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A Model for Abundances in Metal-poor Stars

Qian, Y.-Z. and Wasserburg, G. J. (2001) A Model for Abundances in Metal-poor Stars. Astrophysical Journal, 559 (2). pp. 925-941. ISSN 0004-637X. doi:10.1086/322367.

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A model is presented that seeks to explain quantitatively the stellar abundances of r-process elements and other elements associated with the r-process sites. It is argued that the abundances of all these elements in stars with -3 ≾[Fe/H] < -1 can be explained by the contributions of three sources. The sources are the first generations of very massive (≳100 M_☉) stars that are formed from big bang debris and are distinct from Type II supernovae (SNe II) and two types of SNe II, the H and L events, which can occur only at [Fe/H] ≳-3. The H events are of high frequency and produce dominantly heavy (A > 130) r-elements but no Fe (presumably leaving behind black holes). The L events are of low frequency and produce Fe and dominantly light (A ≾ 130) r-elements (essentially none above Ba). By using the observed abundances in two ultra-metal-poor stars and the solar r-abundances, the initial or prompt inventory of elements produced by the first generations of very massive stars and the yields of H and L events can be determined. The abundances of a large number of elements in a star can then be calculated from the model by using only the observed Eu and Fe abundances. To match the model results and the observational data for stars with -3 < [Fe/H] < -1 requires that the solar r-abundances for Sr, Y, Zr, and Ba must be significantly increased from the standard values. No such changes appear to be required for all other elements. If the changes in the solar r-abundances for Sr, Y, Zr, and Ba are not permitted, the model fails at -3 < [Fe/H] < -1 but still works at [Fe/H] ≈ -3 for these four elements. By using the corrected solar r-abundances for these elements, good agreement is obtained between the model results and data over the range -3 < [Fe/H] < -1. No evidence of s-process contributions is found in this region, but all the observational data in this region now show regular increases of Ba/Eu above the standard solar r-process value. Whether the solar r-components of Sr, Y, Zr, and Ba used here to obtain a fit to the stellar data can be reconciled with those obtained from solar abundances by subtracting the s-components calculated from models is not clear.

Item Type:Article
Related URLs:
URLURL TypeDescription
Wasserburg, G. J.0000-0002-7957-8029
Additional Information:© 2001 American Astronomical Society. Received 2001 February 12; accepted 2001 June 7. We wish to thank the reviewers Achim Weiss and an unidentified person for their comments and for suggesting a more extensive treatment of the model. In particular, Achim Weiss has raised several issues requiring discussion. A new data set that appeared after the original submission and two additional data sets are now treated. We have profited greatly from comments and continued enthusiastic support by Roger Blandford and the interest of Marc Kamionkowski. Maurizio Busso has generously given aid and advice on the s-process problems considered here. A conversation with Wal Sargent stimulated our thinking about the mixing problem. This work was supported in part by DOE grants DE-FG02-87ER40328 and DE-FG02-00ER41149 (Y. Z. Q.) and by NASA grant NAG5-4083 (G. J. W.), Caltech Division Contribution 8741(1072).
Funding AgencyGrant Number
Department of Energy (DOE)DE-FG02-87ER40328
Department of Energy (DOE)DE-FG02-00ER41149
Subject Keywords: Galaxy: evolution; stars: abundances; stars: Population II
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Caltech Division of Geological and Planetary Sciences8741
Lunatic Asylum Lab1072
Issue or Number:2
Record Number:CaltechAUTHORS:20131211-110040374
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Official Citation: A Model for Abundances in Metal-poor Stars Y.-Z. Qian and G. J. Wasserburg 2001 ApJ 559 925
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:42955
Deposited By: Ruth Sustaita
Deposited On:11 Dec 2013 19:25
Last Modified:10 Nov 2021 16:30

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