All Tables

Table 1: Results obtained from least-square fitting of $\log\epsilon_{\rm nor}(X)$ vs. [Fe/H] of normal stars: $\log\epsilon_{\rm nor}(X)$ = A[Fe/H] + B; "cov'' is the covariance between A and B; "d.o.f.'' is the number of degrees of freedom.
Table 2: Abundances obtained from least-square fittings for normal stars with metallicities corresponding to our sample of barium stars. Each set of five lines corresponds to the normal star with the same metallicity as the barium star indicated in parenthesis. $\log\epsilon(X)$ corresponds to $\log\epsilon_{\rm nor}(X)$ and $\epsilon \sb {\rm s,r,p}(X)$ corresponds to $\epsilon _{\rm s,r,p} (X)_{\rm nor}$ from Eq. (2). $\epsilon _{\rm o}(X)$ is from Eq. (6). The full table is only available in electronic form at the CDS.
Table 3: Abundances [ $\log\epsilon_{\rm nor}$ (X)] of Mo, Dy, Gd, and Pb for normal stars. Symbol "*'' indicates that the column was obtained from a least-square fitting.
Table 6: Results relative to the s-, r-, and p-processes for barium stars. $\epsilon _{\rm s}(X)$ , $\epsilon _{\rm sw}(X)$ , and $\epsilon _{\rm st}(X)$ : abundance fractions of s-process main, weak, and strong components; $\epsilon _{\rm r}(X)$ and $\epsilon _{\rm p}(X)$ : abundance fractions of r- and p-processes; $\sigma N$ and $\sigma N$ (Si): cross-section times abundance fraction corresponding to the s-process main component taking the overabundance of barium stars into account on the usual scale and Si scale; $\epsilon _{\rm s} (X)_{\rm nor}$ : abundance fractions of the s-process main component for normal stars; diff: $\epsilon _{\rm s}(X)- \epsilon _{\rm s}(X)_{\rm nor}$ ; $\sigma N$ $_{\rm gs}$ : cross-section times abundance fraction corresponding to the s-process main component without the overabundance of barium stars. The full table is only available in electronic form at the CDS.
Table 9: s-process indices: s, ls, and hs for the present sample of barium stars.
Table 10: s-process indices s, ls, and hs for barium stars collected in the literature. References: N94 - North et al. (1994); LB91 - Luck & Bond (1991).
Table 4: Cross-sections in mb $\sp {-1}$ for 30, 23, and 8 keV and abundance fractions for s-, r-, and p-processes relative to total abundance and to total abundance of each process.
Table 5: Abundance fractions corresponding to the s-process main component for barium stars calculated with Eq. (8) (upper table) and percentage of abundance (lower table) relative to the s-process main component of a barium star compared to normal stars of a same metallicity ( $\epsilon _{\rm s}(X)/\epsilon _{\rm s}(X)_{\rm nor} \times 100$ ).
Table 7: [X/Eu] ( upper table) and [X/Ba] ( lower table) for the barium stars.
Table 8: Results of neutron exposures. Columns 2 and 3 correspond to results of the fittings to the theoretical predictions of Malaney (1987a) and Cols. 4 to 7 to those of Malaney (1987b). $S\sp 2$ (u), $S\sp 2$ (e8), $S\sp 2$ (e12) are the fit quality, respectively, for single exposure, exponential exposure under neutron density 10 $\sp 8$ cm $\sp {-3}$ , and exponential exposure under neutron density 10 $\sp {12}$ cm $\sp {-3}$ . $\tau _{\rm o}^{\rm a}$ , $\tau _{\rm o}^{\rm b}$ , and $\tau _{\rm o}^{\rm c}$ are the mean distributions of neutron exposure corresponding to $S\sp 2$ (u), $S\sp 2$ (e8), and $S\sp 2$ (e12), respectively. $\tau _{\rm o}$ (f) and $n\sb {\rm n}$ are results corresponding to smaller $S\sp 2$ . Column 10 shows if the best fit corresponds to exponential (exp) or single (sing) exposure. Columns 11 to 13 correspond to the results of the fit of $\sigma N$ curves, with $\chi _{\rm red}$ as the quality of the fit. Numbers in parenthesis are errors in last decimals and were estimated directly from the fittings. The uncertainties on $\tau _{\rm o}^{\rm a}$ , $\tau _{\rm o}^{\rm b}$ , and $\tau _{\rm o}^{\rm c}$ were estimated in 0.1 mb $\sp {-1}$ . For all cases, $\tau _{\rm o}$ is given in mb $\sp {-1}$ .