Issue |
A&A
Volume 500, Number 3, June IV 2009
|
|
---|---|---|
Page(s) | 1263 - 1269 | |
Section | Atomic, molecular, and nuclear data | |
DOI | https://doi.org/10.1051/0004-6361/200911866 | |
Published online | 08 April 2009 |
R-matrix electron-impact excitation data for the Na-like
iso-electronic sequence![[*]](/icons/foot_motif.png)
G. Y. Liang - A. D. Whiteford - N. R. Badnell
Department of Physics, University of Strathclyde, Glasgow, G4 0NG, UK
Received 17 February 2009 / Accepted 26 March 2009
Abstract
We present results for the outer-shell electron-impact
excitation of all Na-like ions from Mg+ to Kr25+ obtained
using the intermediate-coupling frame transformation R-matrix
approach. For each ion's calculation, the target and
close-coupling expansions are both taken to be the 18 LS terms (32 levels) belonging to configurations
,
4l, 5l and 6l (l=0-5). Effective collision strengths
(
s) are presented at temperatures ranging from
K to
K (where q is the
residual charge of ions, i.e. Z-11). Detailed comparisons for
the
s are made with the results of previous calculations
for several ions, which span the sequence. Furthermore, we examine
the iso-electronic trends of both low- and high-temperature
effective collision strengths
Key words: atomic data - atomic processes - plasmas
1 Introduction
Emission lines arising from outer-shell transitions in ions of the sodium iso-electronic sequence are widely detected in astrophysical objects (see e.g. Acton et al. 1985; Thomas & Neupert 1997; Behar et al. 2001; Keenan et al. 2003) using present ground and space observatories. These emission lines are potential diagnostics of the electron temperature and density of coronal-like hot plasmas (Flower & Nussbaumer 1975; Feldman & Doschek 1977). The most frequently observed emission lines in Na-like ions are from Fe15+ in stars, which is due to its large cosmic abundance. Such line identifications and diagnostics in astrophysical spectroscopy require accurate atomic data.
The astrophysical analysis (e.g. for solar flare spectra obtained with the X-ray Spectrometer/Spectrograph Telescope and observation of Capella with the Low-Energy Transmission Grating Spectrometer on the Chandra X-ray observatory) based upon updated R-matrix excitation data for Fe15+ has shown a considerable improvement (Keenan et al. 2007) in recent years over earlier theoretical predictions for the Fe15+ spectrum. The large amount of high-resolution astrophysical spectroscopy available from past, present & future and ground & space observatories and fusion research provides the need for a large set of accurate baseline atomic data (see e.g. Brown et al. 2008; Summers et al. 2002).
To-date, a large amount of excitation data has been calculated
using the distorted-wave (DW) method, using different sizes of
configuration interaction (CI) expansions. Sampson et al. (1990) first reported comprehensive
relativistic DW collision strengths of outer-shell ()
excitations for Na-like ions with
.
The first
R-matrix calculations for outer-shell excitations of the Na-like
iso-electronic sequence were the work of Dufton &
Kingston (1987) for Al2+, Si3+ and S5+, in
which results for excitations among 5-states (3s, 3p, 3d, 4s and
4p) were reported. Kimura et al. (1998) made
extensive (for the 11 terms of 3l, 4l and 5l, l=0-3configurations) LS-coupling R-matrix calculations for Al2+,
Si3+, S5+, Ar7+ and Ca9+. Thereafter, more
elaborate calculations have been performed for several ions. For
example, Eissner et al. (1999) presented
Breit-Pauli R-matrix results for electron-impact excitations
amongst the 12 fine-structure levels of the
configurations of Fe15+; Hudson & Bell (2005)
reported R-matrix results for level-resolved excitations among
the lowest 17 fine-structure levels belonging to 3l, 4l, 5s,
5p and 5d configurations of Al2+ by re-coupling LS-coupling
results via the JAJOM code; Aggarwal & Keenan (2006)
reported results for level-resolved excitations among the
lowest 39 levels amongst the
(
)
configurations
of Fe15+ by using the Dirac atomic R-matrix code DARC.
