Non-LTE effects on the lead and thorium abundance determinations for
  cool stars
  Knowing accurate Pb abundances of metal-poor stars provides constraints on
the Pb production mechanisms in the early Galaxy. Accurately deriving Th
abundances permits a nucleo-chronometric age determination of the star. We
improve the calculation of the Pb I and Th II lines in stellar atmospheres
based on non-LTE line formation and evaluate the influence of departures from
LTE on Pb and Th abundance determinations through a range of stellar
parameters. Comprehensive model atoms for Pb I and Th II are presented. The
departures from LTE lead to systematically depleted total absorption in the Pb
I lines and positive abundance corrections. Non-LTE removes the discrepancy
between the solar and the meteoritic Pb abundance. With the Holweger & Mueller
(1974) solar model atmosphere, log eps(Pb, non-LTE) = 2.09. We revise the Pb
and Eu abundances of the strongly r-process enhanced (r-II) stars CS 31082-001
and HE 1523-0901 and the Roederer et al. (2010) stellar sample. Our results
provide strong evidence for universal Pb/Eu relative r-process yields during
course of the Galaxy evolution. The stars with -2.3<[Fe/H]< -1.4 have, on
average, 0.51 dex higher Pb/Eu ratios compared with that of the r-II stars
suggesting that the s-process synthesis of Pb started as early as the time when
Galactic metallicity had grown to [Fe/H] = -2.3. The average Pb/Eu ratio of the
-1.4<[Fe/H]< -0.59 stars is close to the solar value, in line with the
predictions of Travaglio et al. (2001) that AGB stars with [Fe/H] ~ -1 provided
the largest contribution to the solar s-nuclei of Pb. Non-LTE leads to weakened
Th II lines. Overall, the abundance correction does not exceed +0.2 dex when
collisions with H I atoms are taken into account in non-LTE calculations.
