On the chemical homogeneity of the 30 Doradus H II region and a local enrichment by Wolf-Rayet stars

Details On the chemical homogeneity of the 30 Doradus H II region and a local enrichment by Wolf-Rayet stars On the chemical homogeneity of the 30 Doradus H II region and a local enrichment by Wolf-Rayet stars

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...317..163r&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 317, June 1, 1987, p. 163-172.

Astronomy and Astrophysics

Astronomy

56

Abundance, Emission Spectra, H Ii Regions, Local Group (Astronomy), Nebulae, Stellar Composition, Wolf-Rayet Stars, Chemical Composition, Homogeneity, Line Spectra, Magellanic Clouds, Supernova Remnants

Scientific paper

Emission-line strengths have been obtained at 10 positions in the outer regions of the 30 Dor nebula and analyzed in the standard way. There are two major results: (1) the elemental abundances for nine of the outer regions are remarkably similar to those previously measured in the core. This result implies the spectra of the cores and halos of giant H II regions (subject to the different ionizing radiation fields) are analyzed correctly by the standard methods. Hence measurements of extragalactic H II regions with poor spatial resolution correctly represent the abundances of the whole nebula. The O/H ratio in 30 Dor, by number, is 0.30 solar. The Ne/O, S/O, Ar/O, and Cl/O are close to solar. The gas-phase Fe/O is about 0.2 solar, which probably implies that most of the iron is within solid grains. The He/H is 0.0810 as shown by each of the three strong lines available. One region is cool and rich in helium and all other heavy elements except nitrogen. The spectrum of the region does not resemble that of a supernova remnant in that the forbidden O I and S II lines are not nearly strong enough. The abundances can be explained fairly well as over 10 solar masses of H-poor material ejected during the evolution of a single massive (about 80 solar masses) star during its late O-star and Wolf-Rayet phases.

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