All Tables
- Table 2:
The configurations used to calculate the radiative data.
The configurations are ordered according to their
relative energies, and grouped by odd or even parity.
- Table 3:
The details of the four most important configurations in
Fe X. The percentage of level mixing (>10%) is indicated
in second column. For example, level 27 is mixed with
level 3 of configuration c2 by 23%.
indicates the best energies (cm-1)
which we propose in this work.
The uncertainties in the energies reflect the
estimated errors in the wavelength measurements.
Levels with uncertain identification are assigned
an uncertainty of 500 cm-1.
The following columns indicate the differences between our
and the energies from NIST
,
the collisional
calculations
,
and the adjusted SS values
.
Levels are ordered according to the
energies
from the collisional calculations.
- Table 4:
Results for the brightest lines in Fe X.
The lines are grouped in three wavelength ranges
(150-300; 300-900 ; 900-20000 Å), and are
displayed in decreasing order of intensity.
Columns 2 and 3 show the relative line intensities (photons)
calculated at T=1 MK and 108, 1012 cm-3,
normalised to the intensity of the brightest
1-30 line (
).
Columns 4 and 5 show the gf and A values calculated
in this work. Column 6 shows, for comparison, the
NIST A values.
The last two columns show the wavelengths corresponding to the
best energies
of Table 3 and the NIST values.
The uncertainties on the proposed wavelengths are derived from the uncertainties
assigned to the energies.
- Table 5:
Measured and predicted lifetimes (ms) for some of the
levels in Fe X.
Measured values are from:
(1) Moehs et al. (2001);
(2) Träbert (2004);
(3) Träbert (1996);
(4) Träbert et al. (2003);
(5) Moehs et al. (2000);
(6) Träbert et al. (2002).
Note the excellent agreement between measured and
predicted lifetimes.
The predicted values have been calculated here
with SUPERSTRUCTURE and adjusted energies.
- Table 6:
Level populations
of the most spectroscopically-important levels
(in decreasing order of level population),
calculated at 1010 cm-3 and T=1 MK.
The first two columns list the
values Nj [cm-3] calculated with the present ion model,
including all excitations between all the 54 levels
(case A), and only excitations from the
first three levels (case B, see also Fig. 2).
The last two columns report, for comparison, the values calculated
by Bhatia & Doschek (1995) [BD] and Pelan & Berrington (2001) [PB]
at a density of 1010 cm-3. The metastable levels are marked M.
- Table 7:
Summary of the line identifications for Fe X
(see the Appendix for details).
The columns indicate:
1) the indexes corresponding to Table 3;
2) the relative intensity (at 108 cm-3), scaled to the brightest line;
3) the wavelengths calculated from our best energies
;
4) observed solar wavelengths
(unless specified otherwise values are from Behring et al. 1976);
some blends are indicated (bl = blend; bl-mr = blend in medium-resolution spectra;
bl-w = blend with a weak line);
lines with no or a tentative identification have a question mark; 5 and 6) previous identifications consistent or not with ours
(with observed wavelengths in Å; note that
observed and calculated wavelengths in the cited literature
can differ from the values reported here).
Legenda:
B = Bromage et al. (1977);
BR = Brooks et al. (1999);
BD = Bhatia & Doschek (1995);
E42 = Edlén (1942);
E = Edlén (1969);
ES = Edlen & Smitt (1978);
FG = Fawcett & Gabriel (1966);
F = Fawcett (1971);
FE = Feldman et al. (1997);
G = Gabriel et al. (1966);
J = Jupen et al. (1993);
JE = Jefferies et al. (1971) (wavelengths in air);
M = Mason & Nussbaumer (1977);
MH = Malinovsky & Heroux (1973);
MC = Magnant-Crifo (1973);
S = Smitt (1977);
SBT = Sandlin et al. (1977);
ST = Sandlin & Tousey (1979);
TN = Thomas & Neupert (1994).