Determination of nitrogen to carbon abundance ratios from transition layer emission lines

Details Determination of nitrogen to carbon abundance ratios from transition layer emission lines Determination of nitrogen to carbon abundance ratios from transition layer emission lines

Aug 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992uwse.reptq....b&link_type=abstract

Final Report, Sep. 1990 - Aug. 1992 Washington Univ., Seattle.

Astronomy and Astrophysics

Astronomy

Carbon, Emission Spectra, Giant Stars, Nitrogen, Stellar Composition, Stellar Spectra, Supergiant Stars, Ultraviolet Astronomy, Ultraviolet Spectra, Abundance, Anomalies, F Stars, G Stars, Hertzsprung-Russell Diagram, Iue, Main Sequence Stars, Stellar Magnitude

Scientific paper

We have finished studying the nitrogen to carbon abundance ratios for stars with different effective temperatures Teff and luminosities using transition layer emission lines and using spectra available in the IUE archives. The N/C abundance ratio determinations using transition layer emission lines are as accurate as the photospheric abundance determinations as found by comparison of results obtained by both methods for the same stars. Our measurements confirm photospheric abundance determinations in regions of the HR diagram where they can be obtained. Our studies have extended the temperature range to higher temperatures. They have shown the exact positions in the HR diagram where the mixing due to the outer convection zones reaches deep enough to bring nuclear processed material to the surface. This occurs at effective temperatures which are higher by delta log Teff approximately 0.04 or roughly 400 K than expected theoretically. Since the depth of the convection zone increases rapidly with decreasing Teff this may indicate considerable overshoot beyond the lower boundary of the convection zone. Our N/C abundance ratio determinations from transition layer emission lines have confirmed that the actual enrichment observed for some cool giants is larger than expected theoretically, again indicating a larger degree of mixing in several stars either from below or from above. For the supergiants it probably indicates overshoot above the convective core in the progenitor main sequence stars. For the more massive giants this may also be the case, though we did not find a correlation between delta log N/C and the absolute magnitudes, but these are rather uncertain. As byproducts of these studies we also found anomalies in Si/C and N/C abundance ratios for F giants which can be understood as the relict of surface abundance changes for their main sequence progenitors due to diffusion. This anomaly disappears for G giants, for which the depths of the convection zones are apparently deep enough to wipe out these element separations (Bohm-Vitense 1992).

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