Abundance gradients in the Galaxy derived from H II regions

Details Abundance gradients in the Galaxy derived from H II regions Abundance gradients in the Galaxy derived from H II regions

Mar 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...220..516p&link_type=abstract

Astrophysical Journal, Part 1, vol. 220, Mar. 1, 1978, p. 516-524.

Astronomy and Astrophysics

Astrophysics

138

Abundance, Astronomical Spectroscopy, H Ii Regions, Milky Way Galaxy, Planetary Nebulae, Electrophotometry, Emission Spectra, Galactic Structure, Gradients, Heavy Elements, Hydrogen Ions, Line Spectra, Spectrophotometry

Scientific paper

Photoelectric spectrophotometry of emission lines in the 3700-7400-A range is presented for the Eta Carinae nebula, NGC 2359, and NGC 2467. From these observations the chemical abundances of He, N, O, Ne, S, Ar, and Cl relative to hydrogen are derived. These abundances are used, together with those of the Orion Nebula and M8, to obtain abundance gradients across the disk of the Galaxy. The sample covers a galactocentric radial range of about 6 kpc. The values for the oxygen and nitrogen gradients evaluated at the solar distance are d log(O/H)/dR equals -0.13 plus or minus 0.04 per kpc and d log(N/H)/dR equals -0.23 plus or minus 0.06 per kpc. The oxygen gradient is steeper than that derived from planetary nebulae and steeper than the metallicity gradient derived from intermediate-age stars. The nitrogen gradient is similar to that derived from planetary nebulae. The values of the enrichment of helium and nitrogen relative to oxygen are compared with those derived from planetary nebulae and extragalactic H II regions.

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