Prediction For The First Generation Stars From A Galactic Halo Chemical Evolution Model With Miller-Scalo Initial Mass Function

A model of supernova-driven chemical evolution of the Galactic halo proposed by Tsujimoto et al. (1999) (TSY) is used to investigate the observations of the first generation stars (FGS). We assume in this paper that a star with a metallicity [Fe/H] less than or equal to -6 is truly a FGS. We obtain FGS probabilities with the Miller-Scalo form of the stellar initial mass function and limit our model parameters to values consistent with the observed metallicity distributions of metal-poor stars in the range of -4.0 < [Fe/H] < -1.0. We find a metallicity distribution function (MDF) of the long-lived halo field stars for [Fe/H] < -1 against the iron abundance in agreement with the observations. If the star formation in the halo is confined to individual gas clouds with masses from 1 10(7) to 1 10(8) M., our model suggests that the probability of identifying FGS in the halo is about 6.14 10(-5) to 6.14 10(-6).