Due to the advantages (high accuracy and less-time demanding) of the intermediate coupling frame transformation (ICFT) R-matrix codes and the high capability of parallel computer clusters, it is now feasible to provide the excitation data for iso-electronic sequences across the entire range of astrophysical interest within the R-matrix framework (see the work of Witthoeft et al. 2007, for the F-like iso-electronic sequence - Ne+ to Kr27+). Based upon the robustness of the current suite of R-matrix codes, the R-matrix calculation of effective collision strengths currently can be performed automatically for each ion without manual intervention along an iso-electronic sequence. This ensures that each calculation is performed uniformly and reliably. Careful analysis of the results is still essential so as to further validate the accuracy of the data along the sequence.
In the present work, we study the outer-shell electron impact
excitation of Na-like iso-electronic sequence (from Mg+ to
Kr25+), via the ICFT R-matrix approach. In Sect. 2, we
discuss details of the calculational method and compare our
structure results with those of previous calculations, for the
iso-electronic sequence. The excitation results are discussed in
Sect. 3. Our work is a part of ongoing collaborative work - the
UK Atomic Processes for Astrophysical Plasmas (APAP)
network, a broadening of
scope of the original UK RmaX network.
2 Sequence calculation
The aim of this work is to perform R-matrix calculation
employing intermediate-coupling frame transformation (ICFT) method
(see Griffin et al. 1998) for all Na-like ions from Mg+to Kr25+. The details of the calculation for each ion follow
closely to those in the work of Witthoeft et al. (2006)
for Fe19+. In our calculations
we included the following configuration basis set:
[
,
4l, 5l and 6l (l=0-5)
in both the target and close-coupling expansions.
2.1 Structure: levels
The orbital basis functions were obtained from AUTOSTRUCTURE (Badnell 1986) using the Thomas-Femi-Dirac-Amaldi model potential. Relativistic effects were included perturbatively from the one-body Breit-Pauli operators (viz. mass-velocity, spin-orbit and Darwin). The radial scaling parameters were obtained separately for each ion by minimizing the weighted sum of energies of all 18 LS terms.
The resulting energies along the sequence are displayed in Fig. 1a, in which they have been scaled by a factor of 1/(q+1)2 (where q=Z-11 for the Na-like sequence), as well as listed in Table 1 for 13 ions spanning Mg+ to Kr25+.
![]() |
Figure 1: Energy levels for all ions considered. a) The present theoretical energies in units of (q+1)2 Ryd (where q=Z-11). b) Comparison with observed energies listed in NIST v.3 for several levels. |
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In order to maintain consistency and not to introduce arbitrary changes
in comparisons across the sequence, we performed the optimization
procedure automatically in AUTOSTRUCTURE without manual
re-adjustment. So, the energies for the first couple of ions in the
sequences show poorer agreement with available
experimental values (from NIST
v.3)
as shown in Fig. 1b. Coupling to the continuum and
highly-excited bound states would need to be taken account of, either
explicitly via Laguerre pseudo-states or implicitly via a polarization
potential, to improve results here. Thereafter (Z=14),
the agreement is within 1% of NIST values.
2.2 Structure: gf-values
A further test of the accuracy our structure is to compare gf-values with those of other calculations. Our main comparison is with previous sequence calculations of Sampson et al. (1990) for Ti11+-U81+ and Kimura et al. (1998) for Al2+-Ca9+.
The present results show good agreement with those of Sampson et al. (1990), within 10% for
,
e.g. for
the
transitions shown in Fig. 2a. The data of Aggarwal &
Keenan (2006) in Fe15+ are also overlapped for
comparison. For Al2+-S5+, Kimura et al. (1998)
reported the gf-values between LS terms. We partition
statistically - such an assumption is a good one at low nuclear charge.
