Dielectronic Recombination Rate Coefficients for H-like through Ne-like Isosequences of Mg, Si, S, Ar, Ca, Fe, and Ni

Details Dielectronic Recombination Rate Coefficients for H-like through Ne-like Isosequences of Mg, Si, S, Ar, Ca, Fe, and Ni Dielectronic Recombination Rate Coefficients for H-like through Ne-like Isosequences of Mg, Si, S, Ar, Ca, Fe, and Ni

Jun 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003apj...590.1131g&link_type=abstract

The Astrophysical Journal, Volume 590, Issue 2, pp. 1131-1140.

Astronomy and Astrophysics

Astronomy

83

Atomic Data, Atomic Processes

Scientific paper

We present distorted-wave calculations and analytic fits to the dielectronic recombination (DR) rate coefficients of H-like to Ne-like isosequences of seven abundant astrophysical elements, including Mg, Si, S, Ar, Ca, Fe, and Ni. Both ΔN=0 (low-temperature) and ΔN>0 (high-temperature) DR channels are included for L-shell ions. Values of ΔN>0 DR for less abundant ions between Mg and Ni are also obtained through interpolation along the isosequences. Interpolation is not performed for ΔN=0 DR, since such rate coefficients are not smooth along the isosequences in general. Comparison is made with existing theoretical and experimental results, and collisional ionization equilibria resulting from the current DR rate coefficients are presented.

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