Issue 
A&A
Volume 581, September 2015



Article Number  A122  
Number of page(s)  13  
Section  Interstellar and circumstellar matter  
DOI  https://doi.org/10.1051/00046361/201526468  
Published online  21 September 2015 
Spinstate chemistry of deuterated ammonia^{⋆}
^{1}
MaxPlanckInstitute for Extraterrestrial Physics (MPE),
Giessenbachstr. 1,
85748
Garching,
Germany
email:
osipila@mpe.mpg.de
^{2}
Department of Physics, PO Box 64, 00014 University of Helsinki,
Finland
^{3}
I. Physikalisches Institut, Universität zu Köln,
Zülpicher Strasse 77,
50937
Köln,
Germany
Received: 5 May 2015
Accepted: 10 July 2015
Aims. We aim to develop a chemical model that contains a consistent description of spinstate chemistry in reactions involving chemical species with multiple deuterons. We apply the model to the specific case of deuterated ammonia, to derive values for the various spinstate ratios.
Methods. We applied symmetry rules in the context of the complete scrambling assumption to calculate branching ratio tables for reactions between chemical species that include multiple protons and/or deuterons. New reaction sets for both gasphase and grainsurface chemistry were generated using an automated routine that forms all possible spinstate variants of any given reaction with up to six H/D atoms, using the predetermined branching ratios. Both a singlepoint and a modified BonnorEbert model were considered to study the density and temperature dependence of ammonia and its isotopologs, and the associated spinstate ratios.
Results. We find that the spinstate ratios of the ammonia isotopologs are, at late times, very different from their statistical values. The ratios are rather insensitive to variations in the density, but present strong temperature dependence. We derive high peak values (~0.1) for the deuterium fraction in ammonia, in agreement with previous (gasphase) models. The deuterium fractionation is strongest at high density, corresponding to a high degree of depletion, and also presents temperature dependence. We find that in the temperature range 5 K to 20 K, the deuterium fractionation peaks at ~15 K, while most of the ortho/para (and meta/para for ND_{3}) ratios present a minimum at 10 K (ortho/para NH_{2}D has instead a maximum at this temperature).
Conclusions. Owing to the density and temperature dependence found in the abundances and spinstate ratios of ammonia and its isotopologs, it is evident that observations of ammonia and its deuterated forms can provide important constraints on the physical structure of molecular clouds.
Key words: ISM: abundances / ISM: clouds / ISM: molecules / astrochemistry
Appendix A is available in electronic form at http://www.aanda.org
© ESO, 2015
1. Introduction
The chemical evolution of cold molecular cloud cores is characterized by increasing abundances of the nitrogencontaining species N_{2}H^{+} and NH_{3} and by the enhancement of deuterium fractionation (e.g., Tiné et al. 2000; Tafalla et al. 2002). The three isotopologs of deuterated ammonia, NH_{2}D, NHD_{2}, and ND_{3}, therefore look like particularly useful indicators of temporal changes in the chemical composition of starless and prestellar cores. Besides the likelihood that the NH_{2}D/NH_{3}, NHD_{2}/ NH_{2}D, and ND_{3}/ NHD_{2} abundance ratios increase with time (Flower et al. 2006; Roueff et al. 2015), the ratios of different nuclear spin isomers of these molecules can also vary. The reactions leading to ammonia and its deuterated forms are recapitulated in Rodgers & Charnley (2001). Deuteration occurs primarily in reactions between NH_{3} and deuterated ions. In dense, cold clouds this mainly means reactions with the deuterated forms of . Through these reactions, the nuclear spin ratios of NH_{2}D, NHD_{2}, and ND_{3} become dependent on the nuclear spin ratios of H_{2}D^{+}, D_{2}H^{+}, and . The latter set of ratios depend on the H_{2}ortho:para ratio, hereafter o/pH_{2} (e.g., Walmsley et al. 2004), which also influences the formation rate of ammonia (Le Bourlot 1991; Wirström et al. 2012). The o/pH_{2} ratio is predicted to decrease drastically as the core evolves (e.g., Flower & Watt 1984; Pagani et al. 2011; Brünken et al. 2014). While the formation rates of different spin isomers of ammonia probably vary because of competing ionmolecule reactions, grainsurface reactions should produce them in ratios of the nuclear spin statistical weights because H and D atoms are added one by one. However, the accretion of ammonia molecules synthesized in the gas phase leads to gradual changes in the average spin ratios on grains.
The groundstate rotational transitions of the ortho and para species of NH_{2}D and NHD_{2}, as well as those of the meta and para species of ND_{3}, are observable with groundbased telescopes (Shah & Wootten 2001; Lis et al. 2002; van der Tak et al. 2002; Roueff et al. 2005; Gerin et al. 2006; Lis et al. 2006)^{1}. In the few sources where these have been determined, the NH_{2}D/NH_{3} and NHD_{2}/ NH_{2}D column density ratios have been found to lie in the range ~0.1−0.2, whereas the ND_{3}/ NHD_{2} is somewhat lower, ~0.02−0.1, implying that ND_{3}/ NH_{3} ~ 10^{4}−10^{3} (Roueff et al. 2005; Gerin et al. 2006; Lis et al. 2006). These numbers signify enormous deuterium enhancements in ammonia with respect to the cosmic D/H abundance ratio. The observed spin ratios are consistent with the nuclear spin statistical weights, if we take observational uncertainties into account. With the increasing sensitivity of (sub)millimeter telescopes, it will be possible to improve the accuracy of these measurements and to extend the investigation to cover larger and more varied samples of dense cores.
A valid description of chemistry in dense cores should be able to explain, for example, the observed abundances of the different deuterated isotopologs and spin isomers of ammonia, which itself belongs to the most useful probes of dense molecular cloud cores. With this goal in mind, we have developed a comprehensive gasgrain chemistry model that includes deuterium and the spinstate chemistry of molecules containing multiple H and/or D nuclei. In an earlier version of this model, the deuterium fractionation and spin selection rules were applied to light molecules (Sipilä et al. 2013). The model has recently been extended to include heavier deuterated molecules and to take the spin selection rules into account for hydrogen in the formation of ammonia and water (Sipilä et al. 2015, hereafter S15). In the present update, we implement the spin selection rules for reactions that involve up to six hydrogen and deuterium nuclei.
As described in Sect. 2 of this paper,including the spinstate chemistry of multiply deuterated species has required a complete revision of the spin separation routine, which is now based on the symmetries of the nuclear spin functions rather than the angular momentum algebra used in the previous versions of the model. In Sect. 3, we predict the abundances of ammonia and its deuterated forms, and the spin ratios of these molecules as functions of time in homogenous models corresponding to dark cloud and dense core conditions. In Sect. 4, we discuss the temperature dependence of the deuteration of ammonia and derive radial abundance profiles in two modified BonnorEbert sphere models. In this section, we also compare our predictions with the gasphase chemical model of Roueff et al. (2005). Finally, in Sect. 5 we present our conclusions. Appendix A contains a couple of examples of how to calculate the nuclear spin branching ratios using symmetry rules.
2. Model
2.1. Theory