With increasing charge, of course, this assumption breaks down: the
gf-value ratio
to
deviates from the factor of 2,
changing to
2.5 by Kr25+, as shown in
Fig. 2a. The derived gf-values from Kimura et al.'s
data show poorer agreement with the present AUTOSTRUCTURE
results, and are worse for lower charge, but they are still within
20% as shown in Fig. 2a. The data from the NIST
compilation shows better agreement with the present results (see
Fig. 2a). The transitions decaying from more highly
excited levels, e.g. 4s and 5f (see Fig. 2b), also show
good agreement, to within 20%. For lower-charge ions, the data
from the NIST compilation are compared and show good agreement with
the present AUTOSTRUCTURE results. We also note that there
are spikes and dips for the isoelectronic trend of the gf-values
from NIST, which is due to the different data sources in their
database.
![]() |
Figure 2:
Comparison of gf-values
from the present AUTOSTRUCTURE calculation with those
of previous calculations along the sequence.
a)
|
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![]() |
Figure 3: Scatter plot showing the ratio of gf-values of other workers to the present ones, for transitions from the 5 lowest-lying levels to all levels up to 6g. For Al2+: from Hudson & Bell (2005), denoted by HB05, and from NIST v3. For Fe15+: from Aggarwal & Keenan (2006), denoted by AK06. For Kr25+: from Sampson et al. (1990), denoted by SZF90 and from Younis et al. (2007), denoted by YAE06. The horizontal dash-dotted lines mark agreement of 20%. |
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We make a further complete comparison with the results of previous calculations for three ions which span the sequence, viz. Al2+, Fe15+ and Kr25+, by way of a scatter plot in Fig. 3 (only decays to the 5 lowest-lying levels are shown). For Al2+, the present results agree to within 20% when compared with those available from Hudson & Bell (2005) and NIST's v.3 compilation. For Fe15+, a complete set of data from Aggarwal & Keenan (2006) is available and so more transitions are compared. They show that the present gf-values agree to within 20% for most transitions. For Kr25+, the present results also show good agreement (within 20%) with those given by Sampson et al. (1990, see Fig. 3). However, the data of Younis et al. (2007) show a large scatter.
2.3 Scattering
Our ICFT R-matrix calculations over the sequence used 40
continuum basis per orbital angular momentum. Contributions from
partial waves up to J=12 were included in the exchange
R-matrix calculation. The contribution from higher partial waves
up to J=42 were included via a non-exchange R-matrix
calculation. A ``top-up'' was used to complete the partial collision
strength sum over higher J-values by using the
Burgess (1974) sum rule for dipole transitions and a
geometric series for non-dipole transitions, taking care of the
degenerate limit (Badnell & Griffin 2001). In the F-like
iso-electronic sequence calculations, Witthoeft et al. (2007) repeated the calculation for some ions with
different energy meshes in order to check the convergence of the
effective collision strengths (s) with respect to
resonance resolution. In the outer-region calculation, we adopted
the finer energy meshes of the work of Witthoeft et al. (2007) to ensure the convergence of
s along
the Na-like sequence, see Table 2. Beyond the
resonance region, for the exchange calculation, an energy mesh of
0.01 or 0.005 was used. For the non-exchange calculation, we used
a step of
Ryd over the entire energy range.
The R-matrix calculation was carried out up to an incident
energy of 3 times the ionization potential for each ion. We
then used the infinite energy Born limits (non-dipole allowed)
and line-strengths (dipole-allowed) from AUTOSTRUCTURE so
that the reduced collision strengths (
s), as defined by
Burgess & Tully (1992), are interpolated for all
additional higher energies that are necessary to converge the
Maxwellian-averaging. The effective collision strengths
(
s) at 13 electron temperatures ranging from
K to
K (q=Z-11), are
produced as
the end product of the calculation. The data were stored in the
ADAS adf04 format (Summers 2004).
Table 1: The level energies (Ryd) for ions over the sequence.
Table 2: The energy meshes (in unit of q2, residual charge of ion) used for each ion.
