Other
Scientific paper
Sep 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991stin...9211934b&link_type=abstract
Research Report, Oct. 1990 - Sep. 1991 Washington Univ., Seattle.
Other
Abundance, Carbon, Line Spectra, Nitrogen, Spectrum Analysis, Stellar Evolution, Stellar Luminosity, Stellar Spectra, Angular Momentum, Convection, Early Stars, Emission Spectra, F Stars, G Stars, Photosphere, Stellar Composition, Stellar Radiation
Scientific paper
The aim of the proposal was to determine the nitrogen to carbon abundance ratios from transition layer lines in stars with different Teff and luminosities. The equations which give the surface emission line fluxes and the measured ratio of the NV to CIV emission line fluxes are presented and explained. The abundance results are compared with those of photospheric abundance studies for stars in common with the photospheric investigations. The results show that the analyses are at least as accurate as the photospheric determinations. These studies can be extended to F and early G stars for which photospheric abundance determinations for giants are hard to do because molecular bands become too weak. The abundance determination in the context of stellar evolution is addressed. The N/C abundance ratio increases steeply at the point of evolution for which the convection zone reaches deepest. Looking at the evolution of the rotation velocities v sin i, a steep decrease in v sin i is related to the increasing depth of the convection zone. It is concluded that the decrease in v sin i for Teff less than or approximately = 5800 K is most probably due to the rearrangement of the angular momentum in the stars due to deep convective mixing. It appears that the convection zone is rotating with nearly depth independent angular momentum. Other research results and ongoing projects are discussed.
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