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J/ApJS/190/322    R-matrix electron-impact excitation of Fe13+  (Liang+, 2010)

R-matrix electron-impact excitation of Fe13+ and its application to the soft X-ray and extreme-ultraviolet spectroscopy of corona-like plasmas. Liang G.Y., Badnell N.R., Crespo Lopez-Urrutia J.R., Baumann T.M., Del Zanna G., Storey P.J., Tawara H., Ullrich J. <Astrophys. J. Suppl. Ser., 190, 322-333 (2010)> =2010ApJS..190..322L
ADC_Keywords: Atomic physics ; Abundances Keywords: atomic data - line: identification - methods: analytical - methods: laboratory - stars: coronae - X-rays: stars Abstract: Accurate excitation parameters are required to interpret the ultraviolet and X-ray spectra of Fe13+. In this work, we use the autostructure code to describe the atomic structure of Fe13+. The 197 lowest-lying fine-structure levels of the 3sx3py3dz(x+y+z=3), 3s24l, and 3s3p4{s,p, and d} configurations are included along with further correlation configurations: 3s3p4f, 3px3dy4l (x+y=2), 3l4l'4l", and 3l3l'5l". The resultant level energies, lifetimes of excited states, and oscillator strengths of transitions between these levels are assessed by comparison with available experimental data and previous calculations. Electron-impact excitation data among these lowest-lying levels are generated using the intermediate-coupling frame transformation R-matrix method. We assess the present results by comparisons with laboratory measurement for the excitation to the metastable level 3s23p2Po3/2 and with available close-coupling calculations for other excitations. Using these data and a collisional-radiative model, we have analyzed soft X-ray and extreme-ultraviolet spectra from space satellite observations of a stellar corona and of solar flares, as well as measurements from an electron beam ion trap. We assess the contribution from Fe13+ emission lines in the solar and Procyon corona observations, and find and identify new lines in the X-ray region observed in the solar and Procyon coronae. The laboratory measurements also confirm that weak lines (218.177Å and 224.354Å) of Fe13+ contribute to the observed intensities in solar observations. The polarization effect due to the directional monoenergetic distribution of the electron energy has been taken into account in comparison with the laboratory measurements. Electron density diagnostics for the astrophysical plasma sources have been performed using the updated data so as to investigate their sensitivity to the atomic data source. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 80 197 Level energies of Fe13+ from different calculations along with available experimentally derived data taken from NIST v3
See also: J/A+A/418/371 : Electron impact excitation of Fe XIII (Aggarwal+, 2004) J/A+A/466/763 : Electron-impact excitation of Fe19+ (Witthoeft+, 2007) J/A+A/511/A78 : Fe XIII electron impact excitation (Storey+, 2010) http://physics.nist.gov/PhysRefData/ASD/index.html : NIST online database Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq Present AUTOSTRUCTURE calculation level order 5- 20 A16 --- Level Level specification 22- 30 F9.6 Ry NIST ? Level energy from NIST data base 32- 40 F9.6 Ry AS Level energy from present AUTOSTRUCTURE calculation 42- 50 F9.6 Ry FAC ? Level energy from present FAC calculation 52- 60 F9.6 Ry SMY00 ? Level energy from Storey et al., 2000A&AS..141..285S 62- 70 F9.6 Ry T08 ? Level energy from Tayal, 2008ApJS..178..359T 72- 80 F9.6 Ry FTI06 ? Level energy from Froese Fischer et al., 2006ADNDT..92..607F
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 25-Oct-2010
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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