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Directed gas phase formation of silicon dioxide and implications for the formation of interstellar silicates

Abstract

Interstellar silicates play a key role in star formation and in the origin of solar systems, but their synthetic routes have remained largely elusive so far. Here we demonstrate in a combined crossed molecular beam and computational study that silicon dioxide (SiO2) along with silicon monoxide (SiO) can be synthesized via the reaction of the silylidyne radical (SiH) with molecular oxygen (O2) under single collision conditions. This mechanism may provide a low-temperature path—in addition to high-temperature routes to silicon oxides in circumstellar envelopes—possibly enabling the formation and growth of silicates in the interstellar medium necessary to offset the fast silicate destruction.

Introduction

The origin of interstellar silicate grains—nanoparticles consisting primarily of olivine-type ((Mg,Fe)2SiO4) refractory minerals—has remained a controversial topic for more than half a century, since interstellar silicates are faster destroyed by sputtering than formed during the late stages of stellar evolution through nucleation in circumstellar envelopes of oxygen-rich Asymptotic Giant Branch (AGB) and Red Supergiant (RSG) stars1,2,3,4,5. These nanoparticles have been associated with the prebiotic evolution of the interstellar medium (ISM) through the synthesis of molecular building blocks of life such as amino acids and sugars on their ice-coated surfaces by ionizing radiation6. Interstellar silicates also play a critical role in star formation and in the origin of solar systems contributing to the radiation balance and acting as a molecular feedstock, both through the formation of complex organics through the release of icy mantles that cover them and through disruption of grains in interstellar shocks3,7. In molecular clouds, they absorb light and hence shield complex organic molecules (COMs)—organics containing carbon, hydrogen, nitrogen, and oxygen like glycolaldehyde (HCOCH2OH) and formamide (HCONH2)—from the destructive interstellar ultraviolet radiation field8. Therefore, the elucidation of the origin of interstellar silicates is of vital importance to the astrochemistry, astrobiology, and astrophysics communities to eventually understand the fundamental processes that create a visible galaxy including our own.

A crucial point of concern is that the mass of dust ejected during the late stages of stellar evolution is produced at a rate that is significantly slower than the dust destruction time in the ISM, implying that grains also form in the lower density environment of the ISM5,9,10,11,12,13,14. Current astrochemical models of circumstellar envelopes propose that dust formation in AGB stars is driven eventually by clustering and reactions of silicon oxides along with magnesium-type and iron-type oxides2,15,16,17,18,19,20. There does appear to be, however, a severe discrepancy between the formation rates of silicate grains in circumstellar envelopes of 3 × 109 years and their destruction via sputtering once dispersed into the ISM that limits their lifetime to only a few 108 years5,21,22,23. This discrepancy24 may eventually be resolved through a better understanding of the processes of dust destruction5,23, but it remains possible that significant formation of dust needs to occur in the interstellar as opposed to the circumstellar medium12,13,14,15. Indeed, silicate grains may grow in the ISM by accreting and incorporating silicon oxide molecules25,26.

Here we show that the silicon dioxide molecule (SiO2) along with silicon monoxide (SiO) can be efficiently formed via a low-temperature gas phase chemistry even at 10 K. We report the results of a combined crossed molecular beam study and of electronic structure calculations on the reaction of the D1-silylidyne radical (SiD; X2Π) with molecular oxygen (O2, X3Σg) leading to the formation of SiO2 and SiO through a barrierless reaction27. This system represents a proxy for the reaction of the silylidyne radical (SiH) generated via photolysis of silane (SiH4)28,29,30 with O2 to synthesize silicon oxides via a single collision event. In the ISM, the reaction of SiH with O2 may represent a potential pathway to SiO2 and silicon oxide formation in those molecular clouds, where gas phase chemistry follows ice mantle sublimation; these silicon oxides might drive an exothermic chemistry that possibly produces larger silicon oxides25,31 leading ultimately to silicates at low temperatures.

