Theoretical Studies of Dielectronic Recombination of Aluminum-Like Ions

Astronomy and Astrophysics – Astrophysics

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Dielectronic recombination (DR) is an important process occurring in astrophysical plasmas. DR is responsible for the charge state balance as well as the cooling of astrophysical plasmas, and it is the dominant electron-ion recombination process in both photoionized and collisionally-ionized plasmas. Accurate and reliable calculations for DR rate coefficients are needed to analyze the spectra obtained from astrophysical observations. Over the past few years, our group has computed reliable DR data for all isoelectronic sequences up through Mg-like ions using a state-of-the-art multiconfiguration Breit-Pauli (MCBP) distorted wave method. Recently, we have focused our work on the complex third-row M-shell isoelectronic sequences, especially Al-like. Although there exist some DR calculations for S IV, those were performed only within a non-relativistic LS-coupling approximation and for higher temperatures more suitable for collisionally-ionized plasmas but not for the lower temperatures appropriate for photoionized plasmas. Fe XIV DR calculations have been completed and tested against the Heidelberg heavy-ion Test Storage Ring facility measurements. MCBP cross sections and rate coefficients of a wide range of Al-like ions, computed using the AUTOSTRUCTURE suite of atomic structure and collision codes, will be presented. The effect of fine structure splitting in the ground state will be discussed, and comparisons against all available data, theoretical as well as experimental, will be shown. Our results are fitted into a simple formula for easier implementation into modeling codes used by the astrophysics community.
This work was funded in part by NASA (APRA), NASA (SHP) SR&T, and UK PPARC grants.

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