Issue 
A&A
Volume 587, March 2016



Article Number  A84  
Number of page(s)  4  
Section  Atomic, molecular, and nuclear data  
DOI  https://doi.org/10.1051/00046361/201527568  
Published online  23 February 2016 
Research Note
Parameterization of the levelresolved radiative recombination rate coefficients for the SPEX code^{⋆}
^{1} SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
email: J.Mao@sron.nl
^{2} Leiden Observatory, Leiden University, Niels Bohrweg 2, 2300 RA Leiden, The Netherlands
Received: 15 October 2015
Accepted: 2 February 2016
The levelresolved radiative recombination (RR) rate coefficients for Hlike to Nalike ions from H (Z = 1) up to and including Zn (Z = 30) are studied here. For Hlike ions, the quantummechanical exact photoionization cross sections for nonrelativistic hydrogenic systems are usedto calculate the RR rate coefficients under the principle of detailed balance, while for Helike to Nalike ions, the archival data on ADAS are adopted. Parameterizations are made for the direct capture rates in a wide temperature range. The fitting accuracies are better than 5% for about 99% of the ~3 × 10^{4} levels considered here. The ~1% exceptions include levels from lowcharged manyelectron ions, and/or highshell (n ≳ 4) levels are less important in terms of interpreting Xray emitting astrophysical plasmas. The RR data will be incorporated into the highresolution spectral analysis package SPEX.
Key words: atomic data / atomic processes
Results of the parameterizations are only available at the CDS via anonymous ftp to cdsarc.ustrasbg.fr (130.79.128.5) or via http://cdsarc.ustrasbg.fr/vizbin/qcat?J/A+A/587/A84
© ESO, 2016
1. Introduction
Some astrophysical plasmas, for instance, the intracluster medium (ICM), are generally not in local temperature equilibrium (LTE). To determine the ionization state of these plasmas, the individual collisional and radiative ionization and recombination processes need to be considered in great detail. The recombination processes can be divided into three subclasses: (resonant) dielectronic recombination (DR), (nonresonant) radiative recombination (RR), and chargeexchange recombination (CXR). Generally speaking, DR is the dominant recombination process for hot plasmas compared with RR for most ions (Bryans et al. 2009). On the other hand, when the temperature of the plasma is low enough for neutral atoms, molecules, and ions to coexist, CXR can be a process that competes with DR (Arnaud & Rothenflug 1985). Nevertheless, RR cannot be ignored at least in some temperature ranges in terms of the total recombination rate. In addition, knowledge of the levelresolved RR rate coefficient is required to calculate the emission line spectrum of astrophysical plasmas, for instance, the collisional ionization equilibrium (CIE) spectrum and the radiative recombination spectrum (Tucker & Gould 1966).
In Sect. 2 we briefly summarize the main points of the previous studies on RR data, focusing on the parameterizations for the total RR rates. In Sect. 3 we show the details of the numerical approaches to derive the RR rate coefficients for Hlike ions. Subsequently, in Sect. 4, we describe to which extent the archival data on ADAS are analyzed for Helike to Nalike ions. Details of the fitting strategy are shown in Sect. 5. Results of the parameterizations, available in CDS, are discussed in Sect. 6.
2. Historical background
Key issues for atomic data are always how precisely the analytical and/or numerical calculations can be made, and how to parameterize the data for a full description, yet in a quick and accurate way.
The SPEX (Kaastra et al. 1996) code, aiming at interpreting highenergy resolution Xray spectra, allows users to make fast (all the calculations are run on the fly) yet adequately accurate analyses, including spectral fitting, plotting, and diagnostic output of the astrophysical plasma. Driven by the practical user experience, the number of mathematical operations used and atomic data storage for the complete description of the basic atomic processes need to be minimized. The SPEX code makes great efforts to parameterize the detailed atomic data as best possible. The parameterization of the levelresolved RR rate coefficients is one of them.
Previously, only the total RR rates were parameterized, and we briefly summarize them here. To begin with, pioneering work was done by Seaton (1959). With the asymptotic expansion of the Gaunt factor, the photoionization cross sections (PICSs) of the hydrogenic ions were derived. And then the total RR rates are fitted with (1)where , Z is the atomic number, and E_{H} is the Rydberg unit of energy.
