Experimental dielectronic recombination rate coefficients for Nalike S VI and Nalike Ar VIII
I. Orban^{1}  Z. Altun^{2}  A. Källberg^{3}  A. Simonsson^{3}  G. Andler^{3}  A. Paál^{3}  M. Blom^{3}  P. Löfgren^{3}  S. Trotsenko^{4,5}  S. Böhm^{1}  R. Schuch^{1}
1  Department of Atomic Physics, Stockholm University, 10691 Stockholm, Sweden
2  Department of Physics, Marmara University, 81040 Istanbul, Turkey
3  Manne Siegbahn Laboratory, Stockholm University, 11814 Stockholm, Sweden
4  Gesellschaft für Schwerionenforschung, 64291 Darmstadt, Germany
5  Institut für Kernphysik, Universität Frankfurt, 60486 Frankfurt, Germany
Received 5 February 2009 / Accepted 22 February 2009
Abstract
Context. Absolute recombination rate coefficients for two astrophysically relevant Nalike ions are presented.
Aims. Recombination rate coefficients of S VI and Ar VIII are determined from mergedbeam type experiments at the CRYRING electron cooler. Calculated rate coefficients are used to account for recombination into states that are fieldionized and therefore not detected in the experiment.
Methods. Dielectronic recombination rate coefficients were obtained over an energy range covering
core excitations. For Nalike Ar a measurement was also performed over the
type of resonances. In the lowenergy part of the Ar VIII spectrum, enhancements of more than one order of magnitude are observed as compared to the calculated radiative recombination. The plasma recombination rate coefficients of the two Nalike ions are compared with calculated results from the literature. In the
10^{3}10^{4} K range, large discrepancies are observed between calculated plasma rate coefficients and our data. At higher temperatures, above 10^{5} K, in the case of both ions our data is 30% higher than two calculated plasma rate coefficients, other data from the literature having even lower values.
Results. Discrepancies below 10^{4} K show that at such temperatures even stateoftheart calculations yield plasma rate coefficients that have large uncertainties. The main reason for these uncertainties are the contributions from lowenergy resonances, which are difficult to calculate accurately.
Key words: atomic data  plasmas  Sun: corona  Sun: atoms
1 Introduction
Highly charged ions are abundant in astrophysical plasmas. Recently, 40% of the baryons ``missing'' from the nearby universe were found as ionized intergalactic gas, absorbing in the UV spectral range (Danforth & Shull 2008; Day 2008). About 30% of the missing ions are in photoionized plasma at K and another 10% are in the form of shockheated gas at 10^{5}10^{6} K. The remaining part of the missing baryonic matter is believed to be at even higher temperatures, absorbing in the Xray regime.
Dielectronic recombination (DR) was first recognized by Burgess (1964) as the dominant recombination channel in the Solar corona. DR is a strong recombination channel at plasma temperatures where highly charged ions are common. In the calculation of fractional abundances of various charge states the results depend crucially on the atomic data used as input in the calculations (Bryans et al. 2006). Sulfur and argon are astrophysically abundant elements (Anders & Grevesse 1989), accurate DR rate coefficients for their ions are thus important for the diagnostics and modeling of astrophysical plasmas.
The majority of DR data available in the literature originates from calculations. Generally, for open L and M shell ions the discrepancies between the results of stateoftheart calculations amount to 35% (Bryans et al. 2006). For DR resonances below 13 eV energy, the uncertainties are much higher, due to the inability of modern theory to accurately predict resonance positions, widths and strengths. These uncertainties directly affect the plasma recombination rate coefficients below 10^{4} K. In this range, large differences between calculated and measured rate coefficients are common. The low energy recombination spectra of ions belonging to the same isoelectronic sequence can be very different, even for neighboring elements. Consequently, at low temperatures, no clear Zdependence of the plasma DR exists. Therefore, the spectrum of each relevant ion needs to be evaluated individually, especially when lowenergy DR resonances are present.
