CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


K IV - 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]=5.05, 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)

2594.2830 0.00e+00 6.79e-02 1.84e-03 6.97e-03 6.97e-03 6.97e-03 3s2.3p4 3P2 3s2.3p4 1S0 1 5 0 38546.3
2711.8940 0.00e+00 1.02e+01 2.65e-01 1.00e+00 1.00e+00 1.00e+00 3s2.3p4 3P1 3s2.3p4 1S0 2 5 1671.7 38546.3
4512.1670 0.00e+00 3.18e+00 4.97e-02 1.88e-01 1.88e-01 1.88e-01 3s2.3p4 1D2 3s2.3p4 1S0 4 5 16384 38546.3
6103.5161 0.00e+00 8.39e-01 1.00e+00 2.49e-01 2.43e-01 2.43e-01 3s2.3p4 3P2 3s2.3p4 1D2 1 4 0 16384
6797.0342 0.00e+00 2.03e-01 2.17e-01 5.41e-02 5.29e-02 5.29e-02 3s2.3p4 3P1 3s2.3p4 1D2 2 4 1671.7 16384
59819.3516 0.00e+00 1.04e-01 1.56e-01 2.28e-03 2.22e-03 2.22e-03 3s2.3p4 3P2 3s2.3p4 3P1 1 2 0 1671.7
153964.5938 0.00e+00 1.53e-02 4.29e-03 4.32e-05 4.20e-05 4.20e-05 3s2.3p4 3P1 3s2.3p4 3P0 2 3 1671.7 2321.2

Created by Giulio Del Zanna on Wed Apr 16 17:43:23 2025