Issue 
A&A
Volume 553, May 2013



Article Number  A42  
Number of page(s)  5  
Section  Atomic, molecular, and nuclear data  
DOI  https://doi.org/10.1051/00046361/201220957  
Published online  26 April 2013 
Radiative association of He^{+}_{2} revisited
^{1}
Charles University in Prague, Faculty of Mathematics and Physics,
Department of Chemical Physics and Optics, Ke Karlovu 3, 12116 Prague 2, Czech Republic
email:
lucie.augustovicova@mff.cuni.cz
^{2}
Institute of Organic Chemistry and Biochemistry, Academy of
Sciences of the Czech Republic, Flemingovo nám. 2, 16010 Prague 6, Czech Republic
email:
vladimir.spirko@marge.uochb.cas.cz
^{3}
MaxPlanckInstitute of Astrophysics, Postfach 1371, 85741
Garching,
Germany
email:
wpk@mpagarching.mpg.de
^{4}
Charles University in Prague, Faculty of Mathematics and Physics,
Department of Chemical Physics and Optics, Ke Karlovu 3, 12116 Prague 2, Czech Republic
email:
pavel.soldan@mff.cuni.cz
Received:
19
December
2012
Accepted:
13
March
2013
Aims. Rate coefficients for spontaneous and stimulated radiative association of the He^{+}_{2} molecular ion are presented as a function of temperature, considering the association with rotationalvibrational states of the ground X electronic state from the continuum states of the lowest three excited A,C, and E electronic states.
Methods. The rate coefficients are obtained from the cross sections for radiative association, which are calculated by solving the Schrödinger equation for bound and continuum states supported by the corresponding BornOppenheimer potential energy curves.
Results. The rate coefficients for the A → X spontaneous process are in excellent agreement with previous calculations. For temperatures up to about 10 000 K, the spontaneous C → X and E → X processes are dominant, exceeding the A → X rate coefficient by several orders of magnitude. Stimulation of the radiative association by blackbody radiation has significant influence only on the A → X process at temperatures below 1000 K. The blackbody radiation temperature would have to be well above 50 000 K in order to have any noticeable effect on the C → X and E → X processes.
Key words: molecular processes
© ESO, 2013
1. Introduction
The small diatomic ions H or HeH^{+} and are assumed to be significantly abundant in the atmospheres of white dwarf stars, either in the hydrogendominated DAtype stars or the less numerous heliumrich ones, respectively (Koester & Chanmugam 1990). Continuous absorption by these ions has been shown to be a major source of the opacity in the ultraviolet continuum of these stars (Stancil 1994). With their onedimensional potentials originating from solutions of a small fewelectron problem, these ions can be treated on very high theoretical accuracy levels and are therefore ideal test cases for comparisons between theory and results obtained from laboratory experiments or observations.
There have been numerous accurate theoretical studies of the ground electronic state of the ion, culminating in the highly accurate calculations of its adiabatic potential energy curve by Cencek & Rychlewski (1995) and most recently in calculations of the ground state potential including adiabatic corrections by Tung et al. (2012). Theoretical studies on a similar high accuracy level of the excited states are less frequent, which is partly due to the fact that within the adiabatic approximation these states undergo numerous avoided curve crossings. The first serious attempt to clear up the situation for the lowest six excited states went beyond the adiabatic BornOppenheimer approximation, evaluating in addition to the adiabatic potential curves the nonadiabatic matrix elements at the avoided crossings and thus constructing approximate diabatic potential curves (Metropoulos et al. 1987). Other extended calculations focused later on the BornOppenheimer potentials of the lowlying , , , and states (Ackermann & Hogreve 1991; Bawagan & Davidson 1997). Recently, a twostate study of the ground and first excited states was performed, which included an exact treatment of all adiabatic correction terms (Xie et al. 2005).
