Recombination line intensities for hydrogenic ions. II - Case B calculations for C VI, N VII and O VIII

Details Recombination line intensities for hydrogenic ions. II - Case B calculations for C VI, N VII and O VIII Recombination line intensities for hydrogenic ions. II - Case B calculations for C VI, N VII and O VIII

Apr 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.231.1139s&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 231, April 15, 1988, p. 1139-1144.

Statistics

Computation

12

Electron Recombination, Hydrogen Clouds, Particle Collisions, Planetary Nebulae, Abundance, Carbon, H Ii Regions, Nitrogen, Oxygen, Wolf-Rayet Stars

Scientific paper

The intensities of recombination lines formed in extended, optically thin, photoionized plasmas such as those found in PN, H II regions, and winds of certain hot stars are an important source of information on chemical abundances and can sometimes provide estimates of electron temperature. In this paper, the intensities of the recombination lines of C VI, N VII, and O VIII are calculated, accounting for both electron and heavy particle collisions and assuming case B of Baker and Menzel. The computational procedure is explained. The intensities of lines formed by transitions n(u) - n(l) are tabulated for n(u) of 50 or less, n(l) of 29 or less, at log N(e) = 4(1)13 and 10 values of electron temperature in the interval 10,000 K to 500,000 K.

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