Results

Crossed molecular beam studies in the laboratory frame

The reactive scattering experiments were performed using a crossed molecular beam apparatus (Methods). We monitored the scattering signal at mass-to-charge ratio (m/z) 62 (28SiDO2+), 60 (28SiO2+), and 44 (28SiO+). No signal was observed at m/z 62, suggesting that under single collision conditions the lifetime of the 28SiDO2 adduct is shorter than its flight time to the electron-impact ionizer. Reactive scattering signal was detected at m/z 60 (28SiO2+) (Fig. 1). The scattering signal is relatively weak, and at each angle up to 6 × 106 time-of-flight (TOF) spectra (60 h collection time) had to be averaged to obtain a reasonable signal-to-noise ratio. Signal detection at m/z 60 alone provides conclusive evidence on the formation of a molecule with the formula 28SiO2 via a single collision event of two neutral reactants. Taking into account the data accumulation time, the signal-to-noise ratio obtained at m/z 60 and the abundances of naturally occurring silicon isotopes of 30Si(3.10 %), 29Si (4.67 %), and 28Si(92.23 %), we would not expect—as confirmed experimentally—any reactive scattering signal at m/z 62 (30SiO2+). Finally, the background counts at m/z 44 originating from singly ionized carbon dioxide (CO2) in the detector precludes an identification of any reactive scattering signal at m/z 44 (28SiO+). To summarize, the laboratory data indicate that a molecule with the formula 28SiO2 (hereafter: SiO2) along with atomic deuterium is formed under single collision conditions in the reaction of the SiD radical with O2.

Fig. 1
figure1

Laboratory angular distribution and the associated time-of-flight spectra. Laboratory angular distribution at mass-to-charge ratio of 60 (SiO2+) recorded in the reaction of the D1-silylidyne radical with molecular oxygen (a), and the time-of-flight spectra recorded at distinct laboratory angles overlaid with the best fits (b). The solid circles with their error bars indicate the normalized experimental distribution with ±1σ uncertainty (s.d. of the integrals of the time-of-flight spectra for the respective angle), and the open circles indicate the experimental data points of the time-of-flight spectra. The red lines represent the best fits obtained from the optimized center-of-mass (CM) functions, as depicted in Fig. 2

Crossed molecular beam studies in the center-of-mass frame

We transformed the experimental data from the laboratory to the center-of-mass (CM) reference frame32 to gain information on the underlying reaction dynamics, which yields the CM translational energy flux distribution P(ET) and the CM angular flux distribution T(θ) as depicted in Fig. 2. Best fits of the laboratory data are achieved with a single-channel fit forming products with a mass combination of 60 amu (SiO2) and 2 amu (D) (Figs. 1 and 2). A detailed inspection of the CM functions affords crucial information on the pertinent reaction channel(s) and dynamics. First, P(ET) assists in the identification of the product isomer(s). For the reaction products formed without internal excitation, the high energy cutoff of 493 ± 57 kJ mol−1 in P(ET) denotes the sum of the absolute value of the reaction exothermicity plus the collision energy Ec (33.2 ± 2.0 kJ mol−1). A subtraction of the collision energy reveals that the reaction is highly exothermic with the energy of -460 ± 59 kJ mol−1. This finding agrees nicely with our computed value of -441 ± 5 kJ mol−1 (Fig. 3) and the energetics obtained from NIST Webbook (-464 kJ mol−1)33 to form the linear SiO2 molecule (l-SiO2) along with atomic hydrogen (H). This shows for the very first time that a SiO2 molecule is observed in the gas phase as a result of a reaction between two neutral species under controlled experimental conditions. Previously, Ahmed et al. generated SiO2 via laser ablation of silicon (Si) and two successive oxygen abstractions from the seeding and reactant gas—CO2;34 Wang et al. formed gas phase SiO2 through SiO2 electron photodetachment35. A complex forming reaction mechanism is evident from T(θ) which depicts the flux over the complete angular range36. This distribution reveals further a forward-backward symmetry proposing that the lifetime of the decomposing intermediate is longer than its rotational period37. Alternatively, a ‘symmetric’ reaction intermediate can account for these findings by emitting a deuterium atom with equal probabilities into θ and π–θ38.

