The Abundances of the Iron Group Elements in Early B Stars

Details The Abundances of the Iron Group Elements in Early B Stars The Abundances of the Iron Group Elements in Early B Stars

Feb 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000noao.prop..197p&link_type=abstract

NOAO Proposal ID #2000A-0197

Astronomy and Astrophysics

Astrophysics

Scientific paper

Although knowledge of the abundances of heavy elements is important for computing opacities for stellar evolution calculations and verifying theoretical predictions for explosive nucleosynthesis in massive stars, a cosmic abundance for the Fe group elements (Ti, V, Cr, Mn, Fe, Co, & Ni) has not yet been established for nearby B stars. Using the IUE & Voyager UVS databases, in a project funded by NASA's Astrophysics data Program (ADP), we are determining for the first time the mean abundances of the above elements in nearby early B stars and looking for variations between selected OB associations. Whereas the FUV databases provide the unique line data for the Fe group elements, optical spectra are needed to determine the surface gravities (from the profiles of H(gamma) & H(delta)) and microturbulent parameters (from the N II & O II lines) as well as to verify the star's T_eff and light element abundances that are obtained from the FUV spectra. Optical data are also better-suited for determining abundances of moderately-heavy elements such as P, Cℓ, and Ar. To obtain the necessary complementary ground-based data for our ADP project, we are requesting observing time on the Coude Feed Telescope using Camera 5, Grating A, and the Ford F3KB chip.

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