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Fig. 9.


Abundances of C, N, Na, and Mg (from bottom to top) in our programme stars are shown as a function of the s-process abundances [s/Fe], where [s/Fe] = ([Sr/Fe] + [Y/Fe] + [Zr/Fe] + [Nb/Fe] + [La/Fe] + [Ce/Fe] + [Pr/Fe] + [Nd/Fe])/8. Predicted values from 2 M models for different metallicities are shown for comparison (symbols defined in Fig. 2).

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