Fig. 2
figure2

Center-of-Mass (CM) distributions and the associated flux contour map. CM translational energy flux distribution (a), CM angular flux distribution (b), and the top view of their corresponding flux contour map (c) leading to the formation of silicon dioxide plus atomic deuterium in the reaction of D1-silylidyne with molecular oxygen. Shaded areas indicate the error limits of the best fits accounting for the uncertainties of the laboratory angular distribution and TOF spectra, with the red solid lines defining the best-fit functions. The flux contour map represents the flux intensity of the reactive scattering products as a function of the CM scattering angle (θ) and product velocity (u). The color bar indicates the flux gradient from high (H) intensity to low (L) intensity. Colors of the atoms: silicon (purple), oxygen (red), and deuterium (light blue)

Fig. 3
figure3

Potential energy surface. The potential energy surface for the reaction of the silylidyne radical with molecular oxygen including reaction pathways energetically accessible in the crossed molecular beam experiments. The route in red highlights the reaction pathway leading to the formation of silicon dioxide plus atomic hydrogen. Relative energies are given in units of kJ mol−1. Note that the relative energy of silicon dioxide plus atomic deuterium is 3 kJ mol−1 higher as compared to non-deuterated reactants, whereas for the intermediates and transition states in the SiD-O2 and SiH-O2 systems, relative energies are within 1 to 2 kJ mol−1. For [i1], the spin density distribution is also shown. Colors of the atoms: silicon (purple), oxygen (red), and hydrogen (light grey)

Electronic structure calculations and reaction mechanism

We combined the experimental findings with electronic structure calculations on the reaction of SiH with O2 to elucidate the underlying dynamics (Fig. 3). These calculations were performed at a level of theory high enough to predict relative energies of the transition states and local minima as well as reaction energies within 5 kJ mol−1 (Methods). Based on the difference in zero point vibrational energies by replacing hydrogen (H) with deuterium (D) in SiH, the relative energy of SiO2 plus D is 3 kJ mol−1 higher than that of non-deuterated reactants, whereas for the intermediates and transition states in the SiD-O2 and SiH-O2 systems, which maintain the Si-H(D) bond intact, relative energies are within 1 to 2 kJ mol−1. The computations verify the experimental results of an indirect reaction mechanism. Here, the reaction is initiated by a barrierless addition of SiH with its radical center to O2 at a single oxygen atom yielding a Cs symmetric cis-HSiOO intermediate [i1] on the doublet surface. The barrierless addition was verified by a careful examination of the entrance channel, which indicates that the potential energy of the system monotonically decreases as SiH approaches O2. The collision complex [i1] is only metastable and undergoes a rapid atomic oxygen migration to the silicon atom forming the C2v symmetric HSiO2 (2B1) intermediate [i2], which is strongly bound by 538 kJ mol−1 with respect to the separated reactants. This intermediate can either undergo unimolecular decomposition via a loose exit transition state by H loss forming SiO2 (1Σg+) or isomerize via hydrogen migration to trans-HOSiO (Cs, 2A’, [i3]), which in turn undergoes trans-cis isomerization to cis-HOSiO (Cs, 2A’, [i4]). Multireference CASPT2 calculations with full active spaces (17,13) corroborate the conclusions that the reversed addition reaction of H to SiO2 is barrierless. The trans-HOSiO and cis-HOSiO intermediates are isovalent to the well-known trans-HOCO and cis-HOCO intermediates, reside in deep potential energy wells of 685 and 688 kJ mol−1, and can undergo facile Si-O bond cleavages through loose exit transition states yielding a linear van-der-Waals complex between the hydroxyl radical (OH) and SiO [i5], in which OH is hydrogen bridge bonded to the oxygen atom of SiO. This complex is bound by 23 kJ mol−1 with respect to the separated products. Overall, the computations revealed two competing exit channels: the formation of SiO2 plus H and SiO plus OH. With the exception of [i1], the aforementioned energetics are within 13 kJ mol−1 when compared with Schaefer’s study on the stationary points relevant to the reaction of SiO with OH;39 Darling and Schlegel predicted the existence of [i1], but their energetics, computed at the G2 level of theory, forecasted the energy difference between [i1] and [i4] to be about 505 kJ mol−1 compared to 549 kJ mol−1 in our system40. Finally, since our experimental setup could not probe the SiO route, the branching ratios were determined computationally exploiting Rice–Ramsperger–Kassel–Marcus (RRKM) theory (Methods). The relative yields of SiO2 and SiO were virtually independent of the collision energy between 0 and 36 kJ mol−1 and varied in the ranges of 49.5 ± 2.5 and 50.5 ± 2.5%. We should note, however, that the energy content in the intermediates [i1] to [i5] is so significant that the RRKM rate constants are close to the applicability of the statistical theory. Therefore, dynamical effects might affect the branching ratios, but a 50–50% partition is reasonable given the closeness of the reaction energies.

