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Chemical Evolution and Extremely Metal-Poor Stars

Published online by Cambridge University Press:  14 August 2015

Andrew McWilliam
Andrew McWilliam*
Affiliation:
Observatories of the Carnegie Institution of Washington 813 Santa Barbara St., Pasadena, CA. 91101, U.S.A. andy@marmite.ociw.edu

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Early abundance studies (e.g. Pagel 1968) showed that neutron-capture heavy elements (Z > 30) are present in halo stars, but deficient relative iron. Truran (1981) argued that at low [Fe/H] the chemical enrichment time scale was shorter than the lifetime of low-mass AGB progenitors, which are the main source of solar system heavy elements. He proposed that in the halo the heavy elements were produced by high mass stars, in type II supernova events (SNII), by rapid neutron capture nucleosynthesis (the r-process).

Spite & Spite (1978) investigated the trend of heavy element abundances with metallicity, from a small sample of halo stars. They found that at [Fe/H]~ -1.5 the halo [heavy element/Fe] ratio is approximately solar; but at lower [Fe/H] there is a roughly linear decrease of [heavy element/Fe] with declining [Fe/H]. Subsequent observations confirmed the general trend of heavy elements in the halo: [M/Fe]~0 down to [Fe/H]~ -2, followed by a linear decline in [M/Fe] to lower [Fe/H] (e.g. Gilroy et al 1988, Lambert 1987).

Additional evidence for the role of SNII in halo heavy element synthesis comes from the trend of [Eu/Fe] with [Fe/H]. Europium is an almost pure r-process element (Käppeler et al. 1989) and its abundance trend with metallicity is similar to the α element trend (e.g. O and Mg made in massive stars). The element ratios show an increase in [M/Fe] as [Fe/H] decreases from 0 to —1; below this point [Eu/Fe] and [α/Fe] remain constant at ~+0.3 dex. For α elements this behavior is thought to be due to the change in the relative contributions from type II SN and type la SN in the disk and halo (Tinsley 1979). The trend for Eu also indicates production by massive stars (e.g. SNII). Near [Fe/H]~ -2.5 Eu appears to decline relative to [Fe/H] (like other heavy elements, but unlike the α elements). This abundance trend has been used to constrain the numerous proposed astrophysical sites of the r-process (e.g. Mathews & Cowan 1990).

Type
II. Joint Discussions
Information
Highlights of Astronomy , Volume 11 , Issue 1: Highlights of Astronomy. As presented at the XXIIIrd General Assembly of the IAU (Part A), 1997 , 1998 , pp. 49 - 52
Copyright
Copyright © Kluwer 1998

References

Audouze, J., & Silk, J. 1995, ApJ, 451, L49 Google Scholar
Baraffe, L., & Takahashi, K. 1993, A&A, 280, 476 Google Scholar
Beers, T.C., Preston, G.W., & Shectman, S.A. 1992, AJ, 103, 1987 Google Scholar
Gilroy, K.K., Sneden, C., Pilachowski, C.A., & Cowan, J.J. 1988, ApJ, 327, 298 Google Scholar
Gratton, R.G., & Sneden, C. 1990, A&A, 234, 366 Google Scholar
Gratton, R.G., & Sneden, C. 1991, A&A, 241, 241 Google Scholar
Gratton, R.G., & Sneden, C. 1994, A&A, 287, 287 Google Scholar
Griffin, R., Griffin, R., Gustafteon, B., & Vieira, T. 1982, MNRAS, 198, 198 Google Scholar
Käppeler, F., Beer, H., & Wieshak, K. 1989. Rep. Prog. Phys., 52, 52 Google Scholar
Lambert, D.L. 1987, Attron. Attrophyi., 8, 8 Google Scholar
Mathews, G.J. & Cowan, J.J. 1990, Nature, 345, 345 Google Scholar
McWilliam, A., Preston, G.W., Sneden, C., & Searle, L. 1995, AJ, 109, 2736 (MPSS95)Google Scholar
McWilliam, A. 1997, AJ, in pressGoogle Scholar
Ostriker, J.P. & Gnedin, N.Y. 1997, ApJ, 486, 486 Google Scholar
Pagel, B.E.J. 1968. In Origin and Dittribution of the Elementi, ed. Ahrens, L.H., pp 195–204 Google Scholar
Ryan, S.G., Norris, J.E., & Beers, T.C. 1996, ApJ, 471, 471 Google Scholar
Ryan, S.G., Norris, J.E., & Bessell, M.S. 1991, AJ, 102, 102 Google Scholar
Searle, L. & McWilliam, A. 1997, in progressGoogle Scholar
Spite, M. & Spite, F. 1978, A&A, 67, 67 Google Scholar
Tinsley, B.M. 1979, ApJ, 229, 229 Google Scholar
Truran, J.W. 1981, A&A, 97, 97 Google Scholar