Chemical enrichment in halo planetary nebulae

Details Chemical enrichment in halo planetary nebulae Chemical enrichment in halo planetary nebulae

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981rmxaa...6..315t&link_type=abstract

(International Astronomical Union, Reunion Regional Latinoamericana de Astronomia, 2nd, Merida, Venezuela, Jan. 19-23, 1981) Rev

Astronomy and Astrophysics

Astronomy

25

Abundance, Chemical Evolution, Halos, Planetary Nebulae, Stellar Evolution, Astronomical Spectroscopy, Carbon, Electrophotometers, Emission Spectra, Helium, Hydrogen, Line Spectra, Neon, Nitrogen, Oxygen, Spectrophotometry

Scientific paper

Photoelectric spectrophotometry of emission lines in the 3400-7400 A region for the planetary nebula 108-76 deg 1 (BB1) is presented. These observations are then used to derive the relative abundances of H, He, C, N, O, and Ne. The abundances of the halo PN (BB1, H4-1 and K648) are compared with those predicted by stellar evolution theory under the assumption that the envelope has the chemical composition of the matter located between the H burning shell and the surface. The observed He/H and C/O values are found to be higher than predicted, implying that the halo PN contains matter from deeper layers than the H burning shell. Moreover, the O/Ar, N/Ar and Ne/Ar values in the halo are higher than in the solar neighborhood, and at least part of this enrichment is produced by the PN progenitors.

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