CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


Ar III - 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]=4.65, 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)

3006.0969 0.00e+00 3.49e-02 1.68e-03 9.10e-03 9.10e-03 9.10e-03 3s2.3p4 3P2 3s2.3p4 1S0 1 5 0 33265.724
3110.0769 0.00e+00 3.97e+00 1.84e-01 1.00e+00 1.00e+00 1.00e+00 3s2.3p4 3P1 3s2.3p4 1S0 2 5 1112.175 33265.724
5193.2622 0.00e+00 2.69e+00 7.48e-02 4.06e-01 4.06e-01 4.06e-01 3s2.3p4 1D2 3s2.3p4 1S0 4 5 14010.004 33265.724
7137.7568 0.00e+00 3.24e-01 1.00e+00 3.34e-01 3.31e-01 3.31e-01 3s2.3p4 3P2 3s2.3p4 1D2 1 4 0 14010.004
7753.2432 0.00e+00 8.44e-02 2.40e-01 7.99e-02 7.93e-02 7.93e-02 3s2.3p4 3P1 3s2.3p4 1D2 2 4 1112.175 14010.004
89913.9062 0.00e+00 3.05e-02 5.78e-02 2.27e-03 2.25e-03 2.25e-03 3s2.3p4 3P2 3s2.3p4 3P1 1 2 0 1112.175
218314.8750 0.00e+00 5.35e-03 1.41e-03 5.38e-05 5.33e-05 5.33e-05 3s2.3p4 3P1 3s2.3p4 3P0 2 3 1112.175 1570.229

Created by Giulio Del Zanna on Wed Apr 16 17:42:13 2025