Issue |
Astron. Astrophys. Suppl. Ser.
Volume 137, Number 1, May II 1999
|
|
---|---|---|
Page(s) | 157 - 163 | |
DOI | https://doi.org/10.1051/aas:1999242 | |
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
Received:
1
February
1999
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
© European Southern Observatory (ESO), 1999