CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


Mg IV - VERSION 6.0


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]=5.20, 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)

320.9950 3.66e-01 1.19e+10 1.00e+00 1.00e+00 1.00e+00 1.00e+00 2s2.2p5 2P3/2 2s.2p6 2S1/2 1 3 0 311532
323.3070 1.81e-01 5.78e+09 4.84e-01 4.84e-01 4.84e-01 4.84e-01 2s2.2p5 2P1/2 2s.2p6 2S1/2 2 3 2228 311532
44883.3867 0.00e+00 1.98e-01 7.16e-02 1.76e-04 1.76e-09 2.00e-12 2s2.2p5 2P3/2 2s2.2p5 2P1/2 1 2 0 2228

Created by Giulio Del Zanna on Fri Sep 4 09:45:53 2009