In the present model, the different nuclear spin symmetry states of molecules containing two or more hydrogen and/or deuterium nuclei are treated as separate species. This implies that for the doubly deuterated ammonium ion, , for example, we keep track of four different forms depending on the two possible spin symmetries, “ortho” (A) and “para” (B), of the pairs of the H and D nuclei. In reactions involving multiple H or D nuclei, the branching ratios between different nuclear spin channels are assumed to be determined by their pure nuclear spin statistical weights, that is, the number of nuclear spin functions belonging to each channel, which are calculated using permutation symmetry algebra (Quack 1977; Park & Light 2007b; Hugo 2009; Hugo et al. 2009). This method uses the assumptions of nuclear spin conservation and full scrambling of nuclei in reactive collisions. The branching ratios are calculated for reactions involving up to six hydrogen or deuterium nuclei.
In our previous papers (Sipilä et al. 2013; S15), the nuclear spin branching ratios were deduced using the method of Oka (2004) based on angular momentum algebra. The same method was applied to nuclearspin selection rules of nitrogen hydrides by Rist et al. (2013). For reactions where several deuterium nuclei are involved, Oka’s method is, however, impractical, because species are distinguished by their nuclear spin symmetries, but there is no onetoone correspondence between angular momentum and symmetry representations for systems with three or more D nuclei (Hugo 2009). A comparison between the total angular momentum and the total symmetry representations of systems containing up to five spin1/2 and spin1 particles is presented in Table 2.13 of Hugo (2009). For multiple H nuclei (or any system of spin1/2 particles), the method using symmetry rules gives the same results as Oka’s method, because for these systems each value of the spin angular momentum is associated with one and only one symmetry representation. Also in the case of multiple D nuclei, the total nuclear spin is conserved when using the symmetry rules. This could be seen from branching ratio tables if the symmetry species were subdivided according to the total nuclear spin (an example of this is given in Hugo 2009; Table 2.1).
For calculating the statistical branching ratios using symmetry rules, one needs to determine the possible symmetry species (i.e., representations) of the reactants (Γ_{i} ⊗ Γ_{j}; where ⊗ denotes a direct product), the intermediate complex (Γ_{n}), and the products (Γ_{k} ⊗ Γ_{l}, i + j = n = k + l), in appropriate permutation groups (S_{i} ⊗ S_{j}, S_{n}, and S_{k} ⊗ S_{l}). In addition, one needs to derive the correlation tables between the group of the complex and its subgroups, which represent the reactants and products. This is done by applying the standard methods of group theory. The correlation tables tell us which nuclear spin symmetry species of the reaction complex are feasible given the symmetries of the reactants and which symmetry states of the products are possible when the complex decays (cf. Quack 1977; Eqs. (12)−(15)). In this description, the statistical weight of the product Γ_{k} ⊗ Γ_{l} is given by f(Γ_{k} ⊗ Γ_{l}) × dim(Γ_{k}) × dim(Γ_{k}), where f(Γ_{k} ⊗ Γ_{l}) is the frequency of Γ_{k} ⊗ Γ_{l} in the total symmetry representation generated by the nuclear spin functions of the product molecules in S_{k} ⊗ S_{l}, and dim(Γ) is the dimension of the representation Γ.
Besides being proportional to the number of nuclear spin functions belonging to each channel, branching ratios calculated in this manner are proportional to the number of rovibronic states occupied by these species in the high temperature limit (Park & Light 2007a, their Appendix A). A couple of examples of the procedure are given in Appendix A. The determination of the symmetries of the nuclear spin wave functions is explained lucidly in Bunker (1979) and in Bunker & Jensen (2006). In this work, where we do not consider the rovibronic states of the molecules, it is sufficient to classify the nuclear spin functions in the complete nuclear spin permutation group, which does not include the inversion operation (see also Crabtree & McCall 2013). Most of the statistical branching ratio tables needed in the present study are available in Tables 3 and 4 of Hugo et al. (2009). To also cover reactions with six identical nuclei, such as and , and to transfer the spin selection rules to the chemical network, we developed an automated routine for producing these tables. The character tables for permutation groups needed in this process were obtained using GAP (2015)^{2}.
2.2. Application
We designed a new routine for the spinstate separation of chemical reactions involving multiple protons and/or deuterons, utilizing the grouptheoretical approach described above. As opposed to the model described in S15, the new routine produces consistent branching ratios for reactions involving deuterated species, instead of copying the spinstate separation rules from the purehydrogen counterpart reactions.
Because hydrogen and deuterium are distinguishable, we can divide each reaction involving both hydrogen and deuterium into two parts. For example, the reaction (1)is divided into where we have ignored the carbon and oxygen atoms and the charge. The selection rules for hydrogen split reaction (2) into the following branches: while the selection rules for deuterium split reaction (3) into We then combine the hydrogen and deuterium branches by multiplying all possible combinations together, and we end up with 4 × 4 = 16 different branches for reaction (1). As a result, receives a composite spin made up of hydrogen and deuterium spin states, for example, .
The spinstate separation routine presented here allows us to explicitly consider the spin states of all species that contain multiple H and/or D atoms. However, we do not track the spin states of all species because this would lead to an enormous reaction network with a total reaction count far into the hundreds of thousands. Instead, we adopt the averaging process described in S15, in which we assume a 1:1 spinstate abundance ratio for those species whose spin states we do not want to keep track of. We have verified that this assumption has a negligible influence on the results presented below. In this paper, we focus on the spinstate chemistry of ammonia and its deuterated forms. We also keep the spin states of the species included in the formation network of water, so that we can compare our new model to the one presented in S15. In reaction (1), the only species for which we retain the spin states is H_{2}DO^{+}, and the averaging process finally results in two branches: The separation process is fully automated, so any reaction involving multiple protons in our base reaction set (see S15) is automatically deuterated and spinstateseparated according to the selection rules discussed above. The only exception to this is charge transfer reactions, for which we assume that the spin states are conserved in the reaction. The reaction N^{+} + H_{2} initiating the ammonia synthesis has been treated in the same manner as in Dislaire et al. (2012) and Roueff et al. (2015), who both use the experimental data from Marquette et al. (1988). In addition to the updates listed in S15, the new reaction set includes the rate coefficients for N^{+} + HD and N^{+} + D_{2} from Marquette et al., taking the slightly different groundstate energies of oD_{2} and pD_{2} in the reaction enthalpies into account. For the reactions , we adopt the rate coefficients from Le Gal et al. (2014), which correspond to those used in Roueff et al. (2005).
In what follows, we show results calculated with the gasgrain chemical code discussed in S15. In summary, we choose the osu_01_2009 reaction set as the basis set which is deuterated and spinstate separated according to the approaches discussed above. The initial grainsurface chemistry reaction set is adopted from Semenov et al. (2010), and it is similarly deuterated and spinstateseparated. A complete description of the model including adopted model parameters and updates to the (basis) reaction sets is presented in S15.
3. Results
3.1. Comparison to S15
Fig. 1 Spinstate ratios of NH_{3} (upper panels) and H_{2}O (lower panels) as functions of time at different densities, labeled in the upper left panel. The lefthand panels present results calculated with the (gasgrain) model of S15, while the righthand panels correspond to the present work. 

