Determination of N/O from far-infrared line observations of Galactic H II regions

Details Determination of N/O from far-infrared line observations of Galactic H II regions Determination of N/O from far-infrared line observations of Galactic H II regions

Apr 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...327..377r&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 327, April 1, 1988, p. 377-388.

Statistics

Computation

71

Abundance, Far Infrared Radiation, Galactic Structure, H Ii Regions, Infrared Spectra, Nitrogen Ions, Oxygen Ions, Astronomical Models, Computational Chemistry, Optics, Stellar Coronas

Scientific paper

The procedure for deriving the N/O abundance ratio in H II regions from far-infrared (FIR) observations of [N III] and [O III] lines yields systematically much higher values than that used to obtain N/O from optical observations of [N II] and [O II] lines. The authors attribute the disparity to two effects that are not accounted for in the standard derivation of N/O by either procedure. New, more precise measurements made from NASA's Kuiper Airborne Observatory are presented of the [O III] 52, 88, and [N III] 57 μm line ratios for six H II regions. The authors apply the "geometry effect" correction as derived from their models to their own and previous FIR data. They find that the N/O ratio for most Galactic H II regions is ≡0.2 - 0.3 rather than the ≡0.05 - 0.1 derived from optical studies, thus raising the average N/O ratio from less than to greater than the solar value of 0.12. This has important implications for comparisons with theories of galactic chemical evolution and heavy element nucleosynthesis.

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