Discussion

Let us first address the barrierless character of the reaction of SiH with O2. The initial addition step to [i1] has no barrier because it represents an association of two species, each of them having at least one unpaired electron, in this case a radical (SiH) and a diradical (O2). During the association process two unpaired electrons from the two interacting moieties form an electron pair thus creating a new Si-O single bond. Such radical/(di)radical reactions occur without barriers. While the complex [i1] is formed, the total spin of the doublet/triplet pair is converted to a doublet due to the formation of the extra electron pair. The calculated spin density distribution in [i1] shows that the remaining unpaired electron in HSiOO is localized on the terminal oxygen atom, which exhibits a spin density of 0.91 (Fig. 3). It is interesting to note that the related reactions of Si with O2 (diradical/diradical) and singly ionized silicon (Si+) with O2 (radical/diradical) are also barrierless41,42. However, these reactions cannot produce SiO2 or singly ionized silicon dioxide (SiO2+) under single collision conditions as prevailing in the low density ISM. Here, SiO2 and SiO2+ represent highly exothermic reaction intermediates residing in deep potential wells, and their internal energy due to chemical activation has to be dissipated. The energy dissipation may occur either via deactivation through third-body collisions or via fragmentation to SiO plus O or singly ionized silicon monoxide (SiO+) plus O, respectively. Whereas third-body collisions prevent the dissociation of SiO2 when the reaction of Si with O2 takes place in a 0.37 K superfluid helium droplet43, the fragmentation channels take over at low pressures where collision deactivations are inefficient. Indeed, the reaction of Si with O2 is usually invoked as one of the main source of SiO44. Crossed molecular beam studies of this system have firmly established SiO plus O as the reaction products under nearly zero-pressure conditions45 as corroborated by theoretical quasiclassical trajectory calculations46. An alternative reaction leading to the formation of SiO2 plus O, i.e., the reaction of SiO with O2, which plays an important role in fabrication of silicon oxide films at elevated temperatures47, is known to be endothermic by 28 kJ mol−1 and has a barrier of at least 91 kJ mol−1 and hence cannot occur in low-temperature interstellar environments48.

The SiH reaction with O2 is akin to reaction of the isovalent methylidyne radical (CH) with O2, which is also known to be barrierless and consequently very fast at the collisional kinetic limit even at extremely low temperatures such as 13 K49. Theoretically, low-temperature rate coefficients for this system have been evaluated using long-range transition state theory and the calculations reproduced the experimental values within a factor of two to three50. Here we exploited the same theoretical method to compute rate coefficients for the SiH-O2 reaction and obtained values slightly increasing from 3.1×10−10 cm3 molecule-1 s-1 at 10 K to 4.4×10−10 and 5.3×10−10 cm3 molecule-1 s-1 at 100 and 300 K, respectively, compared to an experimental value of 1.7×10−10 cm3 molecule-1 s-1 at 298 K51. A comparison of the rate coefficients at 13 K for the CH-O2 (1.5×10−10 cm3 molecule-1 s-1 (experiment) and 2.9×10−10 cm3 molecule-1 s-1 (theory)) and SiH-O2 (3.2×10−10 cm3 molecule-1 s-1 (theory)) reveals that both reactions should be nearly equally fast. The calculations also demonstrate that the long-range SiH/O2 interaction is dominated by dispersion forces, with small contributions from dipole (SiH)—induced dipole (O2) and dipole (SiH)—quadrupole (O2) interactions.