Aldrovandi & Pequignot (1973) calculated the radiative recombination data for the nonhydrogenic ions of He, C, N, O, Ne, Mg, Si, and S by using the groundstate PICSs from literature and extrapolating along the isoelectronic sequences. Furthermore, a powerlaw (PL) fitting function for the total RR rates was proposed, (2)where A and η are the fitting parameters, and T_{4} is the electron temperature in units of 10^{4} K. The PL model was subsequently also favored by Shull & van Steenberg (1982), Arnaud & Rothenflug (1985), Landini & Monsignori Fossi (1990) and Landini & Fossi (1991).
Pequignot et al. (1991) took advantage of the latest references available at that time for the ground states and part of the excited states (n = 2 or 3) of PICSs, as well as the proper extrapolation and scaling law (analogy with the hydrogenic ions). RR data for H, He, C, N, O, and Ne ions were obtained. The total RR rates were fit to the following expression: (3)where t = T_{4}/Z^{2} and Z is the ionic charge (Z = 1 for recombination toward the neutral state).
Using the HartreeFock wave functions, the standard partial PICSs for subshells (nl) up to 5g of Helike through Allike ions were provided by Clark et al. (1986). Based on this important progress, Arnaud & Raymond (1992) calculated the RR data of Fe^{+ 14} through Fe^{+ 25}. The total RR rates of these iron ions in the temperature range of 10^{5}−10^{8} K were described (with a fitting accuracy better than 5%) by a log parabola function (4)where A,α and β are the fitting parameters. Additionally, Mazzotta et al. (1998) summarized the RR data mentioned above, and more importantly, updated the ionization balance for optically thin plasmas by collecting all the available ionization and recombination (RR + DR) data.
Verner & Ferland (1996a) extended the calculation of the RR data for the radiative recombination toward Hlike, Helike, Lilike, and Nalike ions for all the elements from H up to and including Zn. For the PICSs of the ground states of Helike, Lilike, and Nalike ions, the latest results provided by Verner et al. (1996b) were adopted. For those of the excited states with n ≤ 5 of the highly ionized (at least five times) species, the partial PICSs of Clark et al. (1986) were used. To calculate excited states with n ≤ 10 of the first four ionization states, correction for incomplete shielding (Gould 1978) was required. The hydrogenic approximation was used for the remaining states. We note that a comparison with the Opacity Project (OP) calculations (Seaton et al. 1992) were made, and the conclusion was that the accuracies were better than 10%. The fitting model used for the total RR rates in the temperature range from 3 K to 10^{10} K is (5)where a,b,T_{0}, and T_{1} are the fitting parameters.
Gu (2003) used a distortedwave approximation, similar to the DiracHartreeSlater model used in Verner et al. (1993), to calculate the detailed PICSs with n ≤ 10 for bare through Flike isoelectronic sequences of Mg, Si, S, Ar, Ca, Fe, and Ni. For n> 10 shells the semiclassical Kramers formula was used. The computational procedure of the flexible atomic code (FAC, Gu 2003), which provides not only the RR data, but also other important atomic data, is similar to the fully relativistic distortedwave method of Zhang (1998). Based on the fitting model given by Verner & Ferland (1996a), Gu (2003) used a modified expression to fit the total RR rates in the temperature range from 10^{4} to 10^{4} eV, that is, 10 K to 10^{8} K. Compared to Eq. (5), one necessary modification is that for some elements (e.g., Flike Mg, Olike Mg, Flike Si) parameter b is replaced by , which means that two more parameters b_{1} and T_{2} are required. The fitting accuracies are within 5% for the entire temperature range.
