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The O(2+)/H(+) abundance ratio in gaseous nebulae derived from recombination lines
Peimbert, M.; Storey, P. J.; Torres-Peimbert, S.
AA(Universidad Nacional Autonoma de Mexico, Coyoacan), AB(University College, London, United Kingdom), AC(Universidad Nacional Autonoma de Mexico, Coyoacan)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 414, no. 2, p. 626-631. (ApJ Homepage)
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NASA/STI Keywords:
Abundance, Hydrogen Ions, Line Spectra, Nebulae, Oxygen Ions, Oxygen Spectra, Astronomical Spectroscopy, Forbidden Transitions, H Ii Regions, Interstellar Matter, Orion Nebula, Planetary Nebulae, Recombination Reactions
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We present O(2+)/H(+) values for the Orion Nebula, M17, and NGC 6572 based on O II recombination lines, which are independent of the temperature structure of the observed nebulae. In the H II regions sampled (Orion and M17) the O(2+)/H(+) values derived from O II recombination lines are about a factor of two higher than those derived from O III forbidden lines. These differences can be accounted for by the presence of spatial temperature variations over the observed volumes. The abundances derived from the recombination lines eliminate the O/H discrepancy between the stellar values and the H II region values of the solar neighborhood.

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