Stancil et al. (1993) have studied the spontaneous radiativeassociation formation of from collisions of He^{+} ions with He atoms in their ground state and discussed possible astrophysical implications of this reaction in attempts to model abundances in SN 1987A ejecta and in the planetary nebula NGC 7027. They came to the conclusion that the formation of in the early Universe does not have any interesting consequences. In contrast, the heliumcontaining small molecular ions HeH^{+} and are known to be highly abundant in the atmospheres of Herich white dwarf stars (Gaur et al. 1988, 1992) and some planetary nebulae (Black 1978; Flower & Roueff 1979; Stancil 1994). It was demonstrated, for instance, that HeH^{+} can affect significantly the photosphere of such stars (Harris et al. 2004) and that the resulting increased opacity will lengthen their cooling time (Fontaine et al. 2001). The same holds for contributions from He + He^{+} collisional absorption and photodissociation processes (Ignjatovic et al. 2009). Since temperatures in these objects are very high, investigations of possible interactions between excited He atoms and He^{+} ions or protons seem to be appropriate.
On this background the present study intends to go beyond the previous work of Stancil et al. (1993), investigating the different radiativeassociation formation processes of , which can be formulated with the lowest three excited states acting as reactant channels. They are described as where ^{2} [...] _{g} means a doublet g submanifold of the corresponding collisional continuum. According to this scheme, reactions start from collisions of He in one of the lowest three atomic levels (1^{1}S, 2^{3}S, 2^{1}S) with He^{+} ions and proceed via resonance and continuum states of the excited , , and potentials of the collisional complex to form under spontaneous photon emission the molecularion ground state . These processes are characterized in the above scheme as A → X, C → X, or E → X, respectively. Apart from spontaneous emission, processes stimulated by the background radiation with frequency ν_{b} (Stancil & Dalgarno 1997; Zygelman et al. 1998) are also considered: (4)The underlying information necessary for the present dynamics calculations, i.e. potential energy data for the different states and the dipole transition data, is calculated on a high accuracy level of ab initio theory (details of these calculations and a discussion of the methodology used will be collected in a separate paper (Augustovičová et al., in prep.).
2. Methods
In quantum mechanics, the cross sections for radiative association of a diatomic molecule in the presence of blackbody radiation can be expressed as a sum over allowed transitions between a continuum state with a positive energy E and orbital angular momentum N′ to bound rovibrational states with vibrational quantum number v′′ and orbital angular momentum N′′ (Zygelman & Dalgarno 1990): (5)where the temperature T_{b} characterizes the blackbody radiation field. In the case of dipole moment transitions, the individual cross sections can be expressed as (Stancil & Dalgarno 1997) (6)where c is the speed of light in a vacuum, k^{2} = 2μE/ħ^{2}, μ is the “reduced mass” of the molecular ion (μ = 3647.89986 AU for ^{4}), p is the probability of approach in the initial electronic state (p = 1/2 for A → X and E → X and p = 1/6 for C → X), and ν_{E;v′′,N′′} is the emitted photon frequency, hν_{E;v′′,N′′} = E + ▵ E − E_{v′′,N′′}, where ▵ E = 0 cm^{1} for A → X, ▵ E = 19.8176 eV for C → X and ▵ E = 20.6164 eV for E → X (Ralchenko et al. 2010).
For a homonuclear diatomic molecule within the Hund’s case (a) spinless approximation, the dipole moment transitions between Σ_{g} and Σ_{u} states are governed by the rotational selection rules ▵ N = N′ − N′′ = ∓ 1. Thus there are only two branches and the only nonzero HönlLondon coefficients are S_{N′,N′ + 1} = N′ + 1 and S_{N′,N′ − 1} = N′, respectively. (7)is the matrix element of the transition dipole moment function d_{z}(R) between the initial continuum radial wave function χ_{N′}(E,R) for the partial wave N′ and the final boundstate radial wave function ψ_{v′′,N′′}(R). The above formula (6) is derived for the energynormalized continuum wave function χ_{N′}(E,R): (8)where δ_{N′}(E) is the phase shift and (9)Moreover, in the case of a homonuclear diatomic molecule with zero nuclear spin (such as ^{4}), symmetry requires that only even N′ levels are populated in the Σ_{g} electronic states and only odd N′′ levels are populated in the Σ_{u} electronic states. Thus the sum in Eq. (5) goes only over even N′, and then the HönlLondon coefficients conveniently arrange that it also goes only over odd N′′.
