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a monte carlo simulation for the initialmass function (imf) over the range of mass 0.07--0.5m⊙ was undertaken to constrain the initial chemical composition of the inner regions of the model star at the time of its formation, together with its final chemical composition at the end of the main sequence. a low-mass end of the imf in the range 0.04--0.075m⊙ was adopted to minimize the number of imdf stars. the gaussian shape of the imf was chosen for simplicity, but may be an oversimplification. this imf was compared to the salpeter imf of the same mass range to determine whether a better fit is possible with a different shape. the binary fraction of stars was constrained by the observations, especially the macho data on the galactic bulge. we examined a broad range of initial conditions that could produce acceptable fits. the chemical composition of the inner regions of the star can be written:


where m(m) is the ms mass of the star (mi and mf are the initial and final masses of the star) and the term rsb represents the change in the mass of the star due to any mass loss during the ms phase. the stellar mass is assumed to increase logarithmically with time during the ms phase, and the ms lifetime was taken as 108 yr. concerning the chemical composition, n and c are assumed to be constant throughout the star. the fe-peak elements were assigned initial abundances according to preston et al. ( 2006 ) and the bulk (i.e., non-s-process) $s$-process abundances were set to be a linear interpolation between the initial and final values taken from d'antona and mazzitelli ( 1994 ). for the neutron-capture process (n-capture) s-process, the initial abundances were taken from busso et al. 84d34552a1