CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


Ni XIX - 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]=6.75, 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)

334.3810 1.12e-01 2.30e+09 1.47e-03 1.48e-03 2.62e-03 5.84e-05 2s2 2p5 3s 3P0 2s2 2p5 3p 3D1 4 12 7247699.5 7546760
346.4280 1.78e-01 3.41e+09 2.11e-03 2.11e-03 3.75e-03 8.36e-05 2s2 2p5 3s 3P1 2s2 2p5 3p 3D1 5 12 7258099.5 7546760
348.0510 2.59e-01 2.94e+09 3.22e-03 3.22e-03 8.24e-03 1.67e-04 2s2 2p5 3s 1P1 2s2 2p5 3p 3D2 3 7 7122600 7409914.5
361.3630 2.46e-01 4.27e+09 5.65e-03 5.65e-03 1.89e-02 1.76e-04 2s2 2p5 3s 3P2 2s2 2p5 3p 3S1 2 6 7105259.5 7381989.5
799.3640 0.00e+00 4.58e+04 1.99e-03 1.98e-03 2.45e-05 2.12e-10 2s2 2p5 3s 1P1 2s2 2p5 3s 3P0 3 4 7122600 7247699.5

Created by Giulio Del Zanna on Wed Apr 16 17:43:50 2025