Search for Technetium in Barium Stars

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Scientific paper

This proposal will provide a critical test of the hypothesis that the s-process enhancements in both classical and mild barium stars is a consequence of recent mass exchange or mixing. To test this hypothesis, we will search for the lines of ionized technetium (Tc II) at 2543, 2610, and 2647 A. Since all the isotopes of Tc are radioactive and 99 Tc, the isotope produced by the s-process, has a half life of 200,000 years, the mere detection of Tc will establish if the s-process enrichment has occurred relatively recently in these stars. Classical barium stars are now all thought to be binary and the s-process material enrichment is presumed to have occurred during the red giant phase of evolution of-the original primary star. Our search for the lines of Tc II in HD 116713, if successful, would eliminate that possibility. On the other hand, some mild barium stars do not show any indication of a binary nature (e.g. omicron Vir) but do show enhancements of s-process isotopes by a factor of 4. Hence the detection of Tc II lines in this star would definitely establish that the enrichment episode occurred recently. The discovery of differences in the occurrence or strength of technetium would confirm that classical and mild barium stars are two distinct classes of objects whose s-process enrichments come from different sources, and that they do not just represent different ends of a continuous sequence of s-process enhancements.

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