Astron. Astrophys. Suppl. Ser.
Volume 137, Number 1, May II 1999
|Page(s)||157 - 163|
|Published online||15 May 1999|
Recombination coefficients for the 5g - 4f transitions of O at nebular temperatures and densities*
Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK
Send offprint request to: P.J. Storey
Accepted: 22 February 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, Te in the range K and electron densities, Ne in the range cm-3.
Key words: atomic data / atomic processes / line: formation / ISM: H ii regions / ISM: planetary nebulae: general
All tables are available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsweb.u-strasbg.fr/Abstract.html
© European Southern Observatory (ESO), 1999