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

G. J. Wasserburg; Y. Z. Qian

doi:10.1086/312455

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

G. J. Wasserburg, Y. Z. Qian

Physics and Astronomy (Twin Cities)

Research output: Contribution to journal › Article › peer-review

74 Scopus citations

Abstract

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.

Original language	English (US)
Pages (from-to)	L21-L24
Journal	Astrophysical Journal
Volume	529
Issue number	1 PART 2
DOIs	https://doi.org/10.1086/312455
State	Published - Jan 20 2000

Bibliographical note

Funding 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).

Keywords

Galaxy: Evolution
Stars: Abundances
Stars: Population II

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title = "Prompt iron enrichment, two R-process components, and abundances in very metal-poor stars",

abstract = "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.",

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author = "Wasserburg, {G. J.} and Qian, {Y. Z.}",

note = "Funding 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).",

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AU - Qian, Y. Z.

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N2 - 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.

AB - 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.

KW - Galaxy: Evolution

KW - Stars: Abundances

KW - Stars: Population II

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

Abstract

Bibliographical note

Keywords

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