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Because of the isomorphism between the symmetry and angular momentum representations for hydrogenated species, we recover for these the same branching ratios in the present model as with the method of Oka (2004) employed in S15. However, the branching ratios in reactions involving deuterated species are in many cases significantly different between the two models.
Fig. 2 Principal reactions determining the abundances and spin ratios of deuterated ammonia isotopologs at late stages of chemical evolution in cold, dense cores. The reactions are indicated with blue arrows. 

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In Fig. 1, we compare the o/p ratios of ammonia and water predicted by the S15 model and the present model. The temperature is set to T = 10 K, and the other physical parameters are the same as in S15. The addition of spin states for multiply deuterated species generally has little effect on the spinstate ratios of undeuterated species, but some difference is evident, especially for water at high density. Inspection of the reaction rates reveals that the differences between the models seen in both the ammonia and water o/p ratios are mainly caused by the electron recombinations of (o/p) NH_{3}D^{+} and (o/p) H_{2}DO^{+}. The S15 model contains some pathways for these reactions that are forbidden by the proper selection rules adopted in this work. Nevertheless, the difference between the models is small, and we have checked that this agreement holds for other (undeuterated) species as well.
The results shown in the following sections were calculated with the S15 chemical code, adopting the new reaction sets developed for this paper. As in the test above, the temperature is set to T = 10 K in all calculations, and the other physical parameters are the same as in S15.
3.2. Deuterium fractionation of ammonia
By inspecting the production and destruction rates of deuterated forms of ammonia at various stages of the simulation, one finds that at late times, the deuteration of ammonia proceeds as outlined in the steadystate model of Rodgers & Charnley (2001). The NH_{3} abundance has already built up when the gasphase deuteration becomes effective, and deuteron transfer reactions between ammonia and deuterated ions form, e.g., NH_{3}D^{+}, which can recombine with an electron to give NH_{2}D, etc. In the present model, however, H_{2}D^{+}, D_{2}H^{+}, and are the most important sources of deuterons at late times. The dominant reactions forming NH_{2}D, NHD_{2}, and ND_{3} are shown in Fig. 2. This diagram, which is an extension to the schematic NH_{3} cycle shown in Fig. A.1. of S15, should be compared with Fig. 1 of Rodgers & Charnley (2001). Besides the deuteration pathways, the diagram shows the constant recycling between NH_{3}, , and , and similar cyclic processes among their deuterated variants, caused by charge transfer reactions with H^{+}. This recycling tends to reduce the deuterium fractionation, because NH_{2}D^{+} + H_{2}, for example, also leads to . (We assume a statistical branching ratios, in this case 4:1 in favor of NH_{3}D^{+}.) The reaction N^{+} + HD → ND^{+} + H with very low endothermicity (Marquette et al. 1988) speeds up the deuteration of ammonia at early stages, but this pathway has no influence on the abundances at the deuterium peak.
Figure 3 shows the total abundances, i.e., sums over spin states, of ammonia and its deuterated forms. At late times at high density, ammonia starts to deplete from the gas phase (see also S15). For the various forms of deuterated ammonia, an abundance peak is observed that coincides with the initiation of deuterium chemistry due to CO depletion. Like ammonia, its isotopologs also deplete from the gas phase, and do so more strongly than ammonia itself. This is because of the depletion of deuterated molecules (including the ammonia isotopologs) onto grain surfaces, which traps deuterium onto the surfaces; this ultimately results in HD depletion and consequently the overall gasphase deuteration efficiency decreases (Sipilä et al. 2013; S15).
The abundance ratios of ammonia and its isotopologs are presented in Fig. 4. The deuterium fractionation is highest at high density where depletion is strongest. The relative depletion of the ammonia isotolopogs is fairly uniform, with all abundance ratios ultimately dropping by a factor of 3 to 4 from their peak values. A high degree of fractionation is observed, and the peak values for all of the ratios are ≳0.1. This is further discussed in Sect. 4.3, where we compare our gasgrain modeling results to the gasphase models of Roueff et al. (2005).
3.3. The spinstate ratios of deuterated ammonia
Spin symmetries of molecules with 2−4 H or D nuclei.
In Fig. 5, we show the spinstate ratios of the deuterated forms of ammonia. All of the ratios show dependence on both time and density. For all of the ammonia isotopologs, the most important formation mechanism is the electron recombination of the (singly or multiply) deuterated ammonium ion. To complement Fig. 5, we show in Fig. 6 the spinstate ratios of selected ions. In the following, we quote the spin symmetries of the various species; these are tabulated in Table 1. The numbers in front of the symmetry labels indicate their frequencies in the total nuclear spin representation of the complex. The values of the possible nuclear spin angular momenta, I, and the nuclear spin statistical weights, g_{I}, are given below each symmetry species, along with their “para”, “ortho”, and “meta” appellations, when applicable.
Fig. 3 Abundances of ammonia and its deuterated forms as functions of time at different densities, labeled in the upper right panel. 