Even seemingly insignificant differences in the description of free and bound electron orbitals can lead to large differences in the calculated DR rate coefficients (see e.g. Fu et al. 2008, where depending on the description, 50% difference was observed in the DR rate coefficients of Nelike Mg). Additionally, calculation of the DR spectra of even relatively lowZ and lowcharged ions require relativistic treatment (Mannervik et al. 1998). Storage rings equipped with electron cooler devices presently yield the most accurate lowenergy recombination spectra and can benchmark the different theoretical descriptions.
In this publication we present absolute recombination rate coefficients for two astrophysically relevant Nalike ions, S VI and Ar VIII, measured at the CRYRING electron cooler (Danared et al. 2000). The DR of these ions in the presence of external electric fields has been investigated in another publication (Orban et al. 2009). This paper is organized as follows: In the next section we give a short description of the DR process. In Sect. 3 the experiment and data analysis are presented. We describe the calculations in Sect. 4. Mergedbeam and plasma DR rate coefficients of the two Nalike ions are compared with data available in the literature in Sects. 5.1 and in 5.2, respectively. Our conclusions are given in Sect. 6.
2 Dielectronic recombination
Dielectronic recombination is a resonant recombination channel that takes place through an intermediate doubly excited state (Burgess 1964; Tokman et al. 2002). The first step of DR is dielectronic capture, in which a free electron is attached typically into a Rydberg state of a nonbare ion, with the simultaneous excitation of a core electron.
The energy balance of DR is given by:
i.e., the sum of the kinetic energy and the binding energy of the Rydberg electron equals the excitation energy of the core (initially bound) electron in the presence of the Rydberg electron. We use here the convention of identifying the recombination spectra by the charge state of the ion prior recombination.
3 Experiment
Figure 1: Mergedbeam rate coefficients of a) S VI and b) Ar VIII. Note the different scales on the vertical axis, before and after the axis brake. Experimentally derived spectra are shown by the gray areas. The RR contribution to the experimental spectrum is shown by the hatched area. All solid lines show and all dashed lines show fieldionizationfree AUTOSTRUCTURE DR rate coefficients, scaled to 80%, and summed with the RR contribution. Vertical bars show DR resonance positions, with the principal quantum numbers of the Rydberg electrons above the corresponding bars. The last bar shows the limit of the respective series. The insets show the low energy parts of the spectra in more detail. 

Open with DEXTER 
Recombination spectra of both Nalike ions were measured in separate experiments at the CRYRING storage ring (Abrahamsson et al. 1993), located at the Manne Siegbahn Laboratory in Stockholm, Sweden. The ions were produced in an electron cyclotron resonance ion source and were transported to the storage ring. Following injection and storage on a stable orbit, the S and Ar ions were accelerated in the storage ring to energies of 74 MeV and 115 MeV, respectively. Following acceleration, about 1.4 10^{6} S^{5+} and 10^{6} Ar^{7+} ions were circulating in the ring. In the electron cooler, a lowtemperature electron beam was merged with the stored ions over an interaction length of 0.8 m. The ion beam was electron cooled for 2 s with a velocity matched, cold electron beam. Following electron cooling, the electron energy was scanned in a zigzag pattern. First, the electron energy was increased in order to cover the electronion collisionenergy range of DR resonances associated with excitation of the 3s core electron within the same n=3 shell ( type DR), up to the 3pnl series limit. Then the electron energy was decreased through the ionelectron velocitymatch condition and the same collision energy range was covered with electrons slower than the ions. The electron energy was then scanned back to the velocity match cooling condition. After the electron energy scan, the ions were dumped and a new ioninjection was performed. After the measurement of the type DR resonances, the DR spectrum of Ar VIII covering the type of DR resonances was also measured. The energy scan over this range was performed only with electrons faster than the ions.
During the measurements, the electron current was kept constant, with electron densities at cooling energy, of 4 10^{6} and 7.9 10^{6} in case of the S VI and Ar VIII experiments, respectively. Recombined ions were separated from the stored beam in the first dipole magnet after the electron cooler and were detected by a surface barrier silicon detector with unity efficiency.