Having established the formation of SiO2 along with SiO under single collision conditions in the laboratory and through electronic structure calculations, we now discuss potential astrochemical implications. It is essential to transfer these findings to ‘real’ extraterrestrial environments since all experiments conducted under well-defined laboratory conditions can hardly mimic the chemical complexity of the ISM, where both neutral–neutral and ion–molecule reactions along with photochemical processes occur simultaneously6,38,52. Our studies indicate unambiguously that the reaction has no entrance barrier, all barriers involved in the formation of the silicon oxides are well below the energy of the separated reactants, and the overall reactions to form the silicon oxides are exothermic. These findings represent a crucial prerequisite for this reaction to be important in low-temperature molecular clouds; any barrier would block these reactions in low-temperature interstellar environments. Therefore, our results can be universally applied to any cold interstellar environment such as molecular clouds, where ice mantles can be removed from grains, and where adequate concentrations of SiH radicals and O2 exist.

In cold molecular clouds, O2 is difficult to detect. This is in part due to the fact that this diatomic molecule is homopolar, and that observations are best made from space platforms such as Herschel53. The former implies that large concentrations (or column densities) are needed for detection, the latter that small telescope diameters and large beam sizes dilute the signal intensity thus making molecular oxygen difficult to detect even in sources such as hot molecular cores. Hence, the recent detection of O2 toward Orion and ρ Ophiuchi A is truly extraordinary53,54,55,56. Gas phase abundances of O2 with respect to molecular hydrogen (H2) at the order of 10−7–10−6 would be in good agreement with astronomical observations53,57, however, they are still significantly lower than the upper limit to the O2 abundance in interstellar ice. Due to its non-polar nature, upper limits to the abundance of O2 in interstellar ice are difficult but its effect on the carbon monoxide (CO) vibrational absorption band at 4.673 µm (2140 cm−1) is consistent with ice mixtures in which O2 is comparable to or a few times more abundant than CO57. Vandenbussche et al. (1999) provided upper limits58 on the O2 ice abundance based on the non-detection of its fundamental vibrational band in the solid state, at 6.45 µm (1550 cm−1), as well as on observations of the 4.673 µm (2140 cm−1) CO band. Toward the protostar R CrA IRS2, they find an upper limit of 50 % with respect to solid CO and, in NGC7538 IRS9, an upper limit of 20 % to water ice which has an estimated abundance of 10−4 with respect to H2. In general, the few sources in which observations have been carried out are consistent with upper limits to the O2 ice abundances in the range 10−5–10−4 with respect to H2. This abundance is consistent with O2 to water ratio (0.038) recently detected in comet 67 P/Churyumov–Gerasimenko59. Indeed, Taquet et al. argued that the high abundance of O2 as seen in this 67 P is of interstellar origin60. Further, we should note that the abundance of SiH depends on the removal of the ice mantles. Removal provides a parent species (silane; SiH4) to the gas phase with subsequent photodissociation producing SiH28,29,30, a molecule with a very small dipole moment of only 0.12 Debye61. Gas phase detection has therefore been difficult with only a tentative identification to date in Orion62. While multiple reaction pathways can lead to SiO2, the neutral–neutral reaction of SiH with O2 has a universal potential to synthesize SiO2 along with SiO in cold molecular clouds when the fractional abundance of O2 in the gas phase is sufficient. Both SiO2 and SiO—as derived from laboratory studies of barrier-less condensation of silicon oxides in helium droplet experiments25,43 and theoretical chemistry calculations that show reactions between these oxides produce larger silicon oxides in exothermic chemistry16,17,31—may eventually play a role in the formation and growth of interstellar silicates. It should be noted that the elementary reactions leading to small silicon oxides may also be relevant to the chemistry of silicon oxide plasmas, such as those widely used in the semiconductor industry for depositing thin film insulators in integrated circuits like memory or processor chips63. During the Si and SiO2 chemical vapor deposition (CVD) processes, primary precursors such as silane or disilane (Si2H6) undergo bond cleavage processes with the fragments adsorbing on the surfaces of the substrates, during which complex gas-phase and gas–surface reactions are involved64. Layered films of silicon oxides can be processed by mixing silane or disilane with O2 and dinitrogen monoxide (N2O), for instance65. Here depositions at low temperatures are preferred, since high-temperature instabilities on the substrates can substantially reduce the film production rates66. Plasma-enhanced CVD (PECVD) represents the main processing route for silicon oxide film growth; here, a radio frequency (RF) discharge supplies energy to initiate bond rupture processes and hence to promote the chemical reaction67,68. Since silicon hydride radical species such as SiHm and Si2Hn (m = 1–3, n = 1–5) are generated as well, PECVD is extraordinarily complex64,69. Therefore, it is vital to untangle the reaction mechanisms from the fundamental, microscopic point of view.

