CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


Fe X d - VERSION 5.1


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]=6.10, 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)

1.7488 6.04e-02 6.58e+13 1.85e-01 1.85e-01 1.85e-01 1.85e-01 3s2.3p5 2P3/2 1s.3s2.3p6 2S1/2 1 5 0 57182828
1.7493 3.02e-02 3.29e+13 9.27e-02 9.27e-02 9.27e-02 9.27e-02 3s2.3p5 2P1/2 1s.3s2.3p6 2S1/2 2 5 15683.1 57182828
1.9369 4.42e-01 3.93e+14 1.00e+00 1.00e+00 1.00e+00 1.00e+00 2p5.3s2.3p6 2P3/2 1s.3s2.3p6 2S1/2 3 5 5553336.2 57182828
1.9407 2.21e-01 1.96e+14 4.98e-01 4.98e-01 4.98e-01 4.98e-01 2p5.3s2.3p6 2P1/2 1s.3s2.3p6 2S1/2 4 5 5652546.1 57182828

Created by Giulio Del Zanna on Wed Sep 14 15:46:37 2005