3 Results and discussion
3.1 Comparison with previous results for
and
We compare the present ICFT R-matrix results with those of
previous works for three ions (Al2+, Fe15+and Kr25+) which span the range of astrophysical interest for
the iso-electronic sequence. Aggarwal & Keenan (2006)
noted sudden rises and drops in the
background of the ordinary collision strength ()
in the
Breit-Pauli R-matrix results of Eissner et al. (1999), and suggested it could be a numerical
problem in their adopted code. So, we selected the affected
transition (see the
bottom panel in Fig. 6) as a check. As shown in
Fig. 4a, for Al2+ and Fe15+, our
results show an excellent agreement over the entire temperatures
with the JAJOM and Dirac R-matrix results of Hudson
& Bell (2005) and Aggarwal & Keenan (2006),
respectively. Moreover, there is no sudden jump in the present
ordinary
(see Fig. 6) as reported in the
work of Eissner et al. (1999), which results in a
reduction of
at low temperatures in their results. For
transitions without sudden jumps in their
,
Eissner et al.'s results show good agreement with the present ICFT results
and the DARC results at the low temperature. For example, in
the
transition,
the
is 0.104 (Breit-Pauli), 0.113 (ICFT) and 0.106
( DARC) at
K, respectively.
![]() |
Figure 4:
Comparison of the
present ICFT R-matrix results with those of other workers for several ions
spanning the iso-electronic sequence.
a) Effective collision strengths (
|
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For the highly-charged ion, Kr25+, no R-matrix data and no
data for excitations from n=4 levels are available, to our
knowledge. So the
transition was used to test our calculation against DW. Sampson et al. (1990) presented the DW
s at 6 scaled energies
grids ranging from 1.9 to 306.0 Ryd for Kr25+, from which we
derived the effective collision strengths at several temperatures.
The enhancement of the present ICFT R-matrix results at low
temperatures is due to the resonances near the threshold of the
transition with respect to the non-resonant DW calculations, which
is confirmed by the comparison of the original collision strengths
between the two calculations, as displayed in
Fig. 4b. The background of the present ICFT
R-matrix calculation shows excellent agreement with the DW values
of Sampson et al. (1990). With increasing temperature,
the difference between the two calculations decreases and comes into
close agreement.
By way of a scatter plot of
ratios between the results
of the two different calculations, we make a complete comparison
for the effective collision strengths in Fe15+ at a low
(105 K) and a high (107 K) temperature, see
Fig. 5. At the low temperature, the
Dirac R-matrix results of Aggarwal & Keenan (2006)
are systematically slightly higher than the
present ones. There are 64% and 100% transitions showing
agreement within 20% and a factor of 2, respectively. The weaker
excitations show poorer agreement, for example, excitations with
occupy 91% of the excitations with the
difference over 20%. On increasing the temperature to 107 K,
82% transitions of all points in the scatter plot are in
agreement within 20%. This indicates that the background of the
two R-matrix calculations show agood agreement, and that
indirectly reveals that the structure calculations in the two
works are in agreement again. For those transitions with
differences being larger than 20%, the most likely reason maybe
due to the resolution and/or positioning of near threshold
resonances. In the present sequence calculations, the energy mesh
in the resonance region for Fe15+ is
10-5q2 Ryd (q=15here), which is two times larger than that (0.001 Ryd) used in
work of Aggarwal & Keenan (2006). So, we performed an
additional calculation with a comparable energy mesh (
Ryd)
to that used in the work of Aggarwal & Keenan (2006), which
reveals only a slight improvement in the agreement. Therefore, it
is likely that the differences are mainly from the differences in
near-threshold resonance positions, which results from the two
different structures used. As such, it gives an indication of
current theoretical accuracy.
![]() |
Figure 5:
Scatter
plot showing the ratio of |
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![]() |
Figure 6:
Collision strengths ( |
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In work of Aggarwal & Keenan (2006), the authors
noticed sudden dips in their background
for some
transitions and attributed it to numerical difficulties in
their adopted code. For example, the
transition (see middle panel in
Fig. 6). A check on the
from our calculation
shows that the phenomenon does not appear and the resonance
structure basically agrees with the DARC result (see
Fig. 6). Moreover, no sudden jumps, as reported by
Eissner et al. (1999, see bottom panel in
Fig. 6) appear in the present ICFT R-matrix
results.
