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 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:
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FileName Lrecl Records Explanations
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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
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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
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Bytes Format Units Label Explanations
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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 2000A&AS..141..285S
62- 70 F9.6 Ry T08 ? Level energy from Tayal, 2008ApJS..178..359T 2008ApJS..178..359T
72- 80 F9.6 Ry FTI06 ? Level energy from Froese Fischer et al.,
2006ADNDT..92..607F 2006ADNDT..92..607F
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 25-Oct-2010