The radial wave functions may be determined by numerical integration of the Schrödinger equations where U_{C}(R) and U_{B}(R) are the potential energy functions supporting the initial continuum state E, N′ and the final bound state v′′, N′′, respectively. The wave functions χ_{N′}(E,R) and ψ_{v′′,N′′}(R) were calculated by numerical integration of the radial Schrödinger equation using the NumerovCooley method (Numerov 1933; Cooley 1961). Resonance positions and tunneling widths were calculated employing the computer program LEVEL 7.7 (Le Roy 2005) and making use of the Airyfunction boundary condition at the outermost classical turning point (Le Roy & Liu 1978) and the uniform semiclassical method (Connor & Smith 1981; Huang & Le Roy 2003).
Molecular characteristics of the potential energy curves used in the crosssection calculations of the radiative association.
For evaluation of the continuum and boundstate wave functions in Eqs. (10, 11) and the dipole moment matrix elements in Eq. (7), it is necessary to have either analytical or numerical representation of the potential energy and dipole moment functions. We chose numerical representation by the onedimensional reciprocalpower reproducing kernel Hilbert space (RPRKHS) interpolation method (Ho & Rabitz 1996). This method allows not only for qualitatively correct extrapolation in the longrange region of the A + A^{+} interaction potential (12)but also for the use of predetermined values of longrange coefficients (Ho & Rabitz 2000). In the case of potential energy curves U, the interpolation was done with respect to r^{2} (Soldán & Hutson 2000) using RPRKHS parameters m = 1 and n = 2, the coefficient D_{4}, which is equal to α_{d}/2, was kept fixed to the values given by static dipole polarisabilities α_{d} [He(1^{1}S)] = 1.383191 AU (Pachucki & Sapirstein 2000), α_{d} [He(2^{3}S)] = 800.31633 AU and α_{d} [He(2^{1}S)] = 315.631468 AU (Yan & Babb 1998). Very accurate interaction energies of the ground state (Tung et al. 2012) were exploited as known data points for the interpolation. We calculated ab initio interaction energies for the excited states , , and and the corresponding transition dipole moment values employing the multireference configuration interaction method (combined with a very large electron basis set) as implemented in the quantum chemistry program suite MOLPRO (Werner et al. 2010). Further details of these extensive quantum chemistry calculations will be published later elsewhere (Augustovičová et al., in prep.).
Having obtained the corresponding cross sections (5), the rate coefficients for formation of a molecule by (spontaneous and stimulated) radiative association at temperature T is then defined by (13)To evaluate this integral as accurately as possible, we followed the approach of Augustovičová et al. (2012), where contributions from wide and narrow resonances are treated separately from the background contribution. This method was successfully used for very recent calculations of radiativeassociation rate coefficients of the molecular ion LiHe^{+} (Augustovičová et al. 2012).
