Physics – Atomic Physics
Scientific paper
Jan 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...384..385k&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 384, Jan. 1, 1992, p. 385-389.
Physics
Atomic Physics
23
Cosmic Plasma, Iron, Planetary Nebulae, Atomic Physics, Computational Astrophysics, Plasma Physics, Stellar Physics
Scientific paper
Recent R-matrix calculations of electron impact excitation rates in Fe III, which are significantly different from the earlier results of Garstang, Robb, & Rountree, are used to derive relative populations for the 17 fine-structure levels in the 5D, 3P, 3H, 3F, and 3G states of the 3d6 configuration. Populations are presented for a wide range of electron temperatures (Te = 5000-20,000 K) and densities (Ne = 102-109 cm-3) applicable to astrophysical plasmas. A comparison of theoretical emission-line ratios generated using these results with observational data for the planetary nebulae DDDM-1, Vy 2-2, and NGC 7027 reveals general agreement between theory and observation, with discrepancies that average only 10%. In addition, the present calculations remove the disagreement found between theory and observation for the I(4881 Å)/I(4658 Å) line intensity ratio in DDDM-1 when the theoretical ratios of Garstang et al. are adopted, which provides experimental support for the accuracy of the current results.
Berrington Keith A.
Burke P. G.
Clegg Robin E. S.
Keenan Francis P.
Le Dourneuf M.
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