Our combined crossed molecular beam and electronic structure calculations provide compelling evidence on the formation of SiO2 along with SiO under single collision conditions. The bimolecular neutral–neutral reaction of SiH with O2 represents a single step mechanism to form two silicon oxides—SiO and SiO2. In combination with astrochemical modeling, our study suggests that silicon oxides may form not only in hot circumstellar envelopes of oxygen-rich stars as thought previously, but also in interstellar clouds via facile, barrierless reactions involving the simplest silicon-bearing radical (SiH) and O2. These pathways provide a population of silicon oxides, which can possibly provide a basis for the regeneration of interstellar silicates thus leading us closer to solving the paradox of the injection and destruction timescales of silicates5,21,22,23,24. The ability of barrierless, exothermic reactions between SiO and SiO2 to form larger silicon oxides such as Si2O5 and Si3O5 suggests that such reactions31 may play a central role in the process by which reformation of silicate grains must occur in the ISM.

Although there is no detailed description to date of how silicate dust grains might form in the ISM, silicon oxides are likely involved. Therefore, the work reported here represents an important step toward a systematic understanding of the fundamental chemical processes eventually leading to the formation of silicate grains in the ISM. Since distinct types of interstellar grains (silicates, carbonaceous grains, and silicon carbide) exist, the current work resembles a template for future studies of elementary chemical reactions relevant to grain formation. This requires a sophisticated link of laboratory, theoretical, and modeling study with astronomical observations, particularly for those high-density regions in circumstellar envelopes, hot molecular cores, shocked gas, including supernova remnants. Considering the crucial role of interstellar dust in star and hence solar system formation70 and in the chemical evolution of the universe, with grains providing critical molecular factories to even synthesize bio-relevant organics like amino acids and sugars7, the unraveling of the cosmic dust enigma is of fundamental importance to the understanding of our origins.

Methods

Crossed molecular beam experiments

The experiments were conducted in a crossed molecular beam machine under single-collision conditions at the University of Hawai’i at Mānoa71,72. In the primary reactant chamber, a pulsed and supersonic beam of the D1-silylidyne radical (SiD; X2Π) at fractions of about 0.5% was prepared in situ by ablation of a rotating silicon rod with the output from a Spectra-Physics Quanta-Ray Pro 270 Nd:YAG laser (30 Hz, 266 nm, 10–15 mJ pulse energies), with the ablated species further entrained by molecular deuterium (D2, 99.7%; Icon Isotopes, Inc.). The D2 gas acts as a carrier and reactant gas, and no other silicon-deuterium-bearing molecules were found to be present in the beam under the experimental conditions. Considering the natural isotope abundances of silicon, it was easier to optimize a SiD beam at m/z 31. The molecular beam entraining the SiD radicals then passed a skimmer and a chopper wheel, generating a pulsed radical beam of a well-defined peak velocity of 1981 ± 38 m s−1 and speed ratio of 5.2 ± 1.0. Notice that even if SiD radicals of A2Δ state were formed, they can decay to the ground state during the travel time of about 18 μs to the interaction region of the scattering chamber73. In the scattering chamber, this segment crossed a supersonic beam of pure oxygen gas (O2; 99.998%; Matheson) perpendicularly, which had a velocity of 778 ± 20 m s−1 and a speed ratio of 15.6 ± 1.0. This setup eventually yielded a collision energy of 33.2 ± 2.0 kJ mol−1 and a center-of-mass (CM) angle of 23.3 ± 1.2°. The reactive scattering products were ionized by an electron-impact ionizer operating at 80 eV and 2 mA emission current, before they entered a quadrupole mass spectrometer (QMS, Extrel QC 150) operating in the time-of-flight (TOF) mode. The selected ion species filtered by the QMS at a specific m/z travelled towards a stainless steel target coated with a thin layer of aluminum biased at −22.5 kV and a cascade-of-electron pulse was initiated upon impact. The electrons were then expelled from the stainless steel target and flew toward an organic scintillator to generate a photon pulse, prior to be detected by a Burle photomultiplier tube (PMT, Model 8850) operating at −1.35 kV. The signal was eventually filtered by a discriminator (Advanced Research Instruments, Model F-100TD) at a level of 1.6 mV before being fed into a Stanford Research System SR430 multichannel scaler. The whole detection region is housed in a triply, differentially pumped vacuum chamber, which can be rotated in a plane defined by the primary and secondary beams, thus we are able to record TOF spectra at discrete angles, integrate and normalize them with respect to the intensity at the CM angle, and then extract the product laboratory angular distribution at a specific m/z74. In order to obtain the information about the reaction dynamics, we employed a forward-convolution routine based on the Jacobian transformation to convert the data in the laboratory frame into the CM frame32,75. This method actually begins with a trial set of parameterized CM functions—the translational energy flux distribution, P(ET), and the angular flux distribution, T(θ), in the CM frame, to iteratively fit the laboratory TOF spectra and the angular distribution until the best fits are reached, accounting for apparatus performances, beam divergences, and velocity spreads. We can then plot a flux contour map, I(θ,u) = P(u) × T(θ), which presents the flux of the reactive scattering products as a function of the CM scattering angle (θ) and product velocity (u), and reveals information on the scattering reaction dynamics76.

