CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


K VI - 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]=5.50, 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)

2368.2429 0.00e+00 1.56e+01 3.86e-01 1.00e+00 1.00e+00 1.00e+00 3s2.3p2 3P1 3s2.3p2 1S0 2 5 1133.4 43358.8
2473.3130 0.00e+00 1.16e-01 2.75e-03 7.12e-03 7.12e-03 7.12e-03 3s2.3p2 3P2 3s2.3p2 1S0 3 5 2927.2 43358.8
4101.5542 0.00e+00 3.88e+00 5.55e-02 1.44e-01 1.44e-01 1.44e-01 3s2.3p2 1D2 3s2.3p2 1S0 4 5 18977.8 43358.8
5603.9990 0.00e+00 5.22e-01 5.07e-01 8.32e-02 7.90e-02 7.90e-02 3s2.3p2 3P1 3s2.3p2 1D2 2 4 1133.4 18977.8
6230.2969 0.00e+00 1.14e+00 1.00e+00 1.64e-01 1.56e-01 1.56e-01 3s2.3p2 3P2 3s2.3p2 1D2 3 4 2927.2 18977.8
55747.5703 0.00e+00 7.73e-02 4.46e-01 1.37e-03 1.27e-03 1.27e-03 3s2.3p2 3P1 3s2.3p2 3P2 2 3 1133.4 2927.2
88230.1016 0.00e+00 2.61e-02 2.10e-01 1.78e-04 1.63e-04 1.63e-04 3s2.3p2 3P0 3s2.3p2 3P1 1 2 0 1133.4

Created by Giulio Del Zanna on Wed Apr 16 17:43:20 2025