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Fig. 4 Abundance ratios of ammonia and its deuterated forms as functions of time at different densities, labeled in the lefthand panel. 

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At late times, the ortho:para ratio of NH_{2}D is largely determined by the cycle (see Fig. 2). The spin ratio of NH_{3} was discussed in Appendix A of S15. The electron recombination of NH_{3}D^{+} yields ortho and para NH_{2}D with the following branching ratios: Since the destruction rates of oNH_{2}D and pNH_{2}D (mainly through reactions with H^{+} and ) are similar, we get o/pNH_{2}D ~ 1 + 2o/pNH_{3}D^{+}. Moreover, because the o/p ratio of NH_{3}D^{+} is ~0.4−0.5 at late times, depending on the density (Fig. 6), o/pNH_{2}D should obtain the values 2 (low density) or 1.8 (high density), in agreement with Fig. 5.
The o/p ratios of NH_{2}D and NH_{3}D^{+} are, however, closely coupled because many of the most important destruction pathways of NH_{2}D return NH_{3}D^{+}. This can be seen by inspection of Figs. 5 and 6, which show the results of the full simulation, and from the schematic presentation of the situation at late times in Fig. 2. The spin state is conserved in the charge exchange reaction . Assuming total scrambling of nuclei in the reaction NH_{2}D^{+} + H_{2}, oNH_{2}D^{+} + pH_{2} gives rise to the intermediate complex NH_{4}(F_{1})D^{+} that dissociates to oNH_{3}D^{+} and pNH_{3}D^{+} in ratio 1:2 (the symmetry of H_{4} is indicated in the brackets, see Table 3 of Hugo et al. 2009). The reaction pNH_{2}D^{+} + pH_{2} produces only pNH_{3}D^{+} through the intermediate complex NH_{4}(E)D^{+} (only reactions with pH_{2} are considered because the oH_{2} abundance is very low at this stage). Using these branching ratios one obtains that the closed cycle should result in o/pNH_{2}D ~ 2.3. As discussed above, in the full reaction network this ratio is, however, about 20% lower.
The doubly and triply deuterated forms of ammonia are primarily formed from the electron recombination of and , respectively. (The recombination of the fully deuterated ammonium ion contributes about 10% to ND_{3}.) The cycle preserves the spin state of D_{2}. The same is true for D_{3} in the corresponding cycle of ND_{3}. forms mainly from the reaction , where the spin state of D_{2}H^{+} is conserved. receives contributions from both D_{2}H^{+} and through the reactions and . In the first of these reactions, the spin ratios of are just copied to NHD. For the second reaction, the branching ratios can be read from Table 4 of Hugo et al. (2009). For example, taking the most common species, the reaction oD_{2}H^{+} + oNHD_{2} forms an intermediate reaction complex with A_{1}, E, and F_{1} symmetries of D_{4} in statistical ratios 15:6:15, and, taking these ratios into account, the complex decay into produces A_{1} (“meta”) and E (“ortho”) symmetries of D_{3} with probabilities 5/9 and 4/9, respectively (the A_{2} “para” symmetry is not formed in this reaction because in D_{4} → D_{3} + D, A_{1} → A_{1}, E → E, and F_{1} → A_{1} + E, Table 4 of Hugo et al. 2009).
What is said above implies that the spin ratios of NHD_{2} and ND_{3} are tied to those of D_{2}H^{+} and , and this is also evident from Figs. 5 and 6. The o/p ratio of NHD_{2} increases constantly until very late times, leveling off only after 10^{7} yr in the models shown in Fig. 5 (i.e., outside the range shown here). This depends on the D_{2}H^{+} o/p ratio, which increases strongly as a function of time (Fig. 6). From Fig. 5 it is observed that paraND_{3} is clearly the least abundant of the three spin states of ND_{3}, while the ortho and meta states are equally abundant at late times regardless of the density. This behavior reflects the spin ratios of shown in Fig. 6.
Fig. 5 Spinstate ratios of the deuterated forms of ammonia as functions of time at different densities, labeled in the lower left panel. 

