CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


Fe XIX - VERSION 11.0.1


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]=6.95, 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)

592.2350 0.00e+00 1.64e+04 9.19e-02 9.85e-02 4.84e-03 8.53e-08 1s2.2s2.2p4 3P2 1s2.2s2.2p4 1D2 1 4 0 168852
1118.0551 0.00e+00 1.45e+04 8.64e-02 9.59e-02 1.85e-03 2.88e-08 1s2.2s2.2p4 3P2 1s2.2s2.2p4 3P1 1 3 0 89441
1259.2710 0.00e+00 6.37e+02 1.68e-03 1.80e-03 8.83e-05 1.56e-09 1s2.2s2.2p4 3P1 1s2.2s2.2p4 1D2 3 4 89441 168852
1328.9041 0.00e+00 5.04e-01 3.11e-02 1.68e-03 1.93e-08 3.00e-13 1s2.2s2.2p4 3P2 1s2.2s2.2p4 3P0 1 2 0 75250

Created by Giulio Del Zanna on Wed Apr 16 17:42:56 2025