Electronic structure calculations

Geometries of most of the intermediates, transition states, and bimolecular fragments were adapted from Schaefer et al.39 where they were optimized at the CCSD(T)//cc-pV(Q + d)Z level of theory. Single-point energies were computed using the explicitly correlated CCSD(T)-F12 method77 with the correlation-consistent aug-cc-pV5Z basis set;78,79 this theoretical approach closely approximates CCSD(T) energies at the complete basis set (CBS) limit and is expected to provide relative energies with an accuracy of 5 kJ mol−1. In addition to the structures considered by Schaefer et al.39, we searched for cis-HSiOO and trans-HSiOO and cyclic HSiO2 intermediates, which may represent initial complexes produced in the reaction of SiH with O2. We employed the same CCSD(T)//cc-pV(Q + d)Z method for their geometry optimization. Only the cis-HSiOO structure [i1] was located as a local minimum on the potential energy surface. A trans-HSiOO structure spontaneously converges to the HSiO2 isomer [i2] during optimization. A cyclic HSiO2 geometry optimizes to a stationary point within C2v symmetry, but shows one imaginary frequency. Once symmetry is released, the further optimization yields the open HSiO2 isomer [i2]. Next, we searched for a transition state connecting cis-HSiOO [i1] with HSiO2 [i2]. The saddle-point optimization gave a non-planar structure typical for a transition state for rotation around the Si-O bond. The transition state would normally connect two planar cis-HSiOO and trans-HSiOO minima, but since the latter spontaneously rearranges to HSiO2, this transition state is in fact between [i1] and [i2]. Furthermore, the transition state appears to be only slightly higher in energy than [i1] at the CCSD(T)//cc-pV(Q + d)Z level, and becomes lower in energy than [i1] when ZPE corrections are included. The transition state energy is below that of cis-HSiOO at our final CCSD(T)-F12/aug-cc-pV5Z + ZPE(CCSD(T)/cc-pV(Q + d)Z) level of theory. This result indicates that [i1] could be only a metastable structure on the potential energy surface, which rapidly isomerizes to HSiO2 [i2]. In this view, the entrance channel of the SiH + O2 reaction can be described as addition of O2 to the radical site on the Si atom either in cis-conformation or trans-conformation followed by spontaneous rearrangement to HSiO2 resulting in formal insertion of HSi into the O = O bond of O2. The process is driven by its very-high exothermic energy of 538 kJ mol−1. We have also carefully mapped out the potential energy surface for H loss from HSiO2 [i2] to verify that this process occurs without an exit barrier. Within C2v symmetry, the electronic state of [i2] is 2B2 but the products, SiO2 + H, correlate to the 2A1 state. Therefore, the H loss is a symmetry-forbidden process within the C2v point group. If symmetry is reduced to Cs, the two states involved are both 2A’ and hence H elimination should take place via a crossing or avoided crossing of the two 2A’ states. Therefore, we scanned the minimal energy path for the H loss from [i2] using the multireference second-order perturbation theory CASPT2 method80 with the full valence active space containing 17 electrons distributed on 13 orbitals (17,13) with the aug-cc-pVDZ basis set. The CASPT2(17,13)/aug-cc-pVDZ geometry optimizations and vibrational frequency calculations were carried out for various Si-H distances frozen at the values from 1.5 Å to 4.0 Å with a step of 0.2 Å. Following these geometry optimizations, relative energies of the MEP structures were refined by employing CASPT2(17,13) calculations with a larger aug-cc-pVTZ basis set and with mixing wave functions of the two lowest 2A’ involved in the process. The MEP has shown a steady energy decrease with the Si-H distance