3.2 Iso-electronic trends
Following-on the above comparison for ordinary collision strengths,
we examine their Maxwell-averaged effective collision strengths
()
trends along the
iso-electronic sequence. In the F-like iso-electronic sequence studied by
Witthoeft et al. (2007), complicated and periodic
spikes and dips of the effective collision strengths appear at low
temperatures along the iso-electronic sequence. It is of interest to
see if this phenomenon appears in the Na-like iso-electronic sequence.
As noted in the work of Witthoeft et al. (2007), the level
mixing of higher excited levels strongly affects the behaviour of
the s along the sequence. Here, we first examine the
gf-values along the iso-electronic sequence, because the
gf-values should vary smoothly along the sequence. In this way,
we can exclude errors induced from mis-indexing of transitions
resulting from the level mixing for different ions.
![]() |
Figure 7:
Present ICFT R-matrix
effective collision strengths ( |
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In Fig. 7a, we show the effective collision
strengths along the iso-electronic sequence at a temperature of
103(q+1)2,
104(q+1)2 and
105(q+1)2 K for the
transition
.
As
seen in this figure,
varies smoothly along the
iso-electronic sequence. This same behaviour as reported by
Kimura et al. (1998) for their LS-coupling results for
Al2+, Si3+, S5+, Ar7+ and Ca9+, also shown here.
Excellent agreement between the two sets of results is obtained at
both low and high temperatures. For highly-charged ions
(
), Sampson et al. (1990) presented the original
DW collision strengths at 6 scaled energies along the sequence.
Using their data, we derived the
s at the temperatures
of
103(q+1)2 and
104(q+1)2 K. The values at
K are not given because they require contributions
from
at higher energies, i.e. we would have to
extrapolate Sampson et al.'s data. The derived
s
show good agreement with the present R-matrix values, even at the low
temperature, which indicates the resonance contribution is negligible
for this dipole transition. For Fe15+, the Dirac R-matrix results of
Aggarwal & Keenan (2006) are also compared and show good
agreement with the present ones.
On the other hand, see Fig. 7b, a check on a
excitation, for example
,
shows that the
does not vary as smoothly along the
iso-electronic sequence at the low temperature, of
103(q+1)2 K,
but it has weak bumps or dips. This differs from the
iso-electronic trend reported by Kimura et al. (1998).
For their selected ions, the
present results shows good agreement with theirs. At the higher
temperatures,
104(q+1)2 and
105(q+1)2 K, the two sets of
results vary smoothly, and show good agreement. For higher charged
ions, the present
s are significantly higher than those
derived from the relativistic DW
s of Sampson et al. (1990) by nearly a factor of 5 at
K. By
104(q+1)2 K, the
differences decreases to 20%, which is due to the contribution
from strong resonances around the threshold becoming weaker at
higher temperatures. As pointed out by Witthoeft et al. (2007), such spikes and dips along the iso-electronic
sequence at low temperatures are due to the steady shifting of
groups of resonances down to threshold, and below, with increasing
ionic charge. The difference with results derived from Sampson et al.'s work decreases with increasing
,
tending to zero.
Finally, we note that for transitions with strong resonances,
the resonance enhancement
is more important for lower charged ions. The
ratio
along the sequence between the low (
103(q+1)2 K) and high
(
105(q+1)2 K) temperatures clearly demonstrates this
- see Fig. 8. The
resonance contribution reaches a maximum at Si3+, and
decreases again with lower charges.
![]() |
Figure 8:
Ratio of effective
collision strengths ( |
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4 Summary
We have performed 32-level ICFT R-matrix calculations for the outer-shell excitation of the Na-like iso-electronic sequence for all ions from Mg+ to Kr25+.
Good agreement with the results of others for level energies and gf-values for the iso-electronic sequence supports the reliability of the present R-matrix excitation data. This was confirmed specifically, by detailed comparisons of ordinary and effective collision strengths, for Al2+, Fe15+ and Kr25+.