Motional electric fields at the dipole magnet fieldionized Rydberg states with the principle quantum number higher than in the S VI experiment and in the Ar VIII experiment. A fraction of the ions recombined into highn states decayed below before arriving at the dipole magnet. These ions were not fieldionized and their contribution can be observed in the experimental spectra above the energy corresponding to the fieldionization limits (see Fig. 1). Hereafter, data affected by fieldionization will be referred to as rate coefficients.
Mergedbeam recombination rate coefficients were obtained from the energydependent count rates, with a similar procedure as described in DeWitt et al. (1996) and in Zong et al. (1997). Corresponding electronion collision energies were calculated using spacecharge corrected electron and dragforce corrected ion energies.
4 AUTOSTRUCTURE calculations
Calculations were carried out within the isolated resonance approximation. The AUTOSTRUCTURE code (Badnell 1986) was used to obtain levelresolved DR cross sections in a multiconfiguration intermediate coupling BreitPauli (MCBP) approximation. Both and core excitations from the ground state were considered. Radiative stabilization of the doubly excited states through both the decay of the excited core and the decay of the Rydberg electron was considered. For coreexcitations, the calculated series limits were adjusted to match the corresponding 3s 3p coreexcitation energies from the NIST evaluated database (Ralchenko et al. 2008).
In the case of type DR, all Rydberg orbitals were explicitly included up to n = 30 and l = 15, and a quantumdefect theory approximation was used for higher levels, up to n = 1000 (Badnell et al. 2003). In the case of core excitations, leading to excited states ( excitations), Rydberg states with and were described explicitly, whereas for excited states ( excitations), Rydberg states with and were calculated explicitly. Again, for higher levels up to n=1000, approximations were used.
Calculations including only states up to the experimental fieldionization limits were also performed (see solid curves in Fig. 1). These curves contain contributions arising from ions that initially recombined into states above the fieldionization limit, but decayed below before arriving at the dipole magnet, as explained in Sect. 3.
In order to compare with the experimentally derived rate coefficients, the calculated cross sections
were multiplied by the average electron velocity
and were convoluted with the electron velocity distribution from the experiment:
where is the mergedbeam rate coefficients and is the anisotropic Maxwellian velocity distribution (DeWitt et al. 1996) characterizing the electron beam in the mergedbeam interaction region, with = 1 meV transversal and T_{} = 0.2 meV longitudinal temperatures.
5 Results and discussion
In order to have a more transparent presentation of our results, we distinguish between the mergedbeam and plasma recombination spectra. The mergedbeam recombination spectra show the resonant peak structure of the DR spectrum as a function of electronion interaction energy. The plasma rate coefficients show the DR rate coefficients as a function of plasma temperature and contain at each temperature contributions from a large number of DR channels, with strengths weighted by the electron energy distribution characteristic for that particular temperature. The mergedbeam and plasma recombination spectra are discussed in the next two sections.
5.1 Mergedbeam rate coefficients
Experimentally derived mergedbeam recombination rate coefficients and AUTOSTRUCTURE results for Nalike S and Nalike Ar, over the energy range of the DR resonances, are shown in Fig. 1. Quantum mechanically, radiative recombination (RR) and DR into the same final states are indistinguishable processes and can interfere. However, interferences between RR and DR have been shown to be usually negligible. Thus treating RR and DR separately is to a first approximation correct (Pindzola et al. 1992). The RR contributions to the experimentally determined recombination spectra, shown by the hatched areas in Fig. 1, were estimated using the Bethe & Salpeter (1957) formula, corrected by the Gaunt factors (Lindroth & Schuch 2003) for recombination into lown states.
In order to compare with the experimentally derived rate coefficients, the AUTOSTRUCTURE rate coefficients were multiplied by 0.8 in the case of both ions and were added to the RR contribution. Such differences between calculated rate coefficients and measured spectra are not uncommon (see e.g. Schippers et al. 2001) and are here at the limit of the experimental systematic uncertainties. DR resonance positions shown by the vertical bars were calculated using Eq. (1), where the binding energy of the Rydberg electrons were estimated with:
where Ry is the Rydberg constant, and Q is the ionic charge. Toward higher energies, DR peaks of the type are positioned increasingly closer to each other and overlap, creating a pileup at the series limit. In the spectrum of S VI, DR peaks belonging to the and series are separated by 156,7 meV (Ralchenko et al. 2008) and are only resolved at low energies, whereas the 336.8 meV fine structure splitting in the spectrum of Ar VIII is observable up to resonances with the Rydberg electron in n = 13.
