CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


Fe IX - VERSION 4.2


Here you find various information on the brightest lines, ordered in wavelength:
Wavelengths (Angstroms); weighted oscillator strengths (gf); transition probabilities (A); intensities (normalised) at 106 , 1010, 1015, 1020 cm-3; together with:
Configuration; Term; Index of the level (1=ground); Energy (observed if available - otherwise theoretical); of the lower (l) and upper levels (u)
Note that intensities have been calculated at log T[K]=5.80, where the ion fraction peaks in ionization equilibrium. Only lines brighter than 0.001 the strongest line (at all densities) are retained.


Wavelength

gf

Aul

R

R

R

R

Cl

Tl

Cu

Tu

Il

Iu

El

Eu

(A)

(s-1)

(106)

(1010)

(1015)

(1020)

(cm-1)

(cm-1)

171.0730 2.93e+00 2.23e+11 1.00e+00 1.00e+00 1.00e+00 1.00e+00 3p6 1S0/2 3p5.3d 1P2/2 1 13 0 584546
216.1620 0.00e+00 4.05e+01 3.25e-03 6.20e-03 5.61e-07 3.42e-10 3p6 1S0/2 3p5.3d 3D4/2 1 11 0 462616.6
217.1010 5.18e-03 2.44e+08 6.38e-03 2.03e-02 4.97e-02 1.24e-03 3p6 1S0/2 3p5.3d 3D2/2 1 10 0 460616
218.9370 0.00e+00 2.72e+01 3.95e-03 6.41e-03 4.00e-07 2.30e-10 3p6 1S0/2 3p5.3d 1D4/2 1 9 0 456752.7
230.5110 0.00e+00 6.80e-01 3.32e-03 4.55e-04 8.76e-09 5.75e-12 3p6 1S0/2 3p5.3d 3F4/2 1 7 0 433818.8
241.7400 0.00e+00 7.05e+01 6.51e-02 3.58e-02 1.27e-06 5.96e-10 3p6 1S0/2 3p5.3d 3P4/2 1 4 0 413669.2
244.9090 3.09e-04 1.14e+07 1.93e-02 2.82e-02 3.36e-02 5.81e-05 3p6 1S0/2 3p5.3d 3P2/2 1 3 0 408315.1
2384.1919 0.00e+00 1.38e+01 1.63e-03 8.20e-04 2.82e-08 1.50e-11 3p5.3d 3P4/2 3p5.3d 3D6/2 4 8 413669.2 455612.2
2498.8430 0.00e+00 7.09e+01 1.30e-03 1.58e-03 1.35e-07 7.19e-11 3p5.3d 3F8/2 3p5.3d 1F6/2 5 12 425809.8 465828.4

Created by Giulio Del Zanna on Fri Aug 5 13:55:16 2005