Badnell (2006) used the AUTOSTRUCTURE code (Badnell 1986; Badnell & Seaton 2003) to calculate PICSs, thus the RR data, for all the elements up to and including Zn, plus Kr, Mo, and Xe, for all the isoelectronic sequences up to Nalike forming Mglike in the temperature range of Z^{2}(10^{1}−10^{7}) K, where Z is the atomic number. Similar to Gu (2003), Badnell (2006) adopted Eq. (5) to fit the total RR rates. Likewise, the additional fitting parameters b_{1}and T_{2} are also required for some of the lowcharge ions because of the highly nonhydrogenic screening of the wave functions for the low–nl states in lowcharged manyelectron ions. The fits are accurate to within 5% for singly and doubly ionized ions, and better than 1% for multiply charged ions.
In addition, Nahar and coworkers, for example, Nahar (1999), obtained the total (unified DR + RR) rate coefficients for various ions with their Rmatrix calculations. Meanwhile, adopting most recent RR and DR calculations, Bryans et al. (2006) updated the collisional ionization equilibrium for optically thin plasmas.
Throughout the entire analysis, we refer to the recombined ion when we speak of the radiative recombination of a certain ion.
3. RR rate coefficients for Hlike ions
3.1. Photoionization cross sections
For the hydrogen sequence, the archival data on ADAS are ready to use, with fully nLSJ resolved RR rate coefficients complete up to n = 8. With the calculation details described below, we completed the rate coefficients for all the levels up to n = 16.
The timereversed process of (dielectronic and radiative) recombination is (resonant and nonresonant) photoionization (PI). Therefore, in turn, radiative recombination cross sections (RRCSs) can be obtained through the Milne relation under the principle of detailed balance (or microscopic reversibility) for PICSs. The exact PICS for nonrelativistic hydrogenic systems can be obtained with the quantum mechanical treatment provided by Storey & Hummer (1991, SH91). Their FORTRAN code, based on recursion techniques, yields accurate, stable, and fast numerical evaluations of boundfree PICSs (and boundbound electron dipole transition probability) for nonrelativistic hydrogenic systems with n up to 500. Apparently, PICSs of hydrogenic systems can also be precisely calculated with the AUTOSTRUCTURE (Badnell 1986) code.
When PICSs () are available, RRCSs (, which refers to recombination to the nth shell or to the subshell nl, respectively) can be obtained through the Milne relation under the principle of detailed balance.
Alternatively, if only the total RR rates are needed, since the numerical Maxwellian convolution of the RR rates to n ≥ 100 shells are computationally expensive, the semiclassical Kramers formula of the RRCS can be used instead to save computational time, similar to the approach presented by Gu (2003).
3.2. Radiative recombination data
The n(l)resolved radiative recombination rate coefficients R_{n(l)} can then be calculated by (6)where f(v_{e}) is the probability density distribution of the velocity of the free electrons, and the MaxwellBoltzmann distribution for the free electrons is adopted in the following calculation. Accordingly, the total radiative recombination rates (7)We note that the levelresolved RR rate coefficients can be obtained through the termresolved RR rate coefficients (8)where L is the angular momentum quantum number, S is the spin quantum number, and for Hlike ions S = 1 / 2, and J is the total angular momentum quantum number. This distribution (Eq. (8)) agrees with the ADAS termresolved (LS coupling) and levelresolved (intermediate coupling) RR rate coefficients of the hydrogenic systems with n< = 8.
4. RR rate coefficients for Helike to Nalike ions
For RR rate coefficients of Helike to Nalike ions, the archival RR data of ADAS were used. We note that there are two sets of RR data for each ion: the one calculated with LS coupling is termresolved (or nLS resolved), while the other, calculated with intermediate coupling, is levelresolved (or nLSJ resolved). Only the levelresolved data are analyzed here. Moreover, the ADAS RR data (both LS and intermediate coupling) cover not only radiative recombinations from the ground state of the recombining ion, but also from metastable states. Even more complicated, the ground state is not necessary identical to the ground level. For Clike to Flike ions, there are finestructure levels within the ground term of the recombining ion. For Flike ions, for example, the ground term is (1s^{2}2s^{2}2p^{4},^{3}P), and accordingly, the finestructure levels are (the ground level), and . The RR rate coefficients from the excited finestructure levels are lower than those from the ground level as a result of the additional autoionization pathways (Badnell 2006). We here only carried out the parameterization for RR from the ground level of the recombining ion.
