Abundances of Very Heavy Elements in the Early Galaxy. III.

Details Abundances of Very Heavy Elements in the Early Galaxy. III. Abundances of Very Heavy Elements in the Early Galaxy. III.

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6748c&link_type=abstract

HST Proposal ID #6748

Computer Science

Hst Proposal Id #6748 Cool Stars

Scientific paper

We propose to search for spectral lines indicating the presence of the very heavy elements platinum, iridium, lead and osmium in a very old, metal-poor halo star, and to determine the relative abundances of these elements. These elements, synthesized in stellar interiors by r{apid} and s{low} neutron capture processes, had, until our very recent successful detections in Cycle 5, never before been observed in metal-poor stars because their only strong lines lie in the ultraviolet spectral region. The abundances of these r- and s- process nucleosynthesis products in halo stars, and in particular relative and absolute star-to-star comparisons, will serve to provide important constraints on models of both the early history and chemical evolution of the Galaxy and, indirectly, on the age of the Galaxy and the universe.

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