Astron. Astrophys. Suppl. Ser. 137, 157-163
R. Kisielius - P.J. Storey
Send offprint request: P.J. Storey
Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK
Received February 1; accepted February 22, 1999
We calculate effective recombination coefficients for the formation of the 5g - 4f lines of OIII in the intermediate coupling scheme. Photoionization data for the 5g levels calculated using the R-matrix method are used to derive their recombination coefficients. Cascading from higher states is included, allowing for the effects of finite electron density in a hydrogenic approximation. We explicitly include the distribution of population between the two ground levels of O3+ in the calculation of the line intensities. The results are presented as a simple programmeable formula allowing the calculation of recombination line intensities for electron temperatures, in the range K and electron densities, in the range 102-106 cm-3.
Key words: atomic data -- atomic processes -- line: formation -- ISM: H II regions -- ISM: planetary nebulae: general
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