Abundance Ratios in Extreme Metal-Poor Stars

Details Abundance Ratios in Extreme Metal-Poor Stars Abundance Ratios in Extreme Metal-Poor Stars

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999ap%26ss.265..133m&link_type=abstract

Astrophysics and Space Science, v. 265, Issue 1/4, p. 133-140 (1999).

Astronomy and Astrophysics

Astrophysics

8

Scientific paper

In extremely metal-poor stars ([Fe/H]≤ - 2.5) the neutron capture elementsare characterized by a 300-fold dispersion in M/Fe ratios which decreases with increasing metallicity, the median M/Fe ratio increases with increasing [Fe/H], but the averageM/Fe number ratio is approximately constant. These observations are consistent witha highly dispersed intrinsic yield of neutron-capture elements in supernova (SN) events,and a progression to increasing metallicity by stochastic chemical evolution.The abundance trends indicate that the synthesis of elements heavier thanbarium was dominated by the r-process. The Sr/Ba ratio shows a dispersionwhich suggests a stochastic source of Sr in excess of the r-process value;possibly due to the alpha-rich freeze out.The iron-peak elements Cr, Mn, and Co show non-solar abundance ratios forextreme metal-poor stars, and no measurableintrinsic dispersion relative to iron. We discuss chemical evolution models which explain these observations.

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