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The statistical values for the spinstate ratios of ortho/para NH_{2}D, ortho/para NHD_{2} and ortho/meta/para ND_{3} are 3:1, 2:1, and 16:10:1, respectively. From Fig. 5 it is evident that the various ratios deviate strongly from the statistical values at late times, as already found for ammonia in S15 (see also Fig. 1). The various spinstate ratios are generally fairly insensitive to variations in the density. Some density dependence is usually present between 10^{5} and 10^{6} yr of chemical evolution, but even in this time interval, the difference between the low and high density cases is less than a factor of 2.
Assuming there is nuclear spin conservation and that the same selection rules as used in the gas phase can be applied to the H and D addition reactions on grain surfaces, the different spin isomers of ammonia should form on grains according to their nuclear spin statistical weights indicated above. This is what is seen in the beginning of the simulation. Later on, when the gasphase ammonia starts to accrete, the spin ratios change on the grains as well, mimicking the ratios in the gas.
Finally, we note that for the lowest density considered (n_{H} = 10^{3} cm^{3}), many of the plotted spin ratios are increasing even on very long timescales, for example the m/p ratio of ND_{3} which increases by a factor of ~2 from 10^{6} to 10^{7} yr at this density. We note that this effect is due to the very low density and the spin ratios are expected to stabilize at still longer timescales.
It is well established that deuterium fractionation depends not only on the density, but also on the temperature. In particular, deuteration is expected (in starless cores) to be at its strongest in the temperature range ~10−20 K, because on the one hand, this range lies below the sublimation temperature of CO, allowing the main driver ion of deuterium chemistry, H_{2}D^{+}, to transfer its deuteron to other species, and on the other hand, deuteration efficiency drops toward low temperatures because of the decreasing accretion rates (see below).
We plot in Fig. 7 the abundances of ammonia, its deuterated forms, and the associated abundance ratios at different temperatures. Evidently, the deuterium fractionation is strongest around T = 15 K; both the abundances and the deuterium fractionation peak at this temperature. An analysis of the reaction rates shows that if the temperature is reduced from 15 K to 5 K, the decreased accretion rates lead to relatively high abundances of atomic H and D in the gas phase, which enable efficient conversion of D_{2}H^{+} to H_{2}D^{+} through the exchange reaction D_{2}H^{+} + H− → H_{2}D^{+} + D. This decreases the ammonia deuterium fractionation because D_{2}H^{+} is an important part of the production paths of the deuterated forms of ammonia (Fig. 2). On the other hand, as the temperature is increased from 15 K to 20 K, CO starts to desorb efficiently, hindering deuteration in general.
The spinstate ratios of the ammonia isotopologs at different temperatures are shown in Fig. 8. It is observed that the ratios change significantly when the temperature is varied and that the variation is much greater than what is induced by changes in the density. A minimum in the ortho/para (and meta/para for ND_{3}) ratios is observed at T = 10 K, except for the ortho/para ratio of NH_{2}D, which has a maximum at this temperature. These are in contrast to the overall deuteration, which peaks at T = 15 K.
Fig. 6 Spinstate ratios of the deuterated forms of the ammonium ion, as well as D_{2}H^{+} and , as functions of time at different densities, labeled in the lower left panel. 

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3.4. Temperature dependence of ammonia D fractionation and spinstate ratios
Fig. 7 Upper panels: abundances of ammonia and its deuterated forms as functions of time at different temperatures, labeled in the lefthand panel. Lower panels: abundance ratios of ammonia and its deuterated forms as functions of time at different temperatures. In all panels, a constant density of n_{H} = 10^{5} cm^{3} is adopted. 

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As explained in Sect. 3.3, the spinstate ratios of ND_{3} are determined by those of , which are in turn determined by D_{2}H^{+} and . Moving from 10 K to 20 K, the ortho/para ratio of H_{2} increases, leading to higher ortho/para D_{2}H^{+} and meta/ortho (and meta/para) ratios, which ultimately increase the ortho/para and meta/para ratios of ND_{3} with respect to the values at 10 K. On the other hand, at 5 K, the H_{2} ortho/para ratio is low, but the abundances of atomic H and D increase owing to decreased accretion rates, and the proton/deuteron exchange reactions with the isotopologs (for example, ) increase in importance in determining the various spinstate ratios. The spinstate ratios of NH_{2}D and NHD_{2} are affected by similar effects with varying temperature.
Fig. 8 Spinstate ratios of the deuterated forms of ammonia as functions of time at different temperatures, labeled in the lower left panel. A constant density of n_{H} = 10^{5} cm^{3} is adopted. 

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4. Discussion
4.1. Radial profiles for deuterated ammonia
From the above it is clear that both the deuterium fractionation of ammonia and the spinstate ratios depend on time and on the physical parameters (density, temperature). To investigate the implication to observations of deuterated ammonia, we constructed radial abundance profiles for ammonia and its deuterated forms by following the method discussed in Sipilä (2012) and Sipilä et al. (2013), in which chemical calculations are combined with a radiative transfer model to produce selfconsistent chemical abundance profiles as functions of density, temperature, and time. For these calculations, we adopt a modified BonnorEbert sphere as the core model (Galli et al. 2002; Keto & Field 2005; Sipilä et al. 2011) of mass M = 1.0 M_{⊙}. We assumed a visual extinction A_{V} = 10 mag at the edge of the core.
Fig. 9 Lefthand panel: gas density (black), gas temperature (red), and dust temperature (blue) as functions of distance from the core center at different time steps (indicated in the middle panel). Middle panel: abundances of NH_{3} and NH_{2}D as functions of distance from the core center at different time steps. Righthand panel: abundances of NHD_{2} and ND_{3} as functions of distance from the core center at different time steps (same legend as in the other panels). The panels correspond to an MBES of mass 1.0 M_{⊙}. 