At energies above 2.5 eV, good agreement can be observed between the experimentally derived mergedbeam spectra and the scaled AUTOSTRUCTURE rate coefficients, with the S VI experiment containing some spectral features at 7.5 eV and 9.5 eV, most likely due to DR through states, underestimated by the calculation. Below 2.5 eV the agreement is less satisfactory, with the calculated and experimental spectra having different resonance positions and strengths. The insets in Fig. 1 show the lowenergy parts of the mergedbeam spectra in more detail. In the S VI case, the calculated RR contribution is in good agreement with the experiment down to 1 meV. Although the AUTOSTRUCTURE calculation predicts two strong DR resonances at 100 meV, no such resonances are observed in the experiment. Below 1 meV, the experimental recombination rate is clearly enhanced compared to the calculated RR contribution. This lowenergy enhancement is a common characteristic of storage ring experiments and typically amounts to a factor of 3 increase, compared to the calculated RR (Gao et al. 1995).
In contrast to the S VI case, in the Ar VIII spectrum the experimentally determined rate coefficients are substantially larger than the calculated RR rate coefficients already below 100 meV. With the enhancement beginning only below 1 meV, the increasing difference between the experiment and calculated RR toward lower energies is most likely due to DR. However, it is difficult to assess the exact contribution of the lowenergy DR, because of the width of the resonance structure. In the experimental spectrum it seems that the resonance overlaps the 0 eV threshold. Additionally, one should consider the 1/E scaling of DR strength, which produces an increasing tail in the resonance profile toward 0 eV (see e.g. Orban et al. 2007). It is interesting to note that in the recombination spectrum of Ar VIII, the enhancement below 1 meV is quite large, compared to the RR level. Extending a trend line to the lowenergy DR resonance profile, the enhancement at 10^{5} eV is more than an order of magnitude larger than the RR, which seems to suggest that the enhancement takes place not only in the RR, but also in the lowenergy DR channel. Large enhancements were observed in the recombination spectra of other ions, also containing lowenergy DR resonances (see e.g. Ar XIV, Gao et al. 1995; and Pb LIV, Lindroth et al. 2001). The AUTOSTRUCTURE calculation predicts a strong resonance in the lowenergy part of the Ar VIII spectrum, at 30 meV.
Results of AUTOSTRUCTURE calculations, containing recombination into states with the principal quantum number of the Rydberg electron extending up to n=1000 are shown in Fig. 1 by the dashed lines. DR into states with is insignificant, therefore the calculated DR rate coefficients shown by the dashed lines are good approximations for the total DR. Hereafter spectra containing DR up to n=1000 will be referred to as fieldionizationfree DR rate coefficients.
Figure 2: Overview of the Ar VIII mergedbeam rate coefficients up to the series limits. The experimentally derived spectrum is shown by the gray area. Vertical bars show DR resonance positions, with the last bar showing the limit of the respective series. The inset shows the highenergy part of the spectrum in more detail. The solid line shows fieldionizationfree DR rate coefficients obtained with AUTOSTRUCTURE. 

Open with DEXTER 
The recombination spectrum of Ar VIII at higher energies, up to the series limits is shown in Fig. 2. Here the energy scale of the measured spectrum was multiplied by 0.986. As observed in the DR spectra of other Nalike ions, the strongest DR contributions are associated with DR resonances located below the thresholds (Schmidt et al. 2007). This energy range also contains and DR resonances in the case of S VI and Ar VIII having comparable strengths to the peaks. The resonances at energies above the series limits, on the other hand, are about one order of magnitude smaller, due to the opening of alternative autoionization channels to excited states of the Nalike ions. In this range, the agreement between the fieldionizationfree AUTOSTRUCTURE results and experiments is poor. Most notably, the calculation underestimates the size of the and series limits, which even in the fieldionization limited experiment are larger than what the fieldionizationfree calculation predicts.