Additionally, all the levels were coded according to intrinsic level indices of SPEX. The advantage is that a set of group numbers are included to distinguish (by different group numbers) those levels with the exact same nLSJ quantum numbers and slightly different configuration for manyelectron ions. For instance, for Olike ions, the electron configuration of 1s^{2}2s^{2}2p^{3}(^{2}P) np (where n ≥3) has a ^{1}P term, where ^{2}P in the parenthesis denotes the coupling of the 2p^{3} electron configuration, but also the electron configuration of 1s^{2}2s^{2}2p^{3}(^{2}D)np.
5. Fitting strategy
For the hydrogenic systems, the RR data are calculated (following SH91) in a wide temperature grid ranging from 10^{1} to 10^{8} K, with ten steps per decade on a log _{10}scale. At even higher temperature T> 10^{8} K, in principle, relativistic effects for the largeZ elements should be taken into account. However, differences that are due to relativistic effects may not play an important role because the RR rate coefficients at high temperature are lower than those at low temperature, and more importantly, lower than the rate coefficients of other processes at high temperature. Therefore, when the RR data for T> 10^{8} K are not calculated, extrapolation to T> 10^{8} K should be feasible. For the Helike to Nalike ions, the temperature sets in z^{2}(10^{1}−10^{7}) K on ADAS were used, where z is the nuclear charge of the recombining ion.
Sherpa^{1} was used for the fitting procedure, with its Simplex (i.e., Neldermead) optimization method. We propose the following model function for the fitting: (9)where the electron temperature T is in units of eV, a_{0, 1} and b_{0, 1} are primary fitting parameters, c_{0} and (a_{2},b_{2}) are additional fitting parameters. The additional parameters were frozen to zero if they were not used. Furthermore, we constrained b_{0−2} to between −10.0 and 10.0 and c_{0} to between 0.0 and 1.0. The initial values of the four primary fitting parameters a_{0, 1} and b_{0, 1} were set to unity together with the two additional fitting parameters a_{2} and b_{2} when these were thawed. Conversely, the initial value of c_{0}, if it was thawed, was set to either side of its boundary, that is, c_{0} = 0.0 or c_{0} = 1.0 (both were performed).
To estimate the goodness of fit, the fits were performed with a set of artificial relative errors (r). We started with r = 1.25%, followed by increasing r by a factor of two, up to and including 5.0%. The chisquared statistics adopted here were (10)where n_{i} is the ith numerical calculation result and m_{i} is the ith model prediction (Eq. (9)).
On the other hand, for the model comparison, the RR data were first fit with the simplest model (i.e., the three additional parameters were frozen to zero), followed by attempted fits with free c_{0} and/or free (a_{2},b_{2}). We used the chisquared distribution for all the fitting statistics, and thawing one additional parameter decreases the degrees of freedom by one; therefore, only if the final statistic (χ^{2}) improves by at least 2.71, 4.61, or 6.25 for one, two, or three additional free parameter(s) (at a 90% confidence level) is the more complicated model favored.
From these attempted fits and considering both the fitting accuracy and simplicity of the model, we determined the bestfit model.
6. Results and discussion
6.1. Total RR rates
The total RR rates, adding up contributions from n = 1 up to n = 10^{4}, for all the Hlike ions considered here can be parameterized with Eq. (9). This also holds for the total RR rates for Helike to Nalike ions, but no significant improvement can be achieved compared to previous results from Badnell (2006).
6.2. Levelresolved RR rate coefficients
The fitting results, available at the CDS, contain the following information: Column 1 lists the isoelectronic sequence number of the recombined ion, Col. 2 gives the atomic number, Cols. 3−9 list the fitting parameters, Cols. 1012 are the degree of freedom (d.o.f.), the final statistics (χ^{2}), and the maximum deviation (δ_{max}). Columns 1316 indicate the nLSJ quantum numbers, and Col. 17 lists the electron configuration. The fitting accuracies are generally better than 5% with the exceptions described below.
