Table 6
Stellar parameters and mass fractions of the program stars.
| # | M | τ | log (L/L⊙) | R ⋆ | d | Π-1 | X | Y | Z | ||||||||||||||||||
| (M⊙) | (Myr) | (R⊙) | (pc) | ||||||||||||||||||||||||
|
|
|||||||||||||||||||||||||||
| 1 | 9.3 |
|
12 |
|
3.75 |
|
4.4 |
|
380 |
|
270 |
|
0.677 |
|
0.311 |
|
0.012 |
|
|||||||||
| 2 | 6.7 |
|
29 |
|
3.30 |
|
4.0 |
|
400 |
|
400 |
|
0.685 |
|
0.301 |
|
0.014 |
|
|||||||||
| 3 | 12.9 |
|
1 |
|
4.08 |
|
4.3 |
|
450 |
|
... | ... | 0.709 |
|
0.279 |
|
0.012 |
|
|||||||||
| 4p a | 20.7 |
|
7 |
|
4.96 |
|
11.7 |
|
1040 |
|
1000 |
|
0.739 |
|
0.252 |
|
0.009 |
|
|||||||||
| 4s a | 15.2 |
|
0 |
|
4.29 |
|
4.6 |
|
... | ... | ... | ... | ... | ... | ... | ... | ... | ... | |||||||||
| 4p b | 20.2 |
|
7 |
|
4.92 |
|
10.9 |
|
960 |
|
1000 |
|
0.770 |
|
0.220 |
|
0.010 |
|
|||||||||
| 4s b | 11.5 |
|
0 |
|
3.93 |
|
3.9 |
|
... | ... | ... | ... | ... | ... | ... | ... | ... | ... | |||||||||
| 4p c | 21.1 |
|
7 |
|
4.98 |
|
11.8 |
|
1040 |
|
1000 |
|
0.769 |
|
0.222 |
|
0.010 |
|
|||||||||
| 4s c | 13.0 |
|
0 |
|
4.08 |
|
4.2 |
|
... | ... | ... | ... | ... | ... | ... | ... | ... | ... | |||||||||
| 5p | 5.2 |
|
48 |
|
2.90 |
|
3.4 |
|
470 |
|
550 |
|
0.660 |
|
0.327 |
|
0.014 |
|
|||||||||
| 5s | 3.5 |
|
49 |
|
2.18 |
|
2.3 |
|
... | ... | ... | ... | ... | ... | ... | ... | ... | ... | |||||||||
| 6p | 10.4 |
|
20 |
|
4.18 |
|
9.7 |
|
510 |
|
530 |
|
0.700 |
|
0.290 |
|
0.011 |
|
|||||||||
| 6s | 11.1 |
|
18 |
|
4.29 |
|
13.4 |
|
... | ... | ... | ... | ... | ... | ... | ... | ... | ... | |||||||||
|
|
|||||||||||||||||||||||||||
| ⊙ a | 0.716 | 0.270 | 0.014 | ||||||||||||||||||||||||
Notes. Uncertainties cover only the effects induced by variations of 2% in Teff and 0.1 dex in log (g) (see Sect. 4.3 for details) and are formally taken to be 99%-confidence limits. Numbering according to Table 4. Owing to the assumption of a homogeneous chemical composition, abundances of the secondary components “s” are tied to the ones of the primaries “p” during the analysis. Parallaxes Π are from Hipparcos (van Leeuwen 2007), while their original formal errors, which are assumed to be 1σ, are converted to 99%-confidence intervals here.
Protosolar nebula values from Asplund et al. (2009).
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