Figure 3: Various curves showing plasma DR rate coefficients of Ar VIII, with lowenergy parts removed as depicted in the figure inset. The thick dashed curve shows plasma DR rate coefficients containing only contributions from DR resonances located below the series limits. 

Open with DEXTER 
5.2 Plasma DR rate coefficients
To obtain
plasma recombination rate coefficients, the RR contributions first were subtracted from the mergedbeam recombination spectra, using the RR curves shown in Fig. 1. The resulting mergedbeam DR spectra were then convoluted with MaxwellBoltzmann electron energy distributions (Savin 1999):
where is the plasma temperature, is the mergedbeam recombination rate coefficient, and is the MaxwellBoltzmann distribution of the electron energies:
The validity of the above doubleconvolution for the preparation of plasma recombination rate coefficients was investigated by Schippers et al. (2001).
Figure 4: Plasma DR rate coefficients of a) S VI and b) Ar VIII. Solid lines and gray areas show and fieldionizationfree plasma DR rate coefficients, respectively. Dashed lines show plasma DR rate coefficients obtained from the scaled fieldionizationfree AUTOSTRUCTURE calculation. Dashdotted lines shows RR rate coefficients from Badnell (2006). Plasma DR rate coefficients from the literature are shown by the following symbols: squares  Badnell (1991), open circles  Altun et al. (2006), full circles  Aldrovandi & Pequignot (1973), diamonds  Mazzotta et al. (1998), triangles  Gu (2004), and stars  Jacobs et al. (1979). Horizontal arrows show temperature ranges in photoionized (A) and collisionally ionized (B) plasmas, where the abundance of the respective ions is higher than 10% of the maximum occurrence (Kallman & Bautista 2001). 

Open with DEXTER 
Plasma DR rate coefficients obtained from the experimentally derived DR spectrum of Ar VIII are shown in Fig. 3. The contributions from DR resonances located above the series limits are shown by the differences between the solid curve, containing all measured DR resonances and the thick dashed curve, containing only DR resonances below the series limits. The contributions amount to at 10^{6} K.
In order to estimate the contribution from the lowenergy DR structure, several lowenergy ranges of the mergedbeam spectrum were removed. The resulting spectra were then used to obtain plasma rate coefficients, identified by the corresponding labels in Fig. 3. The exclusion of the range up to 10^{3} meV (the typical energy range of enhancements in recombination spectra measured at storage rings) results in a decrease of 8% in the plasma DR rates at 10^{3} K. In contrast, removing the entire lowenergy contribution below 100 meV decreases the plasma DR rates by 98% of the full value at 10^{3} K, and even at 10^{4} K causes a decrease of %. Clearly, recombination in lowtemperature plasma takes place predominantly through these lowenergy DR channels. However, the enhancement of the lowenergy rate coefficients, the experimental broadening, and the vecinity of the threshold in combination with the width of the DR feature which seems to extend over the threshold, hinders the determination of the exact contribution to the plasma DR rate coefficients.
As discussed in Sect. 3, fieldionization limits the range of detectable states populated by recombination. In order to account for the states not detected in the experiment, the experimentally derived and RR subtracted rate coefficient spectra were replaced by the fieldionizationfree calculations over the fieldaffected part of the series limits. The resulting spectra were then convoluted using Eq. (4), to yield fieldionizationfree plasma DR rate coefficients shown by the gray areas in Fig. 4.
The experimental
and fieldionizationfree DR plasma rate coefficients shown in Fig. 4 were fitted using a formula with the same temperature dependence as the formula given by Burgess (1965):
where is the temperature in K, is in eV, c_{i}, and E_{i} are fit coefficients. The resulting fit coefficients are shown in Table 1. Using Eq. (6) with these coefficients reproduces the S VI rate coefficient curves in the 10^{3}10^{5} K temperature range to better than and above that up to 10^{6} K to within 3%. The fit coefficients for Ar VIII reproduce the plasma DR curves over the entire presented temperature range to better than 0.4%.
Table 1: Fit coefficients for the and fieldionizationfree plasma DR rate coefficients of S VI and Ar VIII. The dimensions of c_{i} and E_{i} are and eV, respectively. Numbers in the square brackets are powers of 10.