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The density and temperature profiles of the model core are shown in the lefthand panel in Fig. 9. The density and dust temperature profiles hardly change as functions of time. The density is not high enough even in the core center to equalize the dust and gas temperatures. On the other hand, the gas temperature decreases toward the outer areas because of efficient line cooling by (mainly) CO. As the chemical evolution progresses, CO depletes on grain surfaces, reducing the cooling rates, and the gas temperature rises.
The calculated radial abundance profiles are shown in the middle and righthand panels in Fig. 9. The time steps shown in the figure refer to years of chemical evolution with respect to an initially atomic initial state (except for H and D, which are initially in H_{2} and HD; see S15). The abundances of ammonia and its deuterated isotopologs generally increase as a function of time. Notably, the abundance of ND_{3} increases by about three orders of magnitude across the core from t = 5 × 10^{4} yr to t = 1 × 10^{6} yr, and the increase in time is stronger for species with more D atoms. The difference in abundance between the core center and edge can be close to two orders of magnitude depending on the species considered and on the time. Depletion slightly decreases the abundances at the core center at the last time step, while the abundances keep increasing at the edge where the density is lower and little depletion is present. An exception to the latter behavior is ammonia, whose abundance has a minimum in the outer core around t = 5 × 10^{5} yr; this kind of behavior is also displayed, for example, in Fig. 7 and discussed in Sect. 4.2.
The results shown here demonstrate, on the one hand, the importance of accurate knowledge of the physical structure, and on the other, the necessity of detailed chemical modeling in ascertaining the chemical age of the object in question. However, quantifying the effect of the varying abundance profiles on observable emission requires calculating the line profiles with a radiative transfer model. This will the subject of a future paper.
4.2. Evolution of the ammonia abundance
Characteristic of the time dependence of the NH_{3} abundance at high densities and, to a lesser extent, of that of NH_{2}D is a minimum that occurs somewhere between 10^{5} and 10^{6} yr, and a rapid recovery after this minimum. This tendency is most clearly visible in Fig. 7. The behavior is very different from what is observed in the case of CO or CS, for example, but resembles the variation in the abundances of HCN and HNC seen in the models of Loison et al. (2014).
The ammonia production is assumed to start slowly, the widely recognized bottleneck being the slightly endothermic reaction N^{+} + H_{2}− → NH^{+} + H, which in practice only works with oH_{2} in cold clouds (e.g., Dislaire et al. 2012; Roueff et al. 2015). Once NH^{+} is formed, it is quickly converted to ammonia through etc. In fact, the flow through the bottleneck is so slow that most of the time the chemical network may find other means of producing NH^{+}. In the present model, NH^{+} is copiously formed at early times (~10^{4} yr) from the dissociative ionization of HNC by He^{+}, with the bottleneck reaction coming in second. The efficiency of this channel decreases along with the depletion of HNC, and because NH_{3} accretes onto grains as well, its gasphase abundance decreases some time before 10^{5} yr or slightly after that, depending on the density.
A strong increase in the ammonia abundance is seen, however, after the minimum, as an indirect consequence of the depletion of CO and neutrals like HCN and OH, which are ionized in charge transfer reactions with H^{+}. The disappearance of these molecules greatly enhances the abundances of and H^{+}. The first converts part of N_{2} to NH through the reaction , followed by N_{2}H^{+} + e^{−}− → N_{2} + H/NH + N. Although fewer than 10% of the recombinations lead to NH, this channel is important for ammonia, because the increased abundance of H^{+} directs NH to the ammonia track through the charge transfer reaction H^{+} + NH− → NH^{+} + H. Likewise, all the recombination products of and (NH, NH_{2}, NH_{3}) are efficiently returned to the ammonia cycle by H^{+}. In the present model, ammonia passes the cycle described in Sect. 3.2 several times before colliding with a dust grain. In Fig. 10 we show the fractional abundances of NH_{3}, NH, H^{+}, , and HNC as functions of time for a homogeneous model with n_{H} = 10^{5} cm^{3}, T = 10 K. In this model, NH_{3} and NH are closely correlated after 10^{5} yr and follow the gradual decrease in the N_{2} abundance (not shown) at very late times.
Fig. 10 Fractional abundances (with respect to n_{H}) of selected species (labeled in the plot) in a homogeneous model with n_{H} = 10^{5} cm^{3}, T = 10 K. 

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4.3. Comparison to Roueff et al. (2005)
Roueff et al. (2005) present observations of NH_{2}D, NHD_{2}, and ND_{3} toward prestellar cores and discuss the interpretation of the observations in the context of a gasphase chemical model. Their model is to our knowledge the one that is most directly comparable to our own in terms of the chemistry of deuterated ammonia.
Our model includes timedependent depletion^{3}, and a chemical steadystate is not reached in the time intervals considered here. However, comparing the values given in Table 9 in Roueff et al. (2005) with our results near the deuterium peak for each density (Fig. 3), we find that the agreement between the models is very good, even though we are using a gasgrain model with different initial abundances and a different value for the cosmic ray ionization rate (here 1.3 × 10^{17} s^{1}; 2 × 10^{17} s^{1} in Roueff et al. 2005). It should be noted, however, that in our model, depletion also occurs at a density of 10^{4} cm^{3}, whereas in the Roueff et al. model no depletion is assumed at this density.
Fig. 11 Abundance ratios of ammonia and its deuterated forms (labeled in the plot) as functions of time in a gasphase chemical model, for different initial values of the H_{2} ortho/para ratio: 3 (black lines), 10^{3} (blue), or 10^{5} (green). 

