Table 1
Observed and inferred stellar parameters for HD 27631, HD 98649, HD 106515A, HD 166724, HD 196067, HD 219077, and HD 220689.
| Parameters | HD 27631 | HD 98649 | HD 106515A | HD 166724 | HD 196067 | HD 219077 | HD 220689 | |||
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| Spectral typea | G3 IV/V | G4 V | G5 | K0 IV/V | G1 V | G8 V+ | G3 V | |||
| V a | 8.26 | 8.00 | 7.35 | 9.33 | 6.51 | 6.12 | 7.74 | |||
| B − Va | 0.682 | 0.658 | 0.815 | 0.861 | 0.620 | 0.787 | 0.603 | |||
| π b | [mas] | 22.0 ± 0.7 | 24.1 ± 0.8 | 28.4 ± 1.0 | 23.6 ± 1.2 | 22.6 ± 2.6 | 34.07 ± 0.37 | 22.4 ± 0.7 | ||
| M v | 4.97 | 4.91 | 4.62 | 6.20 | 3.28 | 3.78 | 4.49 | |||
| T eff | [K] | 5737 ± 36c | 5759 ± 35c | 5362 ± 29c | 5127 ± 52d | 6017 ± 46c | 5362 ± 18d | 5921 ± 26c | ||
| log g | [cgs] | 4.48 ± 0.09c | 4.38 ± 0.08c | 4.41 ± 0.04c | 4.43 ± 0.08d | 4.24 ± 0.03c | 4.00 ± 0.03d | 4.32 ± 0.03c | ||
| [Fe/H] | [dex] | –0.12 ± 0.05c | 0.02 ± 0.03c | 0.03 ± 0.02c | –0.09 ± 0.03d | 0.18 ± 0.04c | –0.13 ± 0.01d | 0.00 ± 0.03c | ||
| vsin (i)e | [km s-1] | 1.34 | 1.19 | <1 | 1.42 | 1.45 | 1.46 | 2.3 | ||
| M ∗ f | [M⊙] | 0.94 ± 0.04 | 1.00 ± 0.03 | 0.97 ± 0.01 | 0.81 ± 0.02 | 1.29 ± 0.08 | 1.05 ± 0.02 | 1.04 ± 0.03 | ||
| L g | [L⊙] | 0.88 | 0.86 | 1.23 | 0.31 | 3.73 | 2.66 | 1.24 | ||
| R f | [R⊙] | ≈1.0 | ≈1.0 | 1.62 ± 0.05 | – | 1.73 ± 0.21 | 1.91 ± 0.03 | 1.07 ± 0.04 | ||
log  |
–4.94 ± 0.08c | –4.99 ± 0.08c | –5.09 ± 0.09c | –4.73 ± 0.03h | –5.11 ± 0.08c | –5.12 ± 0.01h | –4.98 ± 0.05c | |||
| P rot i | [days] | 28 ± 4 | 27 ± 4 | 50 ± 5 | 30 ± 5 | 26 ± 3 | 49 ± 4 | 20 ± 3 | ||
| Agef | [Gyr] | 4.4 ± 3.6 | 2.3 ± 2.0 | 11.7 ± 0.2 | 4.0 ± 3.8 | 3.3 ± 0.6 | 8.9 ± 0.3 | 3.5 ± 1.9 | ||
Notes.
Parameter from Hipparcos (ESA 1997).
Parallax from the new Hipparcos reduction (van Leeuwen 2007).
Parameter derived using HARPS spectra (Sousa et al. 2008).
Parameter derived using CORALIE CCF (Santos et al. 2001).
Parameter derived from Girardi et al. (2000) models.
The bolometric correction is computed from Flower (1996).
Parameter derived using HARPS spectra (Lovis et al. 2011).
From the calibration of the rotational period vs. activity (Mamajek & Hillenbrand 2008).
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