3. Results and discussion
Using the highlevel calculations of Tung et al. (2012) for the state as reference, we calculated the potentials of the three lowest states on a comparable accuracy level. In Table 1 some data characterizing the three excited states potentials are summarized. For the A state, degenerate with the X state at dissociation, the equilibrium bond distance R_{e} and the dissociation energy are in perfect agreement with previous accurate results obtained by Xie et al. (2005) and those of Carrington et al. (1995). Relative to the results of Xie et al. (2005), the present R_{e} is smaller by less than 0.3 percent and is larger by less than 1 percent. For the C state, R_{e} and can be compared with earlier calculations by Ackermann & Hogreve (1991), which were performed at a lower accuracy level. Whereas the difference in R_{e} is only about 0.9 percent, differs considerably more: 9173 cm^{1} compared to 8565 cm^{1}. For the E state, accurate results for comparison are not available. Quantitative comparisons with the corresponding basic data used in the white dwarf atmosphere studies of Stancil et al. (1993), Stancil (1994), and Ignjatovic et al. (2009) are not possible, because explicit numerical results are not given there. However, the qualitative agreement with these studies is very good. The potential energy curve of Tung et al. (2012) supports 409 rotationalvibrational bound states as opposed to 411 states found by Stancil et al. (1993). Our maximum rotational quantum numbers differ from those presented by Stancil (1994) for four vibrational states (for v = 1,11,20, and 23 our N_{max} are 55, 35, 13, and 3, respectively). The potential energy curve of Tung et al. (2012), our potential energy curve, and our transition dipole moment function connecting these two states also seem to agree very well with the corresponding function plots of Ignjatovic et al. (2009) with no visible differences.
Fig. 1
Cross sections for spontaneous (T_{b} = 0 K) radiative association of . Only the contribution of resonances wider than 0.1 cm^{1} is shown. 
Cross sections for a spontaneous (T_{b} = 0 K) radiative association are shown graphically in Fig. 1. The cross sections for the C → X and E → X processes are several orders of magnitude larger than the cross sections for the A → X process because of their rather large ▵ E. For these two processes one can also see the highenergy resonance structures. These are consequences of the avoided crossings with higher electronic states, which result in local potential energy minima in the shortrange region (for R between 1 a_{0} and 2.5 a_{0}) (Metropoulos et al. 1987). The corresponding potential energy wells then support many shape resonances in the highenergy region (between 1.7 eV and 6.2 eV and between 6.5 eV and 7.9 eV for the C → X and E → X processes, respectively). The lowenergy resonance structure in the radiativeassociation cross sections, which is created by the quasibound states trapped behind the centrifugal barrier, is the richest for the C → X process. Only quasibound states, which have a symmetryallowed (i.e. for which the corresponding HönlLondon coefficient is nonzero) boundstate partner supported by the electronic state, contribute to rate coefficients. The resonance structures relevant for the studied processes are summarized in Table 2. The corresponding rate coefficients for the spontaneous radiative association are shown graphically in Fig. 2, and their values, evaluated at selected temperatures, are provided in Table 3. Our results for the A → X process are in excellent agreement with the results of Stancil et al. (1993), indicating thus that in this case the rate coefficients are not very sensitive to the potentials used. For temperatures up to about 10 000 K, the processes C → X and E → X are dominant, exceeding the A → X rate coefficient by several orders of magnitude and thus mimicking the crosssection behaviour.
Resonance situation overview for the three studied processes of the radiative association.
Cross sections and rate coefficients for the stimulated radiativeassociation A → X process are shown graphically for different blackbody radiation temperatures T_{b} in Figs. 3 and 4, respectively. The difference in cross sections between the limit (T_{b} = 0 K and T_{b} = 10 000 K) cases starts to be washed out at collision energies around E = 1 eV. However, at lower energies the difference is almost two orders of magnitude in favour of the stimulated process. The difference in the corresponding rate coefficients at low temperatures (around T = 10 K) reaches two orders of magnitude, although it decreases rapidly with increasing temperature until it becomes negligible at temperatures around T = 10 000 K. The cross sections and rate coefficients for the stimulated C → X and E → X processes do not vary significantly with the blackbody radiation temperatures. This is caused by very large ▵ E for these processes, which negates the effect of the blackbody radiation temperature in Eq. (6). Consequently one would need the blackbody radiation temperature around T_{b} = 50 000 K to see an increase by merely 1% in the cross sections or rate coefficients.
Fig. 2
Rate coefficients for spontaneous (T_{b} = 0 K) radiative association of . 