The S VI and Ar VIII plasma DR rate coefficients are compared with data from the literature in Fig. 4. In the spectrum of S VI, DR is higher than the RR rate coefficients (Badnell 2006) for temperatures above 5 10^{3} K, whereas in case of Ar VIII, DR is higher than RR over the entire investigated temperature range.
Above 2 10^{4} K and 3 10^{4} K in the plasma DR rate coefficient spectra of S VI and Ar VIII, respectively, DR into states affected by fieldionization becomes important (see Fig. 4). The contribution from the fieldionized states is shown by the fraction of the gray areas located above the solid curves. At K, where the plasma DR rate coefficients reach their peak values, calculated data from the literature have values between the pure experimentally derived plasma DR rate coefficients and the fieldionizationfree plasma rate coefficients. Closest to our plasma DR rate coefficients above this temperature are the data of Gu (2004) and Aldrovandi & Pequignot (1973) for S VI and the data of Gu (2004) and Mazzotta et al. (1998) in the case of Ar VIII. Above 4 10^{4} K, all these curves are lower than our corresponding fieldionizationfree rate coefficients. S VI plasma rate coefficents by Badnell (1991) and Altun et al. (2006) have similar values and are lower than our data, while above 6 10^{4} K, the rate coefficients by Jacobs et al. (1979) are lower than our data.
Below 1.3 10^{4} K and 2 10^{4} K the S VI and Ar VIII plasma DR rate coefficients respectively contain mostly DR channels located below the fieldionization limits and are not affected by the procedure used to account for the fieldionization in the measurement. In this range, the plasma DR rate coefficients obtained from the AUTOSTRUCTURE calculations are larger than the experimentally derived data for both ions. These discrepancies are due to differences in the lowenergy DR channels (see insets in Fig. 1). In the case of S VI the AUTOSTRUCTURE calculation shows two strong DR peaks at 80 and 145 meV, not observed in the experiment. These two peaks cause a factor of 23 difference between the AUTOSTRUCTURE and experimental plasma DR rate coefficients at 10^{3} K.
In the case of Ar VIII, both the experimentally derived and the calculated merged beam rate coefficients contain DR contributions at low energies. As a consequence of the differences between the experimentally derived and calculated spectra, at 10^{3} K, the AUTOSTRUCTURE plasma DR rate coefficients are a factor of 6.5 larger than the experimentally derived values. The very low energy position, a width that is comparable with the energy position, and the broadening of the lowenergy DR feature by the finite experimental energy resolution, and additionally the enhancement at low energies, all affect the accuracy of our procedure to obtain plasma rate coefficients. It is therefore difficult to make a valid comparison of the Ar VIII plasma rate coefficients at low temperatures.
At low temperatures, below 2 10^{4} K, large spreads can be observed between the data available in the literature for both ions. The S VI plasma rate coefficients by Aldrovandi & Pequignot (1973) and Jacobs et al. (1979) neglect DR into the lowest available n states and have negligible values at these temperatures.
Below 10^{4} K, the rate coefficients by Gu (2004) are lower than our experimentally derived data in the case of S VI and higher in the case of the Ar VIII plasma DR spectrum. These discrepancies with the results of stateoftheart calculations for two ions belonging to the same isoelectronic sequence, differing by only 2 atomic numbers, emphasize the need to individually evaluate the lowtemperature plasma DR rate coefficients of the most relevant ions.
6 Conclusions
We present recombination spectra of two astrophysically relevant Nalike ions, S VI and Ar VIII. At low energies, the mergedbeam spectrum of Ar VIII is strongly enhanced, and at 10^{5} eV is more than a factor of 15 larger than the calculated RR contribution.
At high temperatures the calculated results closest to the obtained plasma DR rate coefficients are those of Gu (2004) and Aldrovandi & Pequignot (1973), in the case of S VI and the calculations by Gu (2004) and Mazzotta et al. (1998), in the case of Ar VIII. Above 10^{5} K these rate coefficients are lower than our results for both ions, with the other data available in the literature having even lower values. At temperatures below 10^{4} K, a large spread exists in the data available in the literature for both ions. Stateoftheart calculations are unreliable in this temperature range, in some cases underestimating and in other cases overestimating the plasma DR rate coefficients. These discrepancies are caused by uncertainties in lowenergy DR resonances, which are difficult to calculate accurately. Storage ring measurements provide high resolution recombination spectra and are the most appropriate method for evaluating the calculated DR results, especially at low energies.