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As an additional check, we ran another calculation using a gasphase model (i.e., no depletion) at n(H_{2}) = 10^{4} cm^{3}, for three different values of the initial H_{2} ortho/para ratio. The resulting abundance ratios for ammonia and its deuterated forms are shown in Fig. 11. The gasphase model predicts a lower deuterium fractionation than the gasgrain model, even for very low initial H_{2} ortho/para ratios. The main reason for this is that the high abundance of CO hinders the formation of H_{2}D^{+}, D_{2}H^{+}, and , which in our model are the principal agents in the formation of deuterated ammonia.
Roueff et al. (2005) assumed that the release of hydrogen is favored (in a 2:1 ratio) over the release of deuterium in the electron recombinations of the various deuterated ammonium ions, whereas in this work the H/D branching ratios for the recombination reactions are statistical. We tested the effect of assuming a 2:1 ratio for the recombination reactions and found that this has only a marginal effect on the abundances of ammonia and its isotopologs. We note that we adopt the reaction rates from Le Gal et al. (2014), which correspond to the values used by Roueff et al. (2005; see also Roueff et al. 2015). We tested the new coefficients given by Roueff et al. (2015) for these reactions and found that they only have a minor effect on our results.
The differences between our gasphase model and that of Roueff et al. (2005) can perhaps be explained by the adoption of different rate coefficients for the reacting system, since the contribution of the isotopologs to the chemistry of deuterated ammonia is significant as discussed earlier in this paper. Finally we reiterate that the depletion present in our gasgrain model, even at lower densities, enhances deuteration and brings the results close to the gasphase model of Roueff et al. (2005).
5. Conclusions
We calculated branching ratios for reactions involving multiply deuterated species using group theory. This method produces identical branching ratios for reactions without deuterium, which can be derived with angular momentum algebra (Oka 2004). Our new model allows us to track the spin states of any species that includes multiple protons and/or deuterons. However, in this paper, we concentrated on the spinstate chemistry of deuterated ammonia.
We found that the deuterium fractionation of ammonia is high especially at high density: the NH_{2}D/NH_{3}, NHD_{2}/ NH_{2}D, and ND_{3}/ NHD_{2} all peak at ~10% for n_{H} = 10^{6} cm^{3}. The high abundance ratios are in line with the earlier gasphase models of Roueff et al. (2005). The various spinstate ratios were found to deviate strongly from the statistical values especially at late times, but on the other hand, the ratios appear rather insensitive to variations in the density. We also found that the abundances of ammonia and its isotopologs and the associated spinstate ratios are highly dependent on the temperature; the meta/para ratio of ND_{3}, for example, can vary by a factor of ~5 in the temperature range 5−20 K.
The abundances of NH_{2}D, NHD_{2}, and ND_{3} and their spinstate ratios in the gas phase are determined by competing ionmolecular reactions, the rates of which depend strongly on the kinetic temperature. The deuterium fractionation is most efficient at 15 K. The temperature dependences of the spinstate ratios are less straightforward: the para species of NHD_{2} and ND_{3} reach their abundance maxima at 10 K, whereas paraNH_{2}D has a minimum at this temperature. The reactions leading to deuterated ammonia involve H_{2}D^{+}, D_{2}H^{+}, and , and benefit from the disappearance of CO, which occurs faster at high densities. Therefore, for objects with density/temperature gradients, such as starless and prestellar cores, significant variations as functions of radius and time can be expected in the abundances and the spinstate ratios of NH_{2}D, NHD_{2}, and ND_{3}. Sensitive observations of these molecules, combined with chemical and radiative transfer modeling, can provide stringent constraints on the physical and chemical structures and on the evolutionary stages of molecular clouds.
The present model does not include corrections to the rate coefficients that result from differences in the zeropoint energies of deuterated and undeuterated species, except for the reacting system given by Hugo et al. (2009) and the N^{+} + H_{2}
reaction (Marquette et al. 1988). Moreover, the use of pure nuclear spin statistical weights is based on the implicit assumption that the exothermicity of the reaction is high enough that Pauliallowed rotational levels of each product species can be populated. For the principal reactions contributing to the interstellar ammonia, this is likely to be true (see also discussion in Rist et al. 2013). However, it is clear that the present model is still incomplete, so an indepth study of energetics is warranted.
GAP is a system for computational group theory, http://www.gapsystem.org
In our model, nitrogen and deuterium deplete as well, unlike in the model of Roueff et al. (2005).
Acknowledgments
We thank the anonymous referee for a careful reading of the manuscript, and Laurent Wiesenfeld for helpful discussions. O.S. and P.C. acknowledge the financial support of the European Research Council (ERC; project PALs 320620)
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Online material
Appendix A: Calculation of nuclear spin branching ratios using symmetry rules
The method used in deriving the nuclear spin branching ratios is demonstrated by three examples, all dealing with varieties of the reaction . The method is described in Quack (1977) and in Park & Light (2007b). The collision partners are classified, or labeled, according to the irreducible representations of an appropriate permutation group. These labels tell how the symmetrized nuclear spin functions belonging to this species transform under operations of the group, such as the transposition of two identical nuclei and the permutation of n identical nuclei (e.g., Bunker & Jensen 2006). The branching ratios are obtained from correlations between the group of the intermediate reaction complex and the direct product groups representing the reactants and products (Quack 1977). The statistical weight of each channel corresponds to the number of nuclear spin functions belonging to that symmetry species.
Appendix A.1: Three identical nuclei
As the first example we consider the reaction D_{2}H^{+} + NH_{2}D →. The H and D symmetries are treated separately. The same result is obtained by considering the mixed system in appropriate direct product groups. From the hydrogen point of view, H_{2} and H form H_{3} which dissociates back to H_{2} + H. On the deuterium side, the reaction forms D_{3} from D_{2} + D. In the present model we assume that the branching ratios are equal to the pure nuclear spin symmetry induction and subduction statistical weights, which for these reactions can be read from Tables 3 and 4 of Hugo et al. (2009). We reproduce the appropriate tables in Table A.1.
Statistical nuclear spin branching ratios for reactions and .
The numbers in the leftmost columns of Table A.1 are the frequencies of the irreducible representations A_{1}, A_{2}, and E, in the representations of the permutation group S_{3} generated by the nuclear spin functions of and . This means that the symmetry representations of H_{3} and D_{3} in S_{3} can be reduced into the following direct sums (denoted by ⊕): (A.1)(e.g., Bunker & Jensen 2006; Hugo et al. 2009). According to Mulliken’s notation used here, onedimensional representations are labeled as either A or B, twodimensional ones are labeled E, threedimensional F, fourdimensional G, etc. The total nuclear spin statistical weight of each symmetry species can be read from these decompositions by multiplying the frequency by the dimension of the representation, f(Γ_{i}) × dim(Γ_{i}). The Greek appellations, para, meta, and ortho are used to indicate these statistical weights for the simplest molecules, so that “ortho” has the highest statistical weight. The “para” (E, I = 1/2) and “ortho” (A_{1}, I = 3/2) species of have, however, equal statistical weights. has no nuclear spin functions of species A_{2}, which is antisymmetric with respect to interchange of two nuclei^{4}. H_{2} and D_{2} can have the symmetries A or B, and the single nuclei H and D have the A symmetry. The number in the bottom righthand corner of each table gives the total number of linearly independent nuclear spin functions of the molecule, (2I + 1)^{3}, where I = 1/2 for H_{3} and I = 1 for D_{3}. The branching ratios in Table A.1 are obtained by multiplying the correlation table between S_{3} and the product group S_{2} ⊗ S_{1} by appropriate frequencies. This correlation table is given by
S _{3}  S_{2} ⊗ S_{1}  
A ⊗ A  B ⊗ A  


