Prompt iron enrichment, two r-process components, and abundances in very metal-poor stars

We present a model to explain the wide range of abundances for heavy r-proc ess 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 e arliest condensed clots of matter in order to provide a prompt or initial F e inventory. Subsequent Fe and r-process enrichment was provided by two typ es of supernovae: one producing heavy r-elements with no Fe on a rather sho rt timescale and the other producing light r-elements (A less than or equal to 130) with Fe on a much longer timescale.