CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


Fe XXIV 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]=7.60, 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)

1.8728 1.13e-01 3.58e+13 1.84e-01 1.84e-01 1.84e-01 1.84e-01 1s2.2p 2P3/2 1s2p2(3P) 4P5/2 3 46 520720 53920192
1.8738 3.27e-02 1.55e+13 3.17e-03 3.17e-03 3.17e-03 3.17e-03 1s2.2s 2S1/2 1s2s2p(3P) 4P3/2 1 38 0 53369295
1.8744 2.23e-02 1.06e+13 7.19e-03 7.19e-03 7.19e-03 7.19e-03 1s2.2p 2P3/2 1s2p2(3P) 4P3/2 3 45 520720 53874217
1.8924 9.96e-03 9.27e+12 3.39e-02 3.39e-02 3.39e-02 3.39e-02 1s2.2p 2P1/2 1s2s2 2S1/2 2 36 392000 53237822
1.8970 1.03e-02 9.52e+12 3.47e-02 3.47e-02 3.47e-02 3.47e-02 1s2.2p 2P3/2 1s2s2 2S1/2 3 36 520720 53237822

Created by Giulio Del Zanna on Wed Sep 14 15:43:34 2005