A _{1}  1  0 
A _{2}  0  1 
The correlation table S_{3} ↔ S_{2} ⊗ S_{1} presented above is derived using the standard methods of group theory, i.e., by forming the character table of direct product group S_{2} ⊗ S_{1}, and the character table for the subduced representations of S_{3} on S_{2} ⊗ S_{1}, S_{3} ↓ S_{2} ⊗ S_{1}. The latter is obtained from that of S_{3} by stripping it from operations that are unfeasible in the direct product group S_{2} ⊗ S_{1}, i.e., the class of cyclic permutations of three nuclei, {(123),(132)}. Finally, the orthogonality relation between the characters of irreducible representations is used.
Tables A.1 can be read either from left to right (“subduction”) or top down (“induction”). For example, one can see that the A_{1} species of H_{3} and D_{3} dissociate exclusively to the A symmetry of H_{2} or D_{2}, whereas the E species dissociate to both A and B symmetries (“ortho” and “para”, respectively) of H_{2} or D_{2} with equal probability. In the reaction oD_{2} + D (A ⊗ A), the A_{1} (“meta”) and E (“ortho”) species of D_{3} are formed with the probabilities 10/18 and 8/18, respectively, whereas in the reaction pD_{2} + D (B ⊗ A), the A_{2} (“para”) and E (“ortho”) species of D_{3} are formed with the probabilities 1/9 and 8/9. These branching ratios determine relative abundances of , , and resulting from the reaction D_{2}H^{+} + NH_{2}D.
Appendix A.2: Six identical nuclei
To determine the nuclear spin branching ratios of the reactions and , one needs to determine the nuclear spin symmetry species of H_{6} and D_{6} in the permutation group S_{6}. We first calculate the characters, χ(R), of the representations generated by the nuclear spin functions of H_{6} and D_{6} under the operations R of S_{6}. Crabtree & McCall (2013) give a convenient formula for this: (A.2)where I is the nuclear spin (1/2 for H and 1 for D), n the number of identical nuclei (here 6), and x the number of transpositions or pairwise permutations, which correspond to the operation R. The number of interchanges corresponding to a cyclic permutation of k elements is k − 1, and so x = k − 1. For example, x = 2 for the ternary permutation (123). The character table of S_{6} is easily obtainable using GAP (2015). By applying the orthogonality relation of the characters of irreducible representations, we derive the following decompositions for the symmetry representations of H_{6} and D_{6}: The correlation tables S_{6} ↔ S_{3} ⊗ S_{3} and S_{6} ↔ S_{4} ⊗ S_{2} needed for the induction and subduction statistics are derived as outlined in the previous example. Finally, the branching ratio tables listed in Tables A.2−A.5 are obtained by multiplying the correlation tables by the frequencies of irreducible representations appearing in the decompositions given above. In addition, the columns of the correlation table are multiplied by the dimensions of the subduced representations in order to make the weights correspond to the total number of nuclear spin functions belonging to each representation. In the previous example, all products had onedimensional representations. The correct normalization of the weights can be checked by inspecting the last rows and columns of the tables. In these tables, species with zero frequencies are not listed.
Statistical nuclear spin branching ratios of the reaction .
Statistical nuclear spin branching ratios of the reaction .
Statistical nuclear spin branching ratios of the reaction .
Statistical nuclear spin branching ratios of the reaction .
The use of the branching ratio tables is illustrated in Figs. A.1 and A.2. Figure A.1 gives the outcome of the reaction assuming that one of the molecules is of the A_{1} (“ortho”) symmetry and the other one is E (“para”). The branching probabilities indicated next to the arrows are obtained from Tables A.2 (reading it top down) and from Table A.3 (reading it from left to right). After combining the probabilities of pathways leading to different symmetry species of , one finds that the F_{1}, A_{1}, and E species are formed in ratios 15:7:2 in this reaction. Figure A.2 describes the branching of the reaction assuming that both species are A_{1} (“meta”). The branching ratios are obtained from Tables A.4 and A.5. This reaction produces the F_{1}, A_{1}, and E species of in ratios 9:9:2.
Fig. A.1 Branching ratios of the reaction when the reactants are of the A_{1} (“ortho”) and E (“para”) symmetries. 

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Fig. A.2 Branching ratios of the reaction when both reactants are of the A_{1} (“meta”) symmetry. 

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All Tables
All Figures
Fig. 1 Spinstate ratios of NH_{3} (upper panels) and H_{2}O (lower panels) as functions of time at different densities, labeled in the upper left panel. The lefthand panels present results calculated with the (gasgrain) model of S15, while the righthand panels correspond to the present work. 

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In the text 
Fig. 2 Principal reactions determining the abundances and spin ratios of deuterated ammonia isotopologs at late stages of chemical evolution in cold, dense cores. The reactions are indicated with blue arrows. 

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In the text 
Fig. 3 Abundances of ammonia and its deuterated forms as functions of time at different densities, labeled in the upper right panel. 

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In the text 
Fig. 4 Abundance ratios of ammonia and its deuterated forms as functions of time at different densities, labeled in the lefthand panel. 

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In the text 
Fig. 5 Spinstate ratios of the deuterated forms of ammonia as functions of time at different densities, labeled in the lower left panel. 

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In the text 
Fig. 6 Spinstate ratios of the deuterated forms of the ammonium ion, as well as D_{2}H^{+} and , as functions of time at different densities, labeled in the lower left panel. 

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In the text 
Fig. 7 Upper panels: abundances of ammonia and its deuterated forms as functions of time at different temperatures, labeled in the lefthand panel. Lower panels: abundance ratios of ammonia and its deuterated forms as functions of time at different temperatures. In all panels, a constant density of n_{H} = 10^{5} cm^{3} is adopted. 

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In the text 
Fig. 8 Spinstate ratios of the deuterated forms of ammonia as functions of time at different temperatures, labeled in the lower left panel. A constant density of n_{H} = 10^{5} cm^{3} is adopted. 

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In the text 
Fig. 9 Lefthand panel: gas density (black), gas temperature (red), and dust temperature (blue) as functions of distance from the core center at different time steps (indicated in the middle panel). Middle panel: abundances of NH_{3} and NH_{2}D as functions of distance from the core center at different time steps. Righthand panel: abundances of NHD_{2} and ND_{3} as functions of distance from the core center at different time steps (same legend as in the other panels). The panels correspond to an MBES of mass 1.0 M_{⊙}. 

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In the text 
Fig. 10 Fractional abundances (with respect to n_{H}) of selected species (labeled in the plot) in a homogeneous model with n_{H} = 10^{5} cm^{3}, T = 10 K. 

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In the text 
Fig. 11 Abundance ratios of ammonia and its deuterated forms (labeled in the plot) as functions of time in a gasphase chemical model, for different initial values of the H_{2} ortho/para ratio: 3 (black lines), 10^{3} (blue), or 10^{5} (green). 

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In the text 
Fig. A.1 Branching ratios of the reaction when the reactants are of the A_{1} (“ortho”) and E (“para”) symmetries. 

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In the text 
Fig. A.2 Branching ratios of the reaction when both reactants are of the A_{1} (“meta”) symmetry. 

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In the text 
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