Determination of Nucleosynthetic Yields of Supernovae and Very Massive Stars from Abundances in Metal-Poor Stars

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Abstract
(Abridged) We determine the yields of Na to Ni for Type II supernovae (SNe II) and the yield patterns of the same elements for Type Ia supernovae (SNe Ia) and very massive (>100 M_sun) stars (VMS) using a phenomenological model of stellar nucleosynthesis and the data on a number of stars with -4<[Fe/H]<-3, a single star with [Fe/H]=-2.04, and the sun. We consider that there are two distinct kinds of SNe II: the high-frequency SNe II(H) and the low-frequency SNe II(L). We also consider that VMS were the dominant first-generation stars formed from big bang debris. The yield patterns of Na to Ni for SNe II(H), II(L), and Ia and VMS appear to be well defined. It is found that SNe II(H) produce almost none of these elements, that SNe II(L) can account for the entire solar inventory of Na, Mg, Si, Ca, Ti, and V, and that compared with SNe II(L), VMS underproduce Na, Al, V, Cr, and Mn, overproduce Co, but otherwise have an almost identical yield pattern. A comparison is made between the yield patterns determined here from the observational data and those from ab initio models of nucleosynthesis in SNe II and VMS. The evolution of the other elements relative to Fe is shown to involve three distinct stages, the earliest of which is directly related to the problems of early aggregation and dispersion of baryonic matter. It is argued that the VMS contributions should represent the typical composition of dispersed baryonic matter in the universe.

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