Values of the total rate coefficients for the three spontaneous processes of the radiative association.
Fig. 3
Cross sections for the stimulated radiative association A → X process in for different background temperatures. 
Fig. 4
Rate coefficients for the stimulated radiative association A → X process in for different background temperatures. 
4. Conclusion
Radiative association formation of the ground electronic state of by spontaneous or stimulated photon emission was investigated considering the lowest three excited electronic states (, , ) as initial reactant channels. The cross sections for spontaneous radiative association via the A → X, C → X, and E → X processes were calculated as functions of the collision energy. The corresponding rate coefficients for the formation of in the ground electronic state were determined as functions over a wide range of temperatures. For the A → X process, the results were found to be in excellent agreement with those of Stancil et al. (1993). Whereas at low temperatures the C → X process is by far the most efficient one (its rate coefficient is more than six orders of magnitude larger than for A → X), the E → X process becomes more efficient at very high temperatures (in the range of 10^{4} to 10^{5} K) with rate coefficients more than an order of magnitude larger than for A → X. Stimulation of the radiative association by blackbody radiation was shown here to be important for the A → X reaction at temperatures up to about 1000 K. For background radiation temperatures of a few thousand K, the increase of the rate coefficient in this temperature range can be by about an order of magnitude and more.
Acknowledgments
L.A. acknowledges funding from the Grant Agency of the Charles University in Prague – GAUK (Grant no. 550112). L.A. and V.Š. also appreciate support of the Czech Science Foundation – GAČR (Grant No. P208/11/0436).
References
 Ackermann, J., & Hogreve, H. 1991, Chem. Phys., 157, 75 [NASA ADS] [CrossRef] [Google Scholar]
 Augustovičová, L., Špirko, V., Kraemer, W. P., & Soldán, P. 2012, Chem. Phys. Lett., 531, 59 [NASA ADS] [CrossRef] [Google Scholar]
 Bawagan, A. D. O., & Davidson, E. R. 1997, Chem. Phys. Lett., 266, 499 [NASA ADS] [CrossRef] [Google Scholar]
 Black, J. 1978, ApJ, 222, 125 [NASA ADS] [CrossRef] [Google Scholar]
 Carrington, A., Pyne, C. H., & Knowles, P. J. 1995, J. Chem. Phys., 102, 5979 [NASA ADS] [CrossRef] [Google Scholar]
 Cencek, W., & Rychlewski, J. 1995, J. Chem. Phys., 102, 2533 [NASA ADS] [CrossRef] [Google Scholar]
 Connor, J. N. L., & Smith, A. D. 1981, Mol. Phys., 43, 397 [NASA ADS] [CrossRef] [Google Scholar]
 Cooley, J. W. 1961, Math. Comput., 15, 363 [Google Scholar]
 Flower, D., & Roueff, E. 1979, A&A, 72, 361 [NASA ADS] [Google Scholar]
 Fontaine, G., Brassard, P., & Bergeron, P. 2001, PASP, 113, 409 [NASA ADS] [CrossRef] [Google Scholar]
 Gaur, V. P., Tripathi, B. M., Joshi, G. C., & Pande, M. C. 1988, Ap&SS, 147, 107 [NASA ADS] [CrossRef] [Google Scholar]
 Gaur, V. P., Joshi, G. C., & Pande, M. C. 1992, Ap&SS, 197, 57 [NASA ADS] [CrossRef] [Google Scholar]
 Harris, G., LynasGray, A., Miller, S., & Tennyson, J. 2004, ApJ, 617, L143 [NASA ADS] [CrossRef] [Google Scholar]
