CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


S I - 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]=4.00, 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)

4508.5659 1.52e-11 5.08e-03 3.32e-04 7.16e-03 7.16e-03 7.16e-03 3s2.3p4 3P2 3s2.3p4 1S0 1 5 0 22180
4590.5459 9.50e-10 3.07e-01 1.97e-02 4.25e-01 4.25e-01 4.25e-01 3s2.3p4 3P1 3s2.3p4 1S0 2 5 396.1 22180
7727.1392 1.15e-08 1.22e+00 4.63e-02 1.00e+00 1.00e+00 1.00e+00 3s2.3p4 1D2 3s2.3p4 1S0 4 5 9238.6 22180
10824.1514 1.98e-09 2.51e-02 1.00e+00 4.79e-01 4.74e-01 4.74e-01 3s2.3p4 3P2 3s2.3p4 1D2 1 4 0 9238.6
11309.0186 6.34e-10 7.46e-03 2.84e-01 1.36e-01 1.35e-01 1.35e-01 3s2.3p4 3P1 3s2.3p4 1D2 2 4 396.1 9238.6
252461.5000 3.61e-08 1.03e-03 1.79e-02 1.80e-03 1.78e-03 1.78e-03 3s2.3p4 3P2 3s2.3p4 3P1 1 2 0 396.1

Created by Giulio Del Zanna on Wed Apr 16 17:44:12 2025