Acknowledgements
We acknowledge the financial support received from the Swedish Research Council VR.
References
 Abrahamsson, K., Andler, G., Bagge, L., et al. 1993, NIMPRB, 79, 269 [NASA ADS] (In the text)
 Aldrovandi, S. M. V., & Pequignot, D. 1973, A&A, 25, 137 [NASA ADS] (In the text)
 Altun, Z., Yumak, A., Badnell, N. R., Loch, S. D., & Pindzola, M. S. 2006, A&A, 447, 1165 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
 Anders, E., & Grevesse, N. 1989, Geochim. Cosmochim. Acta, 53, 197 [NASA ADS] [CrossRef] (In the text)
 Badnell, N. R. 1986, J. Phys. B: Atom. Molec. Phys., 19, 3827 [NASA ADS] [CrossRef] (In the text)
 Badnell, N. R. 1991, ApJ, 379, 356 [NASA ADS] [CrossRef] (In the text)
 Badnell, N. R. 2006, ApJS, 167, 334 [NASA ADS] [CrossRef] (In the text)
 Badnell, N. R., O'Mullane, M. G., Summers, H. P., et al. 2003, A&A, 406, 1151 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
 Bethe, H., & Salpeter, E. 1957, The quantum mechanics of one and twoelectron systems, Handbuch der Physik (Berlin: Springer), 35 (In the text)
 Bryans, P., Badnell, N. R., Gorczyca, T. W., et al. 2006, ApJS, 167, 343 [NASA ADS] [CrossRef] (In the text)
 Burgess, A. 1964, ApJ, 139, 776 [NASA ADS] [CrossRef] (In the text)
 Burgess, A. 1965, ApJ, 141, 1588 [NASA ADS] [CrossRef] (In the text)
 Danared, H., Källberg, A., Andler, G., et al. 2000, NIMPRA, 441, 123 [NASA ADS] [CrossRef] (In the text)
 Danforth, C. W., & Shull, J. M. 2008, ApJ, 679, 194 [NASA ADS] [CrossRef]
 Day, C. 2008, Physics Today, 61, 070000
 DeWitt, D. R., Schuch, R., Gao, H., et al. 1996, Phys. Rev. A, 53, 2327 [NASA ADS] [CrossRef] (In the text)
 Fu, J., Gorczyca, T. W., Nikolic, D., et al. 2008, Phys. Rev. A, Atom., Molec., Opt. Phys., 77, 032713 (In the text)
 Gao, H., DeWitt, D. R., Schuch, R., et al. 1995, Phys. Rev. Lett., 75, 4381 [NASA ADS] [CrossRef] (In the text)
 Gu, M. F. 2004, ApJS, 153, 389 [NASA ADS] [CrossRef] (In the text)
 Jacobs, V. L., Davis, J., Rogerson, J. E., & Blaha, M. 1979, ApJ, 230, 627 [NASA ADS] [CrossRef] (In the text)
 Kallman, T., & Bautista, M. 2001, ApJ, 133, 221 [NASA ADS] [CrossRef] (In the text)
 Lindroth, E., & Schuch, R. 2003, The Physics of Multiply and Highly Charged Ions (Netherlands: Kluvert Academic Publishers), 1, 231 (In the text)
 Lindroth, E., Danared, H., Glans, P., et al. 2001, Phys. Rev. Lett., 86, 5027 [NASA ADS] [CrossRef] (In the text)
 Mannervik, S., DeWitt, D., Engström, L., et al. 1998, Phys. Rev. Lett., 81, 313 [NASA ADS] [CrossRef] (In the text)
 Mazzotta, P., Mazzitelli, G., Colafrancesco, S., & Vittorio, N. 1998, A&AS, 133, 403 [CrossRef] [EDP Sciences] (In the text)
 Orban, I., Böhm, S., & Schuch, R. 2009, ApJ, 694, 354 [NASA ADS] [CrossRef] (In the text)
 Orban, I., Lindroth, E., Glans, P., & Schuch, R. 2007, J. Phys. B: Atom., Molec. Opt. Phys., 40, 1063 (In the text)
 Pindzola, M. S., Badnell, N. R., & Griffin, D. C. 1992, Phys. Rev. A, 46, 5725 [NASA ADS] [CrossRef] (In the text)
 Ralchenko, Y., Kramida, A., Reader, J., & NIST ASD Team 2008, NIST Atomic Spectra Database, version 3.1.4, National Institute of Standards and Technology, Gaithersburg, MD, http://physics.nist.gov/asd3 (In the text)
