*    http://www.apap-network.org                                                                                          ...
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R-matrix calculations for electron impact excitation and modelling application for coronal plasmas

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Poster presented by Liang et al. at the 17th International Conference on Atomic Processes in Plasmas, Queen's University Belfast, 19-22 July 2011

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R-matrix calculations for electron impact excitation and modelling application for coronal plasmas

  1. 1. * http://www.apap-network.org R-MATRIX CALCULATIONS FOR ELECTRON-IMPACT EXCITATION AND THEIR APPLICATION IN ASTROPHYSICAL PLASMAS GY Liang1,2, N R Badnell 1, G Del Zanna3, H E Mason3, P J Storey4 and G Zhao2 1 Department of Physics, University of Strathclyde, Glasgow, G4 0NG, UK 2 National Astronomical Observatories, CAS, Beijing 100012, China 3 DAMTP, Centre for Mathematical Sciences, Cambridge, CB3 0WA, UK 4 Department of Physics and Astronomy, University College London, London, WC1E 6BT, UK Ⅰ. Motivation: from astrophysical and fusion communities Ⅱ. Method  Radial wave-functions are generated by uisng AUTOSTRUCTURE  Line identification: A large amount of emission lines in EUV and X-ray regions were  R-matrix instead of distorted-wave (DW) method was adopted here, which efficiently takes resonances in observed by spectrometers on space satellites (e.g. Hinode/EIS, Chandra, XMM-Newton) with electron-ion interaction into account high-resolution and high collection area, and will be clarified by IXO mission with much high  Intermediate-coupling frame transformation (ICFT)[1] R-matrix instead of Breit-Pauli and fully relativistic resolution and photon-collecting efficiencies. Dirac (DARC) method  Diagnostics: Many emission lines Advantages: detected by spectrometers show 1. Less-time demanding: consider LS-coupled Hamiltonian 2. Level energy correction with available experimental data potential diagnostics of the ne and Te of 3. Eliminates at root the deficiency of previous LS-bashed methods (e.g. JAJOM) via use of multi-channel quantum defect theory (MQDT) coronal-like hot plasmas. Further 4. Has comparable accuracy with other two kinds of R-matrix methods [1] detailed investigation of coronal 5. Auger and radiation damping via spectator electron (n3, 4 or 5) pathways can easily be taken into account via a optical potential [2] 6. Current ICFT code has been parallelized and has shown to be highly robust structure and heating mechanism of hot-plasmas provide the need for B. R-matrix electron-impact excitation data of four iso-nuclear sulphur ions S8+, S9+, S10+ and S11+ [5] a ccura te a tomic data including BL03 11+ Chianti v6 9+ S excitation cross-section 10 0 S 3-21 D5/2 2 MCHF 10 0 5-50 MCHF NSD07 4-50 MVG95  Atomic physics: Many available 10 -1 10 -1 3-50 5-52 4-52 gf (others) gf (others) excitation data are from poor 10 -2 10 -2 3-52 approximation (e.g. distorted-wave). 3-22 D3/2 2 More accurate method (R-matrix) and 10 -3 10 -3 parallel computation are feasible now 10 -4 10 -4  One of goals of UK APAPAtomic Processes for Astrophysical Plasmas network*: provides excitation -4 -3 -2 -1 0 10 -4 10 -3 10 -2 10 -1 10 0 10 10 10 10 10 gf (present) gf (present) data for iso-electronic sequence across an extensive range of astrophysically relevant elements within 0.04 ICFT 1.00 /ln(Ej/Eij + e) BL03 1-2 2-3 ICFT 1 0.03 2-3 LB94 Effective collision strength () AS-DW 1-3 2-4 0.80 CKA92 R-matrix framework 0.02 Chianti (v6) 1-4 3-4 0.60 LB94 Collision strength () 0.01 1-5 4-5 4-5 0.1 Effective collision strength 0 10 0.40 0.00 Ⅲ. Recent results as part of APAP network 0.20 0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 0.01 1-2 1- lnC/ln(Ej/Eij + C) 0.00 0.12 1 ICFT 1 logTe (K)=5.1 -1 0.10 For a summary of earlier work by the APAP Network , see our presentation in XXVI International 10 logTe (K)=6.1 (peak) 10 ICFT Others vs ICFT logTe (K)=7.1 0.08 1-4 CKA92 10 0 LB94 0.1 0.06 conference on Photonic, Electronic and atomic collisions (ICPEAC 2009)[3] 10 -1 0.04 -2 0.02 1-6 0.01 10 A. R-matrix outer- and inner-shell electron-impact excitation for Li-like iso-electronic sequence with Auger and 10 -2 10 -4 10 -3 10 -2 10 -1 10 0 10 1 10 3 10 4 Temperature (K) 10 5 6 10 0.00 10 3 10 4 10 5 10 6 10 7 10 8 0 5 10 15 20 25 ICFT Scattered energy (Ryd) radiation damping[4] Comparison with results from DW (Bhatia & Landi 2003, left) and from R-matrix Temperature (K) 0.03 The target CI and CC expansions are both taken to be 195 fine-structure levels (89 LS terms) of configurations: method (right) with JAJOM transformational approach (Butler & Zeippen 1994) for S8+ 10 2 a) logTe (K)=5.3 logTe (K)=6.3 b) ICFT LB03 1s2{2,3,4}l and 1s2l{2,3,4}l’ logTe (K)=7.3 AS-DW (9 model) Collision strength  0.06 9+ 0.02 AS-DW (24 model) 0.05 ICFT vs DW logTe (K)=5.2 S 10 1 The resonance state configurations are of the form 1s[2s-4f]2nl (n≥5) and they decay via the following channels: 10 1 logTe (K)=6.2 (peak) 0.04 0.03  logTe (K)=6.7 1s[2s, 2p][2s-4f] nl  1s2[2s-4f] + e- 0.02 ICFT 10 0 (1) The participator KLn/KMn/KNn Auger and radiation 0.01 BR00 0.01 BR00 vs ICFT 0 0.00 BR00 (without pseudo-resonance)  1s2nl + e- 10 (2) pathways (1) and (3) are automatically described in the R- 4 5 6 7 8 -1 10 10 10 10 10 10 Temperature (K)  1s2[2s, 2p][2s-4f] + h 0

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