The most inaccurate fitting result (δ_{max} = 5.8%) for the helium sequence captures the free electron to the (1s 6p,^{3}P_{0}) level to form Helike copper (Cu XXVIII). As for the lithium sequence, the poorest fitting (δ_{max} = 7.2%) is achieved for the (1s^{2}6s,^{2}S_{1 / 2}) level of Lilike chromium (Cr XXII). In the beryllium sequence, the (1s^{2}2s 8s,^{1}S_{0}) level of the beryllium atom (Be I) deviates most strongly with 7.8%. From the beryllium sequence, the characteristic hightemperature bump for the lowcharged manyelectron ions is present. In the boron sequence, the poorest fitting is the (1s^{2}2s^{2}8s,^{2}S_{1 / 2}) level of the boron atom (B I), with δ_{max} = 12.2%. However, the RR to this level is overwhelmingly dominated by other channels within the same n = 8 shell, except for the hightemperature end. Nevertheless, at the hightemperature end, the high shell RR rate coefficients are merely a few percent lower than those of the low shell. In this case, for instance, at T = 1 keV (or 10^{7} K), the rate coefficient to the n = 8 shell is lower by a few percent than that of the n = 2 shell. Similarly, in the carbon and nitrogen sequences, all the poorly fitted (δ_{max} ≳ 10%) levels of the carbon atom (C I), nitrogen atom (N I) are also dominated by other channels within their corresponding shells. Again, similar arguments hold for the oxygen sequence, not only for the poorly fitted high shell levels of the oxygen atom (O I), but also for the poorly fitted high shell (n ≳ 4) levels from the lowcharged manyelectron ions of Olike fluorine (F II) and Olike neon (Ne III). As expected, similar results are found in the fluorine sequence for the fluorine atom (F I) and Flike neon (Ne II), in the neon sequence, the neon atom (Ne I) and Nelike soldium (Na II), in the sodium sequence, the soldium atom (Na I) and Nalike magnesium (Mg II).
The relative ion fractions of all the neutral atoms are negligible (≲0.005) for a CIE plasma with a plasma temperature as low as 5 eV and assuming the ionization balance of Bryans et al. (2009); we highlighted the ~1% poor fits above. While the ion fraction of the lowcharged manyelectron ions can be ~0.6 in this extreme case, only a few tens of the high shell levels (in total for F II, Ne II, Na II, Mg II, Ne III, etc.) are poorly fitted. In general, a CIE plasma, such as the intracluster medium (ICM) with a temperature of ~1 keV, does not suffer from the poor fits at all. The situation can be difficult for a nonequilibrium ionization (NEI) plasma or a photoionizied plasma, while emission coming from these poorly fitted levels is either too weak or entirely absent in the Xray wavelength range. Introducing more parameters might improve the fitting results, but for simplicity, we did not add more parameters. Alternatively, if emission from the full wavelength range is needed or very high accuracy is required, interpolation with the original ADAS data should be adopted.
7. Summary
We parameterized for the first time the levelresolved radiative recombination rate coefficients for Hlike to Nalike ions from hydrogen up to and including zinc (Z = 30) in a wide temperature range. For the the hydrogen sequence, we calculated the RR data with the photoionization cross sections for nonrelativistic hydrogenic systems provided by Storey & Hummer (1991). The fully nLSJresolved levels are complete up to n = 16 for Hlike ions. For helium to sodium sequences, the archival data from ADAS (Badnell 2006) were adopted, with levels complete up to n = 8. The bulk (~99%) of the 3 × 10^{4} levels are fitted with accuracies better than 5%. The ~1% exceptions that yield relative poor fitting accuracies from 5% to 40% are less important in terms of interpreting Xray emitting astrophysical plasmas.
Together with updated inner shell ionization data (I. Urdampilleta et al., in prep.), a chargeexchange model (Gu et al. 2016) and other atomic data will be included in the upcoming version (3.0) of the highresolution Xray spectral modeling and fitting code SPEX (Kaastra et al. 1996), which will be highly useful once AstroH/SXS data become available.
Acknowledgments
J.J.M. acknowledges discussions and consultations with L. Gu and A. J. J. Raassen. SRON is supported financially by NWO, the Netherlands Organization for Scientific Research.