Poorer structure for (
Z=12 - 14) increases the uncertainty of our
excitation data of these ions. A more elaborate R-matrix calculation, e.g. with
pseudostates (RMPS), is necessary to test the present data here.
This exceeds the scope of the present work.
Similarly, fully relativistic calculations may be required for the
upper end of the sequence (
Z=34 - 36). For the rest of the
sequence (
Z=15 - 33), the present excitation data are useful and
reliable for spectroscopy/diagnostic research in the astrophysical
and fusion communities. These data are made available through
archives of APAP website1 in the ADAS adf04 format
(Summers 2004), ADAS and
CHIANTI
.
Furthermore, we examined the iso-electronic trends of the effective collision strengths. A complicated pattern of spikes and dips at low temperatures was noted again along the sequence, which precludes interpolation in Z. An extensive check reveals that the spikes and dips are not significant as that in F-like sequence (Witthoeft et al. 2007). Comparison with the results of previous R-matrix calculations shows good agreement for ions along the sequence. With increasing temperature, the difference between the present ICFT R-matrix and previous DW results decreases. For excitations with strong resonances, the resonance contribution at low temperatures becomes stronger for lower charge ions.
In conclusion, we have generated an extensive set of reliable excitation data utilizing the ICFT R-matrix method. This will update the DW data presently used by the astronomical community and its use may overcome some shortcomings in the present astrophysical modelling, as seen in cases of Mg IX (Del Zanna et al. 2008) and Si X (Liang et al. 2009).
Acknowledgements
The work of the UK APAP Network is funded by the UK STFC under grant No. PP/E001254/1 with the University of Strathclyde.
References
- Acton, L. W., Bruner, M. E., Brown, W. A., et al. 1985, ApJ, 291, 865 [NASA ADS] [CrossRef] (In the text)
- Aggarwal, K. M., & Keenan, F. P. 2006, A&A, 450, 1249 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
- Badnell, N. R. 1986, J. Phys. B: At. Mol. Opt. Phys., 19, 3827 [NASA ADS] [CrossRef] (In the text)
- Badnell, N. R., & Griffin, D. C. 2001, J. Phys. B: At. Mol. Opt. Phys., 34, 681 [NASA ADS] [CrossRef] (In the text)
- Behar, E., Cottam, J., & Kahn, S. M. 2001, ApJ, 548, 966 [NASA ADS] [CrossRef] (In the text)
- Brown, C. M., Feldman, U., Seely, J. F., et al. 2008, ApJS, 176, 511 [NASA ADS] [CrossRef] (In the text)
- Burgess, A. 1974, J. Phys. B: At. Mol. Opt. Phys., 7, L364 [NASA ADS] [CrossRef] (In the text)
- Burgess, A., & Tully, J. A. 1992, A&A, 254, 436 [NASA ADS] (In the text)
- Del Zanna, G., Rozum, I., & Badnell, N. R. 2008, A&A, 487, 1203 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
- Dufton, P. L., & Kingston, A. E. 1987, J. Phys. B: At. Mol. Opt. Phys., 20, 3899 [NASA ADS] [CrossRef] (In the text)
- Eissner, W., Galavís, M. E., Mendoza, Z., et al. 1999, A&AS, 136, 385 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
- Feldman, U., & Doschek, G. A. 1977, J. Opt. Soc. Am., 67, 726 [NASA ADS] [CrossRef] (In the text)
- Flower, D. R., & Nussbaumer, H. 1975, A&A, 42, 265 [NASA ADS] (In the text)
- Griffin, D. C., Badnell, N. R., & Pindzola, M. S. 1998, J. Phys. B: At. Mol. Opt. Phys., 31, 3713 [NASA ADS] [CrossRef] (In the text)
- Hudson, C. E., & Bell, K. L. 2005, A&A, 436, 1131 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
