Dielectronic recombination at nebular temperatures

Details Dielectronic recombination at nebular temperatures Dielectronic recombination at nebular temperatures

May 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981mnras.195p..27s&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 195, May 1981, p. 27P-31P.

Astronomy and Astrophysics

Astronomy

93

Astronomical Spectroscopy, Carbon Stars, Planetary Nebulae, Recombination Coefficient, Stellar Temperature, Electron States, Ionization Coefficients, Nitrogen Ions, Oxygen Ions, Radiative Transfer, Resonance Lines, Thermodynamic Equilibrium, Transition Probabilities

Scientific paper

Rate coefficients for dielectronic recombination via low-lying resonance states are calculated for the recombined ions C(+), C(2+), N(2+), N(3+) and O(4+) at the temperatures and densities appropriate to planetary nebulae. The total dielectronic recombination coefficients obtained are substantially larger than the corresponding radiative recombination coefficients, calculated neglecting resonances, and differ considerably from the dielectronic recombination coefficients generally in use. Effective recombination coefficients are given for spectrum lines that are formed during the cascade process. Some of these lines have been observed in IUE spectra of planetary nebulae.

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