from [i2] to the SiO2 + H products confirming the barrierless character of the H elimination. All CCSD(T), CCSD(T)-F12, and CASPT2 calculations in this work were performed using the MOLPRO 2010 program package81. Collision-energy dependent rate constants for chemically activated unimolecular reactions on the HSiO2 surface starting from the intermediate [i2] were carried out employing RRKM theory using the in-house code82. The internal energy of each intermediate was taken as a sum of its chemical activation energy (the negative of its relative energy with respect to the SiH + O2 reactants) plus the collision energy. For reaction steps proceeding well-defined transition states, we used CCSD(T)-F12/aug-cc-pV5Z relative energies calculated here and CCSD(T)/cc-pV(Q + d)Z vibrational frequencies reported by Schaefer et al.39 For the [i2] → SiO2 + H barrierless reaction step, we employed variational transition state theory (VTST)83,84 with transition state candidate structures ranging along the MEP. Here we used vibrational frequencies of the MEP structures calculated at the CASPT2(17,13)/aug-cc-pVDZ level and their relative energies obtained at CASPT2(mix = 2,17,13)/aug-cc-pVTZ. For barrierless dissociation of the OH…OSi complex [i5] to the SiO + OH products, we also utilized the VTST approach. Here, the wave function is single-reference, the interaction has a van der Waals character, and hence the MEP was mapped out using a density functional wB97XD method85 including a dispersion correction with the aug-cc-pVTZ basis set. Single-point relative energies of the MEP structures were refined at our best CCSD(T)-F12/aug-cc-pV5Z level and were used in VTST calculations in conjunction with wB97XD/aug-cc-pVTZ frequencies. The dipole and quadrupole moments and polarizabilities of SiH and O2 required for the calculations of the capture rate coefficients using long-range transition state theory were also computed at the wB97XD/aug-cc-pVTZ level of theory. The unimolecular rate constants obtained from the RRKM and VTST calculations for collision energies in the 0–33.2 kJ mol−1 interval were used to compute the branching ratios for the formation of the SiO2 + H and SiO + OH products within the reaction scheme illustrated in Fig. 3 employing the steady-state approximation. It should be noted that because of very-high-energy content in the intermediate [i2] and relatively low activation energies required for isomerization and dissociation steps, the product branching ratios appeared to be insensitive to the collision energy within the considered range.

Data availability

The data that support the findings of the current research are available from the corresponding authors upon request.

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Acknowledgements

We thank the National Science Foundation (NSF) for support under award CHE-1360658. Astrophysics at Queen’s University Belfast is supported by a grant, ST/P000321/1, from the Science and Technology Facilities Council (UK).

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T.Y., A.M.T., and B.B.D. carried out the experimental measurements; T.Y. performed the data analysis; A.M.M. carried out the theoretical analysis; T.J.M. carried out the astronomical discussion; T.Y., R.I.K. and A.M.M. wrote the paper; and T.Y. and R.I.K. supervised the study.

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Correspondence to Ralf I. Kaiser, Alexander M. Mebel or Tom J. Millar.

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Yang, T., Thomas, A.M., Dangi, B.B. et al. Directed gas phase formation of silicon dioxide and implications for the formation of interstellar silicates. Nat Commun 9, 774 (2018). https://doi.org/10.1038/s41467-018-03172-5

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