CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


Fe XIX - VERSION 8.0


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)

436.7540 0.00e+00 2.47e+09 1.01e-03 1.03e-03 1.76e-03 2.46e-03 2s22p33s 1D2 2s22p33p 1F3 16 33 6839076 7068038
592.2350 0.00e+00 1.64e+04 8.92e-02 9.57e-02 4.63e-03 7.91e-08 2s22p4 3P2 2s22p4 1D2 1 4 0 168852
1118.0551 0.00e+00 1.45e+04 8.55e-02 9.49e-02 1.80e-03 2.74e-08 2s22p4 3P2 2s22p4 3P1 1 3 0 89441
1259.2710 0.00e+00 6.37e+02 1.63e-03 1.75e-03 8.46e-05 1.44e-09 2s22p4 3P1 2s22p4 1D2 3 4 89441 168852
1328.9041 0.00e+00 5.04e-01 3.03e-02 1.62e-03 1.85e-08 2.80e-13 2s22p4 3P2 2s22p4 3P0 1 2 0 75250

Created by Giulio Del Zanna on Fri Sep 18 13:27:05 2015