Dielectronic recombination at nebular temperatures.
Abstract
Rate coefficients for dielectronic recombination via lowlying 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.
 Publication:

Monthly Notices of the Royal Astronomical Society
 Pub Date:
 May 1981
 DOI:
 10.1093/mnras/195.1.27P
 Bibcode:
 1981MNRAS.195P..27S
 Keywords:

 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;
 Astrophysics