We present a model to explain the wide range of abundances for heavy r-process elements (mass number A>130) at low [Fe/H]. This model requires rapid star formation and/or an initial population of supermassive stars in the earliest condensed clots of matter in order to provide a prompt or initial Fe inventory. Subsequent Fe and r-process enrichment was provided by two types of supernovae: one producing heavy r-elements with no Fe on a rather short timescale and the other producing light r-elements (A
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| http://dx.doi.org/10.1086/312455 | DOI Listing |
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