CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


S XIV d - VERSION 5.1


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]=6.80, 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)

64.3142 5.01e-01 1.35e+11 1.76e-03 1.76e-03 1.76e-03 1.76e-03 1s2.3p 2P3/2 1s2.5d 2D5/2 6 20 3286550 4841420
88.7502 6.47e-01 1.37e+11 3.28e-03 3.28e-03 3.28e-03 3.28e-03 1s2.3s 2S1/2 1s2.4p 2P3/2 4 11 3220100 4346860
88.8985 3.23e-01 1.36e+11 1.93e-03 1.93e-03 1.93e-03 1.93e-03 1s2.3s 2S1/2 1s2.4p 2P1/2 4 10 3220100 4344980
417.6611 1.29e-01 1.23e+09 3.11e-02 3.11e-02 3.11e-02 3.11e-02 1s2.2s 2S1/2 1s2.2p 2P3/2 1 3 0 239429
445.7011 6.00e-02 1.01e+09 1.50e-02 1.50e-02 1.50e-02 1.50e-02 1s2.2s 2S1/2 1s2.2p 2P1/2 1 2 0 224366

Created by Giulio Del Zanna on Wed Sep 14 15:47:23 2005