- Keenan, F. P., Katsiyannis, A. C., Brosius, J. W., Davila, J. M., & Thomas, R. J. 2003, MNRAS, 343, 513 [NASA ADS] [CrossRef] (In the text)
- Keenan, F. P., Drake, J. J., & Aggarwal, K. M. 2007, MNRAS, 381, 1727 [NASA ADS] [CrossRef] (In the text)
- Kimura, E., Ohsaki, A., Nakazaki, S., & Itikawa, Y. 1998, A&AS, 132, 99 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
- Liang, G. Y., Whiteford, A. D., & Badnell, N. R. 2009, A&A, 499, 943 [NASA ADS] [CrossRef] [EDP Sciences] DOI: 10.1051/0004-6361/200811423 (In the text)
- Sampson, D. H., Zhang, H. L., & Fontes, C. J. 1990, At. Data and Nucl. Data Tables, 44, 209 [NASA ADS] (In the text)
- Summers, H. P., Badnell, N. R., O'Mullane, M. G., et al. 2002, Plasma Phys. Control. Fusion, 44, B323 [CrossRef] (In the text)
- Summers, H. P. 2004, The ADAS User manual version 2.6, http://www.adas.ac.uk/
- Thomas, R. J., & Neupert, W. M. 1994, ApJS, 91, 461 [NASA ADS] [CrossRef] (In the text)
- Witthoeft, M. C., Badnell, N. R., Del Zanna, G., et al. 2006, A&A, 446, 361 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
- Witthoeft, M. C., Whiteford, A. D., & Badnell, N. R. 2007, J. Phys. B: At. Mol. Opt. Phys., 40, 2969 [NASA ADS] [CrossRef] (In the text)
- Younis, W. O., Allam, S. H., & El-Sherbini, Th. M. 2006, At. Data and Nucl. Data Tables, 92, 187 [NASA ADS] [CrossRef] (In the text)
Footnotes
- ... sequence
- These data are made available in the archives of APAP via http://www.apap-network.org, OPEN-ADAS via http://open.adas.ac.uk as well as anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/500/1263
- ...
network
- http://www.apap-network.org
- ...
v.3
- http://physics.nist.gov/PhysRefData/ASD/levels_form.html
- ... ADAS
- http://www.adas.ac.uk/
- ...
CHIANTI
- http://www.chianti.rl.ac.uk/
All Tables
Table 1: The level energies (Ryd) for ions over the sequence.
Table 2: The energy meshes (in unit of q2, residual charge of ion) used for each ion.
All Figures
![]() |
Figure 1: Energy levels for all ions considered. a) The present theoretical energies in units of (q+1)2 Ryd (where q=Z-11). b) Comparison with observed energies listed in NIST v.3 for several levels. |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
Comparison of gf-values
from the present AUTOSTRUCTURE calculation with those
of previous calculations along the sequence.
a)
|
Open with DEXTER | |
In the text |
![]() |
Figure 3: Scatter plot showing the ratio of gf-values of other workers to the present ones, for transitions from the 5 lowest-lying levels to all levels up to 6g. For Al2+: from Hudson & Bell (2005), denoted by HB05, and from NIST v3. For Fe15+: from Aggarwal & Keenan (2006), denoted by AK06. For Kr25+: from Sampson et al. (1990), denoted by SZF90 and from Younis et al. (2007), denoted by YAE06. The horizontal dash-dotted lines mark agreement of 20%. |
Open with DEXTER | |
In the text |
![]() |
Figure 4:
Comparison of the
present ICFT R-matrix results with those of other workers for several ions
spanning the iso-electronic sequence.
a) Effective collision strengths (
|
Open with DEXTER | |
In the text |
![]() |
Figure 5:
Scatter
plot showing the ratio of |
Open with DEXTER | |
In the text |
![]() |
Figure 6:
Collision strengths ( |
Open with DEXTER | |
In the text |
![]() |
Figure 7:
Present ICFT R-matrix
effective collision strengths ( |
Open with DEXTER | |
In the text |
![]() |
Figure 8:
Ratio of effective
collision strengths ( |
Open with DEXTER | |
In the text |
Copyright ESO 2009
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