Empirical oxygen abundances and physical conditions for relatively low abundance H II regions

Details Empirical oxygen abundances and physical conditions for relatively low abundance H II regions Empirical oxygen abundances and physical conditions for relatively low abundance H II regions

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...347..883s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 347, Dec. 15, 1989, p. 883-893. Research supported by the Robert A. Welch F

Astronomy and Astrophysics

Astrophysics

108

Abundance, Cosmochemistry, Emission Spectra, H Ii Regions, Interstellar Chemistry, Oxygen, Forbidden Transitions, Interstellar Gas, Ionization, Stellar Temperature, Sulfur

Scientific paper

The utility of the emission-line ratio (3727 + 4959 + 5007 A)/H-beta as an estimate of the total oxygen abundance in H II regions of low abundance (less than 10 percent of the solar value) is discussed. Using both observational data where the 4363A line is measured and model H II regions it is concluded that, for low abundance systems, total oxygen abundances can be determined with an accuracy of + or - 0.2 dex in the absence of a 4363A measurement. An attempt is made to study the average behavior of the stellar effective temperature (Teff) and ionization parameter (U) with changing abundance in low abundance systems. It is shown that some diagnostic methods which are viable for high abundance systems are not capable of uniquely determining Teff and U in low abundance systems. The most promising method of determining Teff and U requires measuring emission lines of forbidden O II, O III, S II, and S III.

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