Table 4: Mean values of the derived atmospheric parameters and abundances for the dwarf stars as determined from Methods 1 and 2 ( $\langle\rangle$). Blanks indicate that the equivalent widths could not be reliably measured.
  HD 10780 HD 4628 HD 201091 (61 Cyg)
  Method 1 Method 2 Method 1 Method 2 Method 1b
  N $\langle\rangle$ N $\langle\rangle$ N $\langle\rangle$ N $\langle\rangle$ N $\langle\rangle$
$T_{\rm eff}$ (K)   $5300\pm95$   $5125\pm158$   $5080\pm130$   $4876\pm150$   $4525\pm140$
log g (cm s-2)   $4.13\pm0.23$   $3.79\pm0.35$   $4.59\pm0.26$   $4.12\pm0.28$   $4.65\pm0.25$
$\xi$ (km s-1)   $1.17\pm0.29$   $1.41\pm0.32$   $1.06\pm0.24$   $1.36\pm0.31$   $1.34\pm0.24$
$v\sin i$ (km s-1)       0.6 a       1.7   1.1
${\rm [Fe/H]}$ 25 $-0.10\pm0.10$ 22 $-0.22\pm0.14$ 36 $-0.30\pm0.15$ 32 $-0.42\pm0.18$ 26 $-0.37\pm0.19$
${\rm [O/Fe]}$ 3 $0.13\pm0.09$ 3 $0.34\pm0.12$ 2 $0.27\pm0.23$ 2 $0.51\pm0.22$    
${\rm [Na/Fe]}$         1 $0.04\pm0.06$ 1 $0.05\pm0.08$ 1 $0.10\pm0.06$
${\rm [Mg/Fe]}$         1 $0.31\pm0.04$ 1 $0.42\pm0.02$ 1 $0.02\pm0.04$
${\rm [Al/Fe]}$         2 $0.26\pm0.07$ 2 $0.21\pm0.06$ 2 $0.10\pm0.11$
${\rm [Si/Fe]}$ 3 $-0.01\pm0.07$ 7 $0.05\pm0.10$ 5 $0.02\pm0.15$ 5 $0.13\pm0.15$ 3 $0.07\pm0.12$
${\rm [Ca/Fe]}$ 1 $0.08\pm0.12$ 1 $0.03\pm0.26$ 3 $0.05\pm0.10$ 3 $0.03\pm0.18$ 3 $0.05\pm0.10$
${\rm [Sc/Fe]}$                    
${\rm [Ti/Fe]}$ 1 $-0.02\pm0.07$ 1 $-0.03\pm0.12$ 1 $-0.06\pm0.11$ 1 $0.03\pm0.13$ 1 $0.12\pm0.11$
${\rm [Cr/Fe]}$ 1 $0.08\pm0.10$ 1 $0.04\pm0.15$ 2 $0.03\pm0.10$ 2 $-0.02\pm0.18$ 2 $0.20\pm0.10$
${\rm [Co/Fe]}$ 1 $0.03\pm0.08$ 1 $0.01\pm0.12$ 1 $0.03\pm0.09$ 1 $-0.01\pm0.12$    
${\rm [Ni/Fe]}$ 3 $0.00\pm0.11$ 3 $-0.02\pm0.15$ 4 $-0.06\pm0.12$ 4 $-0.05\pm0.16$ 5 $-0.10\pm0.12$
${\rm [Ba/Fe]}$         1 $-0.25\pm0.31$ 1 $-0.49\pm0.44$ 1 $-0.35\pm0.30$
${\rm [\alpha/Fe]}$   $0.02\pm0.05$       $0.08\pm0.05$       $0.04\pm0.05$
a: From Fekel (1997).
b: Although the approach adopted for the analysis of 61 Cyg A (described in Sect. 4.1) is completely different from the first one, we maintain the notation "Method 1''. We consider the atmospheric parameters ( $T_{\rm eff}$ and $\xi$) obtained in this way, together with the temperature derived from the B-Vindex, which is metallicity-sensitive, as approximate estimates.


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