We determine the yields of the elements from 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 ( \gtrsim 100 M _ { \odot } ) stars ( VMS ) using a phenomenological model of stellar nucleosynthesis and the data on a number of stars with -4 \lesssim { [ Fe / H ] } \lesssim - 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 stage is in the domain of [ Fe/H ] < -3 and is governed by VMS activities with some small contributions from SNe II , all of which are dispersed in a dilution mass of M _ { dil } ^ { VMS } \sim 10 ^ { 6 } – 10 ^ { 7 } M _ { \odot } .
The beginning of the second stage is marked by the cessation of VMS activities and the onset of major formation of normal stars ( with masses of \sim 1 – 60 M _ { \odot } ) at [ Fe/H ] \approx - 3 .
The dilution mass for SN II contributions also drops sharply to M _ { dil } ^ { SNII } \approx 3 \times 10 ^ { 4 } M _ { \odot } .
The subsequent quasi-continuous chemical evolution until [ Fe/H ] \sim - 1 is governed by SNe II ( H ) , which produce mainly the heavy r -process elements above Ba , and SNe II ( L ) , which produce essentially all the other elements .
The third stage starts with the onset of SN Ia contributions to mainly the Fe group elements at [ Fe/H ] \sim - 1 .
The domain of [ Fe/H ] > -1 is then governed by contributions from SNe II ( H ) , II ( L ) , and Ia and other low mass stars .
It is shown that the abundances of non-neutron-capture elements in stars with [ Fe/H ] \leq 0 and those of r -process elements in stars with [ Fe/H ] < -1 can be well represented by the sum of the distinct components in the phenomenological model .
The proposed evolutionary sequence is directly related to the problems of early aggregation and dispersion of baryonic matter and to the onset of formation and chemical evolution of galaxies .
It is argued that the prompt inventory governed by VMS contributions should represent the typical composition of dispersed baryonic matter in the universe .