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 (Λ ≤ 130) with Fe on a much longer timescale.
Bibliographical noteFunding Information:
We thank Roger Blandford, Wallace Sargent, Charles Steidel, and Stan Woosley for helpful discussions and Roberto Gallino for seeking to keep us on the rich road of Ba and proper mixing. Comments by Al Cameron and John Cowan were very valuable. This work was supported in part by the Department of Energy under grants DE-FG03-88ER-13851 and DE-FG02-87ER40328 and by NASA under grant NAG5-4076, Caltech Division Contribution 8647(1039).
- Galaxy: Evolution
- Stars: Abundances
- Stars: Population II