References
 Aldrovandi, S. M. V., & Pequignot, D. 1973, A&A, 25, 137 [NASA ADS] [Google Scholar]
 Arnaud, M., & Rothenflug, R. 1985, A&AS, 60, 425 [NASA ADS] [Google Scholar]
 Arnaud, M., & Raymond, J. 1992, ApJ, 398, 394 [NASA ADS] [CrossRef] [Google Scholar]
 Badnell, N. R. 1986, J. Phys. B At. Mol. Phys., 19, 3827 [NASA ADS] [CrossRef] [Google Scholar]
 Badnell, N. R. 2006, ApJS, 167, 334 [NASA ADS] [CrossRef] [Google Scholar]
 Badnell, N. R., & Seaton, M. J. 2003, J. Phys. B At. Mol. Phys., 36, 4367 [NASA ADS] [CrossRef] [Google Scholar]
 Bryans, P., Badnell, N. R., Gorczyca, T. W., et al. 2006, ApJS, 167, 343 [NASA ADS] [CrossRef] [Google Scholar]
 Bryans, P., Landi, E., & Savin, D. W. 2009, ApJ, 691, 1540 [NASA ADS] [CrossRef] [Google Scholar]
 Clark, R. E. H., Cowan, R. D., & Bobrowicz, F. W. 1986, Atom. Data Nucl. Data Tables, 34, 415 [NASA ADS] [CrossRef] [Google Scholar]
 Gould, R. J. 1978, ApJ, 219, 250 [NASA ADS] [CrossRef] [Google Scholar]
 Gu, M. F. 2003, ApJ, 589, 1085 [NASA ADS] [CrossRef] [Google Scholar]
 Gu, L., Kaastra, J., & Raassen, A. 2016, A&A, in press, DOI: 10.1051/00046361/201527615 [Google Scholar]
 Landini, M., & Fossi, B. C. M. 1991, A&AS, 91, 183 [NASA ADS] [Google Scholar]
 Landini, M., & Monsignori Fossi, B. C. 1990, A&AS, 82, 229 [NASA ADS] [Google Scholar]
 Kaastra, J. S., Mewe, R., & Nieuwenhuijzen, H. 1996, UV and Xray Spectroscopy of Astrophysical and Laboratory Plasmas, 411 [Google Scholar]
 Mazzotta, P., Mazzitelli, G., Colafrancesco, S., & Vittorio, N. 1998, A&AS, 133, 403 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Nahar, S. N. 1999, ApJS, 120, 131 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Pequignot, D., Petitjean, P., & Boisson, C. 1991, A&A, 251, 680 [NASA ADS] [Google Scholar]
 Tucker, W. H., & Gould, R. J. 1966, ApJ, 144, 244 [NASA ADS] [CrossRef] [Google Scholar]
 Seaton, M. J. 1959, MNRAS, 119, 81 [NASA ADS] [Google Scholar]
 Seaton, M. J., Zeippen, C. J., Tully, J. A., et al. 1992, Rev. Mex. Astron. Astrofis, 23, 19 [NASA ADS] [EDP Sciences] [Google Scholar]
 Shull, J. M., & van Steenberg, M. 1982, ApJS, 48, 95 [NASA ADS] [CrossRef] [Google Scholar]
 Storey, P. J., & Hummer, D. G. 1991, Comput. Phys. Comm., 66, 129 [NASA ADS] [CrossRef] [Google Scholar]
 Verner, D. A., Yakovlev, D. G., Band, I. M., & Trzhaskovskaya, M. B. 1993, Atom. Data Nucl. Data Tables, 55, 233 [NASA ADS] [CrossRef] [Google Scholar]
 Verner, D. A., & Ferland, G. J. 1996, ApJS, 103, 467 [NASA ADS] [CrossRef] [Google Scholar]
 Verner, D. A., Ferland, G. J., Korista, K. T., & Yakovlev, D. G. 1996, ApJ, 465, 487 [NASA ADS] [CrossRef] [Google Scholar]
 Zhang, H. L. 1998, Phys. Rev. A, 57, 2640 [NASA ADS] [CrossRef] [Google Scholar]
Current usage metrics show cumulative count of Article Views (fulltext article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 4896 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.