Recombination coefficients for the 5g - 4f transitions of O Iii at nebular temperatures and densities

Details Recombination coefficients for the 5g - 4f transitions of O Iii at nebular temperatures and densities Recombination coefficients for the 5g - 4f transitions of O Iii at nebular temperatures and densities

May 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26as..137..157k&link_type=abstract

Astronomy and Astrophysics Supplement, v.137, p.157-163

Astronomy and Astrophysics

Astrophysics

2

Atomic Data, Atomic Processes, Line: Formation, Ism: H Ii Regions, Ism: Planetary Nebulae: General

Scientific paper

We calculate effective recombination coefficients for the formation of the 5g - 4f lines of O Iii 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 \ion{O}{(3+) } 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 5000 - 20 000 K and electron densities, Ne in the range 10(2-10^6) cm(-3) . All tables are available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html

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