CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


Ti XIV - VERSION 11.0


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]=6.55, 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)

121.9850 2.92e-01 6.54e+10 1.00e+00 1.00e+00 1.00e+00 1.00e+00 2s2.2p5 2P3/2 2s.2p6 2S1/2 1 3 0 819772
129.4410 1.38e-01 2.75e+10 3.96e-01 3.96e-01 3.96e-01 3.96e-01 2s2.2p5 2P1/2 2s.2p6 2S1/2 2 3 47219 819772
2117.7920 0.00e+00 1.86e+03 5.06e-02 5.04e-02 1.18e-04 3.43e-09 2s2.2p5 2P3/2 2s2.2p5 2P1/2 1 2 0 47219

Created by Giulio Del Zanna on Tue Dec 3 13:25:15 2024