09 (+ −0.05) |
Notes. The first errors on elemental abundances refer to the measure of the equivalent width, while the errors in parentheses are obtained from the root sum square of the abundance error caused by uncertainties on Teff, log g, and ξ. (a) Weighted mean between parameter calculated from PARAM 1.3 (see da Silva et al. 2006) and Yonsei-Yale isochrones (see Yi et al. 2008). (b) Calculated from PARAM 1.3. (c)Weighted mean between the values obtained from the two analyses on equivalent width described in Sect. 3. (d) Calculated following Noyes et al. (1984) and Mamajek & Hillenbrand (2008).
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