 Savin, D. W. 1999, ApJ, 523, 855 [NASA ADS] [CrossRef] (In the text)
 Schippers, S., Müller, A., Gwinner, G., et al. 2001, ApJ, 555, 1027 [NASA ADS] [CrossRef] (In the text)
 Schmidt, E. W., Bernhardt, D., Muller, A., et al. 2007, Phys. Rev. A, Atom., Molec., Opt. Phys., 76, 032717 (In the text)
 Tokman, M., Eklöw, N., Glans, P., et al. 2002, Phys. Rev. A, 66, 012703 [NASA ADS] [CrossRef]
 Zong, W., Schuch, R., Lindroth, E., et al. 1997, Phys. Rev. A, 56, 386 [NASA ADS] [CrossRef] (In the text)
All Tables
Table 1: Fit coefficients for the and fieldionizationfree plasma DR rate coefficients of S VI and Ar VIII. The dimensions of c_{i} and E_{i} are and eV, respectively. Numbers in the square brackets are powers of 10.
All Figures
Figure 1: Mergedbeam rate coefficients of a) S VI and b) Ar VIII. Note the different scales on the vertical axis, before and after the axis brake. Experimentally derived spectra are shown by the gray areas. The RR contribution to the experimental spectrum is shown by the hatched area. All solid lines show and all dashed lines show fieldionizationfree AUTOSTRUCTURE DR rate coefficients, scaled to 80%, and summed with the RR contribution. Vertical bars show DR resonance positions, with the principal quantum numbers of the Rydberg electrons above the corresponding bars. The last bar shows the limit of the respective series. The insets show the low energy parts of the spectra in more detail. 

Open with DEXTER  
In the text 
Figure 2: Overview of the Ar VIII mergedbeam rate coefficients up to the series limits. The experimentally derived spectrum is shown by the gray area. Vertical bars show DR resonance positions, with the last bar showing the limit of the respective series. The inset shows the highenergy part of the spectrum in more detail. The solid line shows fieldionizationfree DR rate coefficients obtained with AUTOSTRUCTURE. 

Open with DEXTER  
In the text 
Figure 3: Various curves showing plasma DR rate coefficients of Ar VIII, with lowenergy parts removed as depicted in the figure inset. The thick dashed curve shows plasma DR rate coefficients containing only contributions from DR resonances located below the series limits. 

Open with DEXTER  
In the text 
Figure 4: Plasma DR rate coefficients of a) S VI and b) Ar VIII. Solid lines and gray areas show and fieldionizationfree plasma DR rate coefficients, respectively. Dashed lines show plasma DR rate coefficients obtained from the scaled fieldionizationfree AUTOSTRUCTURE calculation. Dashdotted lines shows RR rate coefficients from Badnell (2006). Plasma DR rate coefficients from the literature are shown by the following symbols: squares  Badnell (1991), open circles  Altun et al. (2006), full circles  Aldrovandi & Pequignot (1973), diamonds  Mazzotta et al. (1998), triangles  Gu (2004), and stars  Jacobs et al. (1979). Horizontal arrows show temperature ranges in photoionized (A) and collisionally ionized (B) plasmas, where the abundance of the respective ions is higher than 10% of the maximum occurrence (Kallman & Bautista 2001). 

Open with DEXTER  
In the text 
Copyright ESO 2009