Electron-ion Recombination of Fe XII forming Fe XI: Laboratory Measurements and Theoretical Calculations

O. Novotnỳ (1), N. R. Badnell (2), D. Bernhardt (3), M. Grieser (4), M. Hahn (1), C. Krantz (4), M. Lestinsky (1,5), A. Müller (3), R. Repnow (4), S. Schippers (3), A. Wolf (4), and D. W. Savin (1) ((1) Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA; (2)Department of Physics, University of Strathclyde, Glasgow G4 0NG, UK; (3) Institut für Atom- und Molekülphysik, Justus-Liebig-Universität Giessen, D-35392 Giessen, Germany;  (4) Max Planck Institute for Nuclear Physics, 69117 Heidelberg, Germany; (5) Present address: GSI Helmholtzzentrum für Schwerionenforschung mbH, D-64291 Darmstadt, Germany)

We have measured electron-ion recombination for Fe XII forming Fe XI using a merged beams configuration at the heavy-ion storage ring TSR located at the Max Planck Institute for Nuclear Physics in Heidelberg, Germany. The measured merged beams recombination rate coefficient (MBRRC) for collision energies from 0 to 1500 eV is presented. This work uses a new method for determining the absolute MBRRC based on a comparison of the ion beam decay rate with and without the electron beam on. For energies below 75 eV, the spectrum is dominated by dielectronic recombination (DR) resonances associated with 3s-3p and 3p-3d core excitations. At higher energies we observe contributions from 3-N’ and 2-N’ core excitations DR. We compare our experimental results to state-of-the-art multi-configuration Breit-Pauli (MCBP) calculations and find significant differences, both in resonance energies and strengths. We have extracted the DR contributions from the measured MBRRC data and transformed them into a plasma recombination rate coefficient (PRRC) for temperatures in the range of 10^3 to 10^7 K. We show that the previously recommended DR data for Fe XII significantly underestimate the PRRC at temperatures relevant for both photoionized plasmas (PPs) and collisionaly ionized plasmas (CPs). This is to be contrasted with our MCBP PRRC results which agree with the experiment to within 30% at PP temperatures and even better at CP temperatures. We find this agreement despite the disagreement shown by the detailed comparison between our MCBP and experimental MBRRC results. Lastly, we present a simple parameterized form of the experimentally derived PRRC for easy use in astrophysical modelling codes.

Complete preprint ==> http://arxiv.org/abs/1204.6215

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