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We present the results of determination of the barium abundance considering the non‐local thermodynamic equilibrium (NLTE) effects in 172 dwarf stars in the metallicity range of −1 &lt; [Fe/H] &lt; +0.3, assigned to different Galactic substructures by kinematic criteria. We used a model of the Ba atom with 31 levels of Ba  i  and 101 levels of Ba  ii . The atmosphere models for the investigated stars were computed using the  atlas9  code modified by new opacity distribution functions by Castelli &amp; Kurucz. The NLTE profiles of the unblended Ba  ii  (4554, 5853, 6496 Å) were computed and then compared to those observed. The line 6141 Å was also used, but with an allowance for its correlation with the iron line. The average barium abundances in the thin and thick discs are 0.01 ± 0.08 and −0.03 ± 0.07, respectively. The comparison to the calculations of the Galactic chemical evolution by Serminato et al. was conducted. The trend obtained for the Ba abundance versus [Fe/H] suggests a complex barium production process in the thin and thick discs.

The non‐local thermodynamic equilibrium barium abundance in dwarf stars in the metallicity range of