 Ho, T. S., & Rabitz, H. 1996, J. Chem. Phys., 104, 2584 [Google Scholar]
 Ho, T. S., & Rabitz, H. 2000, J. Chem. Phys., 113, 3960 [NASA ADS] [CrossRef] [Google Scholar]
 Huang, Y., & Le Roy, R. J. 2003, J. Chem. Phys., 119, 7398 [NASA ADS] [CrossRef] [Google Scholar]
 , erratum 2007, J. Chem. Phys., 126, 9904 [Google Scholar]
 Ignjatovic, L. M., Mihajlov, A. A., Sakan, N. M., Dimitrijevic, M. S., & Metropoulos, A. 2009, MNRAS, 396, 2201 [NASA ADS] [CrossRef] [Google Scholar]
 Koester, D., & Chanmugam, G. 1990, Rep. Prog. Phys., 837, 53 [Google Scholar]
 Le Roy, R. J. 2005, LEVEL 7.7: A Computer Program for Solving the Radial Schrödinger Equation CPRR661 [Google Scholar]
 Le Roy, R. J., & Liu, W. 1978, J. Chem. Phys., 69, 3622 [NASA ADS] [CrossRef] [Google Scholar]
 Metropoulos, A., Nicolaides, C. A., & Buenker, R. J. 1987, Chem. Phys., 114, 1 [NASA ADS] [CrossRef] [Google Scholar]
 Numerov, B. 1933, Math. Comput., 2, 188 [Google Scholar]
 Pachucki, K., & Sapirstein, J. 2000, Phys. Rev. A, 63, 504 [CrossRef] [Google Scholar]
 Ralchenko, Y., Kramida, A. E., Reader, J., & Team, N. A. 2010, NIST Atomic Spectra Database (version 3.1.5), see http://physics.nist.gov/asd3 [Google Scholar]
 Soldán, P., & Hutson, J. M. 2000, J. Chem. Phys., 112, 4415 [NASA ADS] [CrossRef] [Google Scholar]
 Stancil, P. C. 1994, J. Quant. Spec. Radiat. Transf., 51, 655 [NASA ADS] [CrossRef] [Google Scholar]
 Stancil, P. C., & Dalgarno, A. 1997, ApJ, 479, 543 [Google Scholar]
 Stancil, P. C., Babb, J. F., & Dalgarno, A. 1993, ApJ, 414, 672 [NASA ADS] [CrossRef] [Google Scholar]
 Tung, W., Pavanello, M., & Adamowicz, L. 2012, J. Chem. Phys., 136, 104309 [NASA ADS] [CrossRef] [Google Scholar]
 Werner, H.J., Knowles, P. J., Manby, R. R., et al. 2010, Molpro, version 2010.2. A package of ab initio programs, see http://www.molpro.net [Google Scholar]
 Xie, J., Poirier, B., & Gellene, G. 2005, J. Chem. Phys., 122, 310 [Google Scholar]
 Yan, Z., & Babb, J. F. 1998, Phys. Rev. A, 58, 1247 [NASA ADS] [CrossRef] [Google Scholar]
 Zygelman, B., & Dalgarno, A. 1990, ApJ, 365, 239 [NASA ADS] [CrossRef] [Google Scholar]
 Zygelman, B., Stancil, P. C., & Dalgarno, A. 1998, ApJ, 508, 151 [NASA ADS] [CrossRef] [Google Scholar]
All Tables
Molecular characteristics of the potential energy curves used in the crosssection calculations of the radiative association.
Resonance situation overview for the three studied processes of the radiative association.
Values of the total rate coefficients for the three spontaneous processes of the radiative association.
All Figures
Fig. 1
Cross sections for spontaneous (T_{b} = 0 K) radiative association of . Only the contribution of resonances wider than 0.1 cm^{1} is shown. 

In the text 
Fig. 2
Rate coefficients for spontaneous (T_{b} = 0 K) radiative association of . 

In the text 
Fig. 3
Cross sections for the stimulated radiative association A → X process in for different background temperatures. 

In the text 
Fig. 4
Rate coefficients for the stimulated